Jackie BRC 38

Location of BRC 38

I need a picture in my head. I found these helpful. The first is the one Luisa already put up. The 2nd is from APOD (http://apod.nasa.gov/apod/ap110425.html). The 3rd is from Getman et al. 2006

Information about BRC 38

Bright Rimmed Cloud 38 in IC 1396. Since it is located in the north part of IC 1396 is it often referred to as IC 1396N.
It has a C shape with the southern edge as the brightest part (Pottasch et al. 1956).
Location with intermediate mass protostars, though some (Ogura & Sugitani 1999) suggest there is probably a lot of low mass formation going on too. Wang et al. 2009 believes potential for high mass stars forming here also.
H2 jets found (Saraceno et al. 1996; Nisini et al. 2001)
Herbig-Haro objects found (Repurth et al. 2003
Observed in many wavelengths - it would be good to get the specific wavelengths in each band

optical (IPHAS, several optical - including Yerkes in the 1950s - coming from Chicago I have to cheer!!),

infrared (2MASS,

radio (IRAM & BIMA)

x-ray

Draft Proposal

Bright Rimmed Cloud 38 is located in the H2 region IC 1396. Since it is located in the northern part of IC 1396 is it often referred to as IC 1396N. 
It has a C shape with the southern edge as the brightest part (Pottasch et al. 1956). Ogura et al (2002) mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. Intermediate mass protostars have been found there, though some (Ogura & Sugitani 1999) suggest there is probably a lot of low mass formation going on too. Wang et al. 2009 believes there is also potential for high mass stars formation. 
H2 jets were found (Saraceno et al. 1996; Nisini et al. 2001) 
as well as Herbig-Haro objects (Repurth et al. 2003; Nisini et al 2001). The Infrared Astronomical Satellite (IRAS) located the strongest source at 21391+5802, also known as BIMA 2, 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 (Connelley, et al. 2006). These characteristics indicate this source is young object (Beltran et al 2002).
BRC 38 has been observed with IPHAS, Spitzer, and 2MASS surveys (Barensten et al 2011; Choudhury et al 2010; Beltran et al 2002). A survey with VLA and BIMA (Beltran et al 2002) found three intermediate-mass YSO sources in different stages of evolution. A Chandra x-ray study found over one hundred x-ray sources in IC 1396N using the Chandra ACIS detector (Getman et al. 2006). About a quarter of those are associated with YSOs, representing 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 (Getman et al. 2006).
IRAS 2139+5802 has been studied in the 3.1mm radio wavelength with PdBI, the Plateau de Bure Interferometer. Two areas in IC1396N are distinguished: 1. YSOs at the BIMA 3 location and the protocluster BIMA 2 location seen in dust continuum emission; and 2. filaments and clumps seen in molecular N2H emissions (Fuente et al 2009). BRC 38 has also been observed in H alpha emission, which is characteristic of young low mass stars. Nakano et al (2012) found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they observed.

Students from Walter Payton College Prep High School (WPCP) will participate in NITARP as part of WPCP’s seminar program and will be selected through an application process in April 2012. They will meet weekly to develop their understanding of the content and skills needed to participate in this research opportunity. The NITARP CoolWiki site will be utilized for communication among themselves and among the other schools and scientists in the CWAYS network. Professional Development outreach will given through the educational outreach network at Yerkes Observatory and local and national workshops, such as the Illinois Science Teacher Association and the National Science Teachers Association.

Questions

I am sure there are a lot more!! After fooling around with wiki editing, this is all that is left in my head at present.

1. One IRAS (Infrared Astronomical Satellite) location (IRAS 21391+5802) seems to be the central point or at least this location that keeps coming up. What is this?
2. LWS spectrum - is this as simple as long wavelength?
3. Still unclear on what exactly the following are. I have looked them up but they are not clear in my head - maser, Herbig-Haro objects, FIR colors, MIP colors
4. When we talk about BRC 38, are we talking about the whole C rim and globular area it half encircles? Where does the IRAS source 21391+5802 fit in our picture?
5. Is submillimeter wavelengths (SUBA) infrared or microwave?
6. Is HD 206267 affecting the whole region with its radiation?

Search phrases

• BRC 38
• sfo 38
• 21:40:42+52:16:13
• 21391+5802
• IC 1396N
• Cepheus OB2
• IMYSO

Articles

Author Date	Article Title	Comments	URL
1a. Nakano et al. 2012	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.	Media:Nagano_2012.pdf
1b. saurin et al. 2012	the embedded cluster or assoiciation trumpter 37 in ir 1396	Luisa adds: 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
2.. Barensten et al. 2011	T tauri candidates and accretion rates using IPHAS: method and application to IC 1396	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) 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 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
3. choudhury et al. 2010	Triggered star formation and YSO population in Bright Rimmed SRO 38	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
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
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
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
4. beltran et al. 2009	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?	http://arxiv.org/pdf/0902.4543v1.pdf
Morgan L. K., Urquhart J. S., Thompson M. A., 2009 ON LAST YEAR'S LIST	CO observations towards bright-rimmed clouds	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
5. 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
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
6. Chauhan et al. 2009 ON LAST YEAR'S LIST	Triggered star formation & evolution of t-tauri stars in and around BRC	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
Morgan et al. 2007 ON LAST YEAR'S LIST	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
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
7. Getman et al. 2007	X-ray study of triggered star formation and protostars in IC 1396N	Luisa adds: YES this is useful 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 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
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
8. 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
Valdettaro et al. 2005 ON LAST YEAR'S LIST	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
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
9. 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
10. Ogura, et el 2002 ON LAST YEAR"S LIST	Halpha emission stars and Herbig-Haro objects in and around BRC	Luisa adds: YES this is useful - finding YSOs via Halpha 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. 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
11. 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
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)
12. 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
13. Slysh et al. 1999	Prootoplanetary 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
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
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
14. 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)
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
15. 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
Sugitani et al. 1991 ON LAST YEAR"S LIST	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
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
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