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20 April 2024

» arxiv » 1005.2618

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Initial highlights from the Herschel Gould Belt survey
Ph. André ; A. Men'shchikov ; S. Bontemps ; V. Könyves ; F. Motte ; N. Schneider ; P. Didelon ; V. Minier ; P. Saraceno ; D. Ward-Thompson ; J. Di Francesco ; G. White ; S. Molinari ; L. Testi ; A. Abergel ; M. Griffin ; Th. Henning ; P. Royer ; B. Merín ; R. Vavrek ; M. Attard ; D. Arzoumanian ; C. D. Wilson ; P. Ade ; H. Aussel ; J.-P. Baluteau ; M. Benedettini ; J.-Ph. Bernard ; J.A.D.L. Blommaert ; L. Cambrésy ; P. Cox ; A. Di Giorgio ; P. Hargrave ; M. Hennemann ; M. Huang ; J. Kirk ; O. Krause ; R. Launhardt ; S. Leeks ; J. Le Pennec ; J.Z. Li ; P. Martin ; A. Maury ; G. Olofsson ; A. Omont ; N. Peretto ; S. Pezzuto ; T. Prusti ; H. Roussel ; D. Russeil ; M. Sauvage ; B. Sibthorpe ; A. Sicilia-Aguilar ; L. Spinoglio ; C. Waelkens ; A. Woodcraft ; A. Zavagno ;
Date:	14 May 2010
Abstract:	We summarize the first results from the Gould Belt survey, obtained toward the Aquila Rift and Polaris Flare regions during the ’science demonstration phase’ of Herschel. Our 70-500 micron images taken in parallel mode with the SPIRE and PACS cameras reveal a wealth of filamentary structure, as well as numerous dense cores embedded in the filaments. Between ~ 350 and 500 prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquila field, while ~ unbound starless cores and no protostars are observed in the Polaris field. The prestellar core mass function (CMF) derived for the Aquila region bears a strong resemblance to the stellar initial mass function (IMF), already confirming the close connection between the CMF and the IMF with much better statistics than earlier studies. Comparing and contrasting our Herschel results in Aquila and Polaris, we propose an observationally-driven scenario for core formation according to which complex networks of long, thin filaments form first within molecular clouds, and then the densest filaments fragment into a number of prestellar cores via gravitational instability.
Source:	arXiv, 1005.2618
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