A dusty protocluster surrounding the binary galaxy HerBS-70 at z=2.3

被引：2

作者：

Bakx, Tom J. L. C. ^{[1
,2
,3
]}

Berta, S. ^{[4
]}

Dannerbauer, H. ^{[5
,6
]}

Cox, P. ^{[7
,8
]}

Butler, K. M.

Hagimoto, M. ^{[2
]}

Hughes, D. H. ^{[9
]}

Riechers, D. A. ^{[10
]}

van der Werf, P. P. ^{[11
]}

Yang, C.

Baker, A. J. ^{[12
,13
]}

Beelen, A. ^{[14
,15
]}

Bendo, G. J. ^{[16
]}

Borsato, E. ^{[17
]}

Buat, V ^{[18
,19
]}

Cooray, A. R. ^{[20
]}

Dunne, L. ^{[21
]}

Dye, S. ^{[22
]}

Eales, S. ^{[21
]}

Gavazzi, R. ^{[7
,8
,23
]}

Harris, A., I ^{[24
]}

Ismail, D.

Ivison, R. J. ^{[25
]}

Jones, B. ^{[26
]}

Krips, M.

Lehnert, M. D. ^{[27
]}

Marchetti, L. ^{[28
,29
]}

Messias, H. ^{[30
,31
]}

Negrello, M. ^{[21
]}

Neri, R. ^{[4
]}

Omont, A. ^{[7
,8
]}

Perez-Fournon, I ^{[5
,32
]}

Nanni, A. ^{[33
,34
]}

Chartab, N. ^{[11
,35
,36
]}

Serjeant, S. ^{[37
]}

Stanley, F. ^{[4
]}

Tamura, Y. ^{[2
]}

Urquhart, S. A. ^{[37
]}

Vlahakis, C. ^{[38
]}

Weiss, A. ^{[39
]}

Young, A. J. ^{[13
]}

机构：

[1] Chalmers Univ Technol, Dept Earth & Space Sci, Onsala Space Observ, SE-43994 Onsala, Sweden

[2] Nagoya Univ, Grad Sch Sci, Dept Phys, Nagoya, Aichi 4648602, Japan

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

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

[5] Inst Astrofis Canarias IAC, San Cristobal la Laguna 38200, Tenerife, Spain

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

[7] UPMC Univ Paris 6, Sorbonne Univ, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France

[8] CNRS, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France

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

[10] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

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

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

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

[14] CNRS, Inst Astrophys Spatiale IAS, F-13013 Orsay, France

[15] Univ Paris Sud, F-13013 Orsay, France

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

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

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

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

[20] Univ Calif Irvine, Dept Phys & Astron, 4129 Reines Hall, Irvine, CA 92697 USA

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

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

[23] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB30HA, England

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

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

[26] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Nat Sci, Manchester M13 9PL, Lancs, England

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

[28] Univ Cape Town, Dept Astron, Private Bag X3, ZA-7701 Cape Town, South Africa

[29] Ist Radioastron Italian ARC, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy

[30] European So Observ, Alonso De Cordova 3107,Casilla 19001, Santiago, Chile

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

[32] Univ Basque Country, Ikerbasque Fdn, Dipc Donostia 48009, Spain

[33] Natl Ctr Nucl Res, Ul Pasteura 7, PL-02093 Otwock, Poland

[34] INAF Osservatorio Astronomicod Abruzzo, Via Maggini SNC, I-64100 Teramo, Italy

[35] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[36] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA

[37] Open Univ, Sch Phys Sci, Milton Keynes MK7 6AA, England

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 530卷 / 04期

基金：

欧洲研究理事会; 英国科学技术设施理事会; 加拿大创新基金会; 国家重点研发计划;

关键词：

galaxies: clusters: general; galaxies: evolution; galaxies: high-redshift; submillimetre: galaxies; STAR-FORMING GALAXIES; SPECTROSCOPIC REDSHIFT SURVEY; LY-ALPHA-EMITTERS; UBIQUITOUS MOLECULAR OUTFLOWS; LENSED SUBMILLIMETER GALAXIES; MASSIVE QUIESCENT GALAXIES; NEAR-INFRARED SPECTROSCOPY; BRIGHTEST CLUSTER GALAXY; ACTIVE GALACTIC NUCLEUS; JCMT LEGACY SURVEY;

D O I：

10.1093/mnras/stae1155

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on deep SCUBA-2 observations at 850 mu m and NOrthern Extended Millimetre Array (NOEMA) spectroscopic measurements at 2 mm of the environment surrounding the luminous, massive (M* approximate to 2 x 10(11) M circle dot) Herschel-selected source HerBS-70. This source was revealed by previous NOEMA observations to be a binary system of dusty star-forming galaxies at z = 2.3, with the east component (HerBS-70E) hosting an active galactic nucleus. The SCUBA-2 observations detected, in addition to the binary system, 21 sources at >3.5 sigma over an area of similar to 25 square comoving Mpc with a sensitivity of 1 sigma(850) = 0.75 mJy. The surface density of continuum sources around HerBS-70 is three times higher than for field galaxies. The NOEMA spectroscopic measurements confirm the protocluster membership of three of the nine brightest sources through their CO(4-3) line emission, yielding a volume density 36 times higher than for field galaxies. All five confirmed sub-mm galaxies in the HerBS-70 system have relatively short gas depletion times (80-500 Myr), indicating the onset of quenching for this protocluster core due to the depletion of gas. The dark matter halo mass of the HerBS-70 system is estimated around 5 x 10(13) M circle dot, with a projected current-day mass of 10(15) M circle dot, similar to the local Virgo and Coma clusters. These observations support the claim that DSFGs, in particular the ones with observed multiplicity, can trace cosmic overdensities.

引用

页码：4578 / 4596

页数：19

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