A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey

被引：379

作者：

Koenyves, V. ^{[1
,2
]}

Andre, Ph. ^{[1
]}

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

Palmeirim, P. ^{[1
]}

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

Schneider, N. ^{[1
,3
,4
]}

Roy, A. ^{[1
]}

Didelon, P. ^{[1
]}

Maury, A. ^{[1
]}

Shimajiri, Y. ^{[1
]}

Di Francesco, J. ^{[5
,6
]}

Bontemps, S. ^{[3
,4
]}

Peretto, N. ^{[1
,7
]}

Benedettini, M. ^{[8
]}

Bernard, J. -Ph. ^{[9
,10
]}

Elia, D. ^{[8
]}

Griffin, M. J. ^{[7
]}

Hill, T. ^{[1
,11
]}

Kirk, J. ^{[12
]}

Ladjelate, B. ^{[1
]}

Marsh, K. ^{[7
]}

Martin, P. G. ^{[13
]}

Motte, F. ^{[1
]}

Lu'o'ng, Q. Nguyen ^{[1
,13
,14
]}

Pezzuto, S. ^{[8
]}

Roussel, H. ^{[15
]}

Rygl, K. L. J. ^{[16
,17
]}

Sadavoy, S. I. ^{[5
,6
,18
]}

Schisano, E. ^{[8
]}

Spinoglio, L. ^{[8
]}

Ward-Thompson, D. ^{[12
]}

White, G. J. ^{[19
,20
]}

机构：

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

[2] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France

[3] Univ Bordeaux, LAB, UMR5804, F-33270 Floirac, France

[4] CNRS, LAB, UMR5804, F-33270 Floirac, France

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

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

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

[8] INAF, Ist Astrofis & Planetol, I-00133 Rome, Italy

[9] CNRS, IRAP, F-31028 Toulouse 4, France

[10] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France

[11] Joint ALMA Observ, Santiago, Chile

[12] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

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

[14] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[15] Univ Paris 06, Sorbonne Univ, CNRS, Inst Astrophys Paris,UMR 7095, F-75014 Paris, France

[16] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci & Robot Explorat, Sci Support Off, NL-2201 AZ Noordwijk, Netherlands

[17] INAF IRA, I-40129 Bologna, Italy

[18] MPIA, D-69117 Heidelberg, Germany

[19] Rutherford Appleton Lab, RALSpace, Didcot OX11 0QX, Oxon, England

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

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 584卷

基金：

美国国家航空航天局; 欧洲研究理事会;

关键词：

ISM: individual objects: Aquila Rift complex; stars: formation; ISM: clouds; ISM: structure; submillimeter: ISM; STAR-FORMATION RATE; MOLECULAR CLOUD; INITIAL CONDITIONS; PRESTELLAR CORES; FORMATION RATES; MASS FUNCTION; SPITZER C2D; LARGE-SCALE; FILAMENTARY STRUCTURES; DUST TEMPERATURE;

D O I：

10.1051/0004-6361/201525861

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present and discuss the results of the Herschel Gould Belt survey (HGBS) observations in an similar to 11 deg(2) area of the Aquila molecular cloud complex at d similar to 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from 70 mu m to 500 mu m. Using the multi-scale, multi-wavelength source extraction algorithm getsources, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, similar to 60% +/- 10% of which are gravitationally bound prestellar cores, and they will likely form stars in the future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of similar to 40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is similar to 1 Myr, which is typically similar to 4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the Herschel-identified prestellar cores are located above a background column density corresponding to AV similar to 7, and similar to 75% of them lie within filamentary structures with supercritical masses per unit length greater than or similar to 16 M-circle dot/pc. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF) result primarily from the gravitational fragmentation of marginally supercritical filaments. Given that filaments appear to dominate the mass budget of dense gas at A(V) > 7, our findings also suggest that the physics of prestellar core formation within filaments is responsible for a characteristic "efficiency" SFR/M-dense similar to 5(-2)(+2) x 10(-8) yr(-1) for the star formation process in dense gas.

引用

页数：33

共 150 条

[1] Herschel view of the large-scale structure in the Chamaeleon dark clouds [J].

Alves de Oliveira, C. ;

Schneider, N. ;

Merin, B. ;

Prusti, T. ;

Ribas, A. ;

Cox, N. L. J. ;

Vavrek, R. ;

Koenyves, V. ;

Arzoumanian, D. ;

Puga, E. ;

Pilbratt, G. L. ;

Kospal, A. ;

Andre, Ph ;

Didelon, P. ;

Men'shchikov, A. ;

Royer, P. ;

Waelkens, C. ;

Bontemps, S. ;

Winston, E. ;

Spezzi, L. .

ASTRONOMY & ASTROPHYSICS, 2014, 568

[2] The mass function of dense molecular cores and the origin of the IMF [J].

Alves, J. ;

Lombardi, M. ;

Lada, C. J. .

ASTRONOMY & ASTROPHYSICS, 2007, 462 (01) :L17-L21

[3] Internal structure of a cold dark molecular cloud inferred from the extinction of background starlight [J].

Alves, JF ;

Lada, CJ ;

Lada, EA .

NATURE, 2001, 409 (6817) :159-161

[4]

Andre P., 2000, Protostars and planets 4, P59

[5] The initial conditions of star formation in the Ophiuchus main cloud:: Kinematics of the protocluster condensations [J].

Andre, Ph. ;

Belloche, A. ;

Motte, F. ;

Peretto, N. .

ASTRONOMY & ASTROPHYSICS, 2007, 472 (02) :519-535

[6] From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey [J].

Andre, Ph. ;

Men'shchikov, A. ;

Bontemps, S. ;

Koenyves, 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. ;

Merin, 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. ;

Cambresy, 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. .

ASTRONOMY & ASTROPHYSICS, 2010, 518

[7]

[Anonymous], 2014, arXiv:1312.6232, DOI [DOI 10.2458/AZUUAPRESS9780816531240-CH002, 10.2458/azu_uapress_ 9780816531240-ch002, DOI 10.2458/AZU_UAPRESS_9780816531240-CH002, 10.2458/azuuapress9780816531240-ch002]

[8]

[Anonymous], 2014, Protostars and Planets, DOI [10.2458/azu_uapress_9780816531240, DOI 10.2458/AZU_UAPRESS_9780816531240]

[9]

[Anonymous], 1993, Protostars and Planets III

[10] Characterizing interstellar filaments with Herschel in IC 5146 [J].

Arzoumanian, D. ;

Andre, Ph. ;

Didelon, P. ;

Koenyves, V. ;

Schneider, N. ;

Men'shchikov, A. ;

Sousbie, T. ;

Zavagno, A. ;

Bontemps, S. ;

Di Francesco, J. ;

Griffin, M. ;

Hennemann, M. ;

Hill, T. ;

Kirk, J. ;

Martin, P. ;

Minier, V. ;

Molinari, S. ;

Motte, F. ;

Peretto, N. ;

Pezzuto, S. ;

Spinoglio, L. ;

Ward-Thompson, D. ;

White, G. ;

Wilson, C. D. .

ASTRONOMY & ASTROPHYSICS, 2011, 529

← 1 2 3 4 5 6 7 8 9 10 →