TWO MASS DISTRIBUTIONS IN THE L 1641 MOLECULAR CLOUDS: THE HERSCHEL CONNECTION OF DENSE CORES AND FILAMENTS IN ORION A

被引：102

作者：

Polychroni, D. ^{[1
,2
]}

Schisano, E. ^{[2
,3
]}

Elia, D. ^{[2
]}

Roy, A. ^{[4
]}

Molinari, S. ^{[2
]}

Martin, P. ^{[5
]}

Andre, Ph. ^{[4
]}

Turrini, D. ^{[2
]}

Rygl, K. L. J. ^{[2
]}

Di Francesco, J. ^{[6
,7
]}

Benedettini, M. ^{[2
]}

Busquet, G. ^{[2
]}

di Giorgio, A. M. ^{[2
]}

Pestalozzi, M. ^{[2
]}

Pezzuto, S. ^{[2
]}

Arzoumanian, D. ^{[8
]}

Bontemps, S. ^{[9
]}

Hennemann, M. ^{[4
,10
]}

Hill, T. ^{[4
]}

Koenyves, V. ^{[4
,8
]}

Men'shchikov, A. ^{[4
]}

Motte, F. ^{[4
]}

Nguyen-Luong, Q. ^{[5
]}

Peretto, N. ^{[11
]}

Schneider, N. ^{[9
]}

White, G. ^{[12
,13
]}

机构：

[1] Univ Athens, Dept Astrophys, Fac Phys, Athens 15784, Greece

[2] Ist Astrofis & Planetol Spaziali INAF IAPS, I-00133 Rome, Italy

[3] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA

[4] CEA IRFU CNRS INSU Univ Paris Diderot, Lab AIM, F-91191 Gif Sur Yvette, France

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

[6] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada

[7] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada

[8] Univ Paris 11, IAS, CNRS UMR 8617, F-91400 Orsay, France

[9] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS INSU, UMR 5804, F-33271 Floirac, France

[10] MPIA Heidelberg, Heidelberg, Germany

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

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

[13] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2013年 / 777卷 / 02期

关键词：

infrared: ISM; ISM: clouds; ISM: individual objects (L1641); stars: formation; stars: low-mass; YOUNG STELLAR OBJECTS; HI-GAL SURVEY; STAR-FORMATION; PROTOSTARS; POPULATION; EMISSION; CENSUS; ORIGIN; AQUILA; IMF;

D O I：

10.1088/2041-8205/777/2/L33

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present Herschel survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of the dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there, is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 M-circle dot and drives the shape of the core mass function (CMF) at higher masses, which we fit with a power law of the form dN/dlog M proportional to M (1.4 +/- 0.4). The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8 M-circle dot and leads to a flattening of the CMF at masses lower than similar to 4 M-circle dot. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud.

引用

页数：5

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