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The mass distribution and lifetime of prestellar cores in Perseus, Serpens, and Ophiuchus

Enoch, Melissa L. and Evans, Neal J., II and Sargent, Anneila I. and Glenn, Jason and Rosolowsky, Erik and Myers, Philip (2008) The mass distribution and lifetime of prestellar cores in Perseus, Serpens, and Ophiuchus. Astrophysical Journal, 684 (2). pp. 1240-1259. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:ENOapj08

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Abstract

We present an unbiased census of starless cores in Perseus, Serpens, and Ophiuchus, assembled by comparing large-scale Bolocam 1.1 mm continuum emission maps with Spitzer c2d surveys. We use the c2d catalogs to separate 108 starless from 92 protostellar cores in the 1.1 mm core samples from Enoch and Young and their coworkers. A comparison of these populations reveals the initial conditions of the starless cores. Starless cores in Perseus have similar masses but larger sizes and lower densities on average than protostellar cores, with sizes that suggest density profiles substantially flatter than ρ∝r^-2. By contrast, starless cores in Serpens are compact and have lower masses than protostellar cores; future star formation will likely result in lower mass objects than the currently forming protostars. Comparison to dynamical masses estimated from the NH3 survey of Perseus cores by Rosolowsky and coworkers suggests that most of the starless cores are likely to be gravitationally bound, and thus prestellar. The combined prestellar core mass distribution includes 108 cores and has a slope of α = -2.3 ± 0.4 for M > 0.8 M☉. This slope is consistent with recent measurements of the stellar initial mass function, providing further evidence that stellar masses are directly linked to the core formation process. We place a lower limit on the core-to-star efficiency of 25%. There are approximately equal numbers of prestellar and protostellar cores in each cloud; thus the dense prestellar core lifetime must be similar to the lifetime of embedded protostars, or 4.5 x 10^5 yr, with a total uncertainty of a factor of 2. Such a short lifetime suggests a dynamic, rather than quasi-static, core evolution scenario, at least at the relatively high mean densities (n > 2 x 10^4 cm^-3) to which we are sensitive.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/589963DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/684/2/1240/PublisherArticle
ORCID:
AuthorORCID
Sargent, Anneila I.0000-0002-4633-5098
Additional Information:© 2008. The American Astronomical Society. Received 2008 February 1; accepted 2008 May 7; published 2008 September 10. The authors are grateful to Jens Kauffman and Jason Kirk for their insightful comments and suggestions, and to the anonymous referee for raising questions and issues that helped to improve this work. 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. Additional support was provided by NASA through the Spitzer Space Telescope Fellowship Programand obtained from NASA Origins grant NNG04GG24G to the University of Texas at Austin. Support for the development of Bolocam was provided by NSF grants AST 99-80846 and AST 02-06158. M. L. E. acknowledges support of a Caltech Moore Fellowship and a Spitzer Space Telescope Postdoctoral Fellowship.
Funders:
Funding AgencyGrant Number
NASA1224608
NASA1230782
NASA1407
NASANNG04GG24G
NSFAST 99-80846
NSFAST 02-06158
Gordon and Betty Moore FoundationUNSPECIFIED
NASA Spitzer FellowshipUNSPECIFIED
Subject Keywords:infrared : ISM; ISM : clouds; ISM : individual (ophiuchus, perseus, serpens); stars : formation; submillimeter
Issue or Number:2
Record Number:CaltechAUTHORS:ENOapj08
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:ENOapj08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13492
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:14 May 2009 23:19
Last Modified:03 Oct 2019 00:39

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