HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

被引：108

作者：

Meixner, M. ^{[1
,31
]}

Galliano, F. ^{[2
]}

Hony, S. ^{[2
]}

Roman-Duval, J. ^{[1
]}

Robitaille, T. ^{[3
]}

Panuzzo, P. ^{[2
]}

Sauvage, M. ^{[2
]}

Gordon, K. ^{[1
]}

Engelbracht, C. ^{[4
]}

Misselt, K. ^{[4
]}

Okumura, K. ^{[2
]}

Beck, T. ^{[1
]}

Bernard, J. -P. ^{[5
]}

Bolatto, A. ^{[6
]}

Bot, C. ^{[7
]}

Boyer, M. ^{[1
]}

Bracker, S. ^{[8
]}

Carlson, L. R. ^{[9
]}

Clayton, G. C. ^{[10
]}

Chen, C. -H. R. ^{[11
,12
]}

Churchwell, E. ^{[8
]}

Fukui, Y. ^{[13
]}

Galametz, M. ^{[2
]}

Hora, J. L. ^{[3
]}

Hughes, A. ^{[14
]}

Indebetouw, R. ^{[11
,12
]}

Israel, F. P. ^{[15
]}

Kawamura, A. ^{[13
]}

Kemper, F. ^{[16
]}

Kim, S. ^{[17
]}

Kwon, E. ^{[17
]}

Lawton, B. ^{[1
]}

Li, A. ^{[18
]}

Long, K. S. ^{[1
]}

Marengo, M. ^{[19
]}

Madden, S. C. ^{[2
]}

Matsuura, M. ^{[20
,21
]}

Oliveira, J. M. ^{[22
]}

Onishi, T. ^{[23
]}

Otsuka, M. ^{[1
]}

Paradis, D. ^{[24
]}

Poglitsch, A. ^{[25
]}

Riebel, D. ^{[9
]}

Reach, W. T. ^{[24
,26
]}

Rubio, M. ^{[27
]}

Sargent, B. ^{[1
]}

Sewilo, M. ^{[1
]}

Simon, J. D. ^{[28
]}

Skibba, R. ^{[4
]}

Smith, L. J. ^{[1
]}

机构：

[1] Space Telescope Sci Inst, Baltimore, MD 21218 USA

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

[3] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA

[4] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[5] CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France

[6] Univ Maryland, Dept Astron, Lab Millimeter Wave Astron, College Pk, MD 20742 USA

[7] Observ Astron, F-67000 Strasbourg, France

[8] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA

[9] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[10] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

[11] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA

[12] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[13] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 464, Japan

[14] Swinburne Univ Technol, Ctr Supercomp & Astrophys, Hawthorn, Vic 3122, Australia

[15] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands

[16] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[17] Sejong Univ, Seoul 143747, South Korea

[18] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA

[19] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

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

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

[22] Univ Keele, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England

[23] Osaka Prefecture Univ, Dept Phys Sci, Osaka 5998531, Japan

[24] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[25] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[26] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA

[27] Univ Chile, Dept Astron, Santiago, Chile

[28] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[29] CNRS, IAP, UPR 341, F-75014 Paris, France

[30] Space Sci Inst, Boulder, CO 80301 USA

[31] Harvard CfA, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

Magellanic Clouds; dust; extinction; submillimeter: galaxies; submillimeter: ISM; INTERSTELLAR DUST; MOLECULAR CLOUDS; SPITZER SURVEY; EXTINCTION; ABUNDANCE; EMISSION; DISTANCE; CARBON; SAGE; IV;

D O I：

10.1051/0004-6361/201014662

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) of the Magellanic Clouds will use dust emission to investigate the life cycle of matter in both the Large and Small Magellanic Clouds (LMC and SMC). Using the Herschel Space Observatory's PACS and SPIRE photometry cameras, we imaged a 2 degrees x 8 degrees strip through the LMC, at a position angle of similar to 22.5 degrees as part of the science demonstration phase of the Herschel mission. We present the data in all 5 Herschel bands: PACS 100 and 160 mu m and SPIRE 250, 350 and 500 mu m. We present two dust models that both adequately fit the spectral energy distribution for the entire strip and both reveal that the SPIRE 500 mu m emission is in excess of the models by similar to 6 to 17%. The SPIRE emission follows the distribution of the dust mass, which is derived from the model. The PAH-to-dust mass (f(PAH)) image of the strip reveals a possible enhancement in the LMC bar in agreement with previous work. We compare the gas mass distribution derived from the HI 21 cm and CO J = 1-0 line emission maps to the dust mass map from the models and derive gas-to-dust mass ratios (GDRs). The dust model, which uses the standard graphite and silicate optical properties for Galactic dust, has a very low GDR = 65(-18)(+15) making it an unrealistic dust model for the LMC. Our second dust model, which uses amorphous carbon instead of graphite, has a flatter emissivity index in the submillimeter and results in a GDR = 287(-42)(+25) that is more consistent with a GDR inferred from extinction.

引用

页数：5

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