Dataciencia

Colección SciELO Chile

Massive Molecular Gas Reservoir in a Luminous Submillimeter Galaxy during Cosmic Noon

Indexado

WoS	WOS:000781792900001
Scopus	SCOPUS_ID:85129022349

DOI

10.3847/1538-4357/AC5745

Año

2022

Tipo

artículo de investigación

Citas Totales

Autores Afiliación Chile

Instituciones Chile

% Participación
Internacional

Autores
Afiliación Extranjera

Instituciones
Extranjeras

Abstract

We present multiband observations of an extremely dusty star-forming lensed galaxy (HERS1) at z = 2.553. High-resolution maps of HST/WFC3, SMA, and ALMA show a partial Einstein ring with a radius of similar to 3 ''. The deeper HST observations also show the presence of a lensing arc feature associated with a second lens source, identified to be at the same redshift as the bright arc based on a detection of the [N II] 205 mu m emission line with ALMA. A detailed model of the lensing system is constructed using the high-resolution HST/WFC3 image, which allows us to study the source-plane properties and connect rest-frame optical emission with properties of the galaxy as seen in submillimeter and millimeter wavelengths. Corrected for lensing magnification, the spectral energy distribution fitting results yield an intrinsic star formation rate of about 1000 +/- 260 M-circle dot yr(-1), a stellar mass M-* = 4.3(-1.0)(+2.2) x 10(11) M-circle dot, and a dust temperature T-d = 35(-1)(+2) K. The intrinsic CO emission line (J(up) = 3, 4, 5, 6, 7, 9) flux densities and CO spectral line energy distribution are derived based on the velocity-dependent magnification factors. We apply a radiative transfer model using the large velocity gradient method with two excitation components to study the gas properties. The low-excitation component has a gas density nH(2) = 10(3.8 +/- 0.6) cm(-3) and kinetic temperature T-k = 18(-5)(+7) K, and the high-excitation component has n(H2) = 10(3.1 +/- 0.4) cm(-3) and T-k = 480(-220)(+260) K. Additionally, HERS1 has a gas fraction of about 0.19 +/- 0.14 and is expected to last 100 Myr. These properties offer a detailed view of a typical submillimeter galaxy during the peak epoch of star formation activity.

Revista

Revista	ISSN
Astrophysical Journal	0004-637X

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Disciplinas de Investigación

WOS
Astronomy & Astrophysics

Scopus
Sin Disciplinas

SciELO
Sin Disciplinas

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Publicaciones WoS (Ediciones: ISSHP, ISTP, AHCI, SSCI, SCI), Scopus, SciELO Chile.

Colaboración Institucional

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Autores - Afiliación

Ord.	Autor	Género	Institución - País
1	Liu, Bin	-	Beijing Normal Univ - China Univ Calif Irvine - Estados Unidos Beijing Normal University - China University of California, Irvine - Estados Unidos
2	Chartab, N.	Hombre	Univ Calif Irvine - Estados Unidos University of California, Irvine - Estados Unidos
3	Nayyeri, Hooshang	-	Univ Calif Irvine - Estados Unidos University of California, Irvine - Estados Unidos
4	Cooray, A.	-	Univ Calif Irvine - Estados Unidos University of California, Irvine - Estados Unidos
5	Yang, Chentao	-	Atacama Large Millimeter Array - Chile ESO - Chile Atacama Large Millimeter-submillimeter Array - Chile European Southern Observatory Santiago - Chile European Southern Observ - Chile
6	Riechers, Dominik	Hombre	CORNELL UNIV - Estados Unidos Cornell University - Estados Unidos
7	Gurwell, Mark	Hombre	Harvard & Smithsonian - Estados Unidos Harvard-Smithsonian Center for Astrophysics - Estados Unidos
8	Zhu, Zong-hong	-	Beijing Normal Univ - China Wuhan Univ - China Beijing Normal University - China Wuhan University - China
9	Serjeant, S.	Hombre	Open Univ - Reino Unido The Open University - Reino Unido
10	Borsato, E.	-	Univ Padua - Italia Università degli Studi di Padova - Italia
11	Negrello, M.	Hombre	Cardiff Univ - Reino Unido Cardiff University - Reino Unido Prifysgol Caerdydd - Reino Unido
12	Marchetti, L.	Mujer	Open Univ - Reino Unido UNIV CAPE TOWN - República de Sudáfrica INAF Ist Radioastron - Italia The Open University - Reino Unido University of Cape Town - República de Sudáfrica Istituto Di Radioastronomia, Bologna - Italia
13	Corsini, E. M.	Hombre	Univ Padua - Italia Istituto Nazionale di Astrofisica - Italia Università degli Studi di Padova - Italia Osservatorio Astronomico di Padova - Italia INAF Osservatorio Astron Padova - Italia
14	van der Werf, Paul P.	Hombre	Leiden Univ - Países Bajos Sterrewacht Leiden - Países Bajos

Muestra la afiliación y género (detectado) para los co-autores de la publicación.

Financiamiento

Fuente
National Natural Science Foundation of China
National Science Foundation
China Scholarship Council
Chinese Academy of Sciences
NSF
NASA
MIUR
ESO Fellowship
National Aeronautics and Space Administration
Ministero dell’Istruzione, dell’Università e della Ricerca
Smithsonian Institution
Academia Sinica
European School of Oncology
Padua University
Deutsches SOFIA Institut (DSI) under DLR
NASA ADAP
Deutsches Zentrum für Luft- und Raumfahrt
Universität Stuttgart
Universities Space Research Association, Inc.
Beijing Normal University
Strategic Priority Research Program of the Chinese Academy of Sciences
UniversitÃ degli Studi di Padova
China Scholarship Council grant (CSC)
SOFIA
Directorate for Mathematical and Physical Sciences
Interdiscipline Research Funds of Beijing Normal University
Sofia University

Muestra la fuente de financiamiento declarada en la publicación.

Agradecimientos

Agradecimiento
We thank the anonymous referee for reading the manuscript and providing useful suggestions. Financial support for this work was provided by NSF through AST-1313319, PID 05-0087 from SOFIA for H.N. and A.C. A.C., H.N., and N.C. acknowledge support from NASA ADAP 80NSSC20K04337 for archival data analysis of bright Herschel sources. The U.C.I. group also acknowledges NASA support for Herschel/SPIRE GTO and Open-Time Programs. This work is also based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. B.L. is supported by the China Scholarship Council grant (CSC No. 201906040079). Z.-H.Z. is supported by the National Natural Science Foundation of China under grants Nos. 11633001, 11920101003, and 12021003, the Strategic Priority Research Program of the Chinese Academy of Sciences, grant No. XDB23000000 and the Interdiscipline Research Funds of Beijing Normal University. E.B. and E.M.C. are supported by MIUR grant PRIN 2017 20173ML3WW-001 and Padua University grants DOR1885254/18, DOR1935272/19, and DOR2013080/20. C.Y. acknowledges support from an ESO Fellowship. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.2.00105.S and ADS/JAO.ALMA#2018.1.00922.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.
We thank the anonymous referee for reading the manuscript and providing useful suggestions. Financial support for this work was provided by NSF through AST-1313319, PID 05-0087 from SOFIA for H.N. and A.C. A.C., H.N., and N.C. acknowledge support from NASA ADAP 80NSSC20K04337 for archival data analysis of bright Herschel sources. The U.C.I. group also acknowledges NASA support for Herschel/SPIRE GTO and Open-Time Programs. This work is also based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. B.L. is supported by the China Scholarship Council grant (CSC No. 201906040079). Z.-H.Z. is supported by the National Natural Science Foundation of China under grants Nos. 11633001, 11920101003, and 12021003, the Strategic Priority Research Program of the Chinese Academy of Sciences, grant No. XDB23000000 and the Interdiscipline Research Funds of Beijing Normal University. E.B. and E.M.C. are supported by MIUR grant PRIN 2017 20173ML3WW-001 and Padua University grants DOR1885254/18, DOR1935272/19, and DOR2013080/20. C.Y. acknowledges support from an ESO Fellowship. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.2.00105.S and ADS/JAO.ALMA#2018.1.00922.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.

Agradecimiento

We thank the anonymous referee for reading the manuscript and providing useful suggestions. Financial support for this work was provided by NSF through AST-1313319, PID 05-0087 from SOFIA for H.N. and A.C. A.C., H.N., and N.C. acknowledge support from NASA ADAP 80NSSC20K04337 for archival data analysis of bright Herschel sources. The U.C.I. group also acknowledges NASA support for Herschel/SPIRE GTO and Open-Time Programs. This work is also based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. B.L. is supported by the China Scholarship Council grant (CSC No. 201906040079). Z.-H.Z. is supported by the National Natural Science Foundation of China under grants Nos. 11633001, 11920101003, and 12021003, the Strategic Priority Research Program of the Chinese Academy of Sciences, grant No. XDB23000000 and the Interdiscipline Research Funds of Beijing Normal University. E.B. and E.M.C. are supported by MIUR grant PRIN 2017 20173ML3WW-001 and Padua University grants DOR1885254/18, DOR1935272/19, and DOR2013080/20. C.Y. acknowledges support from an ESO Fellowship. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.2.00105.S and ADS/JAO.ALMA#2018.1.00922.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.