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

被引：1205

作者：

Andre, Ph. ^{[1
]}

Men'shchikov, A. ^{[1
]}

Bontemps, S. ^{[1
]}

Koenyves, V. ^{[1
]}

Motte, F. ^{[1
]}

Schneider, N. ^{[1
]}

Didelon, P. ^{[1
]}

Minier, V. ^{[1
]}

Saraceno, P. ^{[5
]}

Ward-Thompson, D. ^{[3
]}

Di Francesco, J. ^{[10
]}

White, G. ^{[18
,21
]}

Molinari, S. ^{[5
]}

Testi, L. ^{[17
]}

Abergel, A. ^{[2
,20
]}

Griffin, M. ^{[3
]}

Henning, Th. ^{[11
]}

Royer, P. ^{[7
]}

Merin, B. ^{[13
]}

Vavrek, R. ^{[13
]}

Attard, M. ^{[1
]}

Arzoumanian, D. ^{[1
]}

Wilson, C. D. ^{[19
]}

Ade, P. ^{[3
]}

Aussel, H. ^{[1
]}

Baluteau, J. -P. ^{[4
]}

Benedettini, M. ^{[5
]}

Bernard, J. -Ph. ^{[6
]}

Blommaert, J. A. D. L. ^{[7
]}

Cambresy, L. ^{[8
]}

Cox, P. ^{[9
]}

Di Giorgio, A. ^{[5
]}

Hargrave, P. ^{[3
]}

Hennemann, M. ^{[1
]}

Huang, M. ^{[12
]}

Kirk, J. ^{[3
]}

Krause, O. ^{[11
]}

Launhardt, R. ^{[11
]}

Leeks, S. ^{[18
]}

Le Pennec, J. ^{[1
]}

Li, J. Z. ^{[12
]}

Martin, P. G. ^{[14
]}

Maury, A. ^{[1
]}

Olofsson, G. ^{[15
]}

Omont, A. ^{[16
]}

Peretto, N. ^{[1
]}

Pezzuto, S. ^{[5
]}

Prusti, T. ^{[22
]}

Roussel, H. ^{[16
]}

Russeil, D. ^{[4
]}

机构：

[1] Univ Paris Diderot, Lab AIM,CEA Saclay, CEA DSM CNRS, IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France

[2] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France

[3] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[4] Univ Aix Marseille 1, CNRS, INSU, Lab Astrophys Marseille, F-13388 Marseille 13, France

[5] INAF Ist Fis Spazio Interplanetario, I-00133 Rome, Italy

[6] Univ Toulouse, CNRS UPS, CESR, Observ Midi Pyrenees, F-31028 Toulouse 04, France

[7] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium

[8] Observ Strasbourg, CDS, F-67000 Strasbourg, France

[9] IRAM, F-38406 St Martin Dheres, France

[10] Herzberg Inst Astrophys, Natl Res Council Canada, Victoria, BC V9E 2E7, Canada

[11] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[12] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China

[13] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain

[14] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[15] AlbaNova Univ Ctr, Stockholm Observ, S-10691 Stockholm, Sweden

[16] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France

[17] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy

[18] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England

[19] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada

[20] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[21] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

[22] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

stars: formation; circumstellar matter; ISM: clouds; ISM: structure; submillimeter: ISM; OPHIUCHI MOLECULAR CLOUD; MASS FUNCTION; INTERSTELLAR CLOUDS; SCUBA SURVEY; PROTOSTARS; FRAGMENTATION; EMISSION; SPECTRA; CLUSTER; ORIGIN;

D O I：

10.1051/0004-6361/201014666

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 mu m 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 similar to 350 and 500 prestellar cores and similar to 45-60 Class 0 protostars can be identified in the Aquila field, while similar to 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.

引用

页数：7

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