C-CWEL Journal Club - Revision history

Rebull at 23:54, 3 April 2013

2013-04-03T23:54:41Z

Rebull at 19:25, 7 March 2013

2013-03-07T19:25:11Z

Rebull at 19:22, 7 March 2013

2013-03-07T19:22:46Z

Rebull at 19:21, 7 March 2013

2013-03-07T19:21:42Z

Rebull at 19:19, 7 March 2013

2013-03-07T19:19:37Z

Rebull at 18:15, 7 March 2013

2013-03-07T18:15:25Z

Rebull at 18:15, 7 March 2013

2013-03-07T18:15:07Z

Rebull at 00:59, 7 March 2013

2013-03-07T00:59:45Z

Rebull: Created page with "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 fol..."

2013-03-07T00:36:35Z

Created page with "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 fol..."

New page

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 ...
*I don't understand this ...
*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!

@@ Line 29: / Line 29: @@
 =Papers for journal club=
 (out of the "papers with data" above, but with more notes and clumping)
 {| {{table}}
 {| border="1"

@@ Line 35: / Line 35: @@
 | align="center" style="background:#f0f0f0;"|'''Week'''
 |-
-| [http://adsabs.harvard.edu/abs/2002AJ....123.2597O Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.]<br> Halpha ||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.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. If you have any lingering questions about Sugitani et al. 1991, ApJS, 77, 59, let's bundle them into this week.
+| [http://adsabs.harvard.edu/abs/2002AJ....123.2597O Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.]<br> Halpha ||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.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. '''If you have any lingering questions about Sugitani et al. 1991, ApJS, 77, 59, let's bundle them into this week.'''
 |  JC 1
 |-
@@ Line 57: / Line 57: @@
 |-
 |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K, Koenig et al., 2012, ApJ, 744, 130]<br> WISE selection mechanism
-|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 REALLY JUST want the selection mechanism). Should read the appendix closely; skip the rest. Do with Gutermuth et al 2008 if you are motivated.
+|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 REALLY JUST want the selection mechanism). Should read the appendix closely; skip the rest. Do with Gutermuth et al 2008 if you are motivated. '''If you have any lingering questions about my Taurus paper or my BRC 27+34 paper, bring them this week.'''
 |JC 6 - JUST APPENDIX
 |-
 |}

@@ Line 51: / Line 51: @@
 |-
 | [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barentsen et al., 2011, MNRAS, 415, 103]<br>IPHAS (r,i,Ha) ||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 field we care about in brc 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 (or if we can't get to it for the region), i will email these guys and ask for source lists at least in the region we care about. 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)
-|JC 5
+|JC 5 WITH NEXT
 |-
 | [http://adsabs.harvard.edu/abs/2012AJ....143...61N, Nakano et al., 2012, AJ, 143, 61]<br>r,i,Halpha, akari|| 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 region we care about. Nakano reports a total of 639 Hα emission-line stars were detected in an area of 4.2 deg2 and their i′-photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H ii region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H ii region. H alpha emission is characteristic of young accreting low mass stars. They found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they saw. They suggest the primary mode of star formation in IC 1396 is the birth of low-mass stars associated with bright rims. Data charts and images showing locations included.
-|JC 5
+|JC 5 WITH PRIOR
 |-
 |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K, Koenig et al., 2012, ApJ, 744, 130]<br> WISE selection mechanism

@@ Line 33: / Line 33: @@
 | align="center" style="background:#f0f0f0;"|'''Author/Date/Title'''
 | align="center" style="background:#f0f0f0;"|'''Comments'''
-| align="center" style="background:#f0f0f0;"|'''Person/week'''
+| align="center" style="background:#f0f0f0;"|'''Week'''
 |-
 | [http://adsabs.harvard.edu/abs/2002AJ....123.2597O Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.]<br> Halpha ||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.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. If you have any lingering questions about Sugitani et al. 1991, ApJS, 77, 59, let's bundle them into this week.
-|  JC week 1 -
+|  JC 1
 |-
 | [http://adsabs.harvard.edu/abs/2007ApJ...654..316G Getman et al. 2007, ApJ, 654, 316]<br>X-rays in BRC38 ||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.  The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found.
+| JC 2
 |-
 | [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran, et al., 2009, A&A, 504, 97B]<br>deep JHK|| JHK filters; 736 sources found in all 3 bands (filters); h2 emission shows jet like structure. 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 bands due to lack of overlap.   OF NOTE: came after Getman et al paper, finds contradictory results. Read with Getman et al.
+|JC 3
 |-
 | [http://adsabs.harvard.edu/abs/2010ApJ...717.1067C Choudhury et al. 2010]<br>Optical, spitzer||Includes 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. 44 YSOs identified in brc 38 - evidence for radiation driven implosion (RDI); Spitzer IRAC & MIPS data, optical BVRI. 13 probable pre-main sequence. ground optical photometric and spectroscopy give estimates of ages between 1-8 Myr, median 3Myr, mass .3-2.2 Mo, median 0.5 Mo, mass accretion rates 10-10 to 10-8 Mo/yr, not spatially symmetric WRT HD 20626.  concentration of YSOs closer to southern rim, evolutionary sequence seen with class II at the rim.  Two different patterns of alignment toward HD 206267 and HD 206773. IRAC-MIPS color composite, Plot of RA/Dec, color-color diagrams, sample spectra, SEDs, photometry table, spectral classification table.
+| JC 4 WITH NEXT
 |-
-| [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C Chauhan et al. 2009] <br> optical, spitzer ||Mostly BRC 27, need to see if they are adding new data to Choudhury's tables for BRC 38.  Optical (BVIc)+2mass+spitzer/irac.  Testing small-scale sequential star formation suggested in their earlier 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. 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!! They are a bit of a mess in brc27, probably relying on choudhury et al. for brc 38, which should be fine.
+| [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C Chauhan et al. 2009] <br> optical, spitzer ||Mostly BRC 27, need to see if they are adding new data to Choudhury's tables for BRC 38. IN YOUR READING, FOCUS ON JUST BRC 38 STUFF!! Optical (BVIc)+2mass+spitzer/irac.  Testing small-scale sequential star formation suggested in their earlier 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. 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!! They are a bit of a mess in brc27, probably relying on choudhury et al. for brc 38, which should be fine.
+| JC 4 WITH PRIOR, and JUST BRC 38 stuff.
 |-
 | [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B  Barentsen et al., 2011, MNRAS, 415, 103]<br>IPHAS (r,i,Ha) ||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 field we care about in brc 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 (or if we can't get to it for the region), i will email these guys and ask for source lists at least in the region we care about. 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)
+|JC 5
 |-
 | [http://adsabs.harvard.edu/abs/2012AJ....143...61N, Nakano et al., 2012, AJ, 143, 61]<br>r,i,Halpha, akari|| 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 region we care about. Nakano reports a total of 639 Hα emission-line stars were detected in an area of 4.2 deg2 and their i′-photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H ii region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H ii region. H alpha emission is characteristic of young accreting low mass stars. They found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they saw. They suggest the primary mode of star formation in IC 1396 is the birth of low-mass stars associated with bright rims. Data charts and images showing locations included.
+|JC 5
 |-
 |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K, Koenig et al., 2012, ApJ, 744, 130]<br> WISE selection mechanism
-|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?
+|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 REALLY JUST want the selection mechanism). Should read the appendix closely; skip the rest. Do with Gutermuth et al 2008 if you are motivated.
 |-
 |}

@@ Line 13: / Line 13: @@
 =Papers with data we need=
 (chronological order)
-*Ogura et al. 2002 - COORD NEED UPDATING, but CWAYS did this for you. Probably good to at least take a quick look at these, just in case. there are finding charts.
+*Ogura et al. 2002 - optical - COORD NEED UPDATING, but CWAYS did this for you. Probably good to at least take a quick look at these, just in case. there are finding charts.
-*Getman et al. 2007 - x-rays. got all tables. includes all relevant results from Nisini et al. coord ok because they are from Chandra. Good to remember that Chandra's PSF changes the further you go off-axis - objects on the edge of the Chandra field are much poorer resolution than near the center.
+*Getman et al. 2007 - x-rays. includes all relevant results from Nisini et al. coord ok because they are from Chandra. Good to remember that Chandra's PSF changes the further you go off-axis - objects on the edge of the Chandra field are much poorer resolution than near the center.
-*Beltran et al. 2009 - NIR. got all tables. coord should be ok.
+*Beltran et al. 2009 - NIR.  coord should be ok.
-*Choudhury et al. 2010 - IRAC, MIPS, optical. got all tables. coord should be ok.
+*Choudhury et al. 2010 - IRAC, MIPS, optical. coord should be ok.
-*Chauhan et al. 2009 - BVI, NIR, IRAC. coord ok. though some inconsistencies. NEED TO CHECK FOR BRC 38. got all tables.
+*Chauhan et al. 2009 - BVI, NIR, IRAC. coord ok. though some inconsistencies. NEED TO CHECK FOR BRC 38.
-*Barentsen et al. 2011 - optical (r,i,Ha). coord ok. got all tables. Would be nice to get table of everything in region we care about, not just that which they are reporting on. Need to go to main IPHAS archive.
+*Barentsen et al. 2011 - optical (r,i,Ha). coord ok. Would be nice to get table of everything in region we care about, not just that which they are reporting on. Need to go to main IPHAS archive.
-*Nakano et al. 2012 - optical (r,i,Ha); IR (AKARI). coord ok. got all tables, i think. Might as well go and get table from AKARI of everything in the region, though I think WISE will be more powerful.
+*Nakano et al. 2012 - optical (r,i,Ha); IR (AKARI). coord ok. Might as well go and get table from AKARI of everything in the region, though I think WISE will be more powerful.
-*Koenig et al., 2012, ApJ, 744, 130 - appendix for selection mechanism?
+*Koenig et al., 2012, ApJ, 744, 130 - appendix for selection mechanism.
 Papers I'm assuming you've already read and thought about, which we will NOT explicitly schedule for journal club.
-*Sugitani et al. 1991, ApJS, 77, 59 - SFO - discovery paper for BRCs
+*Sugitani et al. 1991, ApJS, 77, 59 - SFO - discovery paper for BRCs (though bring any questions to JC week 1)
-*Rebull et al. 2011, ApJS, 196, 4 - I gave you a copy of this at the AAS - me, using WISE data to find new Taurus members
+*Rebull et al. 2011, ApJS, 196, 4 - I gave you a copy of this at the AAS - me, using WISE data to find new Taurus members (though bring any questions to JC week 6)
-*Rebull et al. 2013, AJ, 145, 15 - I ve you a copy of this at the AAS - me, with 2011 NITARP team, using Spitzer in BRC 27 and 34.
+*Rebull et al. 2013, AJ, 145, 15 - I gave you a copy of this at the AAS - me, with 2011 NITARP team, using Spitzer in BRC 27 and 34.(though bring any questions to JC week 6)
 =Papers for journal club=

← Older revision		Revision as of 00:59, 7 March 2013
Line 9:		Line 9:

	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!		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!
		+
		+
		+	=Papers with data we need=
		+	(chronological order)
		+	*Ogura et al. 2002 - COORD NEED UPDATING, but CWAYS did this for you. Probably good to at least take a quick look at these, just in case. there are finding charts.
		+	*Getman et al. 2007 - x-rays. got all tables. includes all relevant results from Nisini et al. coord ok because they are from Chandra. Good to remember that Chandra's PSF changes the further you go off-axis - objects on the edge of the Chandra field are much poorer resolution than near the center.
		+	*Beltran et al. 2009 - NIR. got all tables. coord should be ok.
		+	*Choudhury et al. 2010 - IRAC, MIPS, optical. got all tables. coord should be ok.
		+	*Chauhan et al. 2009 - BVI, NIR, IRAC. coord ok. though some inconsistencies. NEED TO CHECK FOR BRC 38. got all tables.
		+	*Barentsen et al. 2011 - optical (r,i,Ha). coord ok. got all tables. Would be nice to get table of everything in region we care about, not just that which they are reporting on. Need to go to main IPHAS archive.
		+	*Nakano et al. 2012 - optical (r,i,Ha); IR (AKARI). coord ok. got all tables, i think. Might as well go and get table from AKARI of everything in the region, though I think WISE will be more powerful.
		+	*Koenig et al., 2012, ApJ, 744, 130 - appendix for selection mechanism?
		+
		+	Papers I'm assuming you've already read and thought about, which we will NOT schedule for journal club.
		+	*Sugitani et al. 1991, ApJS, 77, 59 - SFO - discovery paper for BRCs
		+	*Rebull et al. 2011, ApJS, 196, 4 - I gave you a copy of this at the AAS - me, using WISE data to find new Taurus members
		+	*Rebull et al. 2013, AJ, 145, 15 - I ve you a copy of this at the AAS - me, with 2011 NITARP team, using Spitzer in BRC 27 and 34.
		+
		+	=Papers for journal club=
		+	(out of the "papers with data" above, but with more notes and clumping)
		+	{\| {{table}}
		+	{\| border="1"
		+	\| align="center" style="background:#f0f0f0;"\|'''Author/Date/Title'''
		+	\| align="center" style="background:#f0f0f0;"\|'''Comments'''
		+	\| align="center" style="background:#f0f0f0;"\|'''Person/week'''
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2002AJ....123.2597O Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597.]<br> Halpha \|\|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. They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs.
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2007ApJ...654..316G Getman et al. 2007, ApJ, 654, 316]<br>X-rays in BRC38 \|\|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. The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found.
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran, et al., 2009, A&A, 504, 97B]<br>deep JHK\|\| JHK filters; 736 sources found in all 3 bands (filters); h2 emission shows jet like structure. 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 bands due to lack of overlap. OF NOTE: came after Getman et al paper, finds contradictory results. Read with Getman et al.
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2010ApJ...717.1067C Choudhury et al. 2010]<br>Optical, spitzer\|\|Includes 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. 44 YSOs identified in brc 38 - evidence for radiation driven implosion (RDI); Spitzer IRAC & MIPS data, optical BVRI. 13 probable pre-main sequence. ground optical photometric and spectroscopy give estimates of ages between 1-8 Myr, median 3Myr, mass .3-2.2 Mo, median 0.5 Mo, mass accretion rates 10-10 to 10-8 Mo/yr, not spatially symmetric WRT HD 20626. concentration of YSOs closer to southern rim, evolutionary sequence seen with class II at the rim. Two different patterns of alignment toward HD 206267 and HD 206773. IRAC-MIPS color composite, Plot of RA/Dec, color-color diagrams, sample spectra, SEDs, photometry table, spectral classification table.
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2009MNRAS.396..964C Chauhan et al. 2009] <br> optical, spitzer \|\|Mostly BRC 27, need to see if they are adding new data to Choudhury's tables for BRC 38. Optical (BVIc)+2mass+spitzer/irac. Testing small-scale sequential star formation suggested in their earlier 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. 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!! They are a bit of a mess in brc27, probably relying on choudhury et al. for brc 38, which should be fine.
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al., 2011, MNRAS, 415, 103]<br>IPHAS (r,i,Ha) \|\|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 field we care about in brc 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 (or if we can't get to it for the region), i will email these guys and ask for source lists at least in the region we care about. 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)
		+	\|
		+	\|-
		+	\| [http://adsabs.harvard.edu/abs/2012AJ....143...61N, Nakano et al., 2012, AJ, 143, 61]<br>r,i,Halpha, akari\|\| 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 region we care about. Nakano reports a total of 639 Hα emission-line stars were detected in an area of 4.2 deg2 and their i′-photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H ii region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H ii region. H alpha emission is characteristic of young accreting low mass stars. They found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they saw. They suggest the primary mode of star formation in IC 1396 is the birth of low-mass stars associated with bright rims. Data charts and images showing locations included.
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		+	\|[http://adsabs.harvard.edu/abs/2012ApJ...744..130K, Koenig et al., 2012, ApJ, 744, 130]<br> WISE selection mechanism
		+	\|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?
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