Details

Autor(en) / Beteiligte

• André, Ph
• Men'shchikov, A.
• Bontemps, S.
• Könyves, V.
• Motte, F.
• Schneider, N.
• Didelon, P.
• Minier, V.
• Saraceno, P.
• Ward-Thompson, D.
• Di Francesco, J.
• White, G.
• Molinari, S.
• Testi, L.
• Abergel, A.
• Griffin, M.
• Henning, Th
• Royer, P.
• Merín, B.
• Vavrek, R.
• Attard, M.
• Arzoumanian, D.
• Wilson, C. D.
• Ade, P.
• Aussel, H.
• Baluteau, J.-P.
• Benedettini, M.
• Bernard, J.-Ph
• Blommaert, J. A. D. L.
• Cambrésy, L.
• Cox, P.
• Di Giorgio, A.
• Hargrave, P.
• Hennemann, M.
• Huang, M.
• Kirk, J.
• Krause, O.
• Launhardt, R.
• Leeks, S.
• Le Pennec, J.
• Li, J. Z.
• Martin, P. G.
• Maury, A.
• Olofsson, G.
• Omont, A.
• Peretto, N.
• Pezzuto, S.
• Prusti, T.
• Roussel, H.
• Russeil, D.
• Sauvage, M.
• Sibthorpe, B.
• Sicilia-Aguilar, A.
• Spinoglio, L.
• Waelkens, C.
• Woodcraft, A.
• Zavagno, A.

Titel

From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey

Ist Teil von

• Astronomy and astrophysics (Berlin), 2010-07, Vol.518 (1), p.L102

Ort / Verlag

Les Ulis: EDP Sciences

Erscheinungsjahr

2010

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• 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 μm 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 ~300 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.