Herschel-ATLAS/GAMA: dusty early-type galaxies and passive spirals

被引：107

作者：

Rowlands, K. ^{[1
]}

Dunne, L. ^{[1
]}

Maddox, S. ^{[1
]}

Bourne, N. ^{[1
]}

Gomez, H. L. ^{[2
]}

Kaviraj, S. ^{[3
]}

Bamford, S. P. ^{[1
]}

Brough, S. ^{[4
]}

Charlot, S. ^{[5
]}

da Cunha, E. ^{[6
]}

Driver, S. P. ^{[7
,8
]}

Eales, S. A. ^{[2
]}

Hopkins, A. M. ^{[4
]}

Kelvin, L. ^{[7
,8
]}

Nichol, R. C. ^{[9
]}

Sansom, A. E. ^{[10
]}

Sharp, R. ^{[11
]}

Smith, D. J. B. ^{[1
,12
]}

Temi, P. ^{[13
]}

van der Werf, P. ^{[14
]}

Baes, M. ^{[15
]}

Cava, A. ^{[16
]}

Cooray, A. ^{[17
]}

Croom, S. M. ^{[18
]}

Dariush, A. ^{[3
]}

De Zotti, G. ^{[19
,20
]}

Dye, S. ^{[1
,2
]}

Fritz, J. ^{[15
]}

Hopwood, R. ^{[3
]}

Ibar, E. ^{[21
]}

Ivison, R. J. ^{[21
,22
]}

Liske, J. ^{[23
]}

Loveday, J. ^{[24
]}

Madore, B. ^{[25
]}

Norberg, P. ^{[22
]}

Popescu, C. C. ^{[10
]}

Rigby, E. E. ^{[1
,22
]}

Robotham, A. ^{[7
]}

Rodighiero, G. ^{[19
]}

Seibert, M. ^{[25
]}

Tuffs, R. J. ^{[26
]}

机构：

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

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

[3] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England

[4] Australian Astron Observ, Epping, NSW 1710, Australia

[5] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[6] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[7] Univ Western Australia, Int Ctr Radio Astron ICRAR, Crawley, WA 6009, Australia

[8] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[9] ICG, Portsmouth PO1 3FX, Hants, England

[10] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[11] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

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

[13] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA

[14] Leiden Univ, NL-2300 RA Leiden, Netherlands

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

[16] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain

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

[18] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia

[19] Univ Padua, Dept Astron, INAF, Vicolo Osservatorio, I-35122 Padua, Italy

[20] SISSA, I-34136 Trieste, Italy

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

[22] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

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

[24] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England

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

[26] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 419卷 / 03期

关键词：

dust; extinction; galaxies: elliptical and lenticular; cD; galaxies: evolution; infrared: galaxies; submillimetre: galaxies; RECENT STAR-FORMATION; MASS ASSEMBLY GAMA; X-RAY-EMISSION; ELLIPTIC GALAXIES; STELLAR MASS; RED-SEQUENCE; DATA RELEASE; COLD DUST; SPITZER OBSERVATIONS; INFRARED-EMISSION;

D O I：

10.1111/j.1365-2966.2011.19905.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the dust properties and star formation histories of local submillimetre-selected galaxies, classified by optical morphology. Most of the galaxies are late types and very few are early types. The early-type galaxies (ETGs) that are detected contain as much dust as typical spirals, and form a unique sample that has been blindly selected at submillimetre wavelengths. Additionally, we investigate the properties of the most passive, dusty spirals. We morphologically classify 1087 galaxies detected in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) Science Demonstration Phase data. Comparing to a control sample of optically selected galaxies, we find 5.5 per cent of luminous ETGs are detected in H-ATLAS. The H-ATLAS ETGs contain a significant mass of cold dust: the mean dust mass is 5.5 x 10(7)M(circle dot), with individual galaxies ranging from 9 x 10(5) to 4 x 10(8)M(circle dot). This is comparable to that of spiral galaxies in our sample, and is an order of magnitude more dust than that found for the control early-types, which have a median dust mass inferred from stacking of (0.8-4.0) x 10(6)M(circle dot) for a cold dust temperature of 25-15 K. The early-types detected in H-ATLAS tend to have bluer NUV - r colours, higher specific star formation rates and younger stellar populations than early-types which are optically selected, and may be transitioning from the blue cloud to the red sequence. We also find that H-ATLAS and control early-types inhabit similar low-density environments. We investigate whether the observed dust in H-ATLAS early-types is from evolved stars, or has been acquired from external sources through interactions and mergers. We conclude that the dust in H-ATLAS and control ETGs cannot be solely from stellar sources, and a large contribution from dust formed in the interstellar medium or external sources is required. Alternatively, dust destruction may not be as efficient as predicted. We also explore the properties of the most passive spiral galaxies in our sample with specific star formation rate (SSFR) < 10(-11) yr(-1). We find these passive spirals have lower dust-to-stellar mass ratios, higher stellar masses and older stellar population ages than normal spirals. The passive spirals inhabit low-density environments similar to those of the normal spiral galaxies in our sample. This shows that the processes which turn spirals passive do not occur solely in the intermediate-density environments of group and cluster outskirts.

引用

页码：2545 / 2578

页数：34

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