Detection of two power-law tails in the probability distribution functions of massive GMCs

被引：57

作者：

Schneider, N. ^{[1
,2
]}

Bontemps, S. ^{[1
]}

Girichidis, P. ^{[3
]}

Rayner, T. ^{[4
]}

Motte, F. ^{[5
]}

Andre, Ph ^{[5
]}

Russeil, D. ^{[6
]}

Abergel, A. ^{[7
]}

Anderson, L. ^{[8
]}

Arzoumanian, D. ^{[7
]}

Benedettini, M. ^{[9
]}

Csengeri, T. ^{[10
]}

Didelon, P. ^{[5
]}

Di Francesco, J. ^{[11
]}

Griffin, M.

Hill, T. ^{[12
]}

Klessen, R. S. ^{[13
]}

Ossenkopf, V. ^{[2
]}

Pezzuto, S. ^{[9
]}

Rivera-Ingraham, A. ^{[14
]}

Spinoglio, L. ^{[9
]}

Tremblin, P. ^{[5
,15
]}

Zavagno, A. ^{[5
]}

机构：

[1] OASU LAB Univ Bordeaux, CNRS, UMR5804, F-33270 Floirac, France

[2] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany

[3] Max Planck Inst Astrophys, D-85741 Garching, Germany

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

[5] Univ Paris Diderot, Lab AIM CNRS, IRFU SAp CEA DSM, F-91191 Gif Sur Yvette, France

[6] AIX Marseille Univ, CNRS, UMR 7326, LAM, F-13388 Marseille, France

[7] Univ Paris 11, CNRS, UMR8617, IAS, F-91400 Orsay, France

[8] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA

[9] INAF, IAPS, I-00133 Rome, Italy

[10] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[11] NRC, Herzberg Inst Astrophys, Victoria, BC, Canada

[12] Joint ALMA Observ, Santiago, Chile

[13] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany

[14] ESA, ESAC, Madrid, Spain

[15] Univ Exeter, Astrophys Grp, Exeter EX4 4QJ, Devon, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 453卷 / 01期

基金：

欧洲研究理事会;

关键词：

ISM: clouds; dust; extinction; MOLECULAR CLOUDS; COLUMN DENSITY; STAR-FORMATION; HERSCHEL; ACCRETION; FILAMENTS; ORION;

D O I：

10.1093/mnrasl/slv101

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC 6334), obtained from dust emission observed withHerschel. The low column density range can be fitted with a lognormal distribution. A first power-law tail starts above an extinctionof similar to 6-14. It has a slope of alpha = 1.3-2 for the rho aaEuro profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. AboveA(V) similar to 40, 60, and 140, we detect an excess that can be fitted by a flatter power-law tail with alpha > 2. It correlates with the central regions of the cloud (ridges/hubs) of size similar to 1 pc and densities above 10(4) cm(-3). This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: (1) rotation, which introduces an angular momentum barrier, (2) increasing optical depth and weaker cooling, (3) magnetic fields, (4) geometrical effects, and (5) protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.

引用

页码：L41 / L45

页数：5

共 45 条

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