Difference between revisions of "BRC Proposal"

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[[2011 proposal instructions]]
 
[[2011 proposal instructions]]
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=Proposal Versions=
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REVISED FINAL with referee suggestions: [[file: BRC_propFINAL.doc]]
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--[[User:CJohnson|CJohnson]] 11:21, 26 May 2011 (CDT)
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WORKING VERSION of FINAL with referee suggestions: [[file: BRC_prop4_revised.doc]]
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--[[User:CJohnson|CJohnson]] 11:51, 25 May 2011 (CDT)
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FINAL VERSION (some tweaks from Luisa with respect to first version below): [[file: BRC_prop3_final.doc]] --[[User:Rebull|Rebull]] 09:29, 21 March 2011 (PDT)
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Third version (includes Luisa's comments, telecon tidbits, abstract):  [[File: BRC_prop3.doc]]
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--[[User:CJohnson|CJohnson]] 14:42, 18 March 2011 (PDT)
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Luisa's hack up of version 2 (i missed version 2a, sorry): [[File: BRC_prop2_lmr.doc]] --[[User:Rebull|Rebull]] 13:46, 16 March 2011 (PDT)
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Second attempt (slightly altered with Diane's changes) [[File: BRC_prop2a.doc]]
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--[[User:CJohnson|CJohnson]] 11:51, 16 March 2011 (PDT)
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Second attempt [[File:BRC_prop2.doc]]
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--[[User:CJohnson|CJohnson]] 12:21, 15 March 2011 (PDT)
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First attempt [[File:BRC_prop1.doc]]
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--[[User:CJohnson|CJohnson]] 13:05, 9 March 2011 (PST)
  
 
=Background on Star Formation=
 
=Background on Star Formation=
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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]
 
[http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]
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--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)
 
--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)
  
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Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper "New Young Star Candidates in CG4 and Sa101", Rebull et all, 2011  [[File:GISS_2011_Legassie_gum_nebula.pptx]]  --[[User:Legassie|Legassie]] 15:04, 18 May 2011 (PDT)
  
 
=Target Selection=
 
=Target Selection=
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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:
 
The list of sources that Lori suggests we consider are here:
*brc34      21h32m51.2s    +58d08m43s
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*[[target selection for brc34]]       21h32m51.2s    +58d08m43s DECIDED ON THIS ONE
*brc36      21h35m32.6s    +57d31m50s
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*[[target selection for brc36]]       21h35m32.6s    +57d31m50s
*brc38      21h40m02.2s    +58d20m31s
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*[[target selection for brc31]]       20h50m43.4s    +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula
*brc31      20h50m43.4s    +44d21m53s
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*[[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]]
*brc27     07h04m07.8s    -11d16m43s
 
  
Let's collect information on literature references for each of these below. Look in both ADS and SIMBAD for papers and previously known sources within about 30' of these positions.
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*[[target selection for brc38]]      21h40m02.2s    +58d20m31s  RULE THIS OUT BECAUSE SPITZER DATA IS DONE
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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.
  
  
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=='''From Marcella'''==
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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."
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papers from discussion on the phone 16:35, 23 February 2011 (PST)
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*[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with "sfo 38"  http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
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*[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper  http://adsabs.harvard.edu/abs/2008A%26A...477..557M
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----
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=STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=
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''Can I delete all this ... now that our proposal has been submitted??''
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--[[User:CJohnson|CJohnson]] 09:42, 23 March 2011 (PDT)
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=Introduction/Background=
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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)
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http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=1655856
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Proceedings of the International Astronomical Union (2007), 3: 164-165
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DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008
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Low-mass star formation in bright rimmed clouds    V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda
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--[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)
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A&A 388, 172-178 (2002)
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DOI: 10.1051/0004-6361:20020451
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The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1
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J. B. Soares and E. Bica
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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)
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A&A 426, 535-545 (2004)
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DOI: 10.1051/0004-6361:20040226
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A radio and mid-infrared survey of northern bright-rimmed clouds
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L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao
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Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK
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--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)
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DOES ANYBODY HAVE ACCESS TO  Ogura's 2010 "Triggered Star Formation associated with HII Regions"  ADS says the full paper is not available.
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--[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)
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'''Science Background and Context: Star Formation'''
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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 vigorous 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, or more).  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 theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths.  The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view.  The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation.  Thus, protostars are detectable within their nebula at infrared wavelengths.  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.
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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 (Migenesa 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.
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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 if the analysis goes 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.
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--[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)
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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.)
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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''  1 proposal to study by Garmire, nothing on SIMBAD
 
  
''BRC 36''   3 articles on ADS two are on star formation but none on SIMBAD
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BRC 34: Marcella
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(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?).
  
''BRC 38''  1 article by Choudhury which identified 45 YSO's
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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).
  
''BRC 31''  nothing on both
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Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).
  
''BRC 27''  Chauhan observed BR 27 and came up with some YSO candidates and a catalog(?) entry on SIMBAD.
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Identifier Dist(asec) RA DEC
  
=='''From John'''==
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IRAS 21319+5755 268.14 21 33 25.0 +58 08 26
  
Ogura. "Triggered Star Formation associated with HII Regions."
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IRAS 21316+5751 283.31 21 33 10.2 +58 04 43
[http://74.125.155.132/scholar?q=cache:aOoo5uLiRrIJ:scholar.google.com/+brc+27+sfo+27&hl=en&as_sdt=0,5]. ''ASI Conference Series.'' 2010, Vol. 1, pp 19–25.
 
  
Ogura, Sugitani and Pickles. "H-alpha Emission Stars and Herbig-Haro Objects in the Vicinity of Bright-Rimmed Clouds." [http://iopscience.iop.org/1538-3881/123/5/2597/pdf/1538-3881_123_5_2597.pdf] ''AJ.'' 123: 2597-2626, 2002 May.  
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IRAS 21320+5752 373.69 21 33 33.4 +58 05 56
  
Morgan, et al. "A Radio and Mid-Infrared Survey of Northern Bright-Rimmed
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IRAS 21314+5802 429.35 21 32 55.5 +58 15 51
Clouds." [http://arxiv.org/PS_cache/astro-ph/pdf/0407/0407167v1.pdf] astro-ph 0407167v1.
 
  
Soares and Bica. "The Embedded Star Clusters in the Nebulae NGC 2327 and BRC 27 in Canis Majoris R1." [http://cds.aanda.org/index.php?Itemid=129&option=com_article&access=bibcode&bibcode=2002A%25252526A...388..172S] ''A&A.'' 388, 172{178 (2002).
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IRAS 21320+5752 436.65 21 32.5 +58 02
  
=='''From Diane'''==
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IRAS 21323+5800 578.04 21 33 52.0 +58 14 04
  
''BRC27''     
 
  
07h04m07.8s   
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Previously identified stars within 10 arcminutes are listed below (SIMBAD).
  
-11d16m43s
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Identifier Class Dist (asec) RA DEC
  
ADS: Chauhan; Simbad: 14 entries (I checked them, not all seem to be on this exact area)
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TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42
  
Images: the Aladdin Sky Atlas (DSS2 & Simbad) shows the image fairly bright where the B & W is dark. Kicking in the IRAS data only makes 5 IR targets show up, plus the cloud near the bottom of the image.
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HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234
  
Where are all the targets & YSOs that are mentioned by Chauhan? Chauhan abstract (2009) “Triggered star formation and evolution of T-Tauri stars in and around bright-rimmed clouds.”  From Chauhan’s data tables 4 & 6 I gleaned the following nuggets of information:
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GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6
table4.dat        85    133  Dereddened magnitude, colors, age and mass of the YSOs associated with the BRCs; Last entry from table 4 and Table 6 each say this: Cl II  YSO class  (meta.code.class)  (CLASS_CODE)
 
  
Coordinates for this cloud come up as:
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BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840
07 03 58.7
 
-11 23 19       
 
IRAS 07016-1118 slightly south and to the right of the main image of BRC27
 
  
From data Table 6: IRAC photometric magnitudes of the disk bearing candidates in BRCs 2, 27 and 13/14  (are we interested in examining this?)
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Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7
  
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Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8
  
''BRC31''     
 
  
20h50m43.4s   
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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.
  
+44d21m53s
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Identifier Dist (asec) RA DEC
  
Busy field; Cloud in center of Aladin Applet image.(right on these coordinates)
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1   2MASS
surrounded by Emission line stars,  HH, and radio sources, and an X-ray source. The frame completely fills up when 2MASS is applied.
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J21332921+5802508 463.43 21 33 29.21 +58 02 50.9
  
DSS2 shows a thick cloud.  Simbad shows the sources described above.
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2 21 33 55.8 +58 01 18
  
''BRC34''     
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21h32m51.2s   
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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.
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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.
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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.
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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.
  
+58d08m43s
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... drop what you have here ...
  
0 ADS abstracts; 0 Simbad citations
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=Analysis Plan=
No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori.  Parts of the cloud are labeled.  The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image)   Many hits on 2MASS
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--[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)
  
''BRC36'' 
 
   
 
21h35m32.6s   
 
  
+57d31m50s
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Spitzer archival data from  IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX.  Data for BRC27 will originate from Spitzer program 30050 (reqkeys 17512192 and 17512448) while BRC34 data will originate from program 202 (reqkeys 6031616 and 6031872).  See Figure 1 for visualization of BRC27 data using the Spitzer Planning and Observation Tool (Spot).  Reference Figure 2 for visualization of BRC34 data.
  
3 results from ADS: 1 abstract, 2 Chandra proposals; 0 results from Simbad,
 
however, Aladin applet Simbad identifies  (and IRAS-IRIS reveals)
 
6 YSO’s, 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?)
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''Figure 1: Spot visualization of BRC27 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''
ADS: Garmire and Getman are both proposing to use Chandra to study this area. (x-rays)
 
  
''BRC38''  (is this SFO 38?)   
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[[File:brc27_final.jpg]]
  
21h40m02.2s   
 
  
+58d20m31s  
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''Figure 2: Spot visualization of BRC34 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed  in the blue and purple regions, while MIPS is shown in tan.''
  
Triggered Star Formation and Young Stellar Population in Bright-rimmed Cloud SFO 38 by Choudhury, Rumpa; Mookerjea, Bhaswati; Bhatt, H. C. [http://arxiv.org/pdf/1005.1841v1]
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[[File:brc34_final.jpg]]
  
They have identified 45 YSO’s in this area, although I only counted 19 in the image I was able to pull up.  They studied the area with a variety of instruments and wavelengths (including Spitzer).  This seems like a fairly comprehensive study. 
 
  
--- This is a fabulous start, Team BRC. Pats on the back to all :)
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Our 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.  To accomplish this, a well-known property of YSOs will be exploited -- namely, large near- and mid-infrared emissions from material surrounding young stars.  Looking for excess emissions will be the main focus of the research, and Spitzer is excellent at detecting these emissions as well as any bipolar outflows.   Using the combined data, we will generate and analyze various plots, including spectral energy distributions (SEDs) , color-magnitude diagrams, and color-color diagrams to search for stars with infrared excesses.
--[[User:CJohnson|CJohnson]] 18:16, 6 February 2011 (PST)
 
  
=='''From Luisa'''==
 
  
OK, just for comparison, here is a walkthrough of what i'd do, but for just one of the objects.
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We will generate mosaics of the BRC objects using MOPEX-Mosaics from Photometry data (Makovoz & Marleau 2005).  For data reduction, the Aperture Photometry Tool (APT) will assist us in obtaining photometry values.  These tools will allow our team to conduct flux analyses as well as spatial analyses and detailed visual observations.  The resultant data will be analyzed further using a spreadsheet program (MS Excel).  Excel will allow students to generate color diagrams and SEDs with the data to test infrared wavelenght theories of identifying and classifying young stellar objects.
from above -- brc27      07h04m07.8s    -11d16m43s.
 
search in SIMBAD, by position, for objects within 10 arcmin.
 
73 objects returned. Some emission stars (EM*LkHa 221 means emission star, from the Lick Halpha survey -- a young star!), a star cluster, some IRAS sources (possibly but not necessarily young stars), a Lynds Dark Nebula (cloud dark in the optical), sources whose name suggests affiliation with BRC27 ("OSP2002 BRC27 xx" sources), x-ray sources (RXJ sources), and several things SIMBAD flags as just emission stars ("Em*", e.g. likely young stars).  Clicking on any of the names leads me to an information page tied to that object.
 
  
The x-ray source 1RXS J070409.5-111707 is closest to the position i asked for. no literature refs on that. Next closest is EM* LkHA 221. There are four synonyms for this one, and 8 references.
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=Education and Outreach=
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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.
  
{| border="1"
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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.
|2004PASJ...56..313K -- 13^CO (J = 1-0) survey toward of molecular clouds toward the Monoceros and Canis Major Region. --  KIM B.G., KAWAMURA A., YONEKURA Y. and FUKUI Y.
 
|there are data tables, but this is a radio survey. unlikely to have much information on the point sources.
 
|-
 
| 2003A&A...399..141M -- Merged catalogue of reflection nebulae. -- MAGAKIAN T.Y.
 
| hm. catalog of nebulae? probably not much information on the pt srcs, but worth tracking down.
 
|-
 
|2002A&A...388..172S -- The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1. -- SOARES J.B. and BICA E.
 
| this one actually uses the term "BRC 27" in the title and talks about stars. definitely look at this one.
 
|-
 
|1999MNRAS.310..175T -- The Cepheid distance to M96 and the Hubble constant. -- TANVIR N.R., FERGUSON H.C. and SHANKS T.
 
| cepheids and the hubble constant?? unlikely to have much to do with the thing we care about.  why is this crosslisted? might look it up just to solve that mystery.
 
|-
 
|1992ApJS...78..239W -- A catalog of co-added IRAS fluxes or Orion population stars. -- WEAVER W.B. and JONES G.
 
| Hm. reanalysis of IRAS data. and Orion population means young. look this one up.
 
|-
 
|1990ApJS...74..575W -- A catalog of pre-main-sequence emission-line stars with IRAS source associations. -- WEINTRAUB D.A. [http://cdsads.u-strasbg.fr/cgi-bin/nph-iarticle_query?1990ApJS...74..575W&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf]
 
| DING DING DING. likely to summarize lots of young stars here. this is likely to be the first one i go grab.
 
|-
 
| 1988LicOB1111....1H -- Third catalog of emission-line stars of the Orion population. -- HERBIG G.H. and BELL K.R.
 
| this is just a catalog. worth looking up to see what is known (or was known in 1988) about stars in this region.
 
|-
 
|1986PASJ...38..395W --  Emission-line stars in the Canis Major star-formation region. -- WIRAMIHARDJA S.D., KOGURE T., NAKANO M. and YOSHIDA S. [http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1986PASJ...38..395W&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf]
 
| another DING DING DING. likely to summarize lots of young stars here.  
 
|}
 
  
Next closest object is [C74] 813 references.
+
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.   
  
{| border="1"
 
|1999MNRAS.310..210S --  The stellar composition of the star formation region CMa R1 - I. Results from new photometric and spectroscopic classifications. -- SHEVCHENKO V.S., EZHKOVA O.V., IBRAHIMOV M.A., VAN DEN ANCKER M.E. and TJIN A DJIE H.R.E. [http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1999MNRAS.310..210S&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf]
 
| this one is worth grabbing too. stellar composition of the SFR also suggests list of objects.
 
|-
 
|1974A&A....37..229C -- A study of stellar association Canis Majoris OB 1. -- CLARIA J.J.
 
| pretty old. probably not worth grabbing? check abs.
 
|-
 
|1974AJ.....79.1022C -- Investigation of a Milky Way region in Canis Majoris. -- CLARIA J.J.
 
|Also old. check abs.
 
|}
 
  
Next closest object is NGC 2327, a cluster. three references.
+
''Team Spitzer at Breck School'' 
{| border="1"
+
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.
|2009A&A...506..711G -- Star formation history of Canis Major R1. I. Wide-field X-ray study of the young stellar population. -- GREGORIO-HETEM J., MONTMERLE T., RODRIGUES C.V., MARCIOTTO E., PREIBISCH T. and ZINNECKER H.
 
| X-rays can indicate youth (see my [[Finding cluster members]] page), and "young stars." get this one.
 
|-
 
|2003A&A...397..177B --  A Catalogue of infrared star clusters and stellar groups. -- BICA E., DUTRA C.M. and BARBUY B.
 
| another promising one.
 
|-
 
|2002A&A...388..172S -- The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1. -- SOARES J.B. and BICA E.
 
| already found above!
 
|}
 
  
Next closest object is HRW 16 -- one reference to an early-type emission star paper. possibly worth tracking down, unlikely to be terribly fruitful.
 
  
Then the next shows you the fallibility of SIMBAD -- NGC 2327 appears listed again, with a different name (and possibly different references!)...
+
Marcella: 
 +
Students at Carmel Catholic High School will participate in the Spitzer research program as an extracurricular activity. Students will meet once a week for two to four hours or as needed. Students will read a variety of resources and participate in activities to learn about the history of astronomy and stellar evolution. Students will become proficient in a variety of image processing software programs. Students will share their research findings at local outreach events at the middle school, high school, and community levels.
  
I scrolled down to the first "[OSP2002] BRC 27 23" reference. That resolves to 2002AJ....123.2597O -- H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds. -- OGURA K., SUGITANI K. and PICKLES AThis is also likely to be a very good paper to examine, including getting the data tables!
+
John: 
 +
Glencoe Astronomy at Glencoe High School.  Glencoe High School students ranging from sophomores to seniors will work together on this BRC project. There are currently seven students starting this project and additional students are anticipated. Students will be given weekly readings that will be discussed during our meetings each Thursday morningWe will begin with the basic principles of stellar evolution with an emphasis on star formation. Resources will include tutorials posted on the CoolWiki website and scientific articles relevant to the BRC projectStudents will work together in teams during the data analysis and continue to meet to discuss their work.
  
I ignored the rest of the list, on the assumption for now that I've probably found most of the significant results. If, however, you ask SIMBAD to plot the sources up, the position I asked for is relatively deficient of sources; there are a bunch more sources to the south. My guess is that the position as given is a little off from what it really should beIt will be worth doing a more exhaustive SIMBAD search once we pick a target and have a better fix on exactly what regions are covered by the Spitzer obs.
+
Diane: 
 +
The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it.  Even when we do not have an organized campaign, the sky always presents something different for us to examine.  The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school yearThey also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events.  Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!
  
I went to ADS next and searched with "BRC 27" (in quotes) in the abstract field.  The first hit is the Soares and Bica paper above. The rest are spurious hits from arXiv. Go back to the ADS search page, and turn off arXiv searching, leaving just "astronomy" checked. Search again.  The second hit (2010 ApJ 717 658) has no "BRC 27" that actually appears in the abstract.  The 3rd is a astrobio article. the 4th is a chandra prop (no content there). the 5th is Chauhan et al., 2009 MNRAS 396, 964. Title sounds promising. Abstract sounds promising. Put this on the list to retrieve and read.  After that, there are radio papers, proposals, AAS posters... and the quality of the relevance goes down. Quit this for now and look at the papers I've got so far.
+
--updated [[User:CJohnson|CJohnson]] 11:20, 15 March 2011 (PDT)

Latest revision as of 16:20, 26 May 2011

Instructions

2011 proposal instructions

Proposal Versions

REVISED FINAL with referee suggestions: File:BRC propFINAL.doc --CJohnson 11:21, 26 May 2011 (CDT)

WORKING VERSION of FINAL with referee suggestions: File:BRC prop4 revised.doc --CJohnson 11:51, 25 May 2011 (CDT)

FINAL VERSION (some tweaks from Luisa with respect to first version below): File:BRC prop3 final.doc --Rebull 09:29, 21 March 2011 (PDT)

Third version (includes Luisa's comments, telecon tidbits, abstract): File:BRC prop3.doc --CJohnson 14:42, 18 March 2011 (PDT)

Luisa's hack up of version 2 (i missed version 2a, sorry): File:BRC prop2 lmr.doc --Rebull 13:46, 16 March 2011 (PDT)

Second attempt (slightly altered with Diane's changes) File:BRC prop2a.doc --CJohnson 11:51, 16 March 2011 (PDT)

Second attempt File:BRC prop2.doc --CJohnson 12:21, 15 March 2011 (PDT)

First attempt File:BRC prop1.doc --CJohnson 13:05, 9 March 2011 (PST)

Background on Star Formation

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

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

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

Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper "New Young Star Candidates in CG4 and Sa101", Rebull et all, 2011 File:GISS 2011 Legassie gum nebula.pptx --Legassie 15:04, 18 May 2011 (PDT)

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:

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 30' 10' of these positions.


Help on: Basic Literature Searching -- Advanced Literature Searching -- 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)



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

Can I delete all this ... now that our proposal has been submitted?? --CJohnson 09:42, 23 March 2011 (PDT)

Introduction/Background

the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --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 --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 )--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 --Sartore 16:03, 23 February 2011 (PST)

DOES ANYBODY HAVE ACCESS TO Ogura's 2010 "Triggered Star Formation associated with HII Regions" ADS says the full paper is not available. --Sartore 12:37, 6 March 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 vigorous 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, or more). 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 theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. 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 (Migenesa 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 if the analysis goes 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.


--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). --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

--Legassie 20:12, 8 March 2011 (PST)


Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. Data for BRC27 will originate from Spitzer program 30050 (reqkeys 17512192 and 17512448) while BRC34 data will originate from program 202 (reqkeys 6031616 and 6031872). See Figure 1 for visualization of BRC27 data using the Spitzer Planning and Observation Tool (Spot). Reference Figure 2 for visualization of BRC34 data.


Figure 1: Spot visualization of BRC27 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.

Brc27 final.jpg


Figure 2: Spot visualization of BRC34 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.

Brc34 final.jpg


Our 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. To accomplish this, a well-known property of YSOs will be exploited -- namely, large near- and mid-infrared emissions from material surrounding young stars. Looking for excess emissions will be the main focus of the research, and Spitzer is excellent at detecting these emissions as well as any bipolar outflows. Using the combined data, we will generate and analyze various plots, including spectral energy distributions (SEDs) , color-magnitude diagrams, and color-color diagrams to search for stars with infrared excesses.


We will generate mosaics of the BRC objects using MOPEX-Mosaics from Photometry data (Makovoz & Marleau 2005). For data reduction, the Aperture Photometry Tool (APT) will assist us in obtaining photometry values. These tools will allow our team to conduct flux analyses as well as spatial analyses and detailed visual observations. The resultant data will be analyzed further using a spreadsheet program (MS Excel). Excel will allow students to generate color diagrams and SEDs with the data to test infrared wavelenght theories of identifying and classifying young stellar objects.

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.


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: Students at Carmel Catholic High School will participate in the Spitzer research program as an extracurricular activity. Students will meet once a week for two to four hours or as needed. Students will read a variety of resources and participate in activities to learn about the history of astronomy and stellar evolution. Students will become proficient in a variety of image processing software programs. Students will share their research findings at local outreach events at the middle school, high school, and community levels.

John: Glencoe Astronomy at Glencoe High School. Glencoe High School students ranging from sophomores to seniors will work together on this BRC project. There are currently seven students starting this project and additional students are anticipated. Students will be given weekly readings that will be discussed during our meetings each Thursday morning. We will begin with the basic principles of stellar evolution with an emphasis on star formation. Resources will include tutorials posted on the CoolWiki website and scientific articles relevant to the BRC project. Students will work together in teams during the data analysis and continue to meet to discuss their work.

Diane: The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!

--updated CJohnson 11:20, 15 March 2011 (PDT)