The ALPINE-ALMA [CII] survey: Obscured star formation rate density and main sequence of star-forming galaxies at z>4

被引：67

作者：

Khusanova, Y. ^{[1
,2
]}

Bethermin, M. ^{[2
]}

Le Fevre, O. ^{[2
]}

Capak, P. ^{[3
,4
]}

Faisst, A. L. ^{[3
]}

Schaerer, D. ^{[5
]}

Silverman, J. D. ^{[6
,7
]}

Cassata, P. ^{[8
]}

Yan, L. ^{[9
]}

Ginolfi, M. ^{[5
]}

Fudamoto, Y. ^{[5
]}

Loiacono, F. ^{[10
,11
]}

Amorin, R. ^{[12
,13
]}

Bardelli, S. ^{[11
]}

Boquien, M. ^{[14
]}

Cimatti, A. ^{[10
,15
]}

Dessauges-Zavadsky, M. ^{[5
]}

Gruppioni, C. ^{[11
]}

Hathi, N. P. ^{[16
]}

Jones, G. C. ^{[17
,18
]}

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

Lagache, G. ^{[2
]}

Maiolino, R. ^{[17
,18
,19
]}

Lemaux, B. C. ^{[20
]}

Oesch, P. ^{[5
]}

Pozzi, F. ^{[10
]}

Riechers, D. A. ^{[1
,21
]}

Romano, M. ^{[8
,22
]}

Talia, M. ^{[10
,11
]}

Toft, S. ^{[4
,23
]}

Vergani, D. ^{[11
]}

Zamorani, G. ^{[11
]}

Zucca, E. ^{[11
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France

[3] CALTECH, IPAC, MC 314-6,1200 E Calif Blvd, Pasadena, CA 91125 USA

[4] Cosm Dawn Ctr DAWN, Copenhagen, Denmark

[5] Univ Geneva, Observ Geneve, 51 Ch Maillettes, CH-1290 Versoix, Switzerland

[6] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan

[7] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

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

[9] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA

[10] Univ Bologna, Dipartimento Fis & Astron, Via Gobetti 93-2, I-40129 Bologna, Italy

[11] Osservatorio Astrofis & Sci Spazio Bologna, Ist Nazl Astrofis, Via Gobetti 93-3, I-40129 Bologna, Italy

[12] Univ La Serena, Inst Invest Multidisciplinar Ciencia & Technol, Raul Bitran 1305, La Serena, Chile

[13] Univ La Serena, Dept Astron, Av Juan Cisternas 1200 Norte, La Serena, Chile

[14] Univ Antofagasta, Ctr Astron CITEVA, Ave Angamos 601, Antofagasta, Chile

[15] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[16] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[17] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge, England

[18] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[19] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[20] Univ Calif Davis, Dept Phys & Astron, One Shields Ave, Davis, CA 95616 USA

[21] Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA

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

[23] Univ Copenhagen, Niels Bohr Inst, Lyngbyvej 2, DK-2100 Copenhagen, Denmark

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 649卷

基金：

英国科学技术设施理事会; 欧洲研究理事会; 美国国家科学基金会; 新加坡国家研究基金会;

关键词：

galaxies: high-redshift; galaxies: evolution; galaxies: star formation; submillimeter: galaxies; LYMAN-BREAK GALAXIES; ULTRA DEEP FIELD; UV LUMINOSITY FUNCTIONS; STELLAR MASS FUNCTION; SPECTROSCOPIC SURVEY; PHOTOMETRIC REDSHIFTS; DUST ATTENUATION; EMISSION-LINES; NUMBER COUNTS; BILLION YEARS;

D O I：

10.1051/0004-6361/202038944

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Star formation rate (SFR) measurements at z>4 have relied mostly on the rest-frame far-ultraviolet (FUV) observations. The corrections for dust attenuation based on the IRX-beta relation are highly uncertain and are still debated in the literature. Hence, rest-frame far-infrared (FIR) observations are necessary to constrain the dust-obscured component of the SFR. In this paper, we exploit the rest-frame FIR continuum observations collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) to directly constrain the obscured SFR in galaxies at 4.4<z<5.9. We used stacks of continuum images to measure average infrared luminosities taking both detected and undetected sources into account. Based on these measurements, we measured the position of the main sequence of star-forming galaxies and the specific SFR (sSFR) at z similar to 4.5 and z similar to 5.5. We find that the main sequence and sSFR do not significantly evolve between z similar to 4.5 and z similar to 5.5, as opposed to lower redshifts. We developed a method to derive the obscured SFR density (SFRD) using the stellar masses or FUV-magnitudes as a proxy of FIR fluxes measured on the stacks and combining them with the galaxy stellar mass functions and FUV luminosity functions from the literature. We obtain consistent results independent of the chosen proxy. We find that the obscured fraction of SFRD is decreasing with increasing redshift, but even at z similar to 5.5 it constitutes around 61% of the total SFRD.

引用

页数：18

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The ALPINE-ALMA [CII] survey: Obscured star formation rate density and main sequence of star-forming galaxies at z&gt;4

The ALPINE-ALMA [CII] survey: Obscured star formation rate density and main sequence of star-forming galaxies at z>4