GAS AND DUST IN A SUBMILLIMETER GALAXY AT z=4.24 FROM THE HERSCHEL ATLAS

被引：158

作者：

Cox, P. ^{[1
]}

Krips, M. ^{[1
]}

Neri, R. ^{[1
]}

Omont, A. ^{[2
,3
]}

Guesten, R. ^{[4
]}

Menten, K. M. ^{[4
]}

Wyrowski, F. ^{[4
]}

Weiss, A. ^{[4
]}

Beelen, A. ^{[5
]}

Gurwell, M. A. ^{[6
]}

Dannerbauer, H. ^{[7
]}

Ivison, R. J. ^{[8
,9
]}

Negrello, M. ^{[10
]}

Aretxaga, I. ^{[11
]}

Hughes, D. H. ^{[11
]}

Auld, R. ^{[12
]}

Baes, M. ^{[13
]}

Blundell, R. ^{[6
]}

Buttiglione, S. ^{[14
,15
]}

Cava, A. ^{[16
]}

Cooray, A. ^{[17
]}

Dariush, A. ^{[12
,18
]}

Dunne, L. ^{[19
]}

Dye, S. ^{[19
]}

Eales, S. A. ^{[12
]}

Frayer, D. ^{[20
]}

Fritz, J. ^{[13
]}

Gavazzi, R. ^{[2
,3
]}

Hopwood, R. ^{[10
]}

Ibar, E. ^{[8
]}

Jarvis, M. ^{[14
,15
]}

Maddox, S. ^{[19
]}

Michallowski, M. ^{[9
]}

Pascale, E. ^{[12
]}

Pohlen, M. ^{[12
]}

Rigby, E. ^{[19
]}

Smith, D. J. B. ^{[19
]}

Swinbank, A. M. ^{[21
]}

Temi, P. ^{[22
]}

Valtchanov, I. ^{[23
]}

van der Werf, P. ^{[24
]}

de Zotti, G. ^{[14
,15
]}

机构：

[1] IRAM, F-38406 St Martin Dheres, France

[2] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France

[3] CNRS, UMR7095, F-75014 Paris, France

[4] MPIfR, D-53121 Bonn, Germany

[5] Univ Paris 11, IAS, F-91405 Orsay, France

[6] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[7] CEA DSM CNRS Univ Paris Diderot, DAPNIA Serv Astrophys, CEA Saclay, AIM, F-91191 Gif Sur Yvette, France

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

[9] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[10] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

[11] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico

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

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

[14] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[15] SISSA, I-34136 Trieste, Italy

[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] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran

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

[20] Natl Radio Astron Observ, Green Bank, WV 24944 USA

[21] Univ Durham, Inst Computat Cosmol, Durham DH1 3EE, England

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

[23] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain

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

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 740卷 / 02期

关键词：

galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: individual (ID 141); galaxies: starburst; submillimeter: galaxies; ULTRALUMINOUS INFRARED GALAXIES; ISO-LWS SPECTROSCOPY; MICRON LINE DEFICIT; STAR-FORMATION; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; ATOMIC CARBON; MU-M; MOLECULAR GAS; PHYSICAL CONDITIONS;

D O I：

10.1088/0004-637X/740/2/63

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report ground-based follow-up observations of the exceptional source, ID 141, one of the brightest sources detected so far in the Herschel Astrophysical Terahertz Large Area Survey cosmological survey. ID 141 was observed using the IRAM 30 m telescope and Plateau de Bure interferometer (PdBI), the Submillimeter Array, and the Atacama Pathfinder Experiment submillimeter telescope to measure the dust continuum and emission lines of the main isotope of carbon monoxide and carbon ([C I] and [C II]). The detection of strong CO emission lines with the PdBI confirms that ID 141 is at high redshift (z = 4.243 +/- 0.001). The strength of the continuum and emission lines suggests that ID 141 is gravitationally lensed. The width (Delta V-FWHM similar to 800 km s(-1)) and asymmetric profiles of the CO and carbon lines indicate orbital motion in a disk or a merger. The properties derived for ID 141 are compatible with an ultraluminous (L-FIR similar to (8.5 +/- 0.3) x 10(13) mu(-1)(L) L-circle dot, where mu L is the amplification factor), dense (n approximate to 10(4) cm(-3)), and warm (T-kin approximate to 40 K) starburst galaxy, with an estimated star formation rate of (0.7-1.7) x 10(4) mu(-1)(L) M-circle dot yr(-1). The carbon emission lines indicate a dense (n approximate to 10(4) cm(-3)) photon-dominated region, illuminated by a far-UV radiation field a few thousand times more intense than that in our Galaxy. In conclusion, the physical properties of the high-z galaxy ID 141 are remarkably similar to those of local ultraluminous infrared galaxies.

引用

页数：10

共 69 条

[1] Confirmation of the effectiveness of submm source redshift estimation based on rest-frame radio-FIR photometry [J].