Difference between revisions of "BRC Proposal"
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Revision as of 06:37, 9 March 2011
Background on Star Formation
STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.
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
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 SPITZER DONE ALREADY DONE in the north american nebula
- 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
30' 10' of these positions.
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)
- Morgan 2009 paper -- has a figure with "sfo 38" http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
- 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.
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 ...
--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 IRAC and MIPS data for BRC27 on a 25-micron view of the region under study. IRAC data is displayed within the light blue and light purple regions, while MIPS is shown within the the smaller tan-colored regions.
Figure 2: Spot visualization of IRAC and MIPS data for BRC34 on a 25-micron view of the region under study. IRAC data is displayed within the light blue and light purple regions, while MIPS is shown within the the smaller tan-colored regions.
- Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)
- Mosaics will be created using MOPEX
- 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
- 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.
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!
--Sartore 14:06, 6 March 2011 (PST)
... drop one paragraph per teacher here ...
--CJohnson 19:40, 22 February 2011 (PST)