Chapman, Nicholas L. and Lai, Shih-Ping and Mundy, Lee G. and Evans, Neal J., II and Brooke, Timothy Y. and Cieza, Lucas A. and Spiesman, William J. and Rebull, Luisa M. and Stapelfeldt, Karl R. and Noriega-Crespo, Alberto and Lanz, Lauranne and Allen, Lori E. and Blake, Geoffrey A. and Bourke, Tyler L. and Harvey, Paul M. and Huard, Tracy L. and Jørgensen, Jes K. and Koerner, David W. and Myers, Philip C. and Padgett, Deborah L. and Sargent, Annelia I. and Teuben, Peter and van Dishoeck , Ewine F. and Wahhaj, Zahed and Young, Kaisa E. (2007) The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. IV. Lupus Observed with MIPS. Astrophysical Journal, 667 (1). pp. 288-302. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20091028-091148540
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We present maps of 7.78 deg^2 of the Lupus molecular cloud complex at 24, 70, and 160 μm. They were made with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) instrument as part of the Spitzer Legacy Program "From Molecular Cores to Planet-Forming Disks" (c2d). The maps cover three separate regions in Lupus, denoted I, III, and IV. We discuss the c2d pipeline and how our data processing differs from it. We compare source counts in the three regions with two other data sets and predicted star counts from the Wainscoat model. This comparison shows the contribution from background galaxies in Lupus I. We also create two color-magnitude diagrams using the 2MASS and MIPS data. From these results, we can identify background galaxies and distinguish them from probable young stellar objects. The sources in our catalogs are classified based on their spectral energy distribution (SED) from 2MASS and Spitzer wavelengths to create a sample of young stellar object candidates. From 2MASS data, we create extinction maps for each region and note a strong correspondence between the extinction and the 160 μm emission. The masses we derived in each Lupus cloud from our extinction maps are compared to masses estimated from ^(13)CO and C^(18) O and found to be similar to our extinction masses in some regions, but significantly different in others. Finally, based on our color-magnitude diagrams, we selected 12 of our reddest candidate young stellar objects for individual discussion. Five of the 12 appear to be newly discovered YSOs.
|Additional Information:||© 2007 The American Astronomical Society. Received 2006 August 16; accepted 2007 June 11. We would like to thank the staff at the Lorentz Center in Leiden for their hospitality in hosting several meetings that contributed to this paper. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230782, and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Astrochemistry in Leiden is supported by a NWO Spinoza grant and a NOVA grant. K. E. Y. was supported by NASA under grant NGT5-50401 issued through the Office of Space Science. The research of J. K. J. was supported by NASA Origins Grant NAG5- 13050. L.G.M. is supported by NASA Origins Grant NAG510611. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.|
|Subject Keywords:||infrared : stars; ISM : clouds; stars : formation|
|Official Citation:||The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. IV. Lupus Observed with MIPS Nicholas L. Chapman, Shih-Ping Lai, Lee G. Mundy, Neal J. Evans II, Timothy Y. Brooke, Lucas A. Cieza, William J. Spiesman, Luisa M. Rebull, Karl R. Stapelfeldt, Alberto Noriega-Crespo, Lauranne Lanz, Lori E. Allen, Geoffrey A. Blake, Tyler L. Bourke, Paul M. Harvey, Tracy L. Huard, Jes K. Jørgensen, David W. Koerner, Philip C. Myers, Deborah L. Padgett, Annelia I. Sargent, Peter Teuben, Ewine F. van Dishoeck, Zahed Wahhaj, and Kaisa E. Young 2007 ApJ 667 288-302 doi: 10.1086/520790|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||29 Oct 2009 20:25|
|Last Modified:||26 Dec 2012 11:30|
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