An Overview of the Dwarf Galaxy Survey

被引：207

作者：

Madden, S. C. ^{[1
]}

Remy-Ruyer, A. ^{[1
]}

Galametz, M. ^{[2
]}

Cormier, D. ^{[1
]}

Lebouteiller, V. ^{[1
]}

Galliano, F. ^{[1
]}

Hony, S. ^{[1
]}

Bendo, G. J. ^{[3
]}

Smith, M. W. L. ^{[4
]}

Pohlen, M. ^{[4
]}

Roussel, H. ^{[5
]}

Sauvage, M. ^{[1
]}

Wu, R. ^{[1
]}

Sturm, E. ^{[6
]}

Poglitsch, A. ^{[6
]}

Contursi, A. ^{[6
]}

Doublier, V. ^{[6
]}

Baes, M. ^{[7
]}

Barlow, M. J. ^{[8
]}

Boselli, A. ^{[9
,10
]}

Boquien, M. ^{[6
]}

Carlson, L. R. ^{[11
]}

Ciesla, L. ^{[9
,10
]}

Cooray, A. ^{[12
,13
]}

Cortese, L. ^{[14
]}

de Looze, I. ^{[7
]}

Irwin, J. A. ^{[15
]}

Isaak, K. ^{[16
]}

Kamenetzky, J. ^{[17
]}

Karczewski, O. L. ^{[8
]}

Lu, N. ^{[18
]}

MacHattie, J. A. ^{[15
]}

O'Halloran, B. ^{[19
]}

Parkin, T. J. ^{[20
]}

Rangwala, N. ^{[17
]}

Schirm, M. R. P. ^{[20
]}

Schulz, B. ^{[18
]}

Spinoglio, L. ^{[21
]}

Vaccari, M. ^{[22
,23
]}

Wilson, C. D. ^{[19
]}

Wozniak, H. ^{[24
]}

机构：

[1] Univ Paris 07, IRFU Serv Astrophys, CEA, Lab AIM, F-91191 Gif Sur Yvette, France

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

[3] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England

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

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

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

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

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

[9] Univ Aix Marseille, LAM, F-13388 Marseille 13, France

[10] CNRS, UMR7326, F-13388 Marseille 13, France

[11] Leiden Univ, Leiden Observ, Leiden, Netherlands

[12] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA

[13] CALTECH, Div Phys Astron & Math, Pasadena, CA 91125 USA

[14] European So Observ, D-85748 Garching, Germany

[15] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada

[16] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands

[17] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

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

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

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

[21] INAF IAPS, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy

[22] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa

[23] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

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

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2013年 / 125卷 / 928期

关键词：

HUBBLE-SPACE-TELESCOPE; AROMATIC-HYDROCARBON EMISSION; SPECTRAL ENERGY-DISTRIBUTION; BLUE COMPACT GALAXIES; 158; MU-M; NEUTRAL HYDROGEN OBSERVATIONS; LOW-METALLICITY ENVIRONMENTS; ASTROPHYSICAL DUST EMISSION; STAR-FORMING GALAXIES; TO-GAS RATIO;

D O I：

10.1086/671138

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dwarf Galaxy Survey (DGS) program is studying low-metallicity galaxies using 230 hr of farinfrared (FIR) and submillimetre (submm) photometric and spectroscopic observations of the Herschel Space Observatory and draws from this a rich database of a wide range of wavelengths tracing the dust, gas and stars. This sample of 50 galaxies includes the largest metallicity range achievable in the local Universe including the lowest metallicity (Z) galaxies, 1/50 Z., and spans four orders of magnitude in star formation rates. The survey is designed to get a handle on the physics of the interstellar medium (ISM) of low metallicity dwarf galaxies, especially their dust and gas properties and the ISM heating and cooling processes. The DGS produces PACS and SPIRE maps of low-metallicity galaxies observed at 70, 100, 160, 250, 350, and 500 mu m with the highest sensitivity achievable to date in the FIR and submm. The FIR fine-structure lines, [CII] 158 mu m, [OI] 63 mu m, [OI] 145 mu m, [OIII] 88 mu m, [NIII] 57 mu m, and [NII] 122 and 205 mu m have also been observed with the aim of studying the gas cooling in the neutral and ionized phases. The SPIRE FTS observations include many CO lines (J = 4-3 to J = 13-12), [NII] 205 mu m, and [CI] lines at 370 and 609 mu m. This paper describes the sample selection and global properties of the galaxies and the observing strategy as well as the vast ancillary database available to complement the Herschel observations. The scientific potential of the full DGS survey is described with some example results included.

引用

页码：600 / 635

页数：36

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