z-GAL: A NOEMA spectroscopic redshift survey of bright Herschel galaxies: II. Dust properties☆

被引：11

作者：

Ismail, D. ^{[1
,2
]}

Beelen, A. ^{[1
,2
,4
,5
]}

Buat, V. ^{[1
,2
]}

Berta, S. ^{[3
]}

Cox, P. ^{[4
,5
]}

Stanley, F. ^{[3
]}

Young, A. ^{[6
]}

Jin, S. ^{[7
]}

Neri, R. ^{[3
]}

Bakx, T. ^{[8
,9
,10
]}

Dannerbauer, H. ^{[11
,12
]}

Butler, K. ^{[3
]}

Cooray, A. ^{[13
]}

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

Omont, A. ^{[4
,5
]}

Serjeant, S. ^{[16
]}

van der Werf, P. ^{[17
]}

Vlahakis, C. ^{[18
]}

Weiss, A. ^{[19
]}

Yang, C. ^{[8
]}

Baker, A. J. ^{[6
,20
]}

Bendo, G. ^{[21
]}

Borsato, E. ^{[22
]}

Chartab, N. ^{[13
]}

Dye, S. ^{[23
]}

Eales, S. ^{[24
]}

Gavazzi, R. ^{[1
,2
]}

Hughes, D. ^{[25
]}

Ivison, R. ^{[26
,27
,28
,29
]}

Jones, B. M. ^{[30
]}

Krips, M. ^{[3
]}

Lehnert, M. ^{[31
]}

Marchetti, L. ^{[32
,33
]}

Messias, H. ^{[34
,35
]}

Negrello, M. ^{[24
]}

Perez-Fournon, I. ^{[11
,12
]}

Riechers, D. A. ^{[30
]}

Urquhart, S. ^{[16
]}

机构：

[1] Aix Marseille Univ, CNRS, 38 Rue Frederic Joliot Curie, F-13013 Marseille, France

[2] CNES, Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13013 Marseille, France

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

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

[5] Inst Astrophys Paris, CNRS, UMR 7095, 98Bis Blvd Arago, F-75014 Paris, France

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

[7] Cosm DAWN Ctr, Radmandsgade 62, DK-2200 Copenhagen N, Denmark

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

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

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

[11] Inst Astrofis Canarias IAC, San Cristobal la Laguna 38205, Tenerife, Spain

[12] Univ La Laguna, Dpto Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

[13] Univ Calif Irvine, Dept Phys & Astron, FRH 2174, Irvine, CA 92697 USA

[14] Natl Ctr Nucl Res, Ul Pasteura 7, PL-02093 Warsaw, Poland

[15] INAF Osservatorio Astron Abruzzo, Via Maggini SNC, I-64100 Teramo, Italy

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

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

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

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

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

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

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

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

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

[25] Inst Nacl Astrofis Opt & Electr, Astrophys Dept, Apdo 51 & 216, Tonantzintla 72000, Puebla, Mexico

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

[27] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW, Australia

[28] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin D02 XF86, Ireland

[29] Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Scotland

[30] Iniversitat Koln, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

[31] Ctr Rech Astrophys Lyon CRAL, CNRS UMR 5574, CNRS, ENS Lyon,UMR 5574, 9 Ave Charles Andre, F-69230 St Genis Laval, France

[32] Univ Western Cape, Dept Phys & Astron, Private Bag X17, ZA-7535 Cape Town, South Africa

[33] Ist Nazl Astrofis, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy

[34] Joint ALMA Observ, Alonso De Cordova 3107, Vitacura 7630355, Santiago De Chi, Chile

[35] European Southern Observ, Alonso Cordova 3107, Vitacura 19001, Santiago De Chi, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 678卷

基金：

美国国家科学基金会;

关键词：

galaxies: high-redshift; galaxies: evolution; infrared: galaxies; submillimeter: galaxies; COSMOLOGY LEGACY SURVEY; FAR-INFRARED PROPERTIES; FORMING GALAXIES; SUBMILLIMETER GALAXIES; TEMPERATURE-DEPENDENCE; MULTIWAVELENGTH PROPERTIES; STARBURST GALAXIES; MASSIVE GALAXIES; SURVEY BEARS; ALMA SURVEY;

D O I：

10.1051/0004-6361/202346804

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the dust properties of 125 bright Herschel galaxies selected from the z-GAL NOEMA spectroscopic redshift survey. All the galaxies have precise spectroscopic redshifts in the range 1.3 < z < 5.4. The large instantaneous bandwidth of NOEMA provides an exquisite sampling of the underlying dust continuum emission at 2 and 3 mm in the observed frame, with flux densities in at least four sidebands for each source. Together with the available Herschel 250, 350, and 500 mu m and SCUBA-2 850 mu m flux densities, the spectral energy distribution (SED) of each source can be analyzed from the far-infrared to the millimeter, with a fine sampling of the Rayleigh-Jeans tail. This wealth of data provides a solid basis to derive robust dust properties, in particular the dust emissivity index (beta) and the dust temperature (T-dust). In order to demonstrate our ability to constrain the dust properties, we used a flux-generated mock catalog and analyzed the results under the assumption of an optically thin and optically thick modified black body emission. The robustness of the SED sampling for the z-GAL sources is highlighted by the mock analysis that showed high accuracy in estimating the continuum dust properties. These findings provided the basis for our detailed analysis of the z-GAL continuum data. We report a range of dust emissivities with beta similar to 1.5 - 3 estimated up to high precision with relative uncertainties that vary in the range 7%-15%, and an average of 2.2 +/- 0.3. We find dust temperatures varying from 20 to 50 K with an average of T-dust similar to 30 K for the optically thin case and T-dust similar to 38 K in the optically thick case. For all the sources, we estimate the dust masses and apparent infrared luminosities (based on the optically thin approach). An inverse correlation is found between T-dust and beta with beta proportional to T-dust(-0.69), which is similar to what is seen in the local Universe. Finally, we report an increasing trend in the dust temperature as a function of redshift at a rate of 6.5 +/- 0.5 K/z for this 500 mu m-selected sample. Based on this study, future prospects are outlined to further explore the evolution of dust temperature across cosmic time.

引用

页数：27

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