Herschel-ATLAS: VISTA VIKING near-infrared counterparts in the Phase 1 GAMA 9-h data

被引：32

作者：

Fleuren, S. ^{[1
]}

Sutherland, W. ^{[1
]}

Dunne, L. ^{[2
]}

Smith, D. J. B. ^{[3
]}

Maddox, S. J. ^{[2
]}

Gonzalez-Nuevo, J. ^{[4
]}

Findlay, J. ^{[1
]}

Auld, R. ^{[5
]}

Baes, M. ^{[6
]}

Bond, N. A. ^{[7
]}

Bonfield, D. G. ^{[3
]}

Bourne, N. ^{[8
]}

Cooray, A. ^{[9
]}

Buttiglione, S. ^{[10
]}

Cava, A. ^{[11
]}

Dariush, A. ^{[12
]}

De Zotti, G. ^{[4
,10
]}

Driver, S. P. ^{[13
,14
]}

Dye, S. ^{[8
]}

Eales, S. ^{[5
]}

Fritz, J. ^{[6
]}

Gunawardhana, M. L. P. ^{[15
,16
]}

Hopwood, R. ^{[12
,17
]}

Ibar, E. ^{[18
]}

Ivison, R. J. ^{[18
,19
]}

Jarvis, M. J. ^{[3
,20
]}

Kelvin, L. ^{[13
,14
]}

Lapi, A. ^{[4
,21
]}

Liske, J. ^{[22
]}

Michalowski, M. J. ^{[23
]}

Negrello, M. ^{[10
,17
]}

Pascale, E. ^{[5
]}

Pohlen, M. ^{[5
]}

Prescott, M. ^{[24
]}

Rigby, E. E. ^{[23
]}

Robotham, A. ^{[13
]}

Scott, D. ^{[25
]}

Temi, P. ^{[26
]}

Thompson, M. A. ^{[3
]}

Valiante, E. ^{[5
]}

van der Werf, P. ^{[27
]}

机构：

[1] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England

[2] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand

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

[4] SISSA ISAS, Astrophys Sect, I-34136 Trieste, Italy

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

[6] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium

[7] NASA, Goddard Space Flight Ctr, Cosmol Lab Code 665, Greenbelt, MD 20771 USA

[8] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 1HR, England

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

[10] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

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

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

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

[14] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia

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

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

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

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

[19] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[20] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa

[21] Univ Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy

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

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

[24] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England

[25] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

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

[27] Leiden Observ, NL-2300 RA Leiden, Netherlands

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 423卷 / 03期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

methods: statistical; infrared: galaxies; submillimetre: galaxies; DEGREE EXTRAGALACTIC SURVEY; DEEP-FIELD; MERGER RATE; WIDE-FIELD; MIDINFRARED COUNTERPARTS; SUBMILLIMETER GALAXIES; RADIO CORRELATION; REDSHIFT SURVEY; SKY SURVEY; MU-M;

D O I：

10.1111/j.1365-2966.2012.21048.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We identify near-infrared Ks-band counterparts to Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) submillimetre (submm) sources, using a preliminary object catalogue from the VISTA Kilo-degree Infrared Galaxy (VIKING) survey. The submm sources are selected from the H-ATLAS Phase 1 catalogue of the Galaxy and Mass Assembly 9-h field, which includes all objects detected at 250, 350 or with the instrument. We apply and discuss a likelihood ratio method for VIKING candidates within a search radius of 10 arcsec of the 22 000 SPIRE sources with a 5s detection at . We estimate the fraction of SPIRE sources with a counterpart above the magnitude limit of the VIKING survey to be Q0 similar to 0.73. We find that 11 294 (51 per cent) of the SPIRE sources have a best VIKING counterpart with a reliability R= 0.8, and the false identification rate of these is estimated to be 4.2 per cent. We expect to miss 5 per cent of true VIKING counterparts. There is evidence from Z-J and J-Ks colours that the reliable counterparts to SPIRE galaxies are marginally redder than the field population. We obtain photometric redshifts for 68 per cent of all (non-stellar) VIKING candidates with a median redshift of . We have spectroscopic redshifts for 3147 (28 per cent) of the reliable counterparts from existing redshift surveys. Comparing to the results of the optical identifications supplied with the Phase 1 catalogue, we find that the use of medium-deep near-infrared data improves the identification rate of reliable counterparts from 36 to 51 per cent.

引用

页码：2407 / 2424

页数：18

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