https://vmcoolwiki.ipac.caltech.edu/api.php?action=feedcontributions&user=Sartore&feedformat=atom CoolWiki - User contributions [en] 2024-03-29T08:32:38Z User contributions MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=Identification_of_Previously_Known_Objects_on_Candidate_List&diff=7531 Identification of Previously Known Objects on Candidate List 2011-08-27T21:08:09Z <p>Sartore: </p> <hr /> <div>Friday: 08/27/2011<br /> Starting the conversation, here is what I sent out Friday about BRC 27.<br /> <br /> Each SED is unique, which should mean that there are no duplications: <br /> '''in addition''':<br /> *Candidates 15 &amp; 16 have the same rough coordinates, but show up as Ogura 8 &amp; 9<br /> <br /> *Evidently I mislabeled Ogura 21 and Ogura 22 as candidates 30 &amp; 29.<br /> *Candidate 29 is Ogura 21<br /> *Candidate 30 is identified as a YSO (Chauhan) not Ogura 22 (as I had previously noted) <br /> *Ogura 22 at 07 04 08.0 -11 23 54.75 is not on our list of candidates. (It is on the full list, but it is not one of the ones we targeted)<br /> <br /> *Candidate 31 is '''NOT''' identified as a YSO, and is not credited to anyone I have found. ''this is a change from Friday''<br /> *At this point, the only candidates that are not designated as either YSO’s or stars seem to be 12, 13, and 19.<br /> <br /> Does anybody else have an opinion on any of this?<br /> <br /> SATURDAY<br /> [[File:CandidateResearch_brc27_dcs_27Aug.xlsx]]<br /> <br /> Clarification on the referenced excel file that I sent out on Friday; <br /> <br /> Column B: Since one of our tasks was to determine which of these objects have been previously identified, I went to Harvard's site for Simbad<br /> <br /> http://vizier.cfa.harvard.edu/viz-bin/nph-aladin.pl<br /> <br /> (be sure you select the Aladin applet for the US, or it will take you to France)<br /> *npd is code for no previous designation (which is what we seem to be hunting)<br /> <br /> For each of the candidates, I looked to see if there was any kind of identification. (You will notice that so many things are labeled, it's actually surprising to find an object that does not have one) Be sure to scroll down the the bottom of the screen to see if they have actual names; many of them are labeled Ogura. <br /> <br /> If it says YSO, it was labeled as such on Simbad, which means somebody identified it at some point in the past... Query: That means we are confirming it?<br /> <br /> When I could find someone to attribute a YSO to, I credited them. (see column AA) Candidates 4, 5, 11 &amp; 28 are are not labelled on the diagram but are Ogura 3, 4, 7 &amp; 19. Since they are in the literature, I'm not sure why they are not labeled on the image. <br /> <br /> Objects that were cited as A's or B's, I took at face value (6,7, 10, 14, &amp; 27). I think I understand how 27 is a blob in IRAC, but a faint point source in JHK, but why is it brighter in its R magnitude than its V magnitude? The U &amp; B magnitudes are dimmer than the V, and I would not expect that from a B. (does that make sense?) <br /> <br /> Candidates 29, 30, &amp; 31 are still interesting. <br /> <br /> <br /> Column I: anything coded yellow is something I thought was a star before I started digging. What I based that on was whether or not we had a V magnitude farther over on the table (which just happens to also be column V). I revised those opinions based on what I found in Simbad and what is in column J.<br /> <br /> Column J: Gator DSS &amp; 2MASS/ This brought up 5 images from DSS (information at the bottom of the column) and JHK, so I was comparing the way each object looked for the different bands.<br /> <br /> Going through it one more time, some of my thoughts have changed, and so has the file, so it is posted above. <br /> <br /> Today's examination has led me to the following issues:<br /> *Is #1 really a star? <br /> <br /> *29 and 30 are actually a trio of objects (and I do not mean #31 as listed). I know that 31 has the same location as 30, but that is not where I find it in Simbad. <br /> The Simbad address is 07:04:08.13 -11:23:08.7 This is a strikingly different location, and I think we need to dig further on this. <br /> *35 is labeled as a reflection nebula. Should we ignore it?<br /> --[[User:Sartore|Sartore]] 14:08, 27 August 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=Identification_of_Previously_Known_Objects_on_Candidate_List&diff=7530 Identification of Previously Known Objects on Candidate List 2011-08-27T21:04:46Z <p>Sartore: </p> <hr /> <div>Friday: 08/27/2011<br /> Starting the conversation, here is what I sent out Friday about BRC 27.<br /> <br /> Each SED is unique, which should mean that there are no duplications: <br /> '''in addition''':<br /> *Candidates 15 &amp; 16 have the same rough coordinates, but show up as Ogura 8 &amp; 9<br /> <br /> *Evidently I mislabeled Ogura 21 and Ogura 22 as candidates 30 &amp; 29.<br /> *Candidate 29 is Ogura 21<br /> *Candidate 30 is identified as a YSO (Chauhan) not Ogura 22 (as I had previously noted) <br /> *Ogura 22 at 07 04 08.0 -11 23 54.75 is not on our list of candidates. (It is on the full list, but it is not one of the ones we targeted)<br /> <br /> *Candidate 31 is '''NOT''' identified as a YSO, and is not credited to anyone I have found. ''this is a change from Friday''<br /> *At this point, the only candidates that are not designated as either YSO’s or stars seem to be 12, 13, and 19.<br /> <br /> Does anybody else have an opinion on any of this?<br /> <br /> SATURDAY<br /> [[File:CandidateResearch_brc27_dcs_27Aug.xlsx]]<br /> <br /> Clarification on the referenced excel file that I sent out on Friday; <br /> <br /> Column B: Since one of our tasks was to determine which of these objects have been previously identified, I went to Harvard's site for Simbad<br /> <br /> http://vizier.cfa.harvard.edu/viz-bin/nph-aladin.pl<br /> <br /> (be sure you select the Aladin applet for the US, or it will take you to France)<br /> '''npd''' is code for no previous designation (which is what we seem to be hunting)<br /> For each of the candidates, I looked to see if there was any kind of identification. (You will notice that so many things are labeled, it's actually surprising to find an object that does not have one) Be sure to scroll down the the bottom of the screen to see if they have actual names; many of them are labeled Ogura. <br /> <br /> If it says YSO, it was labeled as such on Simbad, which means somebody identified it at some point in the past... Query: That means we are confirming it?<br /> <br /> When I could find someone to attribute a YSO to, I credited them. (see column AA) Candidates 4, 5, 11 &amp; 28 are are not labelled on the diagram but are Ogura 3, 4, 7 &amp; 19. Since they are in the literature, I'm not sure why they are not labeled on the image. <br /> <br /> Objects that were cited as A's or B's, I took at face value (6,7, 10, 14, &amp; 27). I think I understand how 27 is a blob in IRAC, but a faint point source in JHK, but why is it brighter in its R magnitude than its V magnitude? The U &amp; B magnitudes are dimmer than the V, and I would not expect that from a B. (does that make sense?) <br /> <br /> Candidates 29, 30, &amp; 31 are still interesting. <br /> <br /> <br /> Column I: anything coded yellow is something I thought was a star before I started digging. What I based that on was whether or not we had a V magnitude farther over on the table (which just happens to also be column V). I revised those opinions based on what I found in Simbad and what is in column J.<br /> <br /> Column J: Gator DSS &amp; 2MASS/ This brought up 5 images from DSS (information at the bottom of the column) and JHK, so I was comparing the way each object looked for the different bands.<br /> <br /> Going through it one more time, some of my thoughts have changed, and so has the file, so it is posted above. <br /> <br /> Today's examination has led me to the following issues:<br /> - Is #1 really a star? <br /> <br /> - 29 and 30 are actually a trio of objects (and I do not mean #31 as listed). I know that 31 has the same location as 30, but that is not where I find it in Simbad. <br /> The Simbad address is 07:04:08.13 -11:23:08.7 This is a strikingly different location, and I think we need to dig further on this. <br /> - 35 is labeled as a reflection nebula. Should we ignore it?<br /> <br /> --[[User:Sartore|Sartore]] 13:31, 27 August 2011 (PDT)--[[User:Sartore|Sartore]] 14:04, 27 August 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=Identification_of_Previously_Known_Objects_on_Candidate_List&diff=7529 Identification of Previously Known Objects on Candidate List 2011-08-27T20:47:01Z <p>Sartore: </p> <hr /> <div>Friday: 08/27/2011<br /> Starting the conversation, here is what I sent out Friday about BRC 27.<br /> <br /> Each SED is unique, which should mean that there are no duplications: <br /> '''in addition''':<br /> Ø Candidates 15 &amp; 16 have the same rough coordinates, but show up as Ogura 8 &amp; 9<br /> <br /> Ø Evidently I mislabeled Ogura 21 and Ogura 22 as candidates 30 &amp; 29.<br /> o Candidate 29 is Ogura 21<br /> o Candidate 30 is identified as a YSO (Chauhan) not Ogura 22 (as I had previously noted) <br /> o Ogura 22 at 07 04 08.0 -11 23 54.75 is not on our list of candidates. (It is on the full list, but it is not one of the ones we targeted)<br /> <br /> Ø Candidate 31 is '''NOT''' identified as a YSO, and is not credited to anyone I have found. ''this is a change from Friday''<br /> Ø At this point, the only candidates that are not designated as either YSO’s or stars seem to be 12, 13, and 19.<br /> <br /> Does anybody else have an opinion on any of this?<br /> <br /> SATURDAY<br /> [[File:CandidateResearch_brc27_dcs_27Aug.xlsx]]<br /> <br /> Clarification on the referenced excel file that I sent out; <br /> <br /> Column B: Since one of our tasks was to determine which of these objects have been previously identified, I went to Harvard's site for Simbad<br /> <br /> http://vizier.cfa.harvard.edu/viz-bin/nph-aladin.pl<br /> <br /> (be sure you select the Aladin applet for the US, or it will take you to France)<br /> <br /> For each of the candidates, I looked to see if there was any kind of identification. (You will notice that so many things are labeled, it's actually surprising to find an object that does not have a one) Be sure to scroll down the the bottom of the screen to see if they have actual names; many of them are labeled Ogura. <br /> <br /> If it says YSO, it was labeled as such on Simbad , which means somebody identified it at some point in the past... Query: That means we are confirming it?<br /> <br /> When I could find someone to attribute a YSO to, I credited them. (see column AA) Candidates 4, 5, 11 &amp; 28 are are not labelled on the diagram but are Ogura 3, 4, 7 &amp; 19. Since they are in the literature, I'm not sure why they are not labeled image. <br /> <br /> Objects that were cited as A's or B's, I took at face value (6,7, 10, 14, &amp; 27). I think I understand how 27 is a blob in IRAC, but a faint point source in JHK, but why is it brighter in its R magnitude than its V magnitude? The U &amp; B magnitudes are dimmer than the V, and I would not expect that from a B. (does that make sense?) <br /> <br /> Candidates 29, 30, &amp; 31 are still interesting. <br /> <br /> <br /> Column I: anything coded yellow is something I thought was a star before I started digging. What I based that on was whether or not we had a V magnitude farther over on the table (which just happens to also be column V). I revised those opinions based on what I found in Simbad and what is in column J.<br /> <br /> Column J: Gator DSS &amp; 2MASS/ This brought up 5 images from DSS (information at the bottom of the column) and JHK, so I was comparing the way each object looked for the different bands.<br /> <br /> Going through it one more time, some of my thoughts have changed, and so has the file. I'll post it to the wiki (if I can). <br /> <br /> Is #1 really a star? <br /> --[[User:Sartore|Sartore]] 13:31, 27 August 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=Identification_of_Previously_Known_Objects_on_Candidate_List&diff=7528 Identification of Previously Known Objects on Candidate List 2011-08-27T20:31:02Z <p>Sartore: Created page with 'File:CandidateResearch_brc27_dcs_27Aug.xlsx Clarification on the referenced excel file that I sent out; Column B: Since one of our tasks was to determine which of these o…'</p> <hr /> <div>[[File:CandidateResearch_brc27_dcs_27Aug.xlsx]]<br /> <br /> Clarification on the referenced excel file that I sent out; <br /> <br /> Column B: Since one of our tasks was to determine which of these objects have been previously identified, I went to Harvard's site for Simbad<br /> <br /> http://vizier.cfa.harvard.edu/viz-bin/nph-aladin.pl<br /> <br /> (be sure you select the Aladin applet for the US, or it will take you to France)<br /> <br /> For each of the candidates, I looked to see if there was any kind of identification. (You will notice that so many things are labeled, it's actually surprising to find an object that does not have a one) Be sure to scroll down the the bottom of the screen to see if they have actual names; many of them are labeled Ogura. <br /> <br /> If it says YSO, it was labeled as such on Simbad , which means somebody identified it at some point in the past... Query: That means we are confirming it?<br /> <br /> When I could find someone to attribute a YSO to, I credited them. (see column AA) Candidates 4, 5, 11 &amp; 28 are are not labelled on the diagram but are Ogura 3, 4, 7 &amp; 19. Since they are in the literature, I'm not sure why they are not labeled image. <br /> <br /> Objects that were cited as A's or B's, I took at face value (6,7, 10, 14, &amp; 27). I think I understand how 27 is a blob in IRAC, but a faint point source in JHK, but why is it brighter in its R magnitude than its V magnitude? The U &amp; B magnitudes are dimmer than the V, and I would not expect that from a B. (does that make sense?) <br /> <br /> Candidates 29, 30, &amp; 31 are still interesting. <br /> <br /> <br /> Column I: anything coded yellow is something I thought was a star before I started digging. What I based that on was whether or not we had a V magnitude farther over on the table (which just happens to also be column V). I revised those opinions based on what I found in Simbad and what is in column J.<br /> <br /> Column J: Gator DSS &amp; 2MASS/ This brought up 5 images from DSS (information at the bottom of the column) and JHK, so I was comparing the way each object looked for the different bands.<br /> <br /> Going through it one more time, some of my thoughts have changed, and so has the file. I'll post it to the wiki (if I can). <br /> <br /> Is #1 really a star? <br /> --[[User:Sartore|Sartore]] 13:31, 27 August 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:CandidateResearch_brc27_dcs_27Aug.xlsx&diff=7527 File:CandidateResearch brc27 dcs 27Aug.xlsx 2011-08-27T20:26:31Z <p>Sartore: 2nd iteration of candidate identities</p> <hr /> <div>2nd iteration of candidate identities</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Fall_work&diff=7526 BRC Fall work 2011-08-27T20:15:42Z <p>Sartore: </p> <hr /> <div>=[[Marcella's July List of Things To Do]]=<br /> <br /> =[[BRC Optical Ground-Based Follow-Up]]=<br /> <br /> =[[Identification of Previously Known Objects on Candidate List]]=</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=7349 BRC Spring work 2011-06-29T15:17:37Z <p>Sartore: /* Literature known YSOs */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information. Here's the bibliography from our proposal (with my comments) --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> {| border=&quot;1&quot;<br /> |'''paper'''<br /> |'''Chelen's notes'''<br /> |'''Luisa's notes'''<br /> |'''presenter/ present with'''<br /> |-<br /> |Guieu, S., et al., [http://adsabs.harvard.edu/abs/2010ApJ...720...46G 2010, ApJ, 720, 46] ([http://web.ipac.caltech.edu/staff/rebull/working/ic2118.pdf pdf])<br /> |<br /> | the 2118 paper (from my first teacher team).... because our work will look a lot like this<br /> | &lt;font color=&quot;red&quot;&gt;3/30, BY MARCELLA&lt;/font&gt;<br /> |-<br /> |Ogura K., Sugitani K., Pickles A., [http://adsabs.harvard.edu/abs/2002AJ....123.2597O 2002, AJ, 123, 2597.] <br /> |''Optical + 2MASS; contains general info of BRCs''<br /> | Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. Need to be sure that this catalog is included in our list of previously known YSOs in this region, compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one. Maybe not the other Sugitanis, but if we do discuss the other Sugitanis (&quot;Group S&quot;) then they should be combined here.<br /> |do this, possibly with rest of group S &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/20 BY DIANE&lt;/font&gt;<br /> |-<br /> |Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] <br /> |'''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> |the original SFO, origin of &quot;BRC&quot; terminology, numbers 1-44. covers the northern hemisphere. has nice intro/summary of what's going on in BRCs, CGs, etc. Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1991'''<br /> |-<br /> |Sugitani K., Ogura K., [http://adsabs.harvard.edu/abs/1994ApJS...92..163S 1994, ApJS, 92, 163.] <br /> |''another survey''<br /> |SFO/BRC catalog/nomenclature continued into the southern hemisphere. (NB: all our obj are in the N. Hem paper!). SFO/BRC numbers 45-89. Second in the Sugitani series. Again, much of detailed analysis now obsolete. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1994'''<br /> |-<br /> |Sugitani K., Tamura M., Ogura K., [http://adsabs.harvard.edu/abs/1995ApJ...455L..39S 1995, ApJ, 455, L39.] <br /> |''IRAS survey'' <br /> | JHK follow-up of IRAS sources from SFO. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Shame on them for not publishing a data table or even a figure with the locations of everything they identify as a YSO! BRC 27 is one that they choose to include in a finder chart, but doesn't do us much good. Nice summary of larger issues, timescales. Short paper. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1995'''<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., [http://adsabs.harvard.edu/abs/2004A%26A...426..535M 2004, A&amp;A, 426, 535.] note has erratum too.<br /> |''Radio and mid-ir survey''<br /> | NRAO/NVSS/VLA (20cm), DSS, MSX data. both 27 and 34 in here, though 34 is a non-det. nice intro to the physics, though they get into far more math than we need to. relevant issues: this radio is thermal (free-free emission). they smoothed data -- spatial resolution (see [[Resolution]]). another nice use of three big surveys. sfo 27 in the online-only fig 1. T3 also online only. identifying ionizing source is not the same as identifying point sources in the images themselves. it's not clear that this is all that relevant for us. part of a PhD thesis.<br /> |Drop? if do, do with &quot;Group M&quot; but skip the math. '''2004''' &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/27 BY CHELEN&lt;/font&gt;<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., [http://adsabs.harvard.edu/abs/2008A%26A...477..557M 2008, A&amp;A, 477, 557.] <br /> |''SCUBA survey''<br /> |SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see [[Resolution]] and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.<br /> |Probably the most worth doing of &quot;Group M&quot;; skip the math. '''2008'''<br /> |-<br /> |Morgan L. K., Urquhart J. S., Thompson M. A., [http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M 2009, MNRAS, 400, 1726.] <br /> |''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> | JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see [[Resolution]] and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.<br /> |Do with &quot;Group M&quot; for fig 2. '''2009'''<br /> |-<br /> |Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C 2009, MNRAS, 396, 964]. <br /> |''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> | BRC27. Optical (BVIc)+2mass+spitzer/irac. yes, this one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. references 'group M' papers, so do this one after those, and right before CG4 for contrast in methods. nice intro. multiwavelength and contaminants (see [[Finding cluster members]]). As I read this, they are using optical+nir to pick their YSOs, not Spitzer-driven. Whoever is presenting this needs to assess this in detail. We ''will'' find a different set of obj, not just classify them differently. Note lots of information is online only, which i attached to article pdf. analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!<br /> |do second to last. read closely! compare to everything above. &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/11 BY JOHN&lt;/font&gt;<br /> |-<br /> |Rebull, L., et al., 2011, AJ, in press (CG4 paper)<br /> | do as last review before we get started on ours?<br /> | this is very close to our analysis, though we may not have any optical at all.<br /> | discuss last, since methodology very similar? &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/18 BY MARK&lt;/font&gt; Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper &quot;New Young Star Candidates in CG4 and Sa101&quot;, Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]]<br /> |-<br /> |<br /> |<br /> |this line separates the &quot;should dos&quot; from the &quot;maybe skips&quot;<br /> |-<br /> |Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., [http://adsabs.harvard.edu/abs/2009A%26A...506..711G 2009, A&amp;A, 2009, 506, 711.] <br /> |''X-ray survey of CMa region''<br /> |BRC 27. ROSAT+VRI data. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Mentions Chandra, XMM data, both of which would cover BRC 27, but I can't find the subsequent analysis that they advertise. We need to include this catalog in what we accumulate, and compare our results to theirs. Not clear if we need to actually discuss it or not.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., [http://adsabs.harvard.edu/abs/1999MNRAS.310..210S 1999, MNRAS, 310, 210.] <br /> |''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> |BRC 27 only. optical. age, distance estimate. photo'''electric''' UBVR(!) and objective prism spectroscopy for Halpha and spectral types. combined with IRAS. using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Not clear if we need to actually discuss it or not. It's old methodology (from an Uzbecki telescope), but good stuff, especially the spectral types. nice &quot;put-it-in-context&quot; discussion at the top for the entire CMa R1 region. <br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., [http://adsabs.harvard.edu/abs/1986PASJ...38..395W 1986, PASJ, 38, 395.]<br /> |''Optical survey of CMa region''<br /> |BRC 27. Halpha plus photo'''graphic''' UBV.(!) using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they say they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Nice cross matching that they've already done for ''their'' previously identified objects. Not clear if we need to actually discuss it or not. It's a really old paper.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2002A%26A...388..172S 2002, A&amp;A, 388, 172.] <br /> |''2MASS obs of BRC 27''<br /> |BRC 27. 2MASS. Editing ghastly. Really simple paper. In theory, we should include their results in what we accumulate, and compare our results, though (a) they are using &quot;prehistoric&quot; 2mass data reduction, and (b) they really make it hard, as they don't even tell us how many YSOs they think they've found, just the numbers of objects for which they've done photometry. So I don't think we really can compare our results to this one. However, nice &quot;put it in larger context&quot; discussion with wide-field IRAS image. <br /> |skip it unless you want to see the IRAS image.<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2003A%26A...404..217S 2003, A&amp;A, 404, 217.] <br /> |''2MASS + optical survey''<br /> | Simple paper elsewhere in the same cloud as BRC 27. Same sort of 2MASS analysis as their 2002 paper. Still archaic 2MASS data reduction. Skip it.<br /> | skip it.<br /> |-<br /> |Valdettaro R., Palla F., Brand J., Cesaroni R., [http://adsabs.harvard.edu/abs/2005A%26A...443..535V 2005, A&amp;A, 443, 535.] <br /> |''Radio survey of water masers''<br /> |22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. Nice to at least scan after the Morgan stuff for context. larger issues: spatial resolution (see [[Resolution]]). Again!! :)<br /> |maybe skip?<br /> |-<br /> |Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., [http://adsabs.harvard.edu/abs/2008ApJ...675.1352V 2008, ApJ, 675, 1352.] <br /> |''VLA obs of water masers; BRC 34''<br /> |more water masers, following up 2005 work. BRC 34 observed, not detected. nice intro that puts their work in context with the rest of what they've done. Lots more non-dets, interpreted as forming low mass and/or older stars than had been assumed. I think they've gotten the interpretation spot-on. <br /> |maybe skip?<br /> |-<br /> |Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. <br /> |Poster from AAS ... good to review?<br /> |ok, but not a lot of content beyond the images and their 'big picture' work.<br /> |skip?<br /> |-<br /> |Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. <br /> |''MOPEX info'' <br /> |VERY technical, not a manual, and not all that terribly relevant to what we're doing. let's drop this one from the list. <br /> |(drop)<br /> |-<br /> |}<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read. --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)<br /> <br /> =Literature known YSOs=<br /> <br /> In the end, we need a master file (text or xls) that has one line per object and all of the information (photometric plus any Ha measurements (usually in equivalent width)) we can gather on that object (along with the origin of that information). Papers in the literature might have rediscovered the same objects themselves, and we will certainly rediscover some of them ourselves. We need to be able to identify them as known objects when we find them.<br /> <br /> We need to scavenge the papers for names, coordinates, and photometry, and then go update the coordinates using 2MASS. [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video on how to do this using the 2MASS archive]. Guidelines: <br /> *(a) watch the units of the coordinates (J2000 or B1950); <br /> *(b) take the closest bright 2MASS source. As in, there should only be one 2MASS source near the target. If there is more than one, take the brighter one. <br /> *(c) Make a note of the 2MASS name as well, but you don't have to write down all the JHK measurements too; I have automatically grabbed those and matched them to the Spitzer catalog. We're trying to get the updated coordinates so that I can automatically merge the old information with our new catalog. <br /> *(d) Do only BRC 27 and 34. Don't do the rest! <br /> *(e) More than one person (at least 2!) should independently work on each of these tables, because transcription errors are ''really'' easy to make.<br /> *(f) During the time in which we are working on this, we can either keep one big master list with everything (which is what we will have in the end), or we can keep tables separately for each paper. If the individual tables have updated good coordinates, then we can have the computer merge them. But, this may mean that you look up the same objects more than once, since the same objects probably appear in more than one paper.<br /> *(note: what do i mean by 'machine readable'? i mean a plain text file that the computer can read in and parse and understand coordinates, etc. PDF is not enough. plain text is what i need.)<br /> <br /> The papers (links above), in order of priority:<br /> *Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- and see also [[file:table5-edited.txt]], which is the file i sent in which i was starting this process with their table 5. (this is what i was using in the youtube video above.) [[file:ogura-table5-diane.txt]] -- diane's version of the coordinates for both BRCs from table 5 (23 June)<br /> *Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- coordinates ok, just get a machine-readable version of the table so that we can make a note of the photometry. FROM LUISA 23 June: [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. 'missing' data in the pdf version are also mising here. just brc27 (that's all we care about).''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. -- coordinates are ok. just get machine-readable version of the main source table so that we can include the information from here. [[file:gregoriohetem-tablea1.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. annoying notes at bottom moved to last column. two-part table combined into one.''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:shev-diane.txt]] (june 26)<br /> [[file:shevchenko stellar.txt]] --[[User:Sartore|Sartore]] 08:26, 28 June 2011 (PDT)<br /> *Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. This was a listing of emission line stars in CMa, and only two of the emission line stars previously listed actually fall into the area assigned to BRC 27. The other entries are generally very close to the boundary in one dimension (or both), so I pulled them out of the original listing. [[file:Wira_separated.txt]]--[[User:Sartore|Sartore]] 08:17, 29 June 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Wira_separated.txt&diff=7348 File:Wira separated.txt 2011-06-29T15:16:18Z <p>Sartore: uploaded a new version of &quot;File:Wira separated.txt&quot;</p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=7347 BRC Spring work 2011-06-29T15:13:58Z <p>Sartore: /* Literature known YSOs */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information. Here's the bibliography from our proposal (with my comments) --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> {| border=&quot;1&quot;<br /> |'''paper'''<br /> |'''Chelen's notes'''<br /> |'''Luisa's notes'''<br /> |'''presenter/ present with'''<br /> |-<br /> |Guieu, S., et al., [http://adsabs.harvard.edu/abs/2010ApJ...720...46G 2010, ApJ, 720, 46] ([http://web.ipac.caltech.edu/staff/rebull/working/ic2118.pdf pdf])<br /> |<br /> | the 2118 paper (from my first teacher team).... because our work will look a lot like this<br /> | &lt;font color=&quot;red&quot;&gt;3/30, BY MARCELLA&lt;/font&gt;<br /> |-<br /> |Ogura K., Sugitani K., Pickles A., [http://adsabs.harvard.edu/abs/2002AJ....123.2597O 2002, AJ, 123, 2597.] <br /> |''Optical + 2MASS; contains general info of BRCs''<br /> | Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. Need to be sure that this catalog is included in our list of previously known YSOs in this region, compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one. Maybe not the other Sugitanis, but if we do discuss the other Sugitanis (&quot;Group S&quot;) then they should be combined here.<br /> |do this, possibly with rest of group S &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/20 BY DIANE&lt;/font&gt;<br /> |-<br /> |Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] <br /> |'''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> |the original SFO, origin of &quot;BRC&quot; terminology, numbers 1-44. covers the northern hemisphere. has nice intro/summary of what's going on in BRCs, CGs, etc. Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1991'''<br /> |-<br /> |Sugitani K., Ogura K., [http://adsabs.harvard.edu/abs/1994ApJS...92..163S 1994, ApJS, 92, 163.] <br /> |''another survey''<br /> |SFO/BRC catalog/nomenclature continued into the southern hemisphere. (NB: all our obj are in the N. Hem paper!). SFO/BRC numbers 45-89. Second in the Sugitani series. Again, much of detailed analysis now obsolete. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1994'''<br /> |-<br /> |Sugitani K., Tamura M., Ogura K., [http://adsabs.harvard.edu/abs/1995ApJ...455L..39S 1995, ApJ, 455, L39.] <br /> |''IRAS survey'' <br /> | JHK follow-up of IRAS sources from SFO. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Shame on them for not publishing a data table or even a figure with the locations of everything they identify as a YSO! BRC 27 is one that they choose to include in a finder chart, but doesn't do us much good. Nice summary of larger issues, timescales. Short paper. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1995'''<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., [http://adsabs.harvard.edu/abs/2004A%26A...426..535M 2004, A&amp;A, 426, 535.] note has erratum too.<br /> |''Radio and mid-ir survey''<br /> | NRAO/NVSS/VLA (20cm), DSS, MSX data. both 27 and 34 in here, though 34 is a non-det. nice intro to the physics, though they get into far more math than we need to. relevant issues: this radio is thermal (free-free emission). they smoothed data -- spatial resolution (see [[Resolution]]). another nice use of three big surveys. sfo 27 in the online-only fig 1. T3 also online only. identifying ionizing source is not the same as identifying point sources in the images themselves. it's not clear that this is all that relevant for us. part of a PhD thesis.<br /> |Drop? if do, do with &quot;Group M&quot; but skip the math. '''2004''' &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/27 BY CHELEN&lt;/font&gt;<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., [http://adsabs.harvard.edu/abs/2008A%26A...477..557M 2008, A&amp;A, 477, 557.] <br /> |''SCUBA survey''<br /> |SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see [[Resolution]] and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.<br /> |Probably the most worth doing of &quot;Group M&quot;; skip the math. '''2008'''<br /> |-<br /> |Morgan L. K., Urquhart J. S., Thompson M. A., [http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M 2009, MNRAS, 400, 1726.] <br /> |''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> | JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see [[Resolution]] and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.<br /> |Do with &quot;Group M&quot; for fig 2. '''2009'''<br /> |-<br /> |Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C 2009, MNRAS, 396, 964]. <br /> |''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> | BRC27. Optical (BVIc)+2mass+spitzer/irac. yes, this one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. references 'group M' papers, so do this one after those, and right before CG4 for contrast in methods. nice intro. multiwavelength and contaminants (see [[Finding cluster members]]). As I read this, they are using optical+nir to pick their YSOs, not Spitzer-driven. Whoever is presenting this needs to assess this in detail. We ''will'' find a different set of obj, not just classify them differently. Note lots of information is online only, which i attached to article pdf. analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!<br /> |do second to last. read closely! compare to everything above. &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/11 BY JOHN&lt;/font&gt;<br /> |-<br /> |Rebull, L., et al., 2011, AJ, in press (CG4 paper)<br /> | do as last review before we get started on ours?<br /> | this is very close to our analysis, though we may not have any optical at all.<br /> | discuss last, since methodology very similar? &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/18 BY MARK&lt;/font&gt; Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper &quot;New Young Star Candidates in CG4 and Sa101&quot;, Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]]<br /> |-<br /> |<br /> |<br /> |this line separates the &quot;should dos&quot; from the &quot;maybe skips&quot;<br /> |-<br /> |Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., [http://adsabs.harvard.edu/abs/2009A%26A...506..711G 2009, A&amp;A, 2009, 506, 711.] <br /> |''X-ray survey of CMa region''<br /> |BRC 27. ROSAT+VRI data. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Mentions Chandra, XMM data, both of which would cover BRC 27, but I can't find the subsequent analysis that they advertise. We need to include this catalog in what we accumulate, and compare our results to theirs. Not clear if we need to actually discuss it or not.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., [http://adsabs.harvard.edu/abs/1999MNRAS.310..210S 1999, MNRAS, 310, 210.] <br /> |''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> |BRC 27 only. optical. age, distance estimate. photo'''electric''' UBVR(!) and objective prism spectroscopy for Halpha and spectral types. combined with IRAS. using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Not clear if we need to actually discuss it or not. It's old methodology (from an Uzbecki telescope), but good stuff, especially the spectral types. nice &quot;put-it-in-context&quot; discussion at the top for the entire CMa R1 region. <br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., [http://adsabs.harvard.edu/abs/1986PASJ...38..395W 1986, PASJ, 38, 395.]<br /> |''Optical survey of CMa region''<br /> |BRC 27. Halpha plus photo'''graphic''' UBV.(!) using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they say they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Nice cross matching that they've already done for ''their'' previously identified objects. Not clear if we need to actually discuss it or not. It's a really old paper.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2002A%26A...388..172S 2002, A&amp;A, 388, 172.] <br /> |''2MASS obs of BRC 27''<br /> |BRC 27. 2MASS. Editing ghastly. Really simple paper. In theory, we should include their results in what we accumulate, and compare our results, though (a) they are using &quot;prehistoric&quot; 2mass data reduction, and (b) they really make it hard, as they don't even tell us how many YSOs they think they've found, just the numbers of objects for which they've done photometry. So I don't think we really can compare our results to this one. However, nice &quot;put it in larger context&quot; discussion with wide-field IRAS image. <br /> |skip it unless you want to see the IRAS image.<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2003A%26A...404..217S 2003, A&amp;A, 404, 217.] <br /> |''2MASS + optical survey''<br /> | Simple paper elsewhere in the same cloud as BRC 27. Same sort of 2MASS analysis as their 2002 paper. Still archaic 2MASS data reduction. Skip it.<br /> | skip it.<br /> |-<br /> |Valdettaro R., Palla F., Brand J., Cesaroni R., [http://adsabs.harvard.edu/abs/2005A%26A...443..535V 2005, A&amp;A, 443, 535.] <br /> |''Radio survey of water masers''<br /> |22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. Nice to at least scan after the Morgan stuff for context. larger issues: spatial resolution (see [[Resolution]]). Again!! :)<br /> |maybe skip?<br /> |-<br /> |Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., [http://adsabs.harvard.edu/abs/2008ApJ...675.1352V 2008, ApJ, 675, 1352.] <br /> |''VLA obs of water masers; BRC 34''<br /> |more water masers, following up 2005 work. BRC 34 observed, not detected. nice intro that puts their work in context with the rest of what they've done. Lots more non-dets, interpreted as forming low mass and/or older stars than had been assumed. I think they've gotten the interpretation spot-on. <br /> |maybe skip?<br /> |-<br /> |Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. <br /> |Poster from AAS ... good to review?<br /> |ok, but not a lot of content beyond the images and their 'big picture' work.<br /> |skip?<br /> |-<br /> |Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. <br /> |''MOPEX info'' <br /> |VERY technical, not a manual, and not all that terribly relevant to what we're doing. let's drop this one from the list. <br /> |(drop)<br /> |-<br /> |}<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read. --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)<br /> <br /> =Literature known YSOs=<br /> <br /> In the end, we need a master file (text or xls) that has one line per object and all of the information (photometric plus any Ha measurements (usually in equivalent width)) we can gather on that object (along with the origin of that information). Papers in the literature might have rediscovered the same objects themselves, and we will certainly rediscover some of them ourselves. We need to be able to identify them as known objects when we find them.<br /> <br /> We need to scavenge the papers for names, coordinates, and photometry, and then go update the coordinates using 2MASS. [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video on how to do this using the 2MASS archive]. Guidelines: <br /> *(a) watch the units of the coordinates (J2000 or B1950); <br /> *(b) take the closest bright 2MASS source. As in, there should only be one 2MASS source near the target. If there is more than one, take the brighter one. <br /> *(c) Make a note of the 2MASS name as well, but you don't have to write down all the JHK measurements too; I have automatically grabbed those and matched them to the Spitzer catalog. We're trying to get the updated coordinates so that I can automatically merge the old information with our new catalog. <br /> *(d) Do only BRC 27 and 34. Don't do the rest! <br /> *(e) More than one person (at least 2!) should independently work on each of these tables, because transcription errors are ''really'' easy to make.<br /> *(f) During the time in which we are working on this, we can either keep one big master list with everything (which is what we will have in the end), or we can keep tables separately for each paper. If the individual tables have updated good coordinates, then we can have the computer merge them. But, this may mean that you look up the same objects more than once, since the same objects probably appear in more than one paper.<br /> *(note: what do i mean by 'machine readable'? i mean a plain text file that the computer can read in and parse and understand coordinates, etc. PDF is not enough. plain text is what i need.)<br /> <br /> The papers (links above), in order of priority:<br /> *Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- and see also [[file:table5-edited.txt]], which is the file i sent in which i was starting this process with their table 5. (this is what i was using in the youtube video above.) [[file:ogura-table5-diane.txt]] -- diane's version of the coordinates for both BRCs from table 5 (23 June)<br /> *Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- coordinates ok, just get a machine-readable version of the table so that we can make a note of the photometry. FROM LUISA 23 June: [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. 'missing' data in the pdf version are also mising here. just brc27 (that's all we care about).''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. -- coordinates are ok. just get machine-readable version of the main source table so that we can include the information from here. [[file:gregoriohetem-tablea1.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. annoying notes at bottom moved to last column. two-part table combined into one.''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:shev-diane.txt]] (june 26)<br /> [[file:shevchenko stellar.txt]] --[[User:Sartore|Sartore]] 08:26, 28 June 2011 (PDT)<br /> *Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. This was a listing of emission line stars in CMa, and only two of the emission line stars previously listed actually fall into the area assigned to BRC 27. The other entries are generally very close to the boundary in one dimension (or both), so I pulled them out of the original listing. [[file:Wira_separated]]--[[User:Sartore|Sartore]] 08:13, 29 June 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Wira_separated.txt&diff=7346 File:Wira separated.txt 2011-06-29T15:12:58Z <p>Sartore: uploaded a new version of &quot;File:Wira separated.txt&quot;</p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=7345 BRC Spring work 2011-06-29T15:04:42Z <p>Sartore: /* Literature known YSOs */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information. Here's the bibliography from our proposal (with my comments) --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> {| border=&quot;1&quot;<br /> |'''paper'''<br /> |'''Chelen's notes'''<br /> |'''Luisa's notes'''<br /> |'''presenter/ present with'''<br /> |-<br /> |Guieu, S., et al., [http://adsabs.harvard.edu/abs/2010ApJ...720...46G 2010, ApJ, 720, 46] ([http://web.ipac.caltech.edu/staff/rebull/working/ic2118.pdf pdf])<br /> |<br /> | the 2118 paper (from my first teacher team).... because our work will look a lot like this<br /> | &lt;font color=&quot;red&quot;&gt;3/30, BY MARCELLA&lt;/font&gt;<br /> |-<br /> |Ogura K., Sugitani K., Pickles A., [http://adsabs.harvard.edu/abs/2002AJ....123.2597O 2002, AJ, 123, 2597.] <br /> |''Optical + 2MASS; contains general info of BRCs''<br /> | Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. Need to be sure that this catalog is included in our list of previously known YSOs in this region, compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one. Maybe not the other Sugitanis, but if we do discuss the other Sugitanis (&quot;Group S&quot;) then they should be combined here.<br /> |do this, possibly with rest of group S &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/20 BY DIANE&lt;/font&gt;<br /> |-<br /> |Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] <br /> |'''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> |the original SFO, origin of &quot;BRC&quot; terminology, numbers 1-44. covers the northern hemisphere. has nice intro/summary of what's going on in BRCs, CGs, etc. Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1991'''<br /> |-<br /> |Sugitani K., Ogura K., [http://adsabs.harvard.edu/abs/1994ApJS...92..163S 1994, ApJS, 92, 163.] <br /> |''another survey''<br /> |SFO/BRC catalog/nomenclature continued into the southern hemisphere. (NB: all our obj are in the N. Hem paper!). SFO/BRC numbers 45-89. Second in the Sugitani series. Again, much of detailed analysis now obsolete. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1994'''<br /> |-<br /> |Sugitani K., Tamura M., Ogura K., [http://adsabs.harvard.edu/abs/1995ApJ...455L..39S 1995, ApJ, 455, L39.] <br /> |''IRAS survey'' <br /> | JHK follow-up of IRAS sources from SFO. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Shame on them for not publishing a data table or even a figure with the locations of everything they identify as a YSO! BRC 27 is one that they choose to include in a finder chart, but doesn't do us much good. Nice summary of larger issues, timescales. Short paper. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1995'''<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., [http://adsabs.harvard.edu/abs/2004A%26A...426..535M 2004, A&amp;A, 426, 535.] note has erratum too.<br /> |''Radio and mid-ir survey''<br /> | NRAO/NVSS/VLA (20cm), DSS, MSX data. both 27 and 34 in here, though 34 is a non-det. nice intro to the physics, though they get into far more math than we need to. relevant issues: this radio is thermal (free-free emission). they smoothed data -- spatial resolution (see [[Resolution]]). another nice use of three big surveys. sfo 27 in the online-only fig 1. T3 also online only. identifying ionizing source is not the same as identifying point sources in the images themselves. it's not clear that this is all that relevant for us. part of a PhD thesis.<br /> |Drop? if do, do with &quot;Group M&quot; but skip the math. '''2004''' &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/27 BY CHELEN&lt;/font&gt;<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., [http://adsabs.harvard.edu/abs/2008A%26A...477..557M 2008, A&amp;A, 477, 557.] <br /> |''SCUBA survey''<br /> |SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see [[Resolution]] and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.<br /> |Probably the most worth doing of &quot;Group M&quot;; skip the math. '''2008'''<br /> |-<br /> |Morgan L. K., Urquhart J. S., Thompson M. A., [http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M 2009, MNRAS, 400, 1726.] <br /> |''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> | JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see [[Resolution]] and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.<br /> |Do with &quot;Group M&quot; for fig 2. '''2009'''<br /> |-<br /> |Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C 2009, MNRAS, 396, 964]. <br /> |''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> | BRC27. Optical (BVIc)+2mass+spitzer/irac. yes, this one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. references 'group M' papers, so do this one after those, and right before CG4 for contrast in methods. nice intro. multiwavelength and contaminants (see [[Finding cluster members]]). As I read this, they are using optical+nir to pick their YSOs, not Spitzer-driven. Whoever is presenting this needs to assess this in detail. We ''will'' find a different set of obj, not just classify them differently. Note lots of information is online only, which i attached to article pdf. analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!<br /> |do second to last. read closely! compare to everything above. &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/11 BY JOHN&lt;/font&gt;<br /> |-<br /> |Rebull, L., et al., 2011, AJ, in press (CG4 paper)<br /> | do as last review before we get started on ours?<br /> | this is very close to our analysis, though we may not have any optical at all.<br /> | discuss last, since methodology very similar? &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/18 BY MARK&lt;/font&gt; Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper &quot;New Young Star Candidates in CG4 and Sa101&quot;, Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]]<br /> |-<br /> |<br /> |<br /> |this line separates the &quot;should dos&quot; from the &quot;maybe skips&quot;<br /> |-<br /> |Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., [http://adsabs.harvard.edu/abs/2009A%26A...506..711G 2009, A&amp;A, 2009, 506, 711.] <br /> |''X-ray survey of CMa region''<br /> |BRC 27. ROSAT+VRI data. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Mentions Chandra, XMM data, both of which would cover BRC 27, but I can't find the subsequent analysis that they advertise. We need to include this catalog in what we accumulate, and compare our results to theirs. Not clear if we need to actually discuss it or not.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., [http://adsabs.harvard.edu/abs/1999MNRAS.310..210S 1999, MNRAS, 310, 210.] <br /> |''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> |BRC 27 only. optical. age, distance estimate. photo'''electric''' UBVR(!) and objective prism spectroscopy for Halpha and spectral types. combined with IRAS. using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Not clear if we need to actually discuss it or not. It's old methodology (from an Uzbecki telescope), but good stuff, especially the spectral types. nice &quot;put-it-in-context&quot; discussion at the top for the entire CMa R1 region. <br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., [http://adsabs.harvard.edu/abs/1986PASJ...38..395W 1986, PASJ, 38, 395.]<br /> |''Optical survey of CMa region''<br /> |BRC 27. Halpha plus photo'''graphic''' UBV.(!) using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they say they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Nice cross matching that they've already done for ''their'' previously identified objects. Not clear if we need to actually discuss it or not. It's a really old paper.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2002A%26A...388..172S 2002, A&amp;A, 388, 172.] <br /> |''2MASS obs of BRC 27''<br /> |BRC 27. 2MASS. Editing ghastly. Really simple paper. In theory, we should include their results in what we accumulate, and compare our results, though (a) they are using &quot;prehistoric&quot; 2mass data reduction, and (b) they really make it hard, as they don't even tell us how many YSOs they think they've found, just the numbers of objects for which they've done photometry. So I don't think we really can compare our results to this one. However, nice &quot;put it in larger context&quot; discussion with wide-field IRAS image. <br /> |skip it unless you want to see the IRAS image.<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2003A%26A...404..217S 2003, A&amp;A, 404, 217.] <br /> |''2MASS + optical survey''<br /> | Simple paper elsewhere in the same cloud as BRC 27. Same sort of 2MASS analysis as their 2002 paper. Still archaic 2MASS data reduction. Skip it.<br /> | skip it.<br /> |-<br /> |Valdettaro R., Palla F., Brand J., Cesaroni R., [http://adsabs.harvard.edu/abs/2005A%26A...443..535V 2005, A&amp;A, 443, 535.] <br /> |''Radio survey of water masers''<br /> |22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. Nice to at least scan after the Morgan stuff for context. larger issues: spatial resolution (see [[Resolution]]). Again!! :)<br /> |maybe skip?<br /> |-<br /> |Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., [http://adsabs.harvard.edu/abs/2008ApJ...675.1352V 2008, ApJ, 675, 1352.] <br /> |''VLA obs of water masers; BRC 34''<br /> |more water masers, following up 2005 work. BRC 34 observed, not detected. nice intro that puts their work in context with the rest of what they've done. Lots more non-dets, interpreted as forming low mass and/or older stars than had been assumed. I think they've gotten the interpretation spot-on. <br /> |maybe skip?<br /> |-<br /> |Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. <br /> |Poster from AAS ... good to review?<br /> |ok, but not a lot of content beyond the images and their 'big picture' work.<br /> |skip?<br /> |-<br /> |Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. <br /> |''MOPEX info'' <br /> |VERY technical, not a manual, and not all that terribly relevant to what we're doing. let's drop this one from the list. <br /> |(drop)<br /> |-<br /> |}<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read. --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)<br /> <br /> =Literature known YSOs=<br /> <br /> In the end, we need a master file (text or xls) that has one line per object and all of the information (photometric plus any Ha measurements (usually in equivalent width)) we can gather on that object (along with the origin of that information). Papers in the literature might have rediscovered the same objects themselves, and we will certainly rediscover some of them ourselves. We need to be able to identify them as known objects when we find them.<br /> <br /> We need to scavenge the papers for names, coordinates, and photometry, and then go update the coordinates using 2MASS. [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video on how to do this using the 2MASS archive]. Guidelines: <br /> *(a) watch the units of the coordinates (J2000 or B1950); <br /> *(b) take the closest bright 2MASS source. As in, there should only be one 2MASS source near the target. If there is more than one, take the brighter one. <br /> *(c) Make a note of the 2MASS name as well, but you don't have to write down all the JHK measurements too; I have automatically grabbed those and matched them to the Spitzer catalog. We're trying to get the updated coordinates so that I can automatically merge the old information with our new catalog. <br /> *(d) Do only BRC 27 and 34. Don't do the rest! <br /> *(e) More than one person (at least 2!) should independently work on each of these tables, because transcription errors are ''really'' easy to make.<br /> *(f) During the time in which we are working on this, we can either keep one big master list with everything (which is what we will have in the end), or we can keep tables separately for each paper. If the individual tables have updated good coordinates, then we can have the computer merge them. But, this may mean that you look up the same objects more than once, since the same objects probably appear in more than one paper.<br /> *(note: what do i mean by 'machine readable'? i mean a plain text file that the computer can read in and parse and understand coordinates, etc. PDF is not enough. plain text is what i need.)<br /> <br /> The papers (links above), in order of priority:<br /> *Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- and see also [[file:table5-edited.txt]], which is the file i sent in which i was starting this process with their table 5. (this is what i was using in the youtube video above.) [[file:ogura-table5-diane.txt]] -- diane's version of the coordinates for both BRCs from table 5 (23 June)<br /> *Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- coordinates ok, just get a machine-readable version of the table so that we can make a note of the photometry. FROM LUISA 23 June: [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. 'missing' data in the pdf version are also mising here. just brc27 (that's all we care about).''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. -- coordinates are ok. just get machine-readable version of the main source table so that we can include the information from here. [[file:gregoriohetem-tablea1.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. annoying notes at bottom moved to last column. two-part table combined into one.''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:shev-diane.txt]] (june 26)<br /> [[file:shevchenko stellar.txt]] --[[User:Sartore|Sartore]] 08:26, 28 June 2011 (PDT)<br /> *Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. This was a listing of emission line stars in CMa, and only two of the emission line stars previously listed actually fall into the area assigned to BRC 27. The other entries are generally very close to the boundary in one dimension (or both), so I pulled them out of the original listing. [[file:Wira_separated.txt]] --[[User:Sartore|Sartore]] 08:04, 29 June 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Wira_separated.txt&diff=7344 File:Wira separated.txt 2011-06-29T14:58:09Z <p>Sartore: </p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=7343 BRC Spring work 2011-06-29T14:54:06Z <p>Sartore: /* Literature known YSOs */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information. Here's the bibliography from our proposal (with my comments) --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> {| border=&quot;1&quot;<br /> |'''paper'''<br /> |'''Chelen's notes'''<br /> |'''Luisa's notes'''<br /> |'''presenter/ present with'''<br /> |-<br /> |Guieu, S., et al., [http://adsabs.harvard.edu/abs/2010ApJ...720...46G 2010, ApJ, 720, 46] ([http://web.ipac.caltech.edu/staff/rebull/working/ic2118.pdf pdf])<br /> |<br /> | the 2118 paper (from my first teacher team).... because our work will look a lot like this<br /> | &lt;font color=&quot;red&quot;&gt;3/30, BY MARCELLA&lt;/font&gt;<br /> |-<br /> |Ogura K., Sugitani K., Pickles A., [http://adsabs.harvard.edu/abs/2002AJ....123.2597O 2002, AJ, 123, 2597.] <br /> |''Optical + 2MASS; contains general info of BRCs''<br /> | Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. Need to be sure that this catalog is included in our list of previously known YSOs in this region, compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one. Maybe not the other Sugitanis, but if we do discuss the other Sugitanis (&quot;Group S&quot;) then they should be combined here.<br /> |do this, possibly with rest of group S &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/20 BY DIANE&lt;/font&gt;<br /> |-<br /> |Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] <br /> |'''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> |the original SFO, origin of &quot;BRC&quot; terminology, numbers 1-44. covers the northern hemisphere. has nice intro/summary of what's going on in BRCs, CGs, etc. Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1991'''<br /> |-<br /> |Sugitani K., Ogura K., [http://adsabs.harvard.edu/abs/1994ApJS...92..163S 1994, ApJS, 92, 163.] <br /> |''another survey''<br /> |SFO/BRC catalog/nomenclature continued into the southern hemisphere. (NB: all our obj are in the N. Hem paper!). SFO/BRC numbers 45-89. Second in the Sugitani series. Again, much of detailed analysis now obsolete. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1994'''<br /> |-<br /> |Sugitani K., Tamura M., Ogura K., [http://adsabs.harvard.edu/abs/1995ApJ...455L..39S 1995, ApJ, 455, L39.] <br /> |''IRAS survey'' <br /> | JHK follow-up of IRAS sources from SFO. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Shame on them for not publishing a data table or even a figure with the locations of everything they identify as a YSO! BRC 27 is one that they choose to include in a finder chart, but doesn't do us much good. Nice summary of larger issues, timescales. Short paper. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1995'''<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., [http://adsabs.harvard.edu/abs/2004A%26A...426..535M 2004, A&amp;A, 426, 535.] note has erratum too.<br /> |''Radio and mid-ir survey''<br /> | NRAO/NVSS/VLA (20cm), DSS, MSX data. both 27 and 34 in here, though 34 is a non-det. nice intro to the physics, though they get into far more math than we need to. relevant issues: this radio is thermal (free-free emission). they smoothed data -- spatial resolution (see [[Resolution]]). another nice use of three big surveys. sfo 27 in the online-only fig 1. T3 also online only. identifying ionizing source is not the same as identifying point sources in the images themselves. it's not clear that this is all that relevant for us. part of a PhD thesis.<br /> |Drop? if do, do with &quot;Group M&quot; but skip the math. '''2004''' &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/27 BY CHELEN&lt;/font&gt;<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., [http://adsabs.harvard.edu/abs/2008A%26A...477..557M 2008, A&amp;A, 477, 557.] <br /> |''SCUBA survey''<br /> |SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see [[Resolution]] and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.<br /> |Probably the most worth doing of &quot;Group M&quot;; skip the math. '''2008'''<br /> |-<br /> |Morgan L. K., Urquhart J. S., Thompson M. A., [http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M 2009, MNRAS, 400, 1726.] <br /> |''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> | JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see [[Resolution]] and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.<br /> |Do with &quot;Group M&quot; for fig 2. '''2009'''<br /> |-<br /> |Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C 2009, MNRAS, 396, 964]. <br /> |''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> | BRC27. Optical (BVIc)+2mass+spitzer/irac. yes, this one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. references 'group M' papers, so do this one after those, and right before CG4 for contrast in methods. nice intro. multiwavelength and contaminants (see [[Finding cluster members]]). As I read this, they are using optical+nir to pick their YSOs, not Spitzer-driven. Whoever is presenting this needs to assess this in detail. We ''will'' find a different set of obj, not just classify them differently. Note lots of information is online only, which i attached to article pdf. analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!<br /> |do second to last. read closely! compare to everything above. &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/11 BY JOHN&lt;/font&gt;<br /> |-<br /> |Rebull, L., et al., 2011, AJ, in press (CG4 paper)<br /> | do as last review before we get started on ours?<br /> | this is very close to our analysis, though we may not have any optical at all.<br /> | discuss last, since methodology very similar? &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/18 BY MARK&lt;/font&gt; Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper &quot;New Young Star Candidates in CG4 and Sa101&quot;, Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]]<br /> |-<br /> |<br /> |<br /> |this line separates the &quot;should dos&quot; from the &quot;maybe skips&quot;<br /> |-<br /> |Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., [http://adsabs.harvard.edu/abs/2009A%26A...506..711G 2009, A&amp;A, 2009, 506, 711.] <br /> |''X-ray survey of CMa region''<br /> |BRC 27. ROSAT+VRI data. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Mentions Chandra, XMM data, both of which would cover BRC 27, but I can't find the subsequent analysis that they advertise. We need to include this catalog in what we accumulate, and compare our results to theirs. Not clear if we need to actually discuss it or not.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., [http://adsabs.harvard.edu/abs/1999MNRAS.310..210S 1999, MNRAS, 310, 210.] <br /> |''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> |BRC 27 only. optical. age, distance estimate. photo'''electric''' UBVR(!) and objective prism spectroscopy for Halpha and spectral types. combined with IRAS. using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Not clear if we need to actually discuss it or not. It's old methodology (from an Uzbecki telescope), but good stuff, especially the spectral types. nice &quot;put-it-in-context&quot; discussion at the top for the entire CMa R1 region. <br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., [http://adsabs.harvard.edu/abs/1986PASJ...38..395W 1986, PASJ, 38, 395.]<br /> |''Optical survey of CMa region''<br /> |BRC 27. Halpha plus photo'''graphic''' UBV.(!) using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they say they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Nice cross matching that they've already done for ''their'' previously identified objects. Not clear if we need to actually discuss it or not. It's a really old paper.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2002A%26A...388..172S 2002, A&amp;A, 388, 172.] <br /> |''2MASS obs of BRC 27''<br /> |BRC 27. 2MASS. Editing ghastly. Really simple paper. In theory, we should include their results in what we accumulate, and compare our results, though (a) they are using &quot;prehistoric&quot; 2mass data reduction, and (b) they really make it hard, as they don't even tell us how many YSOs they think they've found, just the numbers of objects for which they've done photometry. So I don't think we really can compare our results to this one. However, nice &quot;put it in larger context&quot; discussion with wide-field IRAS image. <br /> |skip it unless you want to see the IRAS image.<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2003A%26A...404..217S 2003, A&amp;A, 404, 217.] <br /> |''2MASS + optical survey''<br /> | Simple paper elsewhere in the same cloud as BRC 27. Same sort of 2MASS analysis as their 2002 paper. Still archaic 2MASS data reduction. Skip it.<br /> | skip it.<br /> |-<br /> |Valdettaro R., Palla F., Brand J., Cesaroni R., [http://adsabs.harvard.edu/abs/2005A%26A...443..535V 2005, A&amp;A, 443, 535.] <br /> |''Radio survey of water masers''<br /> |22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. Nice to at least scan after the Morgan stuff for context. larger issues: spatial resolution (see [[Resolution]]). Again!! :)<br /> |maybe skip?<br /> |-<br /> |Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., [http://adsabs.harvard.edu/abs/2008ApJ...675.1352V 2008, ApJ, 675, 1352.] <br /> |''VLA obs of water masers; BRC 34''<br /> |more water masers, following up 2005 work. BRC 34 observed, not detected. nice intro that puts their work in context with the rest of what they've done. Lots more non-dets, interpreted as forming low mass and/or older stars than had been assumed. I think they've gotten the interpretation spot-on. <br /> |maybe skip?<br /> |-<br /> |Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. <br /> |Poster from AAS ... good to review?<br /> |ok, but not a lot of content beyond the images and their 'big picture' work.<br /> |skip?<br /> |-<br /> |Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. <br /> |''MOPEX info'' <br /> |VERY technical, not a manual, and not all that terribly relevant to what we're doing. let's drop this one from the list. <br /> |(drop)<br /> |-<br /> |}<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read. --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)<br /> <br /> =Literature known YSOs=<br /> <br /> In the end, we need a master file (text or xls) that has one line per object and all of the information (photometric plus any Ha measurements (usually in equivalent width)) we can gather on that object (along with the origin of that information). Papers in the literature might have rediscovered the same objects themselves, and we will certainly rediscover some of them ourselves. We need to be able to identify them as known objects when we find them.<br /> <br /> We need to scavenge the papers for names, coordinates, and photometry, and then go update the coordinates using 2MASS. [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video on how to do this using the 2MASS archive]. Guidelines: <br /> *(a) watch the units of the coordinates (J2000 or B1950); <br /> *(b) take the closest bright 2MASS source. As in, there should only be one 2MASS source near the target. If there is more than one, take the brighter one. <br /> *(c) Make a note of the 2MASS name as well, but you don't have to write down all the JHK measurements too; I have automatically grabbed those and matched them to the Spitzer catalog. We're trying to get the updated coordinates so that I can automatically merge the old information with our new catalog. <br /> *(d) Do only BRC 27 and 34. Don't do the rest! <br /> *(e) More than one person (at least 2!) should independently work on each of these tables, because transcription errors are ''really'' easy to make.<br /> *(f) During the time in which we are working on this, we can either keep one big master list with everything (which is what we will have in the end), or we can keep tables separately for each paper. If the individual tables have updated good coordinates, then we can have the computer merge them. But, this may mean that you look up the same objects more than once, since the same objects probably appear in more than one paper.<br /> *(note: what do i mean by 'machine readable'? i mean a plain text file that the computer can read in and parse and understand coordinates, etc. PDF is not enough. plain text is what i need.)<br /> <br /> The papers (links above), in order of priority:<br /> *Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- and see also [[file:table5-edited.txt]], which is the file i sent in which i was starting this process with their table 5. (this is what i was using in the youtube video above.) [[file:ogura-table5-diane.txt]] -- diane's version of the coordinates for both BRCs from table 5 (23 June)<br /> *Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- coordinates ok, just get a machine-readable version of the table so that we can make a note of the photometry. FROM LUISA 23 June: [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. 'missing' data in the pdf version are also mising here. just brc27 (that's all we care about).''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. -- coordinates are ok. just get machine-readable version of the main source table so that we can include the information from here. [[file:gregoriohetem-tablea1.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. annoying notes at bottom moved to last column. two-part table combined into one.''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:shev-diane.txt]] (june 26)<br /> [[file:shevchenko stellar.txt]] --[[User:Sartore|Sartore]] 08:26, 28 June 2011 (PDT)<br /> *Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. Ignore this file[[file:wiram-diane.txt]] (june 26) Use this file. Only two of the emission line stars previously listed actually fall into the area assigned to BRC 27. The other entries are generally very close to the boundary in one dimension (or both), so I have separated them. [[file:Wiramihardja_separated]] --[[User:Sartore|Sartore]] 07:54, 29 June 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Wiramihardja_separated.txt&diff=7342 File:Wiramihardja separated.txt 2011-06-29T14:47:36Z <p>Sartore: </p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=7339 BRC Spring work 2011-06-28T15:26:45Z <p>Sartore: /* Literature known YSOs */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information. Here's the bibliography from our proposal (with my comments) --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> {| border=&quot;1&quot;<br /> |'''paper'''<br /> |'''Chelen's notes'''<br /> |'''Luisa's notes'''<br /> |'''presenter/ present with'''<br /> |-<br /> |Guieu, S., et al., [http://adsabs.harvard.edu/abs/2010ApJ...720...46G 2010, ApJ, 720, 46] ([http://web.ipac.caltech.edu/staff/rebull/working/ic2118.pdf pdf])<br /> |<br /> | the 2118 paper (from my first teacher team).... because our work will look a lot like this<br /> | &lt;font color=&quot;red&quot;&gt;3/30, BY MARCELLA&lt;/font&gt;<br /> |-<br /> |Ogura K., Sugitani K., Pickles A., [http://adsabs.harvard.edu/abs/2002AJ....123.2597O 2002, AJ, 123, 2597.] <br /> |''Optical + 2MASS; contains general info of BRCs''<br /> | Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. Need to be sure that this catalog is included in our list of previously known YSOs in this region, compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one. Maybe not the other Sugitanis, but if we do discuss the other Sugitanis (&quot;Group S&quot;) then they should be combined here.<br /> |do this, possibly with rest of group S &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/20 BY DIANE&lt;/font&gt;<br /> |-<br /> |Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] <br /> |'''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> |the original SFO, origin of &quot;BRC&quot; terminology, numbers 1-44. covers the northern hemisphere. has nice intro/summary of what's going on in BRCs, CGs, etc. Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1991'''<br /> |-<br /> |Sugitani K., Ogura K., [http://adsabs.harvard.edu/abs/1994ApJS...92..163S 1994, ApJS, 92, 163.] <br /> |''another survey''<br /> |SFO/BRC catalog/nomenclature continued into the southern hemisphere. (NB: all our obj are in the N. Hem paper!). SFO/BRC numbers 45-89. Second in the Sugitani series. Again, much of detailed analysis now obsolete. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1994'''<br /> |-<br /> |Sugitani K., Tamura M., Ogura K., [http://adsabs.harvard.edu/abs/1995ApJ...455L..39S 1995, ApJ, 455, L39.] <br /> |''IRAS survey'' <br /> | JHK follow-up of IRAS sources from SFO. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Shame on them for not publishing a data table or even a figure with the locations of everything they identify as a YSO! BRC 27 is one that they choose to include in a finder chart, but doesn't do us much good. Nice summary of larger issues, timescales. Short paper. If we do this one, recommend review with other Sugitani, Ogura papers.<br /> |drop? else w/ group S '''1995'''<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., [http://adsabs.harvard.edu/abs/2004A%26A...426..535M 2004, A&amp;A, 426, 535.] note has erratum too.<br /> |''Radio and mid-ir survey''<br /> | NRAO/NVSS/VLA (20cm), DSS, MSX data. both 27 and 34 in here, though 34 is a non-det. nice intro to the physics, though they get into far more math than we need to. relevant issues: this radio is thermal (free-free emission). they smoothed data -- spatial resolution (see [[Resolution]]). another nice use of three big surveys. sfo 27 in the online-only fig 1. T3 also online only. identifying ionizing source is not the same as identifying point sources in the images themselves. it's not clear that this is all that relevant for us. part of a PhD thesis.<br /> |Drop? if do, do with &quot;Group M&quot; but skip the math. '''2004''' &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 4/27 BY CHELEN&lt;/font&gt;<br /> |-<br /> |Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., [http://adsabs.harvard.edu/abs/2008A%26A...477..557M 2008, A&amp;A, 477, 557.] <br /> |''SCUBA survey''<br /> |SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see [[Resolution]] and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.<br /> |Probably the most worth doing of &quot;Group M&quot;; skip the math. '''2008'''<br /> |-<br /> |Morgan L. K., Urquhart J. S., Thompson M. A., [http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M 2009, MNRAS, 400, 1726.] <br /> |''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> | JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see [[Resolution]] and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.<br /> |Do with &quot;Group M&quot; for fig 2. '''2009'''<br /> |-<br /> |Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C 2009, MNRAS, 396, 964]. <br /> |''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> | BRC27. Optical (BVIc)+2mass+spitzer/irac. yes, this one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. references 'group M' papers, so do this one after those, and right before CG4 for contrast in methods. nice intro. multiwavelength and contaminants (see [[Finding cluster members]]). As I read this, they are using optical+nir to pick their YSOs, not Spitzer-driven. Whoever is presenting this needs to assess this in detail. We ''will'' find a different set of obj, not just classify them differently. Note lots of information is online only, which i attached to article pdf. analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!<br /> |do second to last. read closely! compare to everything above. &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/11 BY JOHN&lt;/font&gt;<br /> |-<br /> |Rebull, L., et al., 2011, AJ, in press (CG4 paper)<br /> | do as last review before we get started on ours?<br /> | this is very close to our analysis, though we may not have any optical at all.<br /> | discuss last, since methodology very similar? &lt;font color=&quot;red&quot;&gt;TO BE DISCUSSED 5/18 BY MARK&lt;/font&gt; Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper &quot;New Young Star Candidates in CG4 and Sa101&quot;, Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]]<br /> |-<br /> |<br /> |<br /> |this line separates the &quot;should dos&quot; from the &quot;maybe skips&quot;<br /> |-<br /> |Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., [http://adsabs.harvard.edu/abs/2009A%26A...506..711G 2009, A&amp;A, 2009, 506, 711.] <br /> |''X-ray survey of CMa region''<br /> |BRC 27. ROSAT+VRI data. relevant issues: using multiple wavelengths to find YSOs (see [[Finding cluster members]]), spatial resolution (see [[Resolution]]). Mentions Chandra, XMM data, both of which would cover BRC 27, but I can't find the subsequent analysis that they advertise. We need to include this catalog in what we accumulate, and compare our results to theirs. Not clear if we need to actually discuss it or not.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., [http://adsabs.harvard.edu/abs/1999MNRAS.310..210S 1999, MNRAS, 310, 210.] <br /> |''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> |BRC 27 only. optical. age, distance estimate. photo'''electric''' UBVR(!) and objective prism spectroscopy for Halpha and spectral types. combined with IRAS. using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Not clear if we need to actually discuss it or not. It's old methodology (from an Uzbecki telescope), but good stuff, especially the spectral types. nice &quot;put-it-in-context&quot; discussion at the top for the entire CMa R1 region. <br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., [http://adsabs.harvard.edu/abs/1986PASJ...38..395W 1986, PASJ, 38, 395.]<br /> |''Optical survey of CMa region''<br /> |BRC 27. Halpha plus photo'''graphic''' UBV.(!) using multiple wavelengths to find YSOs (see [[Finding cluster members]]). We need to include this catalog in what we accumulate, and compare our results to theirs. This is not necessarily a trivial task, as they have photographic 1950 coordinates, which will need to be precessed and then matched to a 2mass source to get a more recent position estimate (they say they have finding charts, which should help), but it only needs to be done for the objects in our field of view (our data). Nice cross matching that they've already done for ''their'' previously identified objects. Not clear if we need to actually discuss it or not. It's a really old paper.<br /> |need someone to scavenge data, maybe not discuss?<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2002A%26A...388..172S 2002, A&amp;A, 388, 172.] <br /> |''2MASS obs of BRC 27''<br /> |BRC 27. 2MASS. Editing ghastly. Really simple paper. In theory, we should include their results in what we accumulate, and compare our results, though (a) they are using &quot;prehistoric&quot; 2mass data reduction, and (b) they really make it hard, as they don't even tell us how many YSOs they think they've found, just the numbers of objects for which they've done photometry. So I don't think we really can compare our results to this one. However, nice &quot;put it in larger context&quot; discussion with wide-field IRAS image. <br /> |skip it unless you want to see the IRAS image.<br /> |-<br /> |Soares J.B., Bica E., [http://adsabs.harvard.edu/abs/2003A%26A...404..217S 2003, A&amp;A, 404, 217.] <br /> |''2MASS + optical survey''<br /> | Simple paper elsewhere in the same cloud as BRC 27. Same sort of 2MASS analysis as their 2002 paper. Still archaic 2MASS data reduction. Skip it.<br /> | skip it.<br /> |-<br /> |Valdettaro R., Palla F., Brand J., Cesaroni R., [http://adsabs.harvard.edu/abs/2005A%26A...443..535V 2005, A&amp;A, 443, 535.] <br /> |''Radio survey of water masers''<br /> |22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. Nice to at least scan after the Morgan stuff for context. larger issues: spatial resolution (see [[Resolution]]). Again!! :)<br /> |maybe skip?<br /> |-<br /> |Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., [http://adsabs.harvard.edu/abs/2008ApJ...675.1352V 2008, ApJ, 675, 1352.] <br /> |''VLA obs of water masers; BRC 34''<br /> |more water masers, following up 2005 work. BRC 34 observed, not detected. nice intro that puts their work in context with the rest of what they've done. Lots more non-dets, interpreted as forming low mass and/or older stars than had been assumed. I think they've gotten the interpretation spot-on. <br /> |maybe skip?<br /> |-<br /> |Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. <br /> |Poster from AAS ... good to review?<br /> |ok, but not a lot of content beyond the images and their 'big picture' work.<br /> |skip?<br /> |-<br /> |Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. <br /> |''MOPEX info'' <br /> |VERY technical, not a manual, and not all that terribly relevant to what we're doing. let's drop this one from the list. <br /> |(drop)<br /> |-<br /> |}<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read. --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)<br /> <br /> =Literature known YSOs=<br /> <br /> In the end, we need a master file (text or xls) that has one line per object and all of the information (photometric plus any Ha measurements (usually in equivalent width)) we can gather on that object (along with the origin of that information). Papers in the literature might have rediscovered the same objects themselves, and we will certainly rediscover some of them ourselves. We need to be able to identify them as known objects when we find them.<br /> <br /> We need to scavenge the papers for names, coordinates, and photometry, and then go update the coordinates using 2MASS. [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video on how to do this using the 2MASS archive]. Guidelines: <br /> *(a) watch the units of the coordinates (J2000 or B1950); <br /> *(b) take the closest bright 2MASS source. As in, there should only be one 2MASS source near the target. If there is more than one, take the brighter one. <br /> *(c) Make a note of the 2MASS name as well, but you don't have to write down all the JHK measurements too; I have automatically grabbed those and matched them to the Spitzer catalog. We're trying to get the updated coordinates so that I can automatically merge the old information with our new catalog. <br /> *(d) Do only BRC 27 and 34. Don't do the rest! <br /> *(e) More than one person (at least 2!) should independently work on each of these tables, because transcription errors are ''really'' easy to make.<br /> *(f) During the time in which we are working on this, we can either keep one big master list with everything (which is what we will have in the end), or we can keep tables separately for each paper. If the individual tables have updated good coordinates, then we can have the computer merge them. But, this may mean that you look up the same objects more than once, since the same objects probably appear in more than one paper.<br /> *(note: what do i mean by 'machine readable'? i mean a plain text file that the computer can read in and parse and understand coordinates, etc. PDF is not enough. plain text is what i need.)<br /> <br /> The papers (links above), in order of priority:<br /> *Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- and see also [[file:table5-edited.txt]], which is the file i sent in which i was starting this process with their table 5. (this is what i was using in the youtube video above.) [[file:ogura-table5-diane.txt]] -- diane's version of the coordinates for both BRCs from table 5 (23 June)<br /> *Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- coordinates ok, just get a machine-readable version of the table so that we can make a note of the photometry. FROM LUISA 23 June: [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. 'missing' data in the pdf version are also mising here. just brc27 (that's all we care about).''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. -- coordinates are ok. just get machine-readable version of the main source table so that we can include the information from here. [[file:gregoriohetem-tablea1.txt]] -- '''important things to note: all plain text. no tabs. columns aligned. annoying notes at bottom moved to last column. two-part table combined into one.''': &lt;font color=red&gt;NOTE: DONE&lt;/font&gt;<br /> *Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:shev-diane.txt]] (june 26)<br /> [[file:shevchenko stellar.txt]] --[[User:Sartore|Sartore]] 08:26, 28 June 2011 (PDT)<br /> *Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- CAUTION, 1950 coords! need to be precessed and updated! Need also to check their finding charts against 2MASS to be sure you've found the right one. [[file:wiram-diane.txt]] (june 26)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Shevchenko_stellar.txt&diff=7338 File:Shevchenko stellar.txt 2011-06-28T15:04:00Z <p>Sartore: uploaded a new version of &quot;File:Shevchenko stellar.txt&quot;:&amp;#32;updated coordinates plus extra data for stars in the BRC 27 area</p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Shevchenko_stellar.txt&diff=7337 File:Shevchenko stellar.txt 2011-06-28T15:01:55Z <p>Sartore: </p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Summer_visit_logistics&diff=7315 BRC Summer visit logistics 2011-06-23T00:24:38Z <p>Sartore: </p> <hr /> <div>I sent out the &quot;big travel document&quot; on or about Apr 7. Please check your mail from about then for it. It's got all the information about how to book flights, etc., etc.<br /> <br /> It references [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/visit/ this page] on the CoolCosmos website. This is where you find the student forms too.<br /> <br /> <br /> =High-level schedule=<br /> <br /> The work days we've agreed upon are Jul 6-9, where there will be minimal help from me on Jul 9 as sort of a &quot;training run&quot; for when you go home.<br /> <br /> I propose you come in relatively early on Jul 5, and plan on doing dinner at my house that night. <br /> <br /> *Tuesday morning/early afternoon - arrive in LA<br /> *Tuesday night, 6pm - pizza party at Luisa's ... 5 or 5:30 if you want to play with Andrew!<br /> *Wednesday morning 8:30-12? - lectures<br /> *Wednesday afternoon 1-5 - software setup. SHA workthrough. Start to work with mosaics.<br /> *Thursday all day - hands-on work with computers<br /> *Friday morning?? - JPL tour<br /> *Friday afternoon - wrapup, plan for when you go home<br /> *Saturday morning - Work on your own or small groups. Try to do some of the tasks we did as a group. Compare notes. Can you work on your own at home without me?<br /> *Saturday afternoon - Reconvene for questions and help.<br /> *Sunday - return home<br /> <br /> =Software to install=<br /> <br /> Make sure you (and all your students who are coming) each have a functional laptop that you know how to use with as much of the relevant software installed as possible well before you get on the plane. Trust me. Makes it '''much''' easier if you do all this ahead of time, including starting it up to make sure it works. <br /> *[http://hea-www.harvard.edu/RD/ds9/ ds9]<br /> *[http://spider.ipac.caltech.edu/staff/laher/apt/ APT]<br /> *a web browser (Firefox, Safari, or Google Chrome)<br /> *Excel or other spreadsheet program<br /> <br /> Also make sure you have all the passwords you need for installing new software, getting on a wireless network, or getting back into your machine if it reboots.<br /> <br /> =Flight &amp; student &amp; housing details=<br /> <br /> More updates to this page as events warrant...<br /> <br /> *Marcella - bringing 1 boy and 1 girl<br /> *Diane - bringing 2 girls<br /> *John - bringing 3 boys and 1 girl <br /> *Chelen - bringing 2 girls<br /> (for hotel rooms, put John's girl with Marcella's girl, and John's 3rd boy with Marcella's boy)<br /> <br /> TOTAL of 14 people.<br /> <br /> ---<br /> <br /> While in Pasadena, we will be staying at the Holiday Inn Express. I have reserved a total of eight rooms.<br /> <br /> John... you'll have a King Suite checking in on 05-July and out on 10-July. <br /> Marcella and I will have a double checking in on 05-July and out on 10-July. <br /> Four more doubles for students checking in on 05-July and out on 10-July. <br /> <br /> Diane ... you'll have a King Suite checking in on 05-July and out on 09-July. <br /> Diane's students will have a double checking in on 05-July and out on 09-July.<br /> <br /> Any cancellations, if necessary, need to be made before 18:00 PDT on 04-July-2011.<br /> <br /> Daily rates: $109 + tax for King, $99 + tax for Double<br /> <br /> ''Holiday Inn Express''<br /> 3500 East Colorado Blvd.<br /> Pasadena, CA 91107<br /> ''(626) 792-1363''<br /> <br /> --&gt;&gt; Confirmation numbers were sent in an e-mail earlier today &lt;&lt;--<br /> <br /> --[[User:CJohnson|CJohnson]] 09:50, 31 May 2011 (PDT)<br /> <br /> ---<br /> <br /> Flights - <br /> <br /> Team Oregon - arr LAX 7/5, 2:25 pm; dep LAX 7/10 12:15pm.<br /> <br /> Team Minnesota - arr LAX 7/5 1:39 pm; depart LAX 7/10 7:55 am <br /> <br /> Team Florida - arr LAX 7/5 10:03 am; depart LAX 7/9 11:05 pm<br /> <br /> Team Illinois -</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Spring_work&diff=6926 BRC Spring work 2011-03-23T19:34:56Z <p>Sartore: /* Papers to discuss */</p> <hr /> <div>= Big Picture =<br /> <br /> We need to come up with a short list of papers to read in detail and discuss. We'll rotate through our short list of papers, and each of you will get one to present to the group. This is modelling a so-called &quot;journal club&quot;, a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. <br /> <br /> =Papers to discuss=<br /> <br /> Type in your paper suggestions here....<br /> <br /> '''Luisa nominates''' - either [http://adsabs.harvard.edu/abs/2010ApJ...720...46G this one] (IC2118, from my original teacher team), or the one I am in the process of finishing writing on CG4 from my team last year. The reason for this is because the analysis we will do for our BRCs is very similar to the analysis we did for IC2118 or CG4.<br /> <br /> '''Chelen's nominees''' - reading the IC2118 and/or the CG4 paper would be good ways to learn the analysis procedure we're going to use/modify/manipulate. I also think a couple of papers on BRCs would be helpful for background information ... my choices are <br /> <br /> Here's the bibliography from our proposal (with my comments):<br /> <br /> Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15. ''Poster from AAS ... good to review?''<br /> <br /> Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. ''Tests S4F theory; survey using Spitzer archival data; not deep enough??''<br /> <br /> Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&amp;A, 2009, 506, 711. ''X-ray survey of CMa region''<br /> <br /> Makovoz D., Marleau F. R., 2005, PASP, 117, 1113. ''MOPEX info''<br /> <br /> Morgan L. K., Urquhart J. S., Thompson M. A., 2009, MNRAS, 400, 1726. ''Radio, mid-ir, SCUBA observations; redefined SFO catalog''<br /> <br /> Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., 2008, A&amp;A, 477, 557. ''SCUBA survey''<br /> <br /> Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., 2004, A&amp;A, 426, 535. ''Radio and mid-ir survey''<br /> <br /> Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. ''Optical + 2MASS; contains general info of BRCs''<br /> <br /> Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. ''Optical catalog that includes both BRC 27 and BRC 34; contains general info on BRCs''<br /> <br /> Soares J.B., Bica E., 2003, A&amp;A, 404, 217. ''2MASS + optical survey''<br /> <br /> Soares J.B., Bica E., 2002, A&amp;A, 388, 172. ''2MASS obs of BRC 27''<br /> <br /> Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. '''''SFO''' article to which many other articles refer ... might be worth a review??''<br /> <br /> Sugitani K., Ogura K., 1994, ApJS, 92, 163. &quot;another survey&quot;<br /> <br /> Sugitani K., Tamura M., Ogura K., 1995, ApJ, 455, L39. ''IRAS survey''<br /> <br /> Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., 2008, ApJ, 675, 1352. ''VLA obs of water masers; BRC 34''<br /> <br /> Valdettaro R., Palla F., Brand J., Cesaroni R., 2005, A&amp;A, 443, 535. ''Radio survey of water masers''<br /> <br /> Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.''Optical survey of CMa region''<br /> --[[User:CJohnson|CJohnson]] 09:55, 23 March 2011 (PDT)<br /> <br /> <br /> I second reading all of the bibliographic articles, plus the one on IC2118. My reasoning is that I think we should be familiar with all of the work for the references we cited, and I would like any preview of the work that we will do. The older articles I have been looking (Stromgren, 1948 &amp; Sharpless 1959)at are interesting for their historical context, but probably not necessary for all of us to read.<br /> <br /> --[[User:Sartore|Sartore]] 12:34, 23 March 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6880 BRC Proposal 2011-03-16T18:14:00Z <p>Sartore: /* Proposal Versions */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Proposal Versions=<br /> <br /> Second attempt [[File:BRC_prop2.doc]]<br /> --[[User:CJohnson|CJohnson]] 12:21, 15 March 2011 (PDT)<br /> <br /> First attempt [[File:BRC_prop1.doc]]<br /> --[[User:CJohnson|CJohnson]] 13:05, 9 March 2011 (PST)<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> --[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)<br /> <br /> <br /> Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. Data for BRC27 will originate from Spitzer program 30050 (reqkeys 17512192 and 17512448) while BRC34 data will originate from program 202 (reqkeys 6031616 and 6031872). See Figure 1 for visualization of BRC27 data using the Spitzer Planning and Observation Tool (Spot). Reference Figure 2 for visualization of BRC34 data.<br /> <br /> <br /> ''Figure 1: Spot visualization of BRC27 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''<br /> <br /> [[File:brc27_final.jpg]]<br /> <br /> <br /> ''Figure 2: Spot visualization of BRC34 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''<br /> <br /> [[File:brc34_final.jpg]]<br /> <br /> <br /> Our plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010), as well as look for new YSOs. To accomplish this, a well-known property of YSOs will be exploited -- namely, large near- and mid-infrared emissions from material surrounding young stars. Looking for excess emissions will be the main focus of the research, and Spitzer is excellent at detecting these emissions as well as any bipolar outflows. Using the combined data, we will generate and analyze various plots, including spectral energy distributions (SEDs) , color-magnitude diagrams, and color-color diagrams to search for stars with infrared excesses.<br /> <br /> <br /> We will generate mosaics of the BRC objects using MOPEX-Mosaics from Photometry data (Makovoz &amp; Marleau 2005). For data reduction, the Aperture Photometry Tool (APT) will assist us in obtaining photometry values. These tools will allow our team to conduct flux analyses as well as spatial analyses and detailed visual observations. The resultant data will be analyzed further using a spreadsheet program (MS Excel). Excel will allow students to generate color diagrams and SEDs with the data to test infrared wavelenght theories of identifying and classifying young stellar objects.<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. <br /> <br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> Students at Carmel Catholic High School will participate in the Spitzer research program as an extracurricular activity. Students will meet once a week for two to four hours or as needed. Students will read a variety of resources and participate in activities to learn about the history of astronomy and stellar evolution. Students will become proficient in a variety of image processing software programs. Students will share their research findings at local outreach events at the middle school, high school, and community levels.<br /> <br /> John: <br /> Glencoe Astronomy at Glencoe High School. Glencoe High School students ranging from sophomores to seniors will work together on this BRC project. There are currently seven students starting this project and additional students are anticipated. Students will be given weekly readings that will be discussed during our meetings each Thursday morning. We will begin with the basic principles of stellar evolution with an emphasis on star formation. Resources will include tutorials posted on the CoolWiki website and scientific articles relevant to the BRC project. Students will work together in teams during the data analysis and continue to meet to discuss their work.<br /> <br /> Diane: <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --updated [[User:CJohnson|CJohnson]] 11:20, 15 March 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:BRC_prop2_dcs_edits.doc&diff=6879 File:BRC prop2 dcs edits.doc 2011-03-16T18:12:15Z <p>Sartore: uploaded a new version of &quot;File:BRC prop2 dcs edits.doc&quot;</p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:BRC_prop2_dcs_edits.doc&diff=6878 File:BRC prop2 dcs edits.doc 2011-03-16T18:07:32Z <p>Sartore: </p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6877 BRC Proposal 2011-03-16T18:03:01Z <p>Sartore: /* Proposal Versions */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Proposal Versions=<br /> <br /> small edits on 2nd attempt<br /> [[Media:Example.ogg]]<br /> <br /> Second attempt [[File:BRC_prop2.doc]]<br /> --[[User:CJohnson|CJohnson]] 12:21, 15 March 2011 (PDT)<br /> <br /> First attempt [[File:BRC_prop1.doc]]<br /> --[[User:CJohnson|CJohnson]] 13:05, 9 March 2011 (PST)<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> --[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)<br /> <br /> <br /> Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. Data for BRC27 will originate from Spitzer program 30050 (reqkeys 17512192 and 17512448) while BRC34 data will originate from program 202 (reqkeys 6031616 and 6031872). See Figure 1 for visualization of BRC27 data using the Spitzer Planning and Observation Tool (Spot). Reference Figure 2 for visualization of BRC34 data.<br /> <br /> <br /> ''Figure 1: Spot visualization of BRC27 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''<br /> <br /> [[File:brc27_final.jpg]]<br /> <br /> <br /> ''Figure 2: Spot visualization of BRC34 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''<br /> <br /> [[File:brc34_final.jpg]]<br /> <br /> <br /> Our plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010), as well as look for new YSOs. To accomplish this, a well-known property of YSOs will be exploited -- namely, large near- and mid-infrared emissions from material surrounding young stars. Looking for excess emissions will be the main focus of the research, and Spitzer is excellent at detecting these emissions as well as any bipolar outflows. Using the combined data, we will generate and analyze various plots, including spectral energy distributions (SEDs) , color-magnitude diagrams, and color-color diagrams to search for stars with infrared excesses.<br /> <br /> <br /> We will generate mosaics of the BRC objects using MOPEX-Mosaics from Photometry data (Makovoz &amp; Marleau 2005). For data reduction, the Aperture Photometry Tool (APT) will assist us in obtaining photometry values. These tools will allow our team to conduct flux analyses as well as spatial analyses and detailed visual observations. The resultant data will be analyzed further using a spreadsheet program (MS Excel). Excel will allow students to generate color diagrams and SEDs with the data to test infrared wavelenght theories of identifying and classifying young stellar objects.<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. <br /> <br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> Students at Carmel Catholic High School will participate in the Spitzer research program as an extracurricular activity. Students will meet once a week for two to four hours or as needed. Students will read a variety of resources and participate in activities to learn about the history of astronomy and stellar evolution. Students will become proficient in a variety of image processing software programs. Students will share their research findings at local outreach events at the middle school, high school, and community levels.<br /> <br /> John: <br /> Glencoe Astronomy at Glencoe High School. Glencoe High School students ranging from sophomores to seniors will work together on this BRC project. There are currently seven students starting this project and additional students are anticipated. Students will be given weekly readings that will be discussed during our meetings each Thursday morning. We will begin with the basic principles of stellar evolution with an emphasis on star formation. Resources will include tutorials posted on the CoolWiki website and scientific articles relevant to the BRC project. Students will work together in teams during the data analysis and continue to meet to discuss their work.<br /> <br /> Diane: <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --updated [[User:CJohnson|CJohnson]] 11:20, 15 March 2011 (PDT)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6802 BRC Proposal 2011-03-07T18:33:02Z <p>Sartore: /* Education and Outreach */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6801 BRC Proposal 2011-03-07T18:28:42Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6794 BRC Proposal 2011-03-06T23:36:32Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages physics dictates that these objects must be very luminous and look like cool red stars, however they not observable at visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6793 BRC Proposal 2011-03-06T23:17:09Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages physics dictates that these objects should be very luminous and look like cool red stars, however they not observable at visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6792 BRC Proposal 2011-03-06T22:06:48Z <p>Sartore: /* Education and Outreach */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages physics dictates that these objects should be very luminous and look like cool red stars, however they not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!<br /> <br /> --[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6791 BRC Proposal 2011-03-06T22:00:26Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages physics dictates that these objects should be very luminous and look like cool red stars, however they not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6790 BRC Proposal 2011-03-06T21:55:28Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6789 BRC Proposal 2011-03-06T21:54:10Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6788 BRC Proposal 2011-03-06T20:37:42Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> DOES ANYBODY HAVE ACCESS TO Ogura's 2010 &quot;Triggered Star Formation associated with HII Regions&quot; ADS says the full paper is not available.<br /> --[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> Is this enough background, or should I add more on protostar formation? <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6787 BRC Proposal 2011-03-05T20:53:27Z <p>Sartore: /* Education and Outreach */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> Is this enough background, or should I add more on protostar formation? <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6776 BRC Proposal 2011-02-27T20:12:44Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> Is this enough background, or should I add more on protostar formation? <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during bi-weekly brown-bag lunches. Members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6775 BRC Proposal 2011-02-27T20:10:39Z <p>Sartore: /* Education and Outreach */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)<br /> <br /> BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui &amp; Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura &amp; Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)<br /> <br /> <br /> BRC 34: Marcella<br /> (This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).<br /> <br /> Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).<br /> <br /> Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Dist(asec) RA DEC<br /> <br /> IRAS 21319+5755 268.14 21 33 25.0 +58 08 26<br /> <br /> IRAS 21316+5751 283.31 21 33 10.2 +58 04 43<br /> <br /> IRAS 21320+5752 373.69 21 33 33.4 +58 05 56<br /> <br /> IRAS 21314+5802 429.35 21 32 55.5 +58 15 51<br /> <br /> IRAS 21320+5752 436.65 21 32.5 +58 02<br /> <br /> IRAS 21323+5800 578.04 21 33 52.0 +58 14 04<br /> <br /> <br /> Previously identified stars within 10 arcminutes are listed below (SIMBAD).<br /> <br /> Identifier Class Dist (asec) RA DEC<br /> <br /> TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42<br /> <br /> HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234<br /> <br /> GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6<br /> <br /> BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840<br /> <br /> Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7<br /> <br /> Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8<br /> <br /> <br /> Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.<br /> <br /> Identifier Dist (asec) RA DEC<br /> <br /> 1 2MASS <br /> J21332921+5802508 463.43 21 33 29.21 +58 02 50.9<br /> <br /> 2 21 33 55.8 +58 01 18<br /> <br /> <br /> <br /> Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.<br /> Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation. <br /> Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution. <br /> Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. As one project winds down, another comes along to replace it. Even when we do not have a big project, the sky always presents something different for us to examine. The team meets during bi-weekly brown-bag lunches. Members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and scout troops. Currently, students are exploring web sites, reading articles, and are anxious to get started with Spitzer analysis.<br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6769 BRC Proposal 2011-02-26T22:09:45Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6768 BRC Proposal 2011-02-26T22:08:30Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6767 BRC Proposal 2011-02-26T22:05:54Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm shock waves. A very large cloud typically contracts to form a number of individual stars. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures and visual component from our view. However, the energy from the protostar warms the dust, which then reradiates the energy as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths. <br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6766 BRC Proposal 2011-02-26T22:02:16Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star Formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm shock waves. A very large cloud typically contracts to form a number of individual stars. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures and visual component from our view. However, the energy from the protostar warms the dust, which then reradiates the energy as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.<br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6765 BRC Proposal 2011-02-26T22:01:50Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Science Background and Context: Star formation'''<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm shock waves. A very large cloud typically contracts to form a number of individual stars. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures and visual component from our view. However, the energy from the protostar warms the dust, which then reradiates the energy as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.<br /> <br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6764 BRC Proposal 2011-02-26T21:58:32Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> '''Star formation: Diane'''<br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm shock waves. A very large cloud typically contracts to form a number of individual stars. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures and visual component from our view. However, the energy from the protostar warms the dust, which then reradiates the energy as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.<br /> <br /> Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et. al. (2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et. al. (2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.<br /> --[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6763 BRC Proposal 2011-02-26T19:26:23Z <p>Sartore: /* Introduction/Background */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> =Target Selection=<br /> <br /> STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like &quot;we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated.&quot; <br /> <br /> papers from discussion on the phone 16:35, 23 February 2011 (PST)<br /> *[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with &quot;sfo 38&quot; http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M <br /> *[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M<br /> <br /> <br /> <br /> ----<br /> <br /> =STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=<br /> <br /> <br /> =Introduction/Background=<br /> <br /> the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> <br /> Star formation: Diane<br /> <br /> Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae; giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar. The energy from the protostar warms the dust, which then reradiates the energy as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Jets from hidden protostars may announce the presence of the protostar itself, as well as the existence of an accompanying disk. Later, as young T-Tauri stage stars, they may blow away enough of their nebula to pierce the obscuring cocoon.<br /> <br /> Only lately has attention turned to Bright Rimmed Clouds (BRC’s) as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> We propose to conduct further examinations of BRC 27 and BRC 34 to search for additional young stellar objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et al. (2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We believe there is more to find in these BRC’s using Spitzer Space Telescope wavelengths.<br /> <br /> ...still in progress...<br /> --[[User:Sartore|Sartore]] 11:26, 26 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> mark, please also dip into the SHA (ops not i&amp;t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)<br /> <br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> * 2MASS <br /> * MSX<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Rollout.jpg&diff=6760 File:Rollout.jpg 2011-02-24T01:40:29Z <p>Sartore: uploaded a new version of &quot;File:Rollout.jpg&quot;</p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Rollout.jpg&diff=6759 File:Rollout.jpg 2011-02-24T01:32:19Z <p>Sartore: </p> <hr /> <div></div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:STS_133_rollout.jpg&diff=6758 File:STS 133 rollout.jpg 2011-02-24T01:28:51Z <p>Sartore: </p> <hr /> <div>01/31/11(best Monday ever)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:STS_133_rollout.jpg&diff=6757 File:STS 133 rollout.jpg 2011-02-24T01:28:07Z <p>Sartore: 01/3 1/11(best Monday ever)</p> <hr /> <div>01/3 1/11(best Monday ever)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=User:Sartore&diff=6756 User:Sartore 2011-02-24T01:25:08Z <p>Sartore: </p> <hr /> <div>Diane Sartore is delighted to be part of this project. <br /> <br /> <br /> --[[User:Sartore|Sartore]] 15:18, 15 February 2011 (PST)<br /> <br /> [[File:Example.jpg]]</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6735 BRC Proposal 2011-02-24T00:07:58Z <p>Sartore: /* Target Selection */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> =Target Selection=<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34!<br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> <br /> Proceedings of the International Astronomical Union<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> Copyright © International Astronomical Union 2008<br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> <br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> e-mail: lkm8@kent.ac.uk <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> =Introduction/Background=<br /> <br /> <br /> Star formation: Diane<br /> <br /> Stars are the most numerous objects in our nighttime sky, and astronomers want to understand the details of their processes. Nebulae have long been identified as “stellar nurseries”, and few issues in astronomy are more fundamental than knowing how stars form. While forming within the clouds of gas and dust, protostars are non-luminous and shielded within their nebula, so are not visible through optical telescopes. However, infrared telescopes are able to peer through obscuring clouds of dust to find the young stellar objects forming within. Only lately has attention turned to Bright Rimmed Clouds (BRC’s) as potential loci for star formation; their “speck globules” and “cometary globules” presented interesting sites for possible star formation.<br /> <br /> The role of BRC’s in star-formation processes makes them a topic of ongoing interest. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen and Peterson (2010?) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> We propose to conduct further examinations of BRC 27 and BRC 34 to search for additional young stellar objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen and Peterson (2010?) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We believe there is more to find in these BRC’s using Spitzer Space Telescope wavelengths.<br /> --[[User:Sartore|Sartore]] 15:01, 23 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> ** Collaboration with Lori Allen (NOAO) for access to already reduced data<br /> * 2MASS ?<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * Hands-On Universe Image Processing (HO-IP) for data analysis<br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6734 BRC Proposal 2011-02-24T00:07:16Z <p>Sartore: /* Background on Star Formation */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> =Target Selection=<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34!<br /> <br /> =Introduction/Background=<br /> <br /> <br /> Star formation: Diane<br /> <br /> Stars are the most numerous objects in our nighttime sky, and astronomers want to understand the details of their processes. Nebulae have long been identified as “stellar nurseries”, and few issues in astronomy are more fundamental than knowing how stars form. While forming within the clouds of gas and dust, protostars are non-luminous and shielded within their nebula, so are not visible through optical telescopes. However, infrared telescopes are able to peer through obscuring clouds of dust to find the young stellar objects forming within. Only lately has attention turned to Bright Rimmed Clouds (BRC’s) as potential loci for star formation; their “speck globules” and “cometary globules” presented interesting sites for possible star formation.<br /> <br /> The role of BRC’s in star-formation processes makes them a topic of ongoing interest. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen and Peterson (2010?) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> We propose to conduct further examinations of BRC 27 and BRC 34 to search for additional young stellar objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen and Peterson (2010?) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We believe there is more to find in these BRC’s using Spitzer Space Telescope wavelengths.<br /> --[[User:Sartore|Sartore]] 15:01, 23 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> ** Collaboration with Lori Allen (NOAO) for access to already reduced data<br /> * 2MASS ?<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * Hands-On Universe Image Processing (HO-IP) for data analysis<br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore https://vmcoolwiki.ipac.caltech.edu/index.php?title=BRC_Proposal&diff=6729 BRC Proposal 2011-02-24T00:03:30Z <p>Sartore: /* Background on Star Formation */</p> <hr /> <div>=Instructions=<br /> <br /> [[2011 proposal instructions]]<br /> <br /> =Background on Star Formation=<br /> <br /> [http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]<br /> <br /> <br /> Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]<br /> <br /> A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]<br /> --[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)<br /> <br /> <br /> http://journals.cambridge.org/action/displayAbstract?fromPage=online&amp;aid=1655856<br /> <br /> Proceedings of the International Astronomical Union<br /> Proceedings of the International Astronomical Union (2007), 3: 164-165 <br /> Copyright © International Astronomical Union 2008<br /> DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008 <br /> <br /> Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda<br /> --[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)<br /> <br /> A&amp;A 388, 172-178 (2002) <br /> DOI: 10.1051/0004-6361:20020451<br /> <br /> The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1<br /> J. B. Soares and E. Bica <br /> <br /> Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> A&amp;A 426, 535-545 (2004) <br /> DOI: 10.1051/0004-6361:20040226<br /> A radio and mid-infrared survey of northern bright-rimmed clouds <br /> L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao <br /> <br /> Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK <br /> e-mail: lkm8@kent.ac.uk <br /> --[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)<br /> <br /> =Target Selection=<br /> <br /> The list of sources that Lori suggests we consider are here:<br /> *[[target selection for brc34]] 21h32m51.2s +58d08m43s<br /> *[[target selection for brc36]] 21h35m32.6s +57d31m50s<br /> *[[target selection for brc31]] 20h50m43.4s +44d21m53s<br /> *[[target selection for brc27]] 07h04m07.8s -11d16m43s HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C<br /> <br /> *[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE<br /> <br /> Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about &lt;s&gt;30'&lt;/s&gt; 10' of these positions.<br /> <br /> <br /> Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]<br /> <br /> <br /> CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34!<br /> <br /> =Introduction/Background=<br /> <br /> <br /> Star formation: Diane<br /> <br /> Stars are the most numerous objects in our nighttime sky, and astronomers want to understand the details of their processes. Nebulae have long been identified as “stellar nurseries”, and few issues in astronomy are more fundamental than knowing how stars form. While forming within the clouds of gas and dust, protostars are non-luminous and shielded within their nebula, so are not visible through optical telescopes. However, infrared telescopes are able to peer through obscuring clouds of dust to find the young stellar objects forming within. Only lately has attention turned to Bright Rimmed Clouds (BRC’s) as potential loci for star formation; their “speck globules” and “cometary globules” presented interesting sites for possible star formation.<br /> <br /> The role of BRC’s in star-formation processes makes them a topic of ongoing interest. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen and Peterson (2010?) imaged 32 of the closest bright-rimmed clouds located at estimated distances d &lt; 1.2 kpc, finding young stellar objects in 75% of the clouds they studied. <br /> <br /> We propose to conduct further examinations of BRC 27 and BRC 34 to search for additional young stellar objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen and Peterson (2010?) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We believe there is more to find in these BRC’s using Spitzer Space Telescope wavelengths.<br /> --[[User:Sartore|Sartore]] 15:01, 23 February 2011 (PST)<br /> <br /> BRC 27: John<br /> <br /> BRC 34: Marcella<br /> <br /> ... drop what you have here ...<br /> <br /> =Analysis Plan=<br /> <br /> --[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)<br /> <br /> '''Available Data'''<br /> <br /> * Archival Spitzer IRAC 4 bands &amp; MIPS (Programs TBD)<br /> ** Collaboration with Lori Allen (NOAO) for access to already reduced data<br /> * 2MASS ?<br /> * Optical?<br /> * Spot visualization of Spitzer data?<br /> <br /> '''Data Reduction'''<br /> <br /> * Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)<br /> * Mosaics will be created using MOPEX<br /> <br /> '''Analysis Plan'''<br /> <br /> * Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs<br /> * Looking for infrared excess emission from material surrounding new stars will be the main focus of the research<br /> * Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses<br /> ** Color-Color diagrams<br /> ** Color-Magnitude diagrams<br /> ** Spectral Energcy Distribution (SED) plots<br /> * Analysis will also involve looking at actual optical and infrared images<br /> <br /> '''Tools'''<br /> <br /> * MOPEX - to create mosaics (Makovoz &amp; Marleau 2005)<br /> * Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010) <br /> * Hands-On Universe Image Processing (HO-IP) for data analysis<br /> * MS Excel – to generate data diagrams (color-color, SEDs)<br /> <br /> =Education and Outreach=<br /> Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.<br /> <br /> A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.<br /> <br /> Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)<br /> <br /> ''Team Spitzer at Breck School'' <br /> Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly &quot;brown-bag discussions.&quot; Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.<br /> <br /> <br /> Marcella: <br /> <br /> John: <br /> <br /> Diane: <br /> <br /> ... drop one paragraph per teacher here ...<br /> <br /> --[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)</div> Sartore