The Spitzer c2d survey of nearby dense cores. III. Low-mass star formation in a small group, L1251B
Abstract
We present a comprehensive study of a low-mass star-forming region, L1251B, at wavelengths from the near-infrared to the millimeter. L1251B, in which only one protostar, IRAS 22376+7455, was known previously, is confirmed to be a small group of protostars on the basis of observations with the Spitzer Space Telescope. The most luminous source of L1251B is located 5" north of the IRAS position. A near-infrared bipolar nebula, which is not associated with the brightest object and is located at the southeast corner of L1251B, has been detected in the IRAC bands. OVRO and SMA interferometric observations indicate that the brightest source and the bipolar nebula source in the IRAC bands are deeply embedded disk sources. Submillimeter continuum observations with single-dish telescopes and the SMA interferometric observations suggest two possible prestellar objects with very high column densities. Outside of the small group, many young stellar object candidates have been detected over a larger region of 12' × 12'. Extended emission to the east of L1251B has been detected at 850µ m; this "east core" may be a site for future star formation since no point source has been detected with IRAC or MIPS. This region is therefore a possible example of low-mass cluster formation, where a small group of pre- and protostellar objects (L1251B) is currently forming, alongside a large starless core (the east core).
Additional Information
© 2006 The American Astronomical Society. Received 2006 April 16; accepted 2006 May 17. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608 and 1230782 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This work was also supported by NASA Origins grant NNG04GG24G. Support for this work was also provided by NASA through Hubble Fellowship grant HST-HF-01187 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We are very grateful to Mario Tafalla for providing the unpublished 1.3 mm continuum map. We also thank Robert Gutermuth for supplying the IDL code used to make Figure 4. J.-E.L. thanks the University of Texas at Austin for the support through the University Continuing Fellowship. We are very grateful to Geoff Blake, Lee Mundy, and the referee of this paper, Paul Ho, for many helpful comments.Attached Files
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Additional details
- Eprint ID
- 5070
- Resolver ID
- CaltechAUTHORS:LEEapj06
- 1224608
- NASA
- 1230782
- NASA
- 1407
- NASA
- NNG04GG24G
- NASA
- HST-HF-01187
- NASA Hubble Fellowship
- NAS 5-26555
- NASA
- Created
-
2006-09-28Created from EPrint's datestamp field
- Updated
-
2021-11-08Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)