C-WAYS Spring work
- 1 Big Picture
- 2 C-WAYS Spring calendar
- 3 C-WAYS Resolution Worksheet
- 4 C-WAYS source matching work
- 5 Communicating on Wiki!!!
- 6 Papers to discuss
- 7 Things Students Should Know b4 CalTech
There are three things I'd like to accomplish before our visit:
(1) Start thinking about the issues of spatial resolution. I have developed a worksheet for this. WE DECIDED TO DO THIS FIRST.
(2) We need read in detail and discuss a short list of carefully selected papers. 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 "journal club", a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. The papers that went into this list came out of the extensive lists you assembled while writing the proposal. I then went through and sorted them into bins -- ones you want to read closely for the astronomy and astrophysics background, and/or for the interpretation, and/or for the big picture... ones from which you need to scavenge data, and you need to read enough to understand what it was they did, and what kinds of data they are reporting... ones you might read if you have time ... and ones you can ignore. WE SHOULD START ON THIS AFTER THE RESOLUTION STUFF.
(3) Actually doing the data scavenging out of those papers mentioned above. This can be as simple as going to the journal website and saving the data table as plain text, but in a handful of cases, it is a LOT more complicated. I am working on more explanation to go with this so-called source-matching work. Some of the work here springboards off of the journal articles we will read in detail, and some involves scanning additional articles. I AM STILL WORKING ON DEVELOPING A FRAMEWORK FOR THIS. It's ok if we don't get through this by the time of our visit, but it will slow us down for our visit.
Not all of us are around and able to work on NITARP stuff for the whole spring.
C-WAYS Resolution Worksheet I hesitate to make a place for everyone to collect their answers on the wiki; in this case, I would like everyone to independently derive their own numbers and compare notes on the telecon together.
C-WAYS source matching work -- this is an overview of what we need to know, and has some instructions, but no specific tasks doled out.
Communicating on Wiki!!!
Here's a useful link Guide to NITARP participants for use of the wiki
If you want to personalize your signature and turn on the email function
-log in, click on my preferences, put your whole name in for your signature if you want, check off all of the boxes at the bottom to turn on the email function If you want the CoolWiki to tell you when anyone makes an edit or comment to any page, first turn on the email function then
-go to the pages you want to "watch" and click on on the Watch tab, you'll get an email if there is a change to these pages
Individual School Pages
This is a place for students to practice using the wiki. You can follow my example for individual student pages below if you'd like. Please make it clear that this information is public.--Peggy Piper 17:46, 20 May 2012 (PDT)
- Lincoln-Way High School,Frankfort/New Lenox, Illinois
- Walter Payton College Prep High School, Chicago, IL
- New Philadelphia High School, New Philadelphia, OH
- Reedley College, Reedley, CA
- Daniel M. Soref Planetarium at the Milwaukee Public Museum, Milwaukee, WI
Papers to discuss
The relevant papers are sorted into the categories below.
I've attempted to make a roughly color-coded grouping of the papers below so that they can be presented in appropriate clumps. There are a LOT of papers to discuss, and I'm trying to make it roughly about the same amount of work per person. Here is the order I propose:
Reading Guide Summaries and questions on discussed papers
- person1 (JC1) -- Lauren -- Guieu et al 2010, Rebull et al 2011a and 2011b; possibly Johnson et al. 2012 and Rebull et al. 2012, or possibly makes more sense to wait until closer to the visit??
- person2 (JC2) -- Peggy -- Ogura et al 2002, Sugitani et al 1991 -- includes responsibility of leading the coordinate updating for these. SFO Paper Journals Guided Reading
- person3 (JC3) -- Jackie -- Getman et al 2007, Beltran et al 2009, should also probably read Choudhury et al. 2010... but Choudhury et al is meaty enough that it should be the next week after these. [Reading Guide Journal Club]
- person4 (JC4) -- Debbie -- Choudhury et al. 2010 and Chauhan et al. 2009 -- Chauhan et al 2009 is not meaty enough on its own, but is very different than Choudhury et al. 2010, despite sharing a few authors. Choudhury et al. pulls together some of the thoughts started in Getman et al and Beltran et al.
- person5 (JC5) -- Bob -- Barentsen et al. 2011 and Nakano et al. 2012
- person6 -- appendices of Koenig et al. 2012 and Gutermuth et al 2008?? depending on time, can/should skip these for now.
- then, starting with Ogura et al. 2002 and Sugitani et al. 1991, start updating coordinates.
- then, Gregorio-Hetem et al. 2009, Shevchenko et al. 1999, Wiramihardja et al 1986, and update those coordinates.
This should work like a journal club or even a book club, as in the named person takes the lead in presenting the article. You should present things along the lines of the following:
- the main point of this work was ...
- what they did was ... (high level summary, no need to get into nitty gritty details)
- the most interesting thing i learned was ...
- what they did that i agree with is ...
- what they did that i disagree with is ...
- and, for us here, the reason we should care about this in the context of our planned YSO work is ...
EVERYONE should read the papers ahead of time, but it's kind of expected that the named person will spend the most time reading the paper in question!
This group of papers are ones we need to read in 'journal club' style - read and discuss them in detail. They provide the scientific context and/or establishes known facts or conclusions about the bright rimmed clouds, or are similar enough to the process we will use that they are worth the investment of time.
|Paper||Notes||Presenter/ present with|
|Guieu et al., 2010, ApJ, 720, 46||Our paper from the IC2118 team (one of the pre-NITARP teams!). Spitzer-based search for YSOs in IC2118 (near Orion's knee). Large map to start from. Ground-based optical obtained specifically to support these observations, much like us. Note serendipitous discovery of high-proper-motion object. This is something Tim and his students found entirely on their own. We tried to obtain follow-up spectroscopy from Palomar, but had bad weather. I need to go back and try again to get these spectra. There is also an opportunity to look at this environment with WISE! do with other Rebull et al papers - "group R". This can be the lowest priority of that group, as it was written the longest time ago. (may be better to focus time and energy on CG4 paper and Taurus with WISE paper.)||(do with group R) person1|
|Rebull et al., 2011a, AJ, 142, 25||our paper from the CG4+Sa101 team (a NITARP 2009 team) (I gave you hard copy of this one at the AAS.) This is a Spitzer-based search for YSOs in this region. Fairly large map to start from, but smaller than IC2118. Ground-based optical pre-obtained through a collaborator to support the observations, similar to us. (She turns out to also have a bunch of spectra, but has other things in front of them in her queue.)||(do with group R) person1|
|Rebull et al., 2011b, ApJS, 196, 4||our paper looking for new YSOs in Taurus using WISE -- the one my recent AAS poster was based on, and I also gave you hard copy of this paper at the AAS. This starts from a HUGE region, 260 sq degrees, and something like 2.6 million sources. This is a far larger region than we will do, but we will use a similar approach -- use WISE, obtain a set of possible YSOs, use all available data we can find to weed down the list, compare to the literature-discovered objects, and present a list of candidates.||(do with group R) person1|
|Johnson et al., 2012, AAS219, 337.05 and Rebull et al. in prep||BRC 27 and 38: The NITARP 2011 team work here. Spitzer-driven search for YSOs, with ground-based optical photometry to support observations. I think most of you have read the poster already. I am still actively working on the draft; whenever this paper comes up in the rotation, I'll give you whatever I have at that point, even if it's unpolished. Sigh.||(do with group R) person1|
|Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.||BRC 27, 34, 38? Optical + 2MASS; general BRC info. Most recent of the Sugitani series of four we found. 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, so we can compare our results to theirs. Finding charts helpfully included so we can match obj. We should discuss this one in some depth; the other Sugitanis don't need to be done in as much depth ("group S").||(do with group S) person2|
|Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59.||SFO article (discovery paper) - the original SFO, origin of "BRC" 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. Review with other Sugitani, Ogura papers, but can skim the surface. You all should have read this in Jan or Feb in the context of our proposal, so maybe we don't have to do this again?||(do w/ group S) person2|
|Getman et al. 2007, ApJ, 654, 316||BRC 38. Chandra, 2MASS, and Spitzer. discusses X-ray sources that are associated with young stars in this region, which they call IC 1396N. Studying triggered star formation and protostars in IC 1396N. Good pictures to help with the visualization of 1396N and these sources; evidence of sequential star formation. really nice intro to put it all in context.
Found 117 x-ray sources in IC 1396N; identify some with central cluster, and some with globule. We are likely to have similar issues since we are looking further out from the globule. Objects at a variety of stages. One of the youngest sources detected in x-ray, #66, is found close to the source IRAS 21391+5802 (also called BIMA 2). List of these sources are included. Nice discussions about finding counterparts across wavelengths, contamination by background sources, predictions for more YSOs here to be found. Dense paper! We need to scavenge these data, compare to our results.
|do in detail. compare and contrast! scavenge data. person3 - Jackie|
|Beltran, et al., 2009, A&A, 504, 97B||BRC 38. this looked for YSOs inside the BRC using deep JHK. Data tables available online only! Comparison of results to Chandra results from Getman; find no evidence for sequential star formation. get and include their data. lots of discussion of extended emission and comparison to other bands. includes figure using IRAC 4.5 um data, but that's it for Spitzer information. Do in detail, with Getman.||do in detail, with Getman. scavenge data. person3 - Jackie|
|Choudhury R., Mookerjea, B., Bhatt, H., 2010, ApJ, 717, 1067||BRC 38, including IRAC+MIPS+optical phot and spec. *REALLY* nice paper. A tremendous amount of work, very nicely done, and very complete data tables. Go through and discuss this one in detail, scavenge all the data. Does a lot of comparison with Getman and Beltran, trying to reconcile all results. Do this one after or with Getman, Beltran; this one is meaty enough that it probably should get its own week.||do in detail. scavenge data. do after Getman, Beltran person4|
|Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964||BRC 27, 38. Optical (BVIc)+2mass+spitzer/irac. This one we should spend considerable time on. Testing small-scale sequential star formation suggested in earlier 'group S' papers. 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, which is different than what we will do. We will find a different set of obj, not just classify them differently. We need to get their data tables and compare our results to theirs. Note lots of information is online only, which i attached to article pdf. Note also that some of their online tables don't contain the same sources as the other tables (they should have caught that before publication). analysis of Halpha-age and mass function is a bit of overinterpretation IMHO. need spectroscopy first!!||do in detail -- read closely, compare and contrast! need to scavenge data too. person4|
|Barensten et al., 2011, MNRAS, 415, 103||BRC 34, 38. T tauri candidates and accretion rates using IPHAS (r, i, Halpha); over the entire huge IC1396 complex. this is a useful paper. data tables of 158 objects they think are young; make sure to grab and incorporate what they found. their shortlist may or may not overlap with the fields we care about in brc 34 (cloud D??) and 38 (cloud E), but still very useful to include. if, when we get to that point of needing these objects, they still haven't released the full IPHAS catalog, i will email these guys and ask for source lists at least in the regions we care about (34 and 38)
Also includes some 2 MASS and Spitzer data but only for T Tauri candidates, or possibly only in the center of the complex? need to read closely enough to figure this out. NB: more evidence for sequential/triggered star formation; find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)
|do this in detail, scavenge data person5|
|Nakano et al., 2012, AJ, 143, 61 Media:Nagano_2012.pdf||BRC 34, 38. Wide Field Survey of Emission-line Stars in IC 1396 (the whole complex). Nakano reports a total of 639 Halpha emission-line stars were detected in an area of 4.2 deg2; they matched to some literature sources, also some Akari sources. Data charts and images showing locations included. We should read this in some detail, and scavenge the data in the regions we care about (brc 34 and 38).||do this in detail, scavenge data. person5|
|Koenig et al., 2012, ApJ, 744, 130||WISE-based YSO selection mechanism (inspired by Gutermuth et al. 2008, 2009) described in appendix. Meat of paper on high-mass star formation (we aren't caring about that particularly here -- we mostly want the selection mechanism).||should read the appendix closely; you can skip the rest if you want. Do with Gutermuth et al 2008 ("colormethods") (person6?)|
|Gutermuth et al., 2008, ApJ, 674, 336||Spitzer color selection (first version - Gutermuth et al. 2009 perturbs it a little) presented here. Some of the selection mechanism is described in the main text, and some is in the appendix. We should read about the selection mechanism.||should read about the selection mechanism closely; you can skip the rest if you want. Do with Koenig et al. 2012. ("colormethods") (person6?)|
This group of papers is essential to read enough to get the data out of them, but we don't need to really study them in tremendous detail.
|Paper||Comments||Presenter/ present with|
|Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 506, 711.||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.||read enough to understand and scavenge data.|
|Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.||BRC 27. optical. age, distance estimate. photoelectric 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 region of interest. It's old methodology (from an Uzbecki telescope), but still good stuff, especially the spectral types. nice "put-it-in-context" discussion at the top for the entire CMa R1 region.||should read enough to understand and scavenge data.|
|Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.||BRC 27. Halpha plus photographic 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. We don't need to read it in detail; it's a really old paper. But we need to read enough to understand and scavenge data.||should read enough to understand and scavenge data.|
This group of papers is useful but not essential.
|Paper||Comments||Presenter/ present with|
|Nisini et al., 2001, A&A 376, 553||BRC 38. Multiple H2 protostellar jets in the bright-rimmed globule IC 1396-N. Jets are indicative of young stars! The H2 excitation inside the globule could be from either shocks driven by the outflow of YSOs or to UV induced fluorescence from the external ionized region. The conclusion states that the emissions originate from non-dissociative shocks, and that they are associated with the most embedded and youngest objects of the field. The near IR confirms the existence of a cluster of young embedded sources and highly efficient star formation activity. Lots of awkward text that English editing did not catch. Has a list of YSO candidates with some cross-ids. Lots of focus on jets and knots too. Much of these cross ids are probably in Choudhury et al.||read and scavenge table of YSOs?|
|Reipurth et al., 2003, ApJ, 123, 2597-2626||BRC 38 Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds. Halpha and other narrowband filters. Reipurth et al usually work in these wavelengths to find HH objects. short paper. they have a list of knots in the region, but that's it. Herbig-Haro flow (HH 777) found coming out of ic 1396N; located at 214041.6+581638 While many near-infrared sources were found that apparently are young stars this study focused on the HH flows found. Computer modeling was used to find a match for observed features.||ok to skip|
|Beltran et al., 2002, ApJ, 573, 1||BRC 38 IRAS 21391+5802: The Molecular Outflow and its Exciting source. VLA and BIMA observations of dust and gas surrounding IRAS source; 3 sources isolated with BIMA, each a YSO. Really good text about the intermediate mass star morphology and evolution compared to that of the low mass stars. There is a table at the end that has point source information of BIMA observations of 5 epochs with bandwidth and spectral resolution. A table with 5 sources and flux density and spectral index, another table with millimeter flux densitites, for 3 BIMA sources, and a table with CO outflow properties. Our focus will be more on the point sources. This paper is really focused on the outflow and its sources. Nice for context of source matching and variations in coordinate accuracy coupled with physical differences in the sources. But not a whole lot appropriate for our point source study.||ok to skip|
|Fuente, et al., 2007, A&A, 468L, 37||BRC 38. very short paper, looking for protostellar clusters in IC 1396N, using PdBI at 1.3, 3.3 mm. Main point as relevant to us -- 4 cores in IC1396N. Yes, strongly tied to Neri et al 2007 paper.||ok to skip|
|Neri, et al. 2007, A&A, 468, 33||BRC 38. found a cluster of hot cores in 1396N. again, a very short paper using PdBI at 1.3, 3.3 mm. Main point as relevant to us -- cluster of cores here. Yes, strongly tied to Fuente et al 2007 paper.||ok to skip|
For the over achievers
Read if you are motivated to do so.
|Paper||Comments||Presenter/ present with|
|Sugitani K., Ogura K., 1994, ApJS, 92, 163.||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 (by time) in the Sugitani series. Again, much of detailed analysis now obsolete. Review with other Sugitani, Ogura papers, but can skim the surface.||if do, do w/ group S|
|Sugitani K., Tamura M., Ogura K., 1995, ApJ, 455, L39.||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 do, review with other Sugitani, Ogura papers, but can skim the surface.||if do, do w/ group S|
|Connelley et al., 2007, AJ, 133, 1528||BRC 38 Infrared Nebulae around Young stellar objects. IRAS 21391+5802 - images show jet-like nebula and large patches of nebulosity. IRAS source thought to be a low mass Class 0 source (Beltran et al. 2002, 2004). This source has H2 emission in the form of bow shocks. We need to check the source in our images, but it's likely bright enough that it appears in many of the other papers.||ok to skip|
|Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., 2008, ApJ, 675, 1352.||BRC 34. (others?) VLA obs of 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.||scan if you want|
|Soares J.B., Bica E., 2002, A&A, 388, 172.||BRC 27. OLD 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 "prehistoric" 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 "put it in larger context" discussion with wide-field IRAS image.||skip it unless you want to see the IRAS image.|
|Soares J.B., Bica E., 2003, A&A, 404, 217.||2MASS + optical. 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.||skip it.|
|Allen L., et al. 2011, American Astronomical Society, BAAS, 43, 258.15.||Poster from AAS ... statistical measurement of YSOs in all of their BRC IRAC observations. not a lot of content beyond the images and their 'big picture' work.||skip it.|
|Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., 2004, A&A, 426, 535. note has erratum too.||BRC 27, 34, 38? Radio and mid-ir survey. 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.||Drop... if you want to, read with "Group M" but skip the math.|
|Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., 2008, A&A, 477, 557.||BRC 27, 34, 38? 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.||Probably the most worth reading of "Group M"; skip the math.|
|Morgan L. K., Urquhart J. S., Thompson M. A., 2009, MNRAS, 400, 1726.||BRC 27, 34, 38? Radio, mid-ir, SCUBA observations; redefined SFO catalog. JCMT (CO) observations. 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.||read with "Group M" for fig 2.|
|Valdettaro R., Palla F., Brand J., Cesaroni R., 2005, A&A, 443, 535.||Radio survey of water masers. 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!! :)||scan if you want with group M.|
|Wang et al., 2009, A&A, 504, 369||The relation between 13CO j=2-1 line width in moelcular clouds and bolometric luminosity of associated IRAS sources. Radio. ignore at least for now IRAS 21391+5802 - suggests that it is a star forming cluster where high-mass stars will form|
|Lynds, 1962, ApJS, 7, 1||The Lynds Dark Nebula paper. some of you were interested in the history of this. At least one if not all three of our BRCs are also associated with Lynds clouds. Read if you want to.|
Do not bother
This group of paper has passing relevance to the science and the goals of NITARP. They are useful references for your readers to follow up on details. It is sufficient that one person (usually Luisa) has enough knowledge to know that the citation is proper. Reading the full paper is not essential.
|Makovoz D., Marleau F. R., 2005, PASP, 117, 1113.||MOPEX info. VERY technical, not a manual, and not all that terribly relevant to what we're doing. skip it. you shouldn't have to get into MOPEX at all, but if you do, there is lots of online help in MOPEX that is really good, and also lots of documentation (aimed at professional astronomers, admittedly) on the SSC website.|
|Wright et al., 2010, AJ, 140, 1868||WISE "seminal paper" reference. Describes the mission. As I recall, there is some discussion of the data products, but for the complete discussion of data products in more of a manual form, consult the document that accompanies the delivery. Read this paper if you want a somewhat technical overview of the mission.|
|Werner et al., 2004, ApJS, 154, 309||Spitzer "seminar paper" reference. Describes the mission. No discussion of data products as I recall. Read this paper if you want a somewhat technical overview of the mission.|
|Bulletin of Astro. Instit. of the Netherlands, Vol 13, 471, 77-88, Pottasch et al., 1956, Bull. Astro. Instit. Netherlands, 13, 471||A study of bright rims in diffuse nebulae. VERY early work describing the location, shape of, density of, brightness of bright rim clouds in several nebula, including IC 1396 and Brc 38. So old that not really useful for assembling list of YSOs in region. skip.|
|Ogura & Sugitani, 1999, Proceedings of Star Formation, pg 381-382||A large number of Halpha Emission Stars associated with BRCs. Conference proceedings, old at that. i'm sure this analysis is already written up in their later papers. ignore this one.|
|Saraceno et al., 1996, A&A, 309, 827-839||An evolutionary diagram for young stellar objects. deep, DEEP background, IGNORE THIS.|
|Beltran et al., 2004, A&A, 426, 941||BRC 38? The dense molecular cores in IRAS 21391 +5802 region. Radio and it sounds like theoretical models. ignore. Three sources found with BIMA (??) observations in 21391+5802; Hard to read as they are trying to use data to fit/model how gas is emitted from the core|
|APT tool Laher et al. 2012, PASP, submitted||there are two papers that Russ is working on. One is a description of the basics of APT, what it's doing etc., and the other (i think) is more of a "what happens when you use APT to extract the photometry" kind of paper. It's been a while since I've seen these drafts; Russ has been going rounds with the referee on these both. He's started working on them again. Read this if you want to know the details of the inner workings of APT, and how it compares to other proven photometry programs.|
|Maoz 2007||Referenced in the proposal; listed here for completeness. Astrophysics in a Nutshell (Princeton, NJ). i think this is someone's (Debbie's?) textbook. don't need to read her textbook, but you might want to find your own! :)|