PACS and SPIRE photometer maps of M33: First results of the HERschel M33 Extended Survey (HERM33ES)

被引：66

作者：

Kramer, C. ^{[1
]}

Buchbender, C. ^{[1
]}

Xilouris, E. M. ^{[2
]}

Boquien, M. ^{[3
]}

Braine, J. ^{[4
]}

Calzetti, D. ^{[3
]}

Lord, S. ^{[5
]}

Mookerjea, B. ^{[6
]}

Quintana-Lacaci, G. ^{[1
]}

Relano, M. ^{[7
]}

Stacey, G. ^{[8
]}

Tabatabaei, F. S. ^{[9
]}

Verley, S. ^{[10
]}

Aalto, S. ^{[11
]}

Akras, S. ^{[2
]}

Albrecht, M. ^{[12
]}

Anderl, S. ^{[12
]}

Beck, R. ^{[9
]}

Bertoldi, F. ^{[12
]}

Combes, F. ^{[13
]}

Dumke, M. ^{[14
]}

Garcia-Burillo, S. ^{[15
]}

Gonzalez, M. ^{[1
]}

Gratier, P. ^{[4
]}

Guesten, R. ^{[9
]}

Henkel, C. ^{[9
]}

Israel, F. P. ^{[16
]}

Koribalski, B. ^{[17
]}

Lundgren, A. ^{[14
]}

Martin-Pintado, J. ^{[18
]}

Roellig, M. ^{[19
]}

Rosolowsky, E. ^{[20
]}

Schuster, K. F. ^{[21
]}

Sheth, K. ^{[22
]}

Sievers, A. ^{[1
]}

Stutzki, J. ^{[19
]}

Tilanus, R. P. J. ^{[23
]}

van der Tak, F. ^{[24
]}

van der Werf, P. ^{[16
]}

Wiedner, M. C. ^{[13
]}

机构：

[1] Inst Radioastron Milimetr, Nucleo Cent, Granada 18012, Spain

[2] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece

[3] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

[4] Univ Bordeaux 1, Lab Astrophys Bordeaux, Observ Bordeaux, OASU,UMR 5804,CNRS INSU, F-33270 Floirac, France

[5] CALTECH, IPAC, Pasadena, CA 91125 USA

[6] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India

[7] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[8] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA

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

[10] Univ Granada, Dept Fis Teor Cosmos, E-18071 Granada, Spain

[11] Chalmers, Onsala Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden

[12] Argelander Inst Astron, D-53121 Bonn, Germany

[13] CNRS, LERMA, Observ Paris, F-75014 Paris, France

[14] ESO, Santiago 19, Chile

[15] Observ Madrid, OAN, Madrid 28014, Spain

[16] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[17] CSIRO, ATNF, Epping, NSW 1710, Australia

[18] CSIC, INTA, Ctr Astrobiol, Madrid 28850, Spain

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

[20] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada

[21] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France

[22] CALTECH, Pasadena, CA 91125 USA

[23] Joint Astron Ctr, Hilo, HI 96720 USA

[24] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

galaxies: individual: M33; galaxies: evolution; Local Group; galaxies: ISM; dust; extinction; INFRARED STRUCTURE; STAR-FORMATION; GALAXY M33; COLD DUST; MILKY-WAY; EMISSION; NEARBY; CLOUD;

D O I：

10.1051/0004-6361/201014613

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Within the framework of the HERM33ES key program, we are studying the star forming interstellar medium in the nearby, metal-poor spiral galaxy M33, exploiting the high resolution and sensitivity of Herschel. Aims. We use PACS and SPIRE maps at 100, 160, 250, 350, and 500 mu m wavelength, to study the variation of the spectral energy distributions (SEDs) with galacto-centric distance. Methods. Detailed SED modeling is performed using azimuthally averaged fluxes in elliptical rings of 2 kpc width, out to 8 kpc galacto-centric distance. Simple isothermal and two-component grey body models, with fixed dust emissivity index, are fitted to the SEDs between 24 mu m and 500 mu m using also MIPS/Spitzer data, to derive first estimates of the dust physical conditions. Results. The far-infrared and submillimeter maps reveal the branched, knotted spiral structure of M33. An underlying diffuse disk is seen in all SPIRE maps (250-500 mu m). Two component fits to the SEDs agree better than isothermal models with the observed, total and radially averaged flux densities. The two component model, with beta fixed at 1.5, best fits the global and the radial SEDs. The cold dust component clearly dominates; the relative mass of the warm component is less than 0.3% for all the fits. The temperature of the warm component is not well constrained and is found to be about 60 K +/- 10 K. The temperature of the cold component drops significantly from similar to 24 K in the inner 2 kpc radius to 13 K beyond 6 kpc radial distance, for the best fitting model. The gas-to-dust ratio for beta = 1.5, averaged over the galaxy, is higher than the solar value by a factor of 1.5 and is roughly in agreement with the subsolar metallicity of M33.

引用

页数：5

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