The WISSH quasars project: IX. Cold gas content and environment of luminous QSOs at z ∼ 2.4-4.7

被引：59

作者：

Bischetti, M. ^{[1
,2
]}

Feruglio, C. ^{[1
]}

Piconcelli, E. ^{[2
]}

Duras, F. ^{[2
,3
]}

Perez-Torres, M. ^{[4
,5
]}

Herrero, R. ^{[6
,7
]}

Venturi, G. ^{[8
]}

Carniani, S. ^{[9
]}

Bruni, G. ^{[10
]}

Gavignaud, I ^{[11
]}

Testa, V ^{[2
]}

Bongiorno, A. ^{[2
]}

Brusa, M. ^{[12
,13
]}

Circosta, C. ^{[14
]}

Cresci, G. ^{[15
]}

D'Odorico, V ^{[1
,9
]}

Maiolino, R. ^{[16
,17
]}

Marconi, A. ^{[15
,18
]}

Mingozzi, M. ^{[19
]}

Pappalardo, C. ^{[20
]}

Perna, M. ^{[15
,21
]}

Traianou, E. ^{[22
]}

Travascio, A. ^{[2
]}

Vietri, G. ^{[23
]}

Zappacosta, L. ^{[2
]}

Fiore, F. ^{[1
]}

机构：

[1] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[2] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy

[3] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy

[4] CSIC, Inst Astrofis Andalucia IAA, Glorieta Astron S-N, Granada 18008, Spain

[5] Univ Zaragoza, Fac Ciencias, Dept Fis Teor, Zaragoza, Spain

[6] European Southern Observ ESO, Alonso Cordova 3107,Casilla 19001, Santiago, Chile

[7] CSIC, Inst Space Sci ICE, Campus UAB, Barcelona 08193, Spain

[8] Pontificia Univ Catolica Chile, Inst Astrofis, Avda Vicuna Mackenna 4860, Santiago 8970117, Chile

[9] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy

[10] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[11] Univ Andres Bello, Dept Ciencias Fis, Campus La Casona,Fernandez Concha 700, Santiago 7500912, Chile

[12] Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, Via Gobetti 93-2, I-40129 Bologna, Italy

[13] INAF Osservatorio Astrofis & Sci Spazio Bologna, Via Gobetti 93-3, I-40129 Bologna, Italy

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

[15] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 2, I-50125 Florence, Italy

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

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

[18] Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Florence, Italy

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

[20] Univ Lisbon, Inst Astrofis & Ciencias Espao, OAL, P-1349018 Lisbon, Portugal

[21] CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, Ctra Ajalvir Km 4, Madrid, Spain

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

[23] INAF Ist Astrofis Spaziale & Fis Cosm Milano, Via A Corti 12, I-20133 Milan, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 645卷

基金：

英国科学技术设施理事会;

关键词：

galaxies: high-redshift; galaxies: ISM; techniques: interferometric; quasars: supermassive black holes; submillimeter: galaxies; quasars: emission lines; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; C II EMISSION; MOLECULAR GAS; HIGH-REDSHIFT; SCALING RELATIONS; HOST GALAXIES; DUST EMISSION; AGN FEEDBACK;

D O I：

10.1051/0004-6361/202039057

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Sources at the brightest end of the quasi-stellar object (QSO) luminosity function, during the peak epoch in the history of star formation and black hole accretion (z similar to 2-4, often referred to as "Cosmic noon") are privileged sites to study the cycle of feeding & feedback processes in massive galaxies.Aims. We aim to perform the first systematic study of cold gas properties in the most luminous QSOs, by characterising their host-galaxies and environment. These targets exhibit indeed widespread evidence of outflows at nuclear and galactic scales.Methods. We analyse ALMA, NOEMA and JVLA observations of the far-infrared continuum, CO and [CII] emission lines in eight QSOs (bolometric luminosity L-Bol greater than or similar to 3x10(47) erg s(-1)) from the WISE-SDSS selected hyper-luminous (WISSH) QSOs sample at z similar to 2.4-4.7.Results. We report a 100% emission line detection rate and a 80% detection rate in continuum emission, and we find CO emission to be consistent with the steepest CO ladders observed so far. Sub-millimetre data reveal presence of (one or more) bright companion galaxies around similar to 80% of WISSH QSOs, at projected distances of similar to 6-130 kpc. We observe a variety of sizes for the molecular gas reservoirs (similar to 1.7-10 kpc), mostly associated with rotating disks with disturbed kinematics. WISSH QSOs typically show lower CO luminosity and higher star formation efficiency than infrared matched, z similar to 0-3 main-sequence galaxies, implying that, given the observed SFR similar to 170-1100 M-circle dot yr(-1), molecular gas is converted into stars in less than or similar to 50 Myr. Most targets show extreme dynamical to black-hole mass ratios M-dyn/M-BH similar to 3-10, two orders of magnitude smaller than local relations. The molecular gas fraction in the host-galaxies of WISSH is lower by a factor of similar to 10-100 than in star forming galaxies with similar M-*.Conclusions. Our analysis reveals that hyper-luminous QSOs at Cosmic noon undergo an intense growth phase of both the central super-massive black hole and of the host-galaxy. These systems pinpoint the high-density sites where giant galaxies assemble, where we show that mergers play a major role in the build-up of the final host-galaxy mass. We suggest that the observed low molecular gas fraction and short depletion timescale are due to AGN feedback, whose presence is indicated by fast AGN-driven ionised outflows in all our targets.

引用

页数：21

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