The physical properties of the dust in the RCW 120 H II region as seen by Herschel

被引：47

作者：

Anderson, L. D. ^{[1
,2
]}

Zavagno, A. ^{[1
,2
]}

Rodon, J. A. ^{[1
,2
]}

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

Abergel, A. ^{[3
]}

Ade, P. ^{[4
]}

Andre, P. ^{[5
]}

Arab, H. ^{[3
]}

Baluteau, J. -P. ^{[1
,2
]}

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

Blagrave, K. ^{[7
]}

Bontemps, S. ^{[8
]}

Boulanger, F. ^{[3
]}

Cohen, M. ^{[9
]}

Compiegne, M. ^{[7
]}

Cox, P. ^{[10
]}

Dartois, E. ^{[3
]}

Davis, G.

Emery, R. ^{[11
]}

Fulton, T. ^{[12
]}

Gry, C. ^{[1
,2
]}

Habart, E. ^{[3
]}

Huang, M.

Joblin, C. ^{[6
]}

Jones, S. C. ^{[13
]}

Kirk, J. M. ^{[4
]}

Lagache, G. ^{[3
]}

Lim, T. ^{[11
]}

Madden, S. ^{[5
]}

Makiwa, G. ^{[13
]}

Martin, P. ^{[7
]}

Miville-Deschenes, M. -A. ^{[3
]}

Molinari, S. ^{[14
]}

Moseley, H.

Motte, F. ^{[5
]}

Naylor, D. A. ^{[13
]}

Okumura, K. ^{[5
]}

Goncalves, D. Pinheiro ^{[7
]}

Polehampton, E. ^{[11
,13
]}

Saraceno, P. ^{[14
]}

Sauvage, M. ^{[5
]}

Sidher, S. ^{[11
]}

Spencer, L. ^{[13
]}

Swinyard, B. ^{[11
]}

Ward-Thompson, D. ^{[4
]}

White, G. J. ^{[11
,15
]}

机构：

[1] CNRS, Lab Astrophys Marseille, UMR 6110, F-13388 Marseille 13, France

[2] Univ Aix Marseille 1, F-13388 Marseille 13, France

[3] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France

[4] Cardiff Univ, Dept Phys & Astron, Cardiff, S Glam, Wales

[5] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France

[6] Univ Toulouse UPS, CESR, CNRS, UMR 5187, F-31028 Toulouse 4, France

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

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

[9] Univ Calif, Radio Astron Lab, Us Berkeley, CA 94720 USA

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

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

[12] Blue Sky Spect Inc, Lethbridge, AB, Canada

[13] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

HII regions; ISM: individual objects: RCW120; dust; extinction; photon-dominated region (PDR); stars: formation infrared: ISM; BUBBLING GALACTIC DISK; 70; MU-M; SPECTRAL INDEX; STAR-FORMATION; TEMPERATURE; EMISSION; NOISE; BORDERS; PLANE;

D O I：

10.1051/0004-6361/201014657

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. RCW 120 is a well-studied, nearby Galactic Hii region with ongoing star formation in its surroundings. Previous work has shown that it displays a bubble morphology at mid-infrared wavelengths, and has a massive layer of collected neutral material seen at sub-mm wavelengths. Given the well-defined photo-dissociation region (PDR) boundary and collected layer, it is an excellent laboratory to study the "collect and collapse" process of triggered star formation. Using Herschel Space Observatory data at 100, 160, 250, 350, and 500 mu m, in combination with Spitzer and APEX-LABOCA data, we can for the first time map the entire spectral energy distribution of an Hii region at high angular resolution. Aims. We seek a better understanding of RCW 120 and its local environment by analysing its dust temperature distribution. Additionally, we wish to understand how the dust emissivity index, beta, is related to the dust temperature. Methods. We determine dust temperatures in selected regions of the RCW 120 field by fitting their spectral energy distribution (SED), derived using aperture photometry. Additionally, we fit the SED extracted from a grid of positions to create a temperature map. Results. We find a gradient in dust temperature, ranging from greater than or similar to 30K in the interior of RCW 120, to similar to 20 K for the material collected in the PDR, to similar to 10 K toward local infrared dark clouds and cold filaments. There is an additional, hotter (similar to 100 K) component to the dust emission that we do not investigate here. Our results suggest that RCW 120 is in the process of destroying the PDR delineating its bubble morphology. The leaked radiation from its interior may influence the creation of the next generation of stars. We find support for an anti-correlation between the fitted temperature and beta, in rough agreement with what has been found previously. The extended wavelength coverage of the Herschel data greatly increases the reliability of this result.

引用

页数：5

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