C-CWEL Proposal - Revision history

Rebull: /* Do these or scan these */

2013-02-27T23:27:43Z

Do these or scan these

Rebull: /* Do these or scan these */

2013-02-27T23:25:58Z

Do these or scan these

Rebull at 16:33, 27 February 2013

2013-02-27T16:33:02Z

Rebull: /* Useful figures */

2013-02-27T16:30:50Z

Useful figures

Rebull: /* Useful figures */

2013-02-27T16:30:18Z

Useful figures

Rebull: /* Useful figures */

2013-02-27T16:29:34Z

Useful figures

Rebull: /* Useful figures */

2013-02-27T16:28:56Z

Useful figures

Rebull at 16:28, 27 February 2013

2013-02-27T16:28:03Z

Rebull at 23:52, 6 February 2013

2013-02-06T23:52:33Z

Rebull: /* Potentially Useful Coordinates */

2013-01-30T23:52:50Z

Potentially Useful Coordinates

@@ Line 38: / Line 38: @@
 |-
 | DO THIS <br>[http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barentsen et al., 2011, MNRAS, 415, 103]<br>T tauri candidates and accretion rates using IPHAS: method and application to IC 1396||'''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) <br>'''Luisa adds:'''  YES this is a useful paper. data tables of objects they think are young. their shortlist may or may not overlap with the fields we care about in brc 34 and 38, 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 in the regions we care about (34 and 38)<br>'''Peggy adds:''' Includes BRC 38 which is called cloud E; Looking for YSOs in all of 1396; list 158 candidates; uses IPHAS survey data - Halpha, r, I filters on isaac newton telescope<BR><BR>Specifically looking for T Tauri through Halpha emissions.  Also includes 2 MASS and Spitzer data but only for T Tauri candidates? Find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)--Peggy Piper 12:47, 21 February 2012 (PST)||http://arxiv.org/pdf/1103.1646v1.pdf
+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) <br>'''Luisa adds:'''  YES this is a useful paper. data tables of objects they think are young. their shortlist may or may not overlap with the fields we care about in brc 34 and 38, 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 in the regions we care about (34 and 38)<br>'''Peggy adds:''' Includes BRC 38 which is called cloud E; Looking for YSOs in all of 1396; list 158 candidates; uses IPHAS survey data - Halpha, r, I filters on isaac newton telescope<BR><BR>Specifically looking for T Tauri through Halpha emissions.  Also includes 2 MASS and Spitzer data but only for T Tauri candidates? Find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)--Peggy Piper 12:47, 21 February 2012 (PST)
 |-
 | DO THIS<br>[http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran, et al., 2009, A&A, 504, 97B]<br>The stellar population and complex structure of the bright-rimmed cloud ic 1396N||'''Luisa adds''': YES very useful!<br> A study through JHK filters; 736 sources found in all 3 bands (filters); h2 emission shows jet like structure<br><br>'''Peggy adds'''deep survey of IC 1396N in J, H, K′ broadband filters and deep high-angular resolution in the H2 narrowband - Near Infrared Camera Spectrometer (NICS) at the National Telescope Galileo (TNG)  Firenze (Italy). 1010 sources photometry data, but not in all sources in all bandswidths due to lack of overlap.   I'm not sure I understand, but I believe they are saying that with reddening falling in the band of the main sequence and little near infrared excess, there are very few YSOs to be found?<br><br> OF NOTE: came after Getman et al paper, finds contradictory results. Read with Getman et al.||http://arxiv.org/pdf/0902.4543v1.pdf
@@ Line 53: / Line 54: @@
 |-
 | DO THIS <br>[http://adsabs.harvard.edu/abs/2007ApJ...654..316G Getman et al. 2007, ApJ, 654, 316]<br>X-ray study of triggered star formation and protostars in IC 1396N||'''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.<br> '''Luisa adds:'''  YES this is useful<br>x-ray sources in the globule of ic 1396N; good pictures to help with the visualization of 1396N and these sources; evidence of sequential star formation<br><br>'''Jackie adds:''' A Chandra study that found 117 x-ray sources in IC 1396N. 25 are associated with YSOs. A variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). 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. These sources were matched against 2MASS and MIR data.  The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found. ||http://arxiv.org/pdf/astro-ph/0607006v2.pdf
+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.<br> '''Luisa adds:'''  YES this is useful<br>x-ray sources in the globule of ic 1396N; good pictures to help with the visualization of 1396N and these sources; evidence of sequential star formation<br><br>'''Jackie adds:''' A Chandra study that found 117 x-ray sources in IC 1396N. 25 are associated with YSOs. A variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). 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. These sources were matched against 2MASS and MIR data.  The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found.
 |-
 |scan<br>[http://adsabs.harvard.edu/abs/2008ApJ...674..336G Gutermuth et al., 2008, ApJ, 674, 336]
@@ Line 68: / Line 70: @@
 |-
 | DO THIS <br>[http://adsabs.harvard.edu/abs/2002AJ....123.2597O Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.]<br> Halpha emission stars and Herbig-Haro objects in and around BRC||'''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.<br>
-'''Luisa adds:'''  YES this is useful - finding YSOs via Halpha<br> Part of Luisa's Notes from last year:  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.<br><br>'''Jackie adds:'''Looked for YSOs with H alpha emission. HH objects studied to learn more about their structure. Finder chart included for BRC 38 (also BRC 27 & 34) of 16 H alpha emission stars and data table with locations. Finder charts are also shown for HH objects in BRC 38.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. It should be studied in optical and IR.  ||http://iopscience.iop.org/1538-3881/123/5/2597/pdf/201506.web.pdf
+'''Luisa adds:'''  YES this is useful - finding YSOs via Halpha<br> Part of Luisa's Notes from last year:  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.<br><br>'''Jackie adds:'''Looked for YSOs with H alpha emission. HH objects studied to learn more about their structure. Finder chart included for BRC 38 (also BRC 27 & 34) of 16 H alpha emission stars and data table with locations. Finder charts are also shown for HH objects in BRC 38.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. It should be studied in optical and IR.
 |-
 |DO THIS<br> [http://adsabs.harvard.edu/abs/2013AJ....145...15R Rebull et al. 2013, AJ, 145, 15]||(I gave you hard copy of this one at the AAS.) Our paper looking for new YSOs in BRC 27 and BRC 34.

@@ Line 38: / Line 38: @@
 |-
 | DO THIS <br>[http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barentsen et al., 2011, MNRAS, 415, 103]<br>T tauri candidates and accretion rates using IPHAS: method and application to IC 1396||'''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) <br>'''Luisa adds:'''  YES this is a useful paper. data tables of objects they think are young. their shortlist may or may not overlap with the fields we care about in brc 34 and 38, 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 in the regions we care about (34 and 38)<br>'''Peggy adds:''' Includes BRC 38 which is called cloud E; Looking for YSOs in all of 1396; list 158 candidates; uses IPHAS survey data - Halpha, r, I filters on isaac newton telescope<BR><BR>Specifically looking for T Tauri through Halpha emissions.  Also includes 2 MASS and Spitzer data but only for T Tauri candidates? Find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)--Peggy Piper 12:47, 21 February 2012 (PST)  ||http://arxiv.org/pdf/1103.1646v1.pdf
+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) <br>'''Luisa adds:'''  YES this is a useful paper. data tables of objects they think are young. their shortlist may or may not overlap with the fields we care about in brc 34 and 38, 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 in the regions we care about (34 and 38)<br>'''Peggy adds:''' Includes BRC 38 which is called cloud E; Looking for YSOs in all of 1396; list 158 candidates; uses IPHAS survey data - Halpha, r, I filters on isaac newton telescope<BR><BR>Specifically looking for T Tauri through Halpha emissions.  Also includes 2 MASS and Spitzer data but only for T Tauri candidates? Find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)--Peggy Piper 12:47, 21 February 2012 (PST)||http://arxiv.org/pdf/1103.1646v1.pdf
 |-
 | DO THIS<br>[http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran, et al., 2009, A&A, 504, 97B]<br>The stellar population and complex structure of the bright-rimmed cloud ic 1396N||'''Luisa adds''': YES very useful!<br> A study through JHK filters; 736 sources found in all 3 bands (filters); h2 emission shows jet like structure<br><br>'''Peggy adds'''deep survey of IC 1396N in J, H, K′ broadband filters and deep high-angular resolution in the H2 narrowband - Near Infrared Camera Spectrometer (NICS) at the National Telescope Galileo (TNG)  Firenze (Italy). 1010 sources photometry data, but not in all sources in all bandswidths due to lack of overlap.   I'm not sure I understand, but I believe they are saying that with reddening falling in the band of the main sequence and little near infrared excess, there are very few YSOs to be found?<br><br> OF NOTE: came after Getman et al paper, finds contradictory results. Read with Getman et al.||http://arxiv.org/pdf/0902.4543v1.pdf

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 |}
 =Useful figures=

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 =Useful figures=
-[[image:Tr37where.png]] The big square is someone else's (published) thesis data. The big blobby thing next to BRC 36 is ,
+[[image:Tr37where.png]] The big square is someone else's (published) thesis data. The big blobby thing next to BRC 36 is [http://www.spitzer.caltech.edu/images/1058-ssc2003-06b-Dark-Globule-in-IC-1396 this].
 here is a pseudo-3d animation of the ic1396 complex. brc 38 is at the top of the 'ring', one of the less prominent black fingers at the top.
 http://astroanarchy.blogspot.fr/2012/10/an-experimental-3d-animation-from-my.html

@@ Line 143: / Line 143: @@
 =Useful figures=
-[[image:Tr37where.png]]
+[[image:Tr37where.png]] The big square is someone else's (published) thesis data. The big blobby thing next to BRC 36 is ,
 here is a pseudo-3d animation of the ic1396 complex. brc 38 is at the top of the 'ring', one of the less prominent black fingers at the top.
 http://astroanarchy.blogspot.fr/2012/10/an-experimental-3d-animation-from-my.html

← Older revision		Revision as of 16:29, 27 February 2013
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−	here is a pseudo-3d animation of the ic1396 complex. brc 38 is at the top of the 'ring', the less prominent black ~~finger~~ at the top.	+	here is a pseudo-3d animation of the ic1396 complex. brc 38 is at the top of the 'ring', one of the less prominent black fingers at the top.
	http://astroanarchy.blogspot.fr/2012/10/an-experimental-3d-animation-from-my.html		http://astroanarchy.blogspot.fr/2012/10/an-experimental-3d-animation-from-my.html

← Older revision		Revision as of 16:28, 27 February 2013
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	=Useful figures=		=Useful figures=
	[[image:Tr37where.png]]		[[image:Tr37where.png]]
		+
		+
		+	here is a pseudo-3d animation of the ic1396 complex. brc 38 is at the top of the 'ring', the less prominent black finger at the top.
		+	http://astroanarchy.blogspot.fr/2012/10/an-experimental-3d-animation-from-my.html

← Older revision		Revision as of 16:28, 27 February 2013
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		+	=Useful figures=
		+	[[image:Tr37where.png]]

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 | align="center" style="background:#f0f0f0;"|'''URL'''
 |-
-| DO THIS <br>[http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barensten et al., 2011, MNRAS, 415, 103]<br>T tauri candidates and accretion rates using IPHAS: method and application to IC 1396||'''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)
+| DO THIS <br>[http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barentsen et al., 2011, MNRAS, 415, 103]<br>T tauri candidates and accretion rates using IPHAS: method and application to IC 1396||'''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) <br>'''Luisa adds:'''  YES this is a useful paper. data tables of objects they think are young. their shortlist may or may not overlap with the fields we care about in brc 34 and 38, 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 in the regions we care about (34 and 38)<br>'''Peggy adds:''' Includes BRC 38 which is called cloud E; Looking for YSOs in all of 1396; list 158 candidates; uses IPHAS survey data - Halpha, r, I filters on isaac newton telescope<BR><BR>Specifically looking for T Tauri through Halpha emissions.  Also includes 2 MASS and Spitzer data but only for T Tauri candidates? Find increasing accretion rates, disc excesses and younger ages as move away from HD 206267 towards Cloud A (BRC 38 is Cloud E)--Peggy Piper 12:47, 21 February 2012 (PST)  ||http://arxiv.org/pdf/1103.1646v1.pdf
 |-

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 =Potentially Useful Coordinates=
-BRC 38: 21h40m02.2s +58d20m43s
+BRC 38: 21h40m02.2s +58d20m43s (J2000)
 =Prior papers=