Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published August 2007 | Published
Journal Article Open

The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. VI. Perseus Observed with MIPS


We present observations of 10.6 deg^2 of the Perseus molecular cloud at 24, 70, and 160 μm with Spitzer MIPS. The images show prominent, complex extended emission dominated by illuminating B stars on the east side of the cloud and by cold filaments of 160 μm emission on the west side. Of 3950 point sources identified at 24 μm, 1141 have 2MASS counterparts. A quarter of these populate regions of the K_s versus K_s - [24] diagram that are distinct from stellar photospheres and background galaxies and thus are likely to be cloud members with infrared excess. Nearly half (46%) of these 24 μm excess sources are distributed outside the IC 348 and NGC 1333 clusters. A significant number of IRAS PSC objects are not recovered by Spitzer MIPS, most often because the IRAS objects were confused by bright nebulosity. The intercluster region contains several tightly clumped (r ~ 0.1 pc) young stellar aggregates whose members exhibit a wide variety of infrared SEDs characteristic of different circumstellar environments. This could be explained by a significant age spread among the aggregate members, or if the members formed at the same time, a remarkably rapid circumstellar evolution would be required to account for the association of Class I and Class III sources at ages ≲1 Myr. We highlight important results for the HH 211 flow, where the bow shocks are detected at both 24 and 70 μm, and for the debris disk candidate BD +31 643, where the MIPS data show the linear nebulosity to be an unrelated interstellar feature. Our data, mosaics, and catalogs are available at the Spitzer Science Archive for use by interested members of the community.

Additional Information

© 2007 American Astronomical Society. Print publication: Issue 2 (2007 August); received 2006 August 9; accepted for publication 2007 January 23. We wish to thank D. Shupe for helpful conversations in regards to differential source counts and S. Strom, J. Muzerolle, and J. Najita for helpful conversations regarding disk lifetimes. We thank R. D. Blum for making a plot of Ks versus Ks - [24] using the LMC data from Blum et al. (2006) and not making us load his extremely large catalog and do it ourselves. We thank the anonymous referee for a thorough and thoughtful report. L. M. R. wishes to acknowledge funding from the Spitzer Science Center to allow her to take ''science retreats'' to work intensively on this paper. Most of the support for this work, part of the Spitzer Space Telescope 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. We thank the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. B. M. acknowledges the Fundacio´n Ramo´n Areces for financial support. Support for J. K. J. and P. C. M. was provided in part by a NASA Origins grant, NAG5-13050. Astrochemistry in Leiden is supported by an 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. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. These data were served by the NASA/IPAC Infrared Science Archive,which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

Attached Files

Published - REBapjss07.pdf


Files (2.4 MB)
Name Size Download all
2.4 MB Preview Download

Additional details

August 22, 2023
October 20, 2023