The bright extragalactic ALMA redshift survey (BEARS) - II. Millimetre photometry of gravitational lens candidates

被引：21

作者：

Bendo, G. J. ^{[1
]}

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

Serjeant, S. ^{[2
]}

Bakx, T. ^{[3
,4
]}

Hagimoto, M. ^{[3
]}

Cox, P. ^{[5
,6
]}

Neri, R. ^{[7
]}

Lehnert, M. D. ^{[8
]}

Dannerbauer, H. ^{[9
,10
]}

Amvrosiadis, A. ^{[11
]}

Andreani, P. ^{[12
]}

Baker, A. J. ^{[13
,14
]}

Beelen, A. ^{[15
,16
]}

Berta, S. ^{[7
]}

Borsato, E. ^{[17
]}

Buat, V ^{[15
,16
]}

Butler, K. M. ^{[18
]}

Cooray, A. ^{[19
]}

De Zotti, G. ^{[20
]}

Dunne, L. ^{[21
]}

Dye, S. ^{[22
]}

Eales, S. ^{[21
]}

Enia, A. ^{[23
,24
]}

Fan, L. ^{[25
,26
]}

Gavazzi, R. ^{[15
,16
]}

Gonzalez-Nuevo, J. ^{[27
,28
]}

Harris, A., I ^{[29
]}

Herrera, C. N. ^{[7
]}

Hughes, D. H. ^{[30
]}

Ismail, D. ^{[15
,16
]}

Jones, B. M. ^{[31
]}

Kohno, K. ^{[32
,33
]}

Krips, M. ^{[7
]}

Lagache, G. ^{[15
,16
]}

Marchetti, L. ^{[34
,35
]}

Massardi, M. ^{[35
,36
]}

Messias, H. ^{[37
,38
]}

Negrello, M. ^{[21
]}

Omont, A. ^{[5
,6
]}

Perez-Fournon, I ^{[9
,10
]}

Riechers, D. A.

Scott, D. ^{[39
]}

Smith, M. W. L.

Stanley, F. ^{[7
]}

Tamura, Y.

Temi, P. ^{[40
]}

van der Werf, P. ^{[18
]}

Verma, A. ^{[41
]}

Vlahakis, C. ^{[42
]}

Weiss, A. ^{[43
]}

机构：

[1] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Oxford Rd, Manchester M13 9PL, England

[2] Open Univ, Sch Phys Sci, Kents Hill, Milton Keynes MK7 6AA, England

[3] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Aichi 4648602, Japan

[4] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[5] UPMC Univ Paris 6, 98bis Blvd Arago, F-75014 Paris, France

[6] Sorbonne Univ, Inst Astrophys Paris, CNRS, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France

[7] Inst Radioastron Millimetr IRAM, 300 Rue Piscine, F-38400 St Martin Dheres, France

[8] Univ Lyon 1, Ctr Rech Astrophys Lyon, ENS Lyon, CNRS,UMR5574, F-69230 St Genis Laval, France

[9] Inst Astrofis Canarias IAC, E-38205 San Cristobal la Laguna, Tenerife, Spain

[10] Univ Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain

[11] Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England

[12] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[13] State Univ New Jersey, Dept Phys & Astron, Rutgers, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA

[14] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa

[15] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, 38 Rue Freder Joliot Curie, F-13388 Marseille, France

[16] Aix Marseille Univ, CNES, Lab Astrophys Marseille, 38 Rue Freder Joliot Curie, F-13388 Marseille, France

[17] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[18] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

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

[20] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[21] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, Wales

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

[23] Univ Bologna, Dept Phys & Astron Augusto Righi DIFA, Via Gobetti 93-2, I-40129 Bologna, Italy

[24] INAF Osservatorio Astrofis & Sci Spazio, Via Gobetti 93-3, I-40129 Bologna, Italy

[25] Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China

[26] Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Peoples R China

[27] Univ Oviedo, Dept Fis, C Federico Garcia Lorca 18, Oviedo 33007, Spain

[28] Inst Univ Ciencias & Tecnol Espaciales Asturias IC, C Independencia 13, Oviedo 33004, Spain

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

[30] Inst Nacl Astrofis Opt & Electr, Luis Enr Erro 1, Puebla 72840, Mexico

[31] Univ Cologne, I Phys Inst, Zulpicher Str 77, D-50937 Cologne, Germany

[32] Univ Tokyo, Inst Astron, Grad Sch Sci, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan

[33] Univ Tokyo, Res Ctr Early Universe, Grad Sch Sci, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan

[34] Univ Cape Town, Dept Astron, ZA-7701 Cape Town, South Africa

[35] INAF Ist Radioastron, via Gobetti 101, I-40129 Bologna, Italy

[36] SISSA, Via Bonomea 265, I-34136 Trieste, Italy

[37] Joint ALMA Observ, Alonso Cordova 3107, Santiago 7630355, Chile

[38] European Southern Observ, Alonso Cordova 3107, Casilla 19001, Santiago, Chile

[39] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada

[40] NASA Ames Res Ctr, Astrophys Branch, MS 245, Moffett Field, CA 94035 USA

[41] Univ Oxford, Sub Dept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[42] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA

[43] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[44] Chalmers Univ Technol, Dept Space Earth & Environm, Onsala Space Observ, SE-43992 Onsala, Sweden

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 522卷 / 02期

基金：

英国科学技术设施理事会;

关键词：

galaxies: high-redshift; galaxies: ISM; infrared: galaxies; submillimetre: galaxies; STAR-FORMING GALAXIES; DEEP FIELD SOUTH; DUST TEMPERATURES; SUBMILLIMETER GALAXIES; HERSCHEL SOURCES; INTERSTELLAR-MEDIUM; SPACE DENSITY; DATA RELEASE; COLD DUST; ATLAS;

D O I：

10.1093/mnras/stac3771

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present 101- and 151-GHz ALMA continuum images for 85 fields selected from Herschel observations that have 500-mu m flux densities >80 mJy and 250-500-mu m colours consistent with z > 2, most of which are expected to be gravitationally lensed or hyperluminous infrared galaxies. Approximately half of the Herschel 500-mu m sources were resolved into multiple ALMA sources, but 11 of the 15 brightest 500-mu m Herschel sources correspond to individual ALMA sources. For the 37 fields containing either a single source with a spectroscopic redshift or two sources with the same spectroscopic redshift, we examined the colour temperatures and dust emissivity indices. The colour temperatures only vary weakly with redshift and are statistically consistent with no redshift-dependent temperature variations, which generally corresponds to results from other samples selected in far-infrared, submillimetre, or millimetre bands but not to results from samples selected in optical or near-infrared bands. The dust emissivity indices, with very few exceptions, are largely consistent with a value of 2. We also compared spectroscopic redshifts to photometric redshifts based on spectral energy distribution templates designed for infrared-bright high-redshift galaxies. While the templates systematically underestimate the redshifts by similar to 15 per cent, the inclusion of ALMA data decreases the scatter in the predicted redshifts by a factor of similar to 2, illustrating the potential usefulness of these millimetre data for estimating photometric redshifts.

引用

页码：2995 / 3017

页数：23

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