The ALMA-CRISTAL survey: Dust temperature and physical conditions of the interstellar medium in a typical galaxy at z=5.66

被引：9

作者：

Villanueva, V. ^{[1
]}

Herrera-Camus, R. ^{[1
]}

Gonzalez-Lopez, J. ^{[2
,29
]}

Aravena, M. ^{[3
]}

Assef, R. J. ^{[3
]}

Baeza-Garay, M. ^{[1
]}

Barcos-Munoz, L. ^{[4
]}

Bovino, S. ^{[5
,6
]}

Bowler, R. A. A. ^{[7
]}

da Cunha, E. ^{[8
]}

De Looze, I. ^{[9
,10
]}

Diaz-Santos, T. ^{[11
,12
]}

Ferrara, A. ^{[29
]}

Foerster Schreiber, N. M. ^{[13
]}

Algera, H. ^{[14
]}

Ikeda, R. ^{[15
,17
]}

Killi, M. ^{[3
]}

Mitsuhashi, I. ^{[16
,17
]}

Naab, T. ^{[18
]}

Relano, M. ^{[19
,20
]}

Spilker, J. ^{[21
,22
]}

Solimano, M. ^{[3
]}

Palla, M. ^{[23
,24
]}

Price, S. H. ^{[25
]}

Posses, A. ^{[3
]}

Tadaki, K. ^{[26
]}

Telikova, K. ^{[3
]}

Ubler, H. ^{[27
,28
,30
]}

机构：

[1] Barrio Univ, Univ Concepcion, Dept Astron, Concepcion, Chile

[2] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile

[3] Univ Diego Portales, Fac Ingn & Ciencias, Inst Estudios Astrofis, Ave Ejercito 441, Santiago 8370191, Chile

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

[5] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy

[6] Sapienza Univ Rome, Chem Dept, Ple A Moro, I-00185 Rome, Italy

[7] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Nat Sci, Dept Phys & Astron, Manchester M13 9PL, England

[8] Int Ctr Radio Astron Res ICRAR, M468,35 Stirling Hwy, Crawley, WA 6009, Australia

[9] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium

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

[11] Fdn Res & Technol Hellas FORTH, Inst Astrophys, GR-70013 Iraklion, Greece

[12] European Univ Cyprus, Sch Sci, Diogenes St, Nicosia, Cyprus

[13] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[14] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, 7398526, Japan

[15] Grad Univ Adv Studies SOKENDAI, Sch Sci, Dept Astron, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[16] Univ Tokyo, Dept Astron, 7-3-1 Hongo,Bunkyo, Tokyo 1130033, Japan

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

[18] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, Garching 85741, Germany

[19] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain

[20] Univ Granada, Inst Univ Carlos I Fis Teor & Computac, E-18071 Granada, Spain

[21] Texas A&M Univ, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA

[22] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamental, 4242 TAMU, College Stn, TX 77843 USA

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

[24] INAF OAS, Via Gobetti 93-3, I-40129 Bologna, Italy

[25] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA

[26] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan

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

[28] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England

[29] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-50126 Pisa, Italy

[30] Carnegie Inst Washington, Las Campanas Observ, Casilla 601, La Serena, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

基金：

欧洲研究理事会; 日本学术振兴会;

关键词：

galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: structure; STAR-FORMING GALAXIES; 158; MU-M; FAR-INFRARED LINES; TO-GAS RATIO; HIGH-REDSHIFT; MOLECULAR GAS; SUBMILLIMETER GALAXIES; SPECTROSCOPIC SURVEY; STARBURST GALAXIES; MAIN-SEQUENCE;

D O I：

10.1051/0004-6361/202451490

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new lambda(rest) = 77 mu m dust continuum observations from the Atacama Large Millimeter/submillimeter Array of HZ10 (CRISTAL-22). This dusty main sequence galaxy at z = 5.66 was observed as part of the [CII] Resolved Ism in STar-forming Alma Large program (CRISTAL). The high angular resolution of the ALMA Band 7 and new Band 9 data (similar to 0 ''.4) reveals the complex structure of HZ10, which comprises two main components (HZ10-C and HZ10-W), along with a bridge-like dusty emission between them (i.e., "the bridge"). Using a modified blackbody function to model the dust spectral energy distribution (SED), we constrained the physical conditions of the interstellar medium (ISM) and its variations among the different components identified in HZ10. We find that HZ10-W (the more UV-obscured component) has an SED dust temperature of T-SED similar to 51.2 +/- 13.1 K; this was found to be similar to 5 K higher (which is statistically insignificant; i.e., less than 1 sigma) than that of the central component and previous global estimations for HZ10. Our new ALMA data allow us to reduce the uncertainties of global T-SED measurements by a factor of similar to 2.3, compared to previous studies. The HZ10 components have [CII]-to-far-infrared (FIR) luminosity ratios and FIR surface densities values that are consistent with local starburst galaxies. However, HZ10-W shows a lower [CII]/FIR ratio compared to the other two components (albeit still within the uncertainties), which may suggest a harder radiation field destroying polycyclic aromatic hydrocarbon associated with [CII] emission (e.g., active galactic nuclei or young stellar populations). While HZ10-C appears to follow the tight IRX-beta(UV) relation seen in local UV-selected starburst galaxies and high-z star-forming galaxies, we find that both HZ10-W and the bridge depart from this relation and are well described by dust-screen models with holes in front of a hard UV radiation field. This suggests that the UV emission, which is likely coming from young stellar populations, is strongly attenuated in the "dustier" components of the HZ10 system.

引用

页数：13

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