C-CWEL Proposal
Contents
Notional plan ...
1/23 - for this week, read Studying Young Stars, BRC 27+34 paper, CWAYS proposal and bring your questions. HWK from this week: read articles listed for next week, start writing your proposal if you can.
1/30 - for this week read 2013 proposal instructions, Choudhury et al 2010, Sugitani et al 1991, which is the discovery paper for these BRCs (otherwise known as SFOs). Also, How can I find out what scientists already know about a particular astronomy topic or object? and I'm ready to go on to the "Advanced" Literature Searching section..There is even a screencapture movie if you want (from the CWAYS team) ... On telecon, talk about these reading assignments and how to search for recent papers using Simbad and ADS. HWK from this week : start writing your proposal, look for new papers on this region that the last group missed or that came out in the past 12 months. I am in the process of collecting the list of papers that the last group weeded for us, and will copy that below.
2/6 - For this week, bring questions on the prior reading and/or your proposal drafts, and any new papers that you find.
2/13 - Luisa will be in Boston, and I think Wendi too (we will be here); you can have a telecon without us, of course ...
2/20 - talk about any questions and issues about proposals
FRIDAY 2/22 - send around your proposal draft to rest of the group
2/27 - read everyone's proposal draft and come with questions and comments. someone (john?) will be given the assignment of merging the best of everything and sending it around within a few days.
3/6 - review nearly final proposal
FRIDAY 3/8 - proposal due
Potentially Useful Coordinates
BRC 38: 21h40m02.2s +58d20m43s (J2000)
Prior papers
This was Jackie's list before, when she was sorting out BRC 38 : Jackie BRC 38
This was our list of "most important" literature last spring: C-WAYS_Spring_work#Papers_to_discuss
Do these or scan these
| Author/Date/Title | Comments | URL |
| DO THIS Barentsen et al., 2011, MNRAS, 415, 103 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) |
http://arxiv.org/pdf/1103.1646v1.pdf |
| DO THIS Beltran, et al., 2009, A&A, 504, 97B The stellar population and complex structure of the bright-rimmed cloud ic 1396N |
Luisa adds: YES very useful! A study through JHK filters; 736 sources found in all 3 bands (filters); h2 emission shows jet like structure Peggy addsdeep 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? OF NOTE: came after Getman et al paper, finds contradictory results. Read with Getman et al. |
http://arxiv.org/pdf/0902.4543v1.pdf |
| scan Beltran et al. 2002 IRAS 21391+5802: The Molecular Outflow and its Exciting source |
Luisa adds: 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. |
http://arxiv.org/pdf/astro-ph/0203206v1.pdf |
| DO THIS Chauhan et al. 2009 Triggered star formation & evolution of t-tauri stars in and around BRC |
BRC 27, 38. Optical (BVIc)+2mass+spitzer/irac. This one was really important for brc27, it's less so for brc 38; we need to see what they say about brc38. 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, 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!! they are a bit of a mess in brc27, probably relying on choudhury et al. for brc 38, which should be fine. Luisa adds: YES this is a useful paper -- they are using JHK to select YSOs and including IRAC (but not MIPS) in their assessment of youth. we will be using longer-wavelength infrared to find the objects, so we will find a different set of objects. (ps they also didn't do that hot a job with source matching to the literature. we can do better.) Study that looked at ages of star forming clusters. Seems to have a lot of background material on BRC 38. Jackie adds: 2MASS and Spitzer-IRAC data was used to support BVIc observations. 18 YSOs were observed and analyzed. There is an age gradient, with younger stars on the inside of the rim or on the rim itself and older stars outside of it. |
2009, MNRAS, 396, 964 |
| DO THIS Choudhury et al. 2010 Triggered star formation and YSO population in Bright Rimmed SFO 38 |
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. Luisa adds: YES this is useful, if for no other reason than they used the Spitzer data. they definitely have data tables too. 44 YSOs identified in brc 38 - evidence for radiation driven implosion (RDI); spitzer IRAC & MIPS data, optical BVRI Peggy adds: Spitzer IRAC and MIPS (3.5 to 24 um) colors and Ha ID 45 YSO adn 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 acretion rates 10-10 to 10-8 Mo/yr, not spacially semetric WRT HD 20626. concentration of YSOs closer to southern rim, evolutionary sequence seen with class II at the rim. Two different patterns of alignment towrd 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://arxiv.org/pdf/1005.1841v1.pdf |
| scan! Connelley et al. 2006 Infrared Nebulae around Young stellar objects |
Luisa adds: 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. |
http://arxiv.org/pdf/astro-ph/0611634v1.pdf |
| DO THIS Getman et al. 2007, ApJ, 654, 316 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. |
http://arxiv.org/pdf/astro-ph/0607006v2.pdf |
| scan 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 enough to get the idea; you can skip the rest if you want. Do with Koenig et al. 2012. | |
| scan 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 | |
| DO THIS Nakano et al., 2012, AJ, 143, 61 Wide Field Survey of Emission-line Stars in IC 1396 |
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). 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. |
Media:Nagano_2012.pdf |
| scan Nisini et al. 2001 Multiple H2 protostellar jets in the bright-rimmed globule IC 1396-N |
Luisa adds: 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. |
A&A 376, 553{560 |
| DO THIS Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. 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. Luisa adds: YES this is useful - finding YSOs via Halpha |
http://iopscience.iop.org/1538-3881/123/5/2597/pdf/201506.web.pdf |
| DO THIS 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. | |
| DO THIS Rebull et al., 2011b, ApJS, 196, 4 |
(I gave you hard copy of this one at the AAS.) our paper looking for new YSOs in Taurus using WISE. 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. | |
| scan. Reipurth et al. 2003 Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds |
Luisa adds: 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) |
2002, ApJ, 123:2597-2626 |
| DO THIS Sugitani et al. 1991 |
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. A catalog of BRC with iras point sources Luisa adds: discovery paper of BRCs, but no source lists of individual YSOs in the region. you guys should've read this already, but not relevant to the assembly of previously known YSOs in the region. Just a list of point sources they invesigated - brc 38 on the list Part of Luisa's old notes: 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. |
1991, ApJS, 77, 59 |
Drop these; keep the list here so you can compare to what you find on simbad or ADS
| Author/Date/Title | Comments | URL |
| drop Saurin et al. 2012 the embedded cluster or assoiciation trumpter 37 in ir 1396 |
Luisa says: no individual data tables to use; they are interested in statistical properties of the regions. good 'big picture' kind of thing, but no real use for us in terms of our specific project. Peggy adds: 2MASS observations of BRC 38, Primary focus Trumpler 37, but analyzed 2Mass photometry of 11 BRCs in IC 1396 including BRC 38. All associated with IRAS sources (prob protostars) massive nearby star HR 8281 may have triggered sequential star formation via winds and UV. Photometric errors </= 0.1 mag removed for stars less than 0.5 arcmin radius for BRC 38 b/c high absorption? Relatively high central densities = small star clusters. Getman et al 2007 found sequential star formation evidence for BRC 38, spatial gradient stellar age in direction to triggering star as well as YSOs. BRC 38 stellar mass of ~15Mo assumed representative of area. Lists ra/dec, angular and linear dist to HR 8281 --Peggy Piper 12:23, 21 February 2012 (PST) |
http://arxiv.org/pdf/1201.2704.pdf |
| drop. Morgan et al. 2010 Ammonia observations of bright-rimmed clouds: establishing a sample of triggered protostars |
Luisa adds: Radio. ignore at least for now Radio observations (Green Bank) of brcs; furthering earlier work of morgan, confirming brc is triggered star formation site |
http://arxiv.org/pdf/1006.0833v1.pdf |
| drop. Crimier et al. 2010 Physical structure of the envelopes of intermediate-mass protostars |
Luisa adds: too theoretical. ignore. a study that says that the mass of the final star of a protostar is linked to the mass of the envelope around the protostar, not the density of the parent cloud - backbground on IM protostars?? |
http://arxiv.org/pdf/1005.0947v1.pdf |
| drop. Ogura 2010 Triggered star formation assoicated with HII regions |
Luisa adds: overview. conference proceedings. meat of this analysis already in other journal articles, i am pretty sure. ignore for now. Not really about BRC 38 but discusses curent state of triggered star formation theory |
ASI Conference Series, 2010, Vol 1, pp 19-25 |
| drop. Morgan L. K., Urquhart J. S., Thompson M. A., 2009 CO observations towards bright-rimmed clouds |
on 2011 list. Luisa adds: Radio. ignore at least for now Luisa's old notes: 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. |
2009, MNRAS, 400, 1726 |
| drop (probably) fuente et al. 2009 Dissecting an intermediate-mass (IM) prostar |
luisa adds: hm. very narrowly focused paper, seems to be just on one object and radio. was ready to say ignore it, but it is probably worth a quick skim to see if they mention anything substantive about the 'YSO BIMA 3' and 'cluster BIMA 2' mentioned in the abstract. A look at IRAS 21391+5802 emissions of N2H+, CH3CN, CS, BIMA (1.2mm & 3.1mm) Jackie adds: IRAS 2139+5802 studied in radio wavelengths (PdBI – Plateau e Bure Interferometer) 3.1mm. Results were compared with older PdBI data (Neri et al. 2007) and BIMA data (Beltran et al 2002). Two areas in IC1396N are distinguished – 1. YSOs BIMA 3 and the protocluster BIMA 2 seen in dust continuum emission and 2. Filaments and clumps seen in molecular emission (N2H+). Interestingly, they claim the ratio of [CH3CN] / [N2H+] is related to the spectral type of the star being formed because the ratio is a good measure of gas kinetic temperature. |
http://arxiv.org/pdf/0909.2267v1.pdf |
| drop. Wang et al. 2009 The relation between 13CO j=2-1 line width in moelcular clouds and bolometric luminosity of associated IRAS sources |
Luisa adds: Radio. ignore at least for now IRAS 21391+5802 - suggests that it is a star forming cluster where high-mass stars will form |
http://arxiv.org/pdf/0909.3312v1.pdf |
| drop. Morgan et al. 2007 A scuba survey of BRC |
Luisa adds: Radio. ignore at least for now BRC 38 included in this study with SUBA data (submillimeter - microwave??); Luisa's notes: 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. |
2008, A&A, 477, 557 |
| drop. Neri et al. 2007 The IC 1396N proto-cluster at a scale of ~250 AU |
Luisa adds: radio. ignore for now at least. observations in millimeter range to help develop understanding of formation of clusters vs individual star formation |
http://arxiv.org/pdf/0705.2663v1.pdf |
| drop. Patel et al. 2007 Submillimeter array observations of 321 ghz water maser emission in cepheus a |
Luisa adds: Radio. ignore at least for now No don\'t think there is anything here |
http://arxiv.org/pdf/astro-ph/0702696v1.pdf |
| drop. Valdettaro et al. 2005 h2o maser emission from bright rimmed clouds in the northern hemisphere |
Luisa adds: Radio. ignore at least for now H2O maser studied in brc 38; points to paper Valdettaro et al. 2005b which is supposed to be about analysis of BRC 38. Luisa's old notes: 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. |
2005, A&A, 443, 535 |
| drop. Beltran et al. 2004 The dense moelcular cores in IRAS 21391 +5802 region |
Luisa adds: 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 |
http://arxiv.org/pdf/astro-ph/0407102v1.pdf |
| drop. Codella et al. 2001 Star formation in the BRC of IC 1396N |
Luisa adds: radio. ignore for now. The density of several different molecular outflows (dense areas of particular molecules)in the globule looked at with 30m IRAM and OVRO interferometer. Demonstrates this area very complex. |
Astron. Astrophys., 376, 271-287 (2001) |
| drop. Slysh et al. 1999 Protoplanetary disk and/or bipolar outflow traced by h2o masers in ic 1396n |
Luisa adds: theoretical papers you can probably ignore. did not look at background discussion, but don't let me stop you if you are motivated! Description of 3 models that may explain how masers form; Gives background on IC 1396 Lauren adds: I agree with Luisa, and if there's time - I'll read it more thoroughly. |
http://iopscience.iop.org/0004-637X/526/1/236/pdf/39770.web.pdf |
| drop. Ogura & Sugitani 1999 A large number of Halpha Emission Stars associated with BRCs |
Luisa adds: conference proceedings, old at that. i'm sure this analysis is already written up in their later papers. ignore this one. Supports \"small-scale sequential star formation\"; suggests low-mass stars formating in area of high-mass star forming area |
Proceedings of Star Formation, 1999, pg 381-382 |
| drop. Sugitani et al. 1999 Small-Scale Sequential Star Formtion in Bright-Rimmed Clouds |
Luisa adds: conference proceedings, old at that. i'm sure this analysis is already written up in their later papers. ignore this one. Discussion of small-scale sequential star formation hypothesis |
Proceedings of Star Formation, 1999, pg 358-364 |
| drop. Saraceno et al. 1996 LWS observations of the bright-rimmed globule IC 1396N |
Luisa adds: LWS is defintiely from ISO, which was a European ir mission prior to spitzer. spectrum of co, oh, h2o are detected in the ISO-LWS spectrum - not sure what that is?? Lauren adds: 1st far IR spectrum of the IRAS source associated with IC 1396N. About 16 pc from O6 star HD 206267. The 1396 region is about 750 pc away, RDI mechanism, 10 thousand years ago. ISO satellite collected spectra in 1996 with the LWS spectrometer – yeah – I don’t know what they’re actually trying to describe in this article – seems that they think they may have made an error in determining a geometry of something - but then, I am still so steep in the learning curve that reality has taken a rather interesting “slant”… |
Astron. Astrophys. 315, L293–L296 (1996) |
| drop. Saraceno et al. 1996 An evolutionary diagram for young stellar objects |
Luisa adds: deep, DEEP background, IGNORE THIS. background - but not sure I understand it |
Astron. Astrophys, 309, 827-839 |
| drop at least for now. Weikard et al. 1996 the structure of the IC 1396 region |
Luisa adds: seems like this would be useful. Discussion of structure of 1c 1396 and the central star O6.5 (HD 206267) radiation on clumping and structure/location of yso; shows locations of yso in brc 38 from their data Lauren adds: Observational data taken with: Nagoya 4 meter millimeter wave telescope; POM-2 2.5 meter millimeter telescope;KOSMA 3 meter sub-millimeter radio telescope; with reduction data in: CO, H 1 and IRAS Conclusion states that a nearby strong heating source is indicated. |
Astron. Astrophys, 309, 581-611 |
| drop Sugitani et al. 1989 Star formation in bright-rimmed globules: evidence for radiation-driven implosion |
Luisa adds: this sets up their subsequent work. you can safely ignore this. Argument for rdiation-driven implosion method of star formation. |
1989, ApJ, 342:L87-90 |
| drop Pottasch et al. 1956 a study of bright rims in diffuse nebulae |
Luisa adds: so old that not really useful for assembling list of YSOs in region. skip. Early work describing the location, shape of, density of, brightness of bright rim clouds in several nebula, including IC 1396 and Brc 38 |
Bulletin of Astro. Instit. of the Netherlands, Vol 13, 471, 77-88 |
| drop? 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! | |
| drop? Rebull et al., 2011a, AJ, 142, 25 |
our paper from the CG4+Sa101 team (a NITARP 2009 team) 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.) |
Cleaner list of papers with data in BRC 38
- 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.
Useful figures
The big square is someone else's (published) thesis data. The big blobby thing next to BRC 36 is 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
