The Herschel Space Observatory view of dust in M81

被引：133

作者：

Bendo, G. J. ^{[1
]}

Wilson, C. D. ^{[2
]}

Pohlen, M. ^{[3
]}

Sauvage, M. ^{[4
]}

Auld, R. ^{[3
]}

Baes, M. ^{[5
]}

Barlow, M. J. ^{[6
]}

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

Boselli, A. ^{[9
]}

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

Buat, V. ^{[9
]}

Castro-Rodriguez, N. ^{[10
]}

Chanial, P. ^{[4
]}

Charlot, S. ^{[11
]}

Ciesla, L. ^{[9
]}

Clements, D. L. ^{[1
]}

Cooray, A.

Cormier, D. ^{[4
]}

Cortese, L. ^{[3
]}

Davies, J. I. ^{[3
]}

Dwek, E. ^{[12
]}

Eales, S. A. ^{[3
]}

Elbaz, D. ^{[4
]}

Galametz, M. ^{[4
]}

Galliano, F. ^{[4
]}

Gear, W. K. ^{[3
]}

Glenn, J. ^{[13
]}

Gomez, H. L. ^{[3
]}

Griffin, M. ^{[3
]}

Hony, S. ^{[4
]}

Isaak, K. G. ^{[14
]}

Levenson, L. R. ^{[7
,8
]}

Lu, N. ^{[7
,8
]}

Madden, S. ^{[4
]}

O'Halloran, B. ^{[1
]}

Okumura, K. ^{[4
]}

Oliver, S. ^{[15
]}

Page, M. J. ^{[16
]}

Panuzzo, P. ^{[4
]}

Papageorgiou, A. ^{[3
]}

Parkin, T. J. ^{[2
]}

Perez-Fournon, I. ^{[10
]}

Rangwala, N. ^{[13
]}

Rigby, E. E. ^{[17
]}

Roussel, H. ^{[11
]}

Rykala, A. ^{[3
]}

Sacchi, N. ^{[18
]}

Schulz, B. ^{[19
]}

Schirm, M. R. P. ^{[2
]}

Smith, M. W. L. ^{[3
]}

机构：

[1] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England

[2] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada

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

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

[5] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium

[6] UCL, Dept Phys & Astron, London WC1E 6BT, England

[7] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[8] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[9] CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille, France

[10] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain

[11] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France

[12] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA

[13] Univ Colorado, Dept Astrophys & Planetary Sci, CASA CB 389, Boulder, CO 80309 USA

[14] Estec, ESA Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands

[15] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9RH, E Sussex, England

[16] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[17] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

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

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

[20] Univ Hertfordshire, Sci & Technol Res Ctr, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

[21] Univ Padua, Dept Astron, I-35122 Padua, Italy

[22] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France

[23] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[24] Univ Vienna, Inst Astron, A-1180 Vienna, Austria

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

galaxies: ISM; galaxies: spiral; galaxies: individual: M81; STAR-FORMATION RATES; H-ALPHA; GALAXIES; TELESCOPE; EMISSION; SPITZER; THINGS; FIELD;

D O I：

10.1051/0004-6361/201014568

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use Herschel Space Observatory data to place observational constraints on the peak and Rayleigh-Jeans slope of dust emission observed at 70-500 mu m in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 mu m are primarily dependent on radius but that the ratio of 70 to 160 mu m emission shows no clear dependence on surface brightness or radius. These results along with analyses of the spectral energy distributions imply that the 160-500 mu m emission traces 15-30 K dust heated by evolved stars in the bulge and disc whereas the 70 mu m emission includes dust heated by the active galactic nucleus and young stars in star forming regions.

引用

页数：4

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