C-WAYS Spring work

Big Picture

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 "journal club", a common occurrence in astronomy departments/groups/centers, where the papers are usually selected out of recent astro-ph mailings. We will assemble this list more or less simultaneously as we are writing our proposal.

In practice, there are two kinds of papers in this list -- ones you want to read closely for the astronomy and astrophysics background, for the interpretation, for the big picture... and 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.

Resolution work

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. DUE 3/23 UNLESS EMAIL SAYS OTHERWISE!

Source matching work

C-WAYS source matching work -- still under construction as of 3/16.

Papers to discuss

We will eventually turn this into a nifty table like we did for the BRC Spring work page, but let's collect the papers themselves first, because working with the wiki table format is, frankly, a pain in the @$$.

Note by Babar: I am re-organzing this section. While this note is listed here, the re-organization is not complete.

The relevant papers are sorted into the 4 categories below:

Essential reading

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.	(do with group R)
Rebull et al., 2011, 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)
Rebull et al., 2011, 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)
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)
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
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.
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 this, with group S
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
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.
Choudhury R., Mookerjea, B., Bhatt, H., 2010, ApJ, 717, 1067	BRC 38, including IRAC+MIPS. Have not read this yet! Will need to review in detail. And scavenge any relevant data.	do in detail. scavenge data.
Getman et al. 2007, ApJ, 654, 316	BRC 38. 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. 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. We need to scavenge these data, compare to our results	read closely, at the very least enough to get the data.
Fuente, et al., 2007, A&A, 468L, 37	BRC 38. Looking for protostellar clusters in IC 1396N.
Neri, et al. 2007, A&A, 468, 33	BRC 38. found a cluster of hot cores in 1396N. This might be the same info in article above.
Beltran, et al., 2009, A&A, 504, 97B	BRC 38. this looked for YSOs inside the bright-rimmed cloud of IC 1396N (I believe Luisa referenced this article before)
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

Should read

This group of papers is useful but not essential.

Paper	Comments	Presenter/ present with
Guieu, S., et al., 2010, ApJ, 720, 46 (pdf)	spitzer and optical data to find new YSOs; ic2118	the 2118 paper (from my first teacher team).... we could read this, because our work will look a lot like this, but may be better to focus time and energy on CG4 paper and Taurus with WISE paper.
Sugitani K., Ogura K., 1994, ApJS, 92, 163.	SFO into the S. Hem.	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. Review with other Sugitani, Ogura papers, but can skim the surface.	do w/ group S 1994
Sugitani K., Tamura M., Ogura K., 1995, ApJ, 455, L39.	JHK follow-up	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. Review with other Sugitani, Ogura papers, but can skim the surface.	do w/ group S 1995
Rebull et al., 2011, AJ, 142, 25	Spitzer+optical to find new YSOs; cg4.	this is very close to our analysis, though we will use WISE instead of Spitzer.	discuss among the last, since methodology very similar?
Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 506, 711.	X-rays; brc27 -- using multiple wavelengths and methods to find YSOs	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.	should 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.	Optical; BRC 27 and BRC 34	BRC 27 only. 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 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 "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.	Optical; brc 27	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. Not clear if we need to actually discuss it or not. It's a really old paper.	should read enough to understand and scavenge data.
Additional references from the proposal
Maoz 2007		Astrophysics in a Nutshell (Princeton, NJ)
Nakano et al., 2012, AJ, 143, 61	Media:Nagano_2012.pdf	Wide Field Survey of Emission-line Stars in IC 1396. 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.” Jackie adds:H alpha emission is characteristic of young low mass stars because these emissions are characteristic of T Tauri 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.
Nisini et al., 2001, A&A 376, 553	Multiple H2 protostellar jets in the bright-rimmed globule IC 1396-N	Jets can be HH objects, or can create them. probably useful to scan this in conjunction with some of the other outflow/hh object papers on this list. 1st detection of H2 jets from YSO. Are these HH objects? Lauren adds: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. Evidence suggests that the jets are likely shocked gas along stellar jets. 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. Triggered mechanisms are not favored, due to the ionization front.
Reipurth et al., 2003, ApJ, 123, 2597-2626	Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds	Reipurth et al usually work in Ha or forbidden emission lines to find HH objects. look to see if they have a list of objects in the region we care about, or if this is a more general paper. Herbig-Haro flow (HH 777) found coming out of ic 1396N; located at 214041.6+581638 Jackie adds: IC 1396N were imaged with H alpha and S2 filters and four new HH flows were found, HH 777, 778, 779, and 780. 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. No list of sources is included. (in IR, I think)
Beltran et al., 2002, ApJ, 573, 1	IRAS 21391+5802: The Molecular Outflow and its Exciting source	This is probably worth looking at to see if there is anything point source-y in here. VLA and BIMA observations of dust and gas surrounding IRAS source; 3 sources isolated with BIMA, each a YSO Lauren adds: 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.
Connelley et al., 2006, AJ, 133, 4	Infrared Nebulae around Young stellar objects	Check this to see if there is anything point source-y in here. IRAS 21391+5802 - images show jet-like nebula and large patches of nebulosity Jackie adds: IRAS located a source at 21391+5802 that is 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.
Lynds, 1962, ApJS, 7, 1	The Lynds Dark Nebula paper	POSSIBLY

For the over achievers

Read, if you are motivated to do so.

Paper	Comments	Luisa's notes	Presenter/ present with
Valdettaro R., Migenes V., Trinidad M.A., Brand J., Palla F., 2008, ApJ, 675, 1352.	VLA obs of water masers; BRC 34	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.	scan if you want
Soares J.B., Bica E., 2002, A&A, 388, 172.	OLD 2MASS obs of BRC 27	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 "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 ... good to review?	ok, but not a lot of content beyond the images and their 'big picture' work.	skip?
Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., Mio J., 2004, A&A, 426, 535. note has erratum too.	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. 2004
Morgan L. K., Thompson M. A., Urquhart J. S., White G. J., 2008, A&A, 477, 557.	SCUBA survey	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. 2008
Morgan L. K., Urquhart J. S., Thompson M. A., 2009, MNRAS, 400, 1726.	Radio, mid-ir, SCUBA observations; redefined SFO catalog	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.	read with "Group M" for fig 2. 2009
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
Additional references from the proposal
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

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.

Paper	Comments
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.