On the shape of the mass-function of dense clumps in the Hi-GAL fields: I. Spectral energy distribution determination and global properties of the mass-functions

Olmi, Luca and Anglés-Alcázar, Daniel and Elia, D. and Molinari, Sergio and Montier, Ludovic A. and Pestalozzi, Michele R. and Pezzuto, Stefano and Polychroni, Danae and Ristorcelli, Isabelle and Rodón, Javier A. and Schisano, Eugenio and Smith, Michael D. and Testi, Leonardo and Thompson, Mark A. (2013) On the shape of the mass-function of dense clumps in the Hi-GAL fields: I. Spectral energy distribution determination and global properties of the mass-functions. Astronomy & Astrophysics, 551 . p. 20409. ISSN 0004-6361. (doi:https://doi.org/10.1051/0004-6361/201220409) (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)

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Official URL
http://www.dx.doi.org/10.1051/0004-6361/201220409

Abstract

Context. Stars form in dense, dusty clumps of molecular clouds, but little is known about their origin and evolution. In particular, the relationship between the mass distribution of these clumps (also known as the clump mass function or CMF) and the stellar initial mass function (IMF), is still poorly understood. Aims. To discern the “true” shape of the CMF and to better understand how the CMF may evolve toward the IMF, large samples of bona-fide pre- and proto-stellar clumps are required. The sensitive observations of the Herschel Space Observatory (HSO) are now allowing us to look at large clump populations in various clouds with different physical conditions.

Item Type: Article
Uncontrolled keywords: stars ; formation ; pre-main sequence ; ISM ; clouds ; structure
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 10 Aug 2015 15:45 UTC
Last Modified: 11 Aug 2015 10:15 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/50083 (The current URI for this page, for reference purposes)
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