CoolWiki - User contributions [en]

C-CWEL Summer visit logistics

2013-07-02T22:11:47Z

Gibbs: /* Travel Logistics */

=High-level schedule=

The work days we've agreed upon are Aug 5-8, where there will be minimal help from me on Aug 8 as sort of a "training run" for when you go home.

I propose you come in relatively early on Aug 4, and plan on doing dinner at my house that night.

*Sunday morning/early afternoon - arrive in LA
*Sunday night - pizza party at Luisa's ... pizza arrives at 6. come by 5 or 5:30 if you want to play with Andrew!
*Monday morning 8:30?-12? - tour of SSC (with Ciardi's team), meet Wannetta and Andrea, lectures
*Monday afternoon 1-5 - software setup. WISE archive workthrough. Start to work with mosaics.
*Tuesday all day - hands-on work with computers, make progress on data
*Wednesday morning - JPL tour??
*Wednesday afternoon - wrapup, plan for when you go home
*Thursday morning - Luisa to stay out of your hair most of the day. Work on your own or small groups. Try to do some of the tasks we did as a group. Compare notes. Can you work on your own at home without me?
*Thursday afternoon - Reconvene for any questions and help, discussion, etc.
*Friday - return home

=Software to install=

Make sure you (and all your students who are coming) '''each''' have a '''functional laptop''' that you know how to use with as much of the relevant software installed as possible well before you get on the plane. Trust me. Makes it '''much''' easier if you do all this ahead of time, including starting it up to make sure it works.
*[http://hea-www.harvard.edu/RD/ds9/ ds9]
*[http://aperturephotometry.org APT]
*a web browser (Firefox, Safari, or Google Chrome -- NOT MICROSOFT INTERNET EXPLORER)
*Excel or other spreadsheet program (Google Docs is ok if your school lets you access it; most of the rest of us will be working with various versions of Excel)

'''Also''' make sure you have all the passwords you need for installing new software, getting on a wireless network, or getting back into your machine if it reboots.

Besides the computer, you will need something to write on and something to write with to take notes! Experience has shown that this should be more than post-it notes. I will give you handouts, so the hyperorganized among you may want, e.g., a 3-ring binder.

'''UPDATE JULY 2, 2013:'''
You should also copy to your laptop your POSS and IRAS images covering about 20 arcminutes from your Resolution worksheet work. This will save you a few minutes in August.

=Travel Logistics=
*John Gibbs: +4 students (1 girl, 3 boys) -> 3 rooms
*Wendi Laurence: +1 kid (her son)
*Robert Marshall: no kids
*Michael Murphy: +4 students (2 girls, 2 boys) -> 3 rooms
*Laura Orr: +2 students (boys) -> 2 rooms
*Christi Whitworth: no kids

11 rooms total.

17 people (not including Luisa)

Connecting flight information:
*John Gibbs: ~3pm, BUR
*Wendi Laurence:
*Robert Marshall: LAX midafternoon
*Michael Murphy: LAX
*Laura Orr: ~3pm, BUR
*Christi Whitworth: ~10:30am LAX

C-CWEL Spring Calendar

2013-03-13T22:15:35Z

Gibbs:

In general, if we're missing only one person, even me, just fine to hold meeting if needed! If we are missing >1, then it becomes a judgement call as to whether or not to hold the meeting.

*March 13 - NO TELECON - Luisa out
*March 20 - NO TELECON - Robert out, Wendi may be out - IASC tutorial so we're trumped anyway. If you have time and inclination, go listen to that, or the ds9 tutorial from January. We will be using ds9, so you might as well get up to speed...
*March 27 - Review of our as-submitted proposal, along with (hopefully) comments from reviewers. Read [[C-CWEL Source Matching Work]] in prep for this, discuss it here.
*April 3 - '''Journal Club #1''' (Wendi) - Ogura et al. 2002. In real time (using join.me or something else), check last few sources that CWAYS said didn't have matches to verify. Start assembling "Wendi's table" of all data sources; add to this table at the end of each JC week.
*April 10 - NO TELECON? - Robert, Wendi at NSTA in TX; Christi out
*April 17 - '''Journal Club #2''' (Mike) - Getman et al. 2007
*April 24 - NO TELECON? - Wendi out. Luisa out.
*May 1 - NO TELECON? - Luisa out.
*May 8 - '''Journal Club #3''' (Robert) - Beltran et al. 2009
*May 15 - (Robert might be out?) - '''Journal Club #4''' (Larua) - Choudhury et al 2010 and JUST THE BRC 38 portion of Chauhan et al. 2009
*May 22 - '''Journal Club #5''' (Christi) - Barentsen et al. 2011 and Nakano et al 2012.
*May 29 - '''Journal Club #6''' (John) - JUST APPENDIX of Koenig et al. 2012 (not Robert, big deadlines at his end?)
*June 5 - JC overflow or [[C-CWEL Resolution Worksheet]] - Source Resolution Work #1
*June 12 - [[C-CWEL Resolution Worksheet]] - Source Resolution Work #1 or 2
*June 19 - Source Resolution Work #2/overflow
*June 26 - tbd

BRC Proposal

2011-02-27T05:26:12Z

Gibbs:

=Instructions=

[[2011 proposal instructions]]

=Background on Star Formation=

STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.

[http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]

Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]

A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]
--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)

=Target Selection=

STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.

The list of sources that Lori suggests we consider are here:
*[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE
*[[target selection for brc36]] 21h35m32.6s +57d31m50s
*[[target selection for brc31]] 20h50m43.4s +44d21m53s
*[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]

*[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE

Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about <s>30'</s> 10' of these positions.

Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]

CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like "we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated."

papers from discussion on the phone 16:35, 23 February 2011 (PST)
*[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with "sfo 38" http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
*[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M

----

=STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=

=Introduction/Background=

the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)

http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=1655856
Proceedings of the International Astronomical Union (2007), 3: 164-165
DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008
Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda
--[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)

A&A 388, 172-178 (2002)
DOI: 10.1051/0004-6361:20020451
The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1
J. B. Soares and E. Bica
Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

A&A 426, 535-545 (2004)
DOI: 10.1051/0004-6361:20040226
A radio and mid-infrared survey of northern bright-rimmed clouds
L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao

Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK
--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

'''Science Background and Context: Star Formation'''

Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of numerous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.

Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenssa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d < 1.2 kpc, finding young stellar objects in 75% of the clouds they studied.

Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.

--[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)

BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)

BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui & Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura & Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)

BRC 34: Marcella
(This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).

Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).

Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).

Identifier Dist(asec) RA DEC

IRAS 21319+5755 268.14 21 33 25.0 +58 08 26

IRAS 21316+5751 283.31 21 33 10.2 +58 04 43

IRAS 21320+5752 373.69 21 33 33.4 +58 05 56

IRAS 21314+5802 429.35 21 32 55.5 +58 15 51

IRAS 21320+5752 436.65 21 32.5 +58 02

IRAS 21323+5800 578.04 21 33 52.0 +58 14 04

Previously identified stars within 10 arcminutes are listed below (SIMBAD).

Identifier Class Dist (asec) RA DEC

TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42

HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234

GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6

BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840

Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7

Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8

Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.

Identifier Dist (asec) RA DEC

1 2MASS
J21332921+5802508 463.43 21 33 29.21 +58 02 50.9

2 21 33 55.8 +58 01 18

Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.
Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation.
Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution.
Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.

... drop what you have here ...

=Analysis Plan=

mark, please also dip into the SHA (ops not i&t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)

--[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)

'''Available Data'''

* Archival Spitzer IRAC 4 bands & MIPS (Programs TBD)
* 2MASS
* MSX
* Optical?
* Spot visualization of Spitzer data?

'''Data Reduction'''

* Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)
* Mosaics will be created using MOPEX

'''Analysis Plan'''

* Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs
* Looking for infrared excess emission from material surrounding new stars will be the main focus of the research
* Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses
** Color-Color diagrams
** Color-Magnitude diagrams
** Spectral Energcy Distribution (SED) plots
* Analysis will also involve looking at actual optical and infrared images

'''Tools'''

* MOPEX - to create mosaics (Makovoz & Marleau 2005)
* Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010)
* MS Excel – to generate data diagrams (color-color, SEDs)

=Education and Outreach=
Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.

A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.

Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)

''Team Spitzer at Breck School''
Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly "brown-bag discussions." Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.

Marcella:

John:

Diane:

... drop one paragraph per teacher here ...

--[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)

Target selection for brc36

2011-02-14T03:36:18Z

Gibbs:

== brc36 21h35m32.6s +57d31m50s ==

* BRC 36 3 articles on ADS two are on star formation but none on SIMBAD

* 3 results from ADS: 1 abstract, 2 Chandra proposals; 0 results from Simbad, however, Aladin applet Simbad identifies (and IRAS-IRIS reveals) 6 YSOs, 10 IR sources, 2 Mol Cld, Rf Neb, Br Neb, Dk Neb, stars in nebulae, and stars in clouds.

* This looks like an interesting field. Lots going on (too much?) ADS: Garmire and Getman are both proposing to use Chandra to study this area. (x-rays)

--[[User:CJohnson|CJohnson]] 16:33, 9 February 2011 (PST)

Using SIMBAD, and searching under coordinates yields 83 objects mostly stars: 17 *iC, 13 TT*, 4 *, 1 **, 8 Y*O, 4 Em*, 1 Or*, 1 *i* (star in double system), 1 *IN (star in nebula), 16 IR sources, 3 smm, 5 Molecular cloud, 2 part of cloud, 1 cloud, 1 dark nebula, 1 bright nebula, 1 reflection nebula, and 1 radio source. One of the molecular clouds is the elephant trunk nebula.--[[User:Linahan|Linahan]] 13:20, 11 February 2011 (PST)

The elephant trunk nebula has 23 references. Here is a sampling of them.
#66 NAME ELEPHANT TRUNK NEBULA 519.38 MoC 21 36 +57.4
2009AJ....137.3685B  Astron. J., 137, 3685-3699 (2009)  An infrared census of star formation in the Horsehead nebula.  BOWLER B.P., WALLER W.H., MEGEATH S.T., PATTEN B.M. and TAMURA M.
2009AJ....138.1116S  Astron. J., 138, 1116-1136 (2009)  A Spitzer view of the young open cluster NGC 2264.  SUNG H., STAUFFER J.R. and BESSELL M.S.
2009ApJ...690..683R  Astrophys. J., 690, 683-705 (2009)  Properties of protostars in the Elephant Trunk in the globule IC 1396A.  REACH W.T., FAIED D., RHO J., BOOGERT A., TAPPE A., JARRETT T.H., MORRIS P., CAMBRESY L., PALLA F. and VALDETTARO R.
2009ApJ...694L..26G  Astrophys. J., 694, L26-L30 (2009)  Driving turbulence and triggering star formation by ionizing radiation.  GRITSCHNEDER M., NAAB T., WALCH S., BURKERT A. and HEITSCH F.
2009ApJ...702.1507M  Astrophys. J., 702, 1507-1529 (2009)  Mid-infrared variability of protostars in IC 1396A.  MORALES-CALDERON M., STAUFFER J.R., REBULL L., WHITNEY B.A., BARRADO Y NAVASCUES D., ARDILA D.R., SONG I., BROOKE T.Y., HARTMANN L. and CALVET N.
2008A&A...485..753H  Astron. Astrophys., 485, 753-763 (2008)  An infrared-submillimeter study of starforming regions selected by the ISOSS 170 {mu}m survey.  HENNEMANN M., BIRKMANN S.M., KRAUSE O. and LEMKE D.
2008ApJ...675.1352V  Astrophys. J., 675, 1352-1360 (2008)  High-resolution H_2_ O maser observations toward IRAS sources in bright-rimmed clouds.  VALDETTARO R., MIGENES V., TRINIDAD M.A., BRAND J. and PALLA F.
flags: (abstract)
2007PASJ...59S.443I  Publ. Astron. Soc. Jap., 59, 443-454 (2007)  AKARI infrared imaging of reflection nebulae IC4954 and IC4955.  ISHIHARA D., ONAKA T., KANEDA H., SUZUKI T., KATAZA H., SAKON I., OKADA Y., DOI Y., FUJISHIRO N., FUJIWARA H., ITA Y., KII T., KIM W., MAKIUTI S., MATSUMOTO T., MATSUHARA H., MURAKAMI H., NAKAGAWA T., OHYAMA Y., OYABU S., SERJEANT S., SHIBAI H., TAKAGI T., TANABE T., UEMIZU K., UENO M., USUI F., WADA T., WATARAI H. and YAMAMURA I.
--[[User:Linahan|Linahan]] 13:33, 11 February 2011 (PST)

#12 and #75 The two larges sources are both stars with 28 and 24 sources. respectively. Looks like it might be a star in the elephant trunk nebula because they have overlapping sources. HD 205794 243.93 *iC 21 35 43.8294 +57 28 03.484 B0.5V 28 and 75 HD 239710 560.65 *iN 21 36 41.0395 +57 30 08.260 B3V 24

Both reference: 2004ApJS..154..385R  Astrophys. J., Suppl. Ser., 154, 385-390 (2004)  Protostars in the Elephant Trunk nebula.  REACH W.T., RHO J., YOUNG E., MUZEROLLE J., FAJARDO-ACOSTA S., HARTMANN L., SICILIA-AGUILAR A., ALLEN L., CAREY S., CUILLANDRE J.-C., JARRETT T.H., LOWRANCE P., MARSTON A., NORIEGA-CRESPO A. and HURT R.L.--[[User:Linahan|Linahan]] 13:46, 11 February 2011 (PST)

Here is the summary of information on the clouds:
#28 [IS94] 1 354.07 MoC 21 35 43 +57 26.1
1994JApA...15..157I  J. Astrophys. Astron., 15, 157-163 (1994)  Observations of the bright-rimmed molecular clouds near the Cepheus OB 2 association.  INDRANI C. and SRIDHARAN T.K.

#29 [PGS95] 14 365.70 PoC 21 36 03.6 +57 27 23
1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#39 IRAS 21346+5714 410.43 Cld 21 36 12.4 +57 27 34 There are 11 sources but a lot of the same sources as elephant trunk.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#40 [IS94] 15 410.44 MoC 21 36 12 +57 27.5
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#61 [DBY94] 099.1+04.0511.24 MoC 21 36 35.4 +57 30 36
1994ApJS...95..419D  Astrophys. J., Suppl. Ser., 95, 419-456 (1994)  Molecular clouds in Cygnus. I. A large-scale survey.  DOBASHI K., BERNARD J.-P., YONEKURA Y. and FUKUI Y.

#70 LBN 098.83+04.12 538.58 MoC 21 35 +57.4
2006MNRAS.369.1822M  Mon. Not. R. Astron. Soc., 369, 1822-1836 (2006)  Photometric distances to nine dark globules.  MAHESWAR G. and BHATT H.C.
1997A&A...325.1001S  Astron. Astrophys., 325, 1001-1012 (1997)  The X-ray view of the central part of IC 1396.  SCHULZ N.S., BERGHOEFER T.W. and ZINNECKER H.
1990ApJ...359..319L  Astrophys. J., 359, 319-343 (1990)  A CO survey of regions around 34 open clusters. II. Physical properties of cataloged molecular clouds.  LEISAWITZ D.
1989ApJS...70..731L  Astrophys. J., Suppl. Ser., 70, 731-812 (1989)  A CO survey of regions around 34 open clusters.  LEISAWITZ D., BASH F.N. and THADDEUS P.

#83 [PGS95] 15598.87 PoC 21 36 03.9 +57 22 47
1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.--[[User:Linahan|Linahan]] 14:16, 11 February 2011 (PST)

I also came across the the Chandra proposals Chelen noted above. I also came across several papers from a group doing research in the radio. One paper "H2O maser emission from bright rimmed clouds in the northern hemisphere" R. Valdettaro1, F. Palla1, J. Brand2, and R. Cesaroni1 http://arxiv.org/abs/astro-ph/0508446v1 . Their other papers 2006RMxAC..26Q.161M and http://iopscience.iop.org/0004-637X/675/2/1352

I also came across this handbook of star forming regions that included BRC36 and a couple of our other targets. http://arxiv.org/PS_cache/arxiv/pdf/0809/0809.4761v1.pdf
--[[User:Gibbs|Gibbs]] 19:36, 13 February 2011 (PST)