A NIKA view of two star-forming infrared dark clouds: Dust emissivity variations and mass concentration

被引：13

作者：

Rigby, A. J. ^{[1
]}

Peretto, N. ^{[1
]}

Adam, R. ^{[2
,3
]}

Ade, P. ^{[1
]}

Andre, P. ^{[4
]}

Aussel, H. ^{[4
]}

Beelen, A. ^{[5
,6
]}

Benoit, A. ^{[7
,8
]}

Bracco, A. ^{[4
]}

Bideaud, A. ^{[7
,8
]}

Bourrion, O. ^{[2
]}

Calvo, M. ^{[7
,8
]}

Catalano, A. ^{[2
]}

Clarke, C. J. R. ^{[1
]}

Comis, B. ^{[2
]}

De Petris, M. ^{[9
]}

Desert, F-X ^{[10
]}

Doyle, S. ^{[1
]}

Driessen, E. F. C. ^{[11
]}

Goupy, J. ^{[7
,8
]}

Kramer, C. ^{[12
]}

Lagache, G. ^{[13
]}

Leclercq, S. ^{[11
]}

Lestrade, J-F ^{[14
]}

Macias-Perez, J. F. ^{[2
]}

Mauskopf, P. ^{[1
,15
,16
]}

Mayet, F. ^{[2
]}

Monfardini, A. ^{[7
,8
]}

Pascale, E. ^{[1
]}

Perotto, L. ^{[2
]}

Pisano, G. ^{[1
]}

Ponthieu, N. ^{[10
]}

Reveret, V ^{[4
]}

Ritacco, A. ^{[12
]}

Romero, C. ^{[11
]}

Roussel, H. ^{[17
]}

Ruppin, F. ^{[2
]}

Schuster, K. ^{[11
]}

Sievers, A. ^{[12
]}

Triqueneaux, S. ^{[7
,8
]}

Tucker, C. ^{[1
]}

Zylka, R. ^{[11
]}

机构：

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

[2] Univ Grenoble Alpes, CNRS, IN2P3, Lab Phys Subatom & Cosmol, 53 Ave Martyrs, Grenoble, France

[3] Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France

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

[5] CNRS, IAS, Orsay, France

[6] Univ Paris Sud, Orsay, France

[7] Inst Neel, CNRS, Grenoble, France

[8] Univ Grenoble Alpes, Grenoble, France

[9] Sapienza Univ Roma, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[10] Univ Grenoble Alpes, CNRS, IPAG, Inst Planetol & Astrophys Grenoble, F-38000 Grenoble, France

[11] IRAM, Grenoble, France

[12] IRAM, Granada, Spain

[13] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[14] Observ Paris, CNRS, LERMA, 61 Ave Observ, Paris, France

[15] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[16] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

[17] Inst Astrophys Paris, CNRS UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 615卷

基金：

欧洲研究理事会;

关键词：

stars: formation; submillimeter: ISM; ISM: clouds; dust; extinction; ISM: structure; GALACTIC PLANE; TEMPERATURE-DEPENDENCE; PHYSICAL-PROPERTIES; MOLECULAR CLOUDS; SIZE RELATION; HI-GAL; CATALOG; GLIMPSE; SAMPLE;

D O I：

10.1051/0004-6361/201732258

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The thermal emission of dust grains is a powerful tool for probing cold, dense regions of molecular gas in the interstellar medium, and so constraining dust properties is key to obtaining accurate measurements of dust mass and temperature. Aims. By placing constraints on the dust emissivity spectral index, beta, towards two star-forming infrared dark clouds SDC18.888-0.476 and SDC24.489-0.689-we aim to evaluate the role of mass concentration in the associated star-formation activity. Methods. We exploited the simultaneous 1.2 and 2.0 mm imaging capability of the NIKA camera on the IRAM 3 '' m telescope to construct maps of beta for both clouds, and by incorporating Herschel observations, we created H-2 column density maps with 13 '' angular resolution. Results. While we find no significant systematic radial variations around the most massive clumps in either cloud on greater than or similar to 0.1 pc scales, their mean beta values are significantly different, with (beta) over bar = 2.07 +/- 0.09 (random) +/- 0.25 (systematic) for SDC18.888-0.476 and (beta) over bar= 1.71 +/- 0.09 (random) +/- 0.25 (systematic) for SDC24.489-0.689. These differences could be a consequence of the very different environments in which both clouds lie, and we suggest that the proximity of SDC18.888-0.476 to the W39 H-II region may raise beta on scales of similar to 1 pc. We also find that the mass in SDC24.489-0.689 is more centrally concentrated and circularly symmetric than in SDC18.888-0.476, and is consistent with a scenario in which spherical globally-collapsing clouds concentrate a higher fraction of their mass into a single core than elongated clouds that will more easily fragment, distributing their mass into many cores. Conclusions. We demonstrate that beta variations towards interstellar clouds can be robustly constrained with high signal-to-noise ratio (S/N) NIKA observations, providing more accurate estimates of their masses. The methods presented here will be applied to the Galactic Star Formation with NIKA2 (GASTON) guaranteed time large programme, extending our analysis to a statistically significant sample of star-forming clouds.

引用

页数：19

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