HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS

被引：149

作者：

Wardlow, Julie L. ^{[1
]}

Cooray, Asantha ^{[1
]}

De Bernardis, Francesco ^{[1
]}

Amblard, A. ^{[2
]}

Arumugam, V. ^{[3
]}

Aussel, H. ^{[4
]}

Baker, A. J. ^{[5
]}

Bethermin, M. ^{[4
,6
,7
]}

Blundell, R. ^{[8
]}

Bock, J. ^{[9
]}

Boselli, A. ^{[10
,11
]}

Bridge, C.

Buat, V. ^{[10
,11
]}

Burgarella, D. ^{[10
,11
]}

Bussmann, R. S. ^{[8
]}

Cabrera-Lavers, A. ^{[12
,13
,14
]}

Calanog, J. ^{[1
]}

Carpenter, J. M.

Casey, C. M. ^{[15
]}

Castro-Rodriguez, N. ^{[12
,13
]}

Cava, A. ^{[16
]}

Chanial, P. ^{[4
]}

Chapin, E. ^{[17
]}

Chapman, S. C. ^{[18
]}

Clements, D. L. ^{[19
]}

Conley, A. ^{[20
]}

Cox, P. ^{[21
]}

Dowell, C. D. ^{[9
]}

Dye, S. ^{[22
]}

Eales, S. ^{[23
]}

Farrah, D. ^{[24
,25
]}

Ferrero, P. ^{[12
,13
]}

Franceschini, A. ^{[26
]}

Frayer, D. T. ^{[27
]}

Frazer, C. ^{[1
]}

Fu, Hai ^{[1
]}

Gavazzi, R. ^{[28
]}

Glenn, J. ^{[19
,20
,29
]}

Solares, E. A. Gonzalez ^{[18
]}

Griffin, M. ^{[23
]}

Gurwell, M. A. ^{[8
]}

Harris, A. I. ^{[30
]}

Hatziminaoglou, E. ^{[31
]}

Hopwood, R. ^{[19
]}

Hyde, A. ^{[19
]}

Ibar, E. ^{[32
]}

Ivison, R. J. ^{[3
,32
]}

Kim, S. ^{[1
]}

Lagache, G. ^{[6
,7
]}

Levenson, L. ^{[9
]}

机构：

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

[2] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

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

[4] Univ Paris Diderot, CNRS, CEA DSM Irfu, CE Saclay,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France

[5] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

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

[7] CNRS, UMR 8617, F-91405 Orsay, France

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

[9] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

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

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

[12] IAC, E-38200 Tenerife, Spain

[13] ULL, Dept Astrofis, E-38205 Tenerife, Spain

[14] GTC Project, E-38205 Tenerife, Spain

[15] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

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

[17] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain

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

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

[20] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA

[21] Inst RadioAstron Millimetr, F-38406 St Martin Dheres, France

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

[23] Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales

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

[25] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA

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

[27] NRAO, Green Bank, WV 24944 USA

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

[29] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[30] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[31] ESO, D-85748 Garching, Germany

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

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

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

[35] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England

[36] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England

[37] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

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

[39] CSIRO, Astron & Space Sci, Epping, NSW 1710, Australia

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

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 762卷 / 01期

基金：

英国科学技术设施理事会; 美国国家科学基金会; 美国国家航空航天局;

关键词：

gravitational lensing: strong; submillimeter: galaxies; SPECTROSCOPICALLY SELECTED SAMPLE; MASS-DENSITY PROFILE; ALL-SKY SURVEY; ACS SURVEY; NUMBER COUNTS; DARK-MATTER; HERSCHEL-ATLAS; STAR-FORMATION; EXTRAGALACTIC SURVEY; INTERSTELLAR-MEDIUM;

D O I：

10.1088/0004-637X/762/1/59

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a list of 13 candidate gravitationally lensed submillimeter galaxies (SMGs) from 95 deg(2) of the Herschel Multi-tiered Extragalactic Survey, a surface density of 0.14 +/- 0.04 deg(-2). The selected sources have 500 mu m flux densities (S-500) greater than 100 mJy. Gravitational lensing is confirmed by follow-up observations in 9 of the 13 systems (70%), and the lensing status of the four remaining sources is undetermined. We also present a supplementary sample of 29 (0.31 +/- 0.06 deg(-2)) gravitationally lensed SMG candidates with S-500 = 80-100 mJy, which are expected to contain a higher fraction of interlopers than the primary candidates. The number counts of the candidate lensed galaxies are consistent with a simple statistical model of the lensing rate, which uses a foreground matter distribution, the intrinsic SMG number counts, and an assumed SMG redshift distribution. The model predicts that 32%-74% of our S-500 >= 100 mJy candidates are strongly gravitationally lensed (mu >= 2), with the brightest sources being the most robust; this is consistent with the observational data. Our statistical model also predicts that, on average, lensed galaxies with S-500 = 100 mJy are magnified by factors of similar to 9, with apparently brighter galaxies having progressively higher average magnification, due to the shape of the intrinsic number counts. 65% of the sources are expected to have intrinsic 500 mu m flux densities less than 30 mJy. Thus, samples of strongly gravitationally lensed SMGs, such as those presented here, probe below the nominal Herschel detection limit at 500 mu m. They are good targets for the detailed study of the physical conditions in distant dusty, star-forming galaxies, due to the lensing magnification, which can lead to spatial resolutions of similar to 0 ''.01 in the source plane.

引用

页数：28

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