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The rate and latency of star formation in dense, massive clumps in the Milky Way

Heyer, M., Gutermuth, R., Urquhart, J.S., Csengeri, T., Wienen, M., Leurini, S., Menten, K., Wyrowski, F. (2016) The rate and latency of star formation in dense, massive clumps in the Milky Way. Astronomy and Astrophysics, 588 . ISSN 0004-6361. (doi:10.1051/0004-6361/201527681) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided. (Contact us about this Publication)
Official URL
http://dx.doi.org/10.1051/0004-6361/201527681

Abstract

Context. Newborn stars form within the localized, high density regions of molecular clouds. The sequence and rate at which stars form in dense clumps and the dependence on local and global environments are key factors in developing descriptions of stellar production in galaxies. Aims. We seek to observationally constrain the rate and latency of star formation in dense massive clumps that are distributed throughout the Galaxy and to compare these results to proposed prescriptions for stellar production. Methods. A sample of 24 ?m-based Class I protostars are linked to dust clumps that are embedded within molecular clouds selected from the APEX Telescope Large Area Survey of the Galaxy. We determine the fraction of star-forming clumps, f?, that imposes a constraint on the latency of star formation in units of a clump’s lifetime. Protostellar masses are estimated from models of circumstellar environments of young stellar objects from which star formation rates are derived. Physical properties of the clumps are calculated from 870 ?m dust continuum emission and NH3 line emission. Results. Linear correlations are identified between the star formation rate surface density, ?SFR, and the quantities ?H2/?ff and ?H2/?cross, suggesting that star formation is regulated at the local scales of molecular clouds. The measured fraction of star forming clumps is 23%. Accounting for star formation within clumps that are excluded from our sample due to 24 ?m saturation, this fraction can be as high as 31%, which is similar to previous results. Dense, massive clumps form primarily low mass (<1–2 M?) stars with emergent 24 ?m fluxes below our sensitivity limit or are incapable of forming any stars for the initial 70% of their lifetimes. The low fraction of star forming clumps in the Galactic center relative to those located in the disk of the Milky Way is verified.

Item Type: Article
DOI/Identification number: 10.1051/0004-6361/201527681
Additional information: Unmapped bibliographic data: C7 - A29 [EPrints field already has value set] LA - English [Field not mapped to EPrints] J2 - Astron. Astrophys. [Field not mapped to EPrints] AD - Department of Astronomy, University of Massachusetts, Amherst, MA, United States [Field not mapped to EPrints] AD - Max Planck Institute for Radio Astronomy, Auf dem Hugel 69, Bonn, Germany [Field not mapped to EPrints] AD - Centre for Astrophysics and Planetary Science, University of Kent, Canterbury, United Kingdom [Field not mapped to EPrints] M3 - Article [Field not mapped to EPrints] DB - Scopus [Field not mapped to EPrints]
Uncontrolled keywords: Galaxy: disk, Infrared: stars, Stars: formation, Stars: protostars, Submillimeter: ISM, Clouds, Dust, Galaxies, Solar system, Galaxy: disks, Infrared: star, Stars: formation, Stars: protostars, Submillimeter: isms, Stars
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: James Urquhart
Date Deposited: 04 May 2016 13:55 UTC
Last Modified: 29 May 2019 17:17 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/55232 (The current URI for this page, for reference purposes)
Urquhart, J.S.: https://orcid.org/0000-0002-1605-8050
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