000099106 001__ 99106
000099106 005__ 20230519145404.0
000099106 0247_ $$2doi$$a10.1051/0004-6361/202039057
000099106 0248_ $$2sideral$$a122781
000099106 037__ $$aART-2021-122781
000099106 041__ $$aeng
000099106 100__ $$aBischetti, M.
000099106 245__ $$aThe WISSH quasars project: IX. Cold gas content and environment of luminous QSOs at z ~2.4-4.7
000099106 260__ $$c2021
000099106 5060_ $$aAccess copy available to the general public$$fUnrestricted
000099106 5203_ $$aContext. 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 ∼ 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 LBol ≳ 3 × 1047 erg s-1) from the WISE-SDSS selected hyper-luminous (WISSH) QSOs sample at z ∼ 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 ∼80% of WISSH QSOs, at projected distances of ∼6-130 kpc. We observe a variety of sizes for the molecular gas reservoirs (∼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 ∼ 0-3 main-sequence galaxies, implying that, given the observed SFR ∼170-1100 M⊙ yr-1, molecular gas is converted into stars in ≲ 50 Myr. Most targets show extreme dynamical to black-hole mass ratios Mdyn/MBH ∼ 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 ∼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.
000099106 536__ $$9info:eu-repo/grantAgreement/ES/MCI-AEI-FEDER/PGC2018-098915-B-C21
000099106 540__ $$9info:eu-repo/semantics/openAccess$$aby-nc$$uhttp://creativecommons.org/licenses/by-nc/3.0/es/
000099106 590__ $$a6.24$$b2021
000099106 592__ $$a1.918$$b2021
000099106 594__ $$a9.9$$b2021
000099106 591__ $$aASTRONOMY & ASTROPHYSICS$$b12 / 69 = 0.174$$c2021$$dQ1$$eT1
000099106 593__ $$aSpace and Planetary Science$$c2021$$dQ1
000099106 593__ $$aAstronomy and Astrophysics$$c2021$$dQ1
000099106 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000099106 700__ $$aFeruglio, C.
000099106 700__ $$aPiconcelli, E.
000099106 700__ $$aDuras, F.
000099106 700__ $$0(orcid)0000-0001-5654-0266$$aPerez-Torres, M.
000099106 700__ $$aHerrero, R.
000099106 700__ $$aVenturi, G.
000099106 700__ $$aCarniani, S.
000099106 700__ $$aBruni, G.
000099106 700__ $$aGavignaud, I.
000099106 700__ $$aTesta, V.
000099106 700__ $$aBongiorno, A.
000099106 700__ $$aBrusa, M.
000099106 700__ $$aCircosta, C.
000099106 700__ $$aCresci, G.
000099106 700__ $$aD'Odorico, V.
000099106 700__ $$aMaiolino, R.
000099106 700__ $$aMarconi, A.
000099106 700__ $$aMingozzi, M.
000099106 700__ $$aPappalardo, C.
000099106 700__ $$aPerna, M.
000099106 700__ $$aTraianou, E.
000099106 700__ $$aTravascio, A.
000099106 700__ $$aVietri, G.
000099106 700__ $$aZappacosta, L.
000099106 700__ $$aFiore, F.
000099106 7102_ $$12004$$2038$$aUniversidad de Zaragoza$$bDpto. Física Teórica$$cÁrea Astronomía y Astrofísica
000099106 773__ $$g645 (2021), A33 [21 pp]$$pAstron. astrophys.$$tAstronomy and Astrophysics$$x0004-6361
000099106 8564_ $$s1262204$$uhttps://zaguan.unizar.es/record/99106/files/texto_completo.pdf$$yVersión publicada
000099106 8564_ $$s3431479$$uhttps://zaguan.unizar.es/record/99106/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000099106 909CO $$ooai:zaguan.unizar.es:99106$$particulos$$pdriver
000099106 951__ $$a2023-05-18-13:45:16
000099106 980__ $$aARTICLE