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dc.contributor.authorCircosta, C.-
dc.contributor.authorMainieri, V.-
dc.contributor.authorLamperti, I.-
dc.contributor.authorPadovani, P.-
dc.contributor.authorBischetti, M.-
dc.contributor.authorHarrison, C. M.-
dc.contributor.authorKakkad, D.-
dc.contributor.authorZanella, A.-
dc.contributor.authorVietri, G.-
dc.contributor.authorLanzuisi, G.-
dc.contributor.authorSalvato, M.-
dc.contributor.authorBrusa, M.-
dc.contributor.authorCarniani, S.-
dc.contributor.authorCicone, C.-
dc.contributor.authorCresci, G.-
dc.contributor.authorFeruglio, C.-
dc.contributor.authorHusemann, B.-
dc.contributor.authorMannucci, F.-
dc.contributor.authorMarconi, A.-
dc.contributor.authorPerna, M.-
dc.contributor.authorPiconcelli, E.-
dc.contributor.authorPuglisi, A.-
dc.contributor.authorSaintonge, A.-
dc.contributor.authorSchramm, M.-
dc.contributor.authorVignali, C.-
dc.contributor.authorZappacosta, L.-
dc.date.accessioned2022-02-15T14:17:44Z-
dc.date.available2022-02-15T14:17:44Z-
dc.date.issued2021-02-16-
dc.identifier.citationAstronomy and Astrophysics 646: A96(2021)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/abs/2021/02/aa39270-20/aa39270-20.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/582-
dc.descriptionData are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/646/A96es
dc.description.abstractFeedback from active galactic nuclei (AGN) is thought to be key in shaping the life cycle of their host galaxies by regulating star-formation activity. Therefore, to understand the impact of AGN on star formation, it is essential to trace the molecular gas out of which stars form. In this paper we present the first systematic study of the CO properties of AGN hosts at z ≈ 2 for a sample of 27 X-ray selected AGN spanning two orders of magnitude in AGN bolometric luminosity (log Lbol / erg s−1 = 44.7 − 46.9) by using ALMA Band 3 observations of the CO(3-2) transition (∼1″ angular resolution). To search for evidence of AGN feedback on the CO properties of the host galaxies, we compared our AGN with a sample of inactive (i.e., non-AGN) galaxies from the PHIBSS survey with similar redshift, stellar masses, and star-formation rates (SFRs). We used the same CO transition as a consistent proxy for the gas mass for the two samples in order to avoid systematics involved when assuming conversion factors (e.g., excitation corrections and αCO). By adopting a Bayesian approach to take upper limits into account, we analyzed CO luminosities as a function of stellar masses and SFRs, as well as the ratio LCO(3–2)′/M∗ (a proxy for the gas fraction). The two samples show statistically consistent trends in the LCO(3–2)′−LFIR and LCO(3–2)′−M∗ planes. However, there are indications that AGN feature lower CO(3-2) luminosities (0.4–0.7 dex) than inactive galaxies at the 2–3σ level when we focus on the subset of parameters where the results are better constrained (i.e., LFIR ≈ 1012.2 L⊙ and M* > 1011 M⊙) and on the distribution of the mean log(LCO(3–2)′/M∗). Therefore, even by conservatively assuming the same excitation factor r31, we would find lower molecular gas masses in AGN, and assuming higher r31 would exacerbate this difference. We interpret our result as a hint of the potential effect of AGN activity (such as radiation and outflows), which may be able to heat, excite, dissociate, and/or deplete the gas reservoir of the host galaxies. Better SFR measurements and deeper CO observations for AGN as well as larger and more uniformly selected samples of both AGN and inactive galaxies are required to confirm whether there is a true difference between the two populations.es
dc.description.sponsorshipWe thank the anonymous referee for carefully reading the manuscript and providing helpful comments. C. Circosta thanks Linda Tacconi for useful advice on the PHIBSS survey and providing the table with measured CO fluxes; Vinod Arumugam and Emanuele Daddi for helpful discussions about ALMA data analysis; Sotiria Fotopoulou and Antonis Georgakakis for providing the photometry of the XMM-XXL targets. C. Circosta and AS acknowledge support from the Royal Society. A. P. gratefully acknowledges financial support from STFC through grants ST/T000244/1 and ST/P000541/1. M. P. is supported by the Programa Atraccion de Talento de la Comunidad de Madrid via Grant 2018-T2/TIC-11715. We acknowledge support from PRIN MIUR project Black Hole winds and the Baryon Life Cycle of Galaxies: the stoneguest at the galaxy evolution supper, contract #2017PH3WAT. GV acknowledges financial support from Premiale 2015 MITic (PI B. Garilli). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00798.S and ADS/JAO.ALMA#2017.1.00893.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC 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. This research has made use of the following data: data based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Data from HerMES project. HerMES is a Herschel Key Programme utilising Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The HerMES data was accessed through the Herschel Database in Marseille (HeDaM -http://hedam.lam.fr) operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille. HerMES DR3 was made possible through support of the Herschel Extragalactic Legacy Project, HELP (http://herschel.sussex.ac.uk), HELP is a European Commission Research Executive Agency funded project under the SP1-Cooperation, Collaborative project, Small or medium-scale focused research project, FP7-SPACE-2013-1 scheme.es
dc.language.isoenges
dc.publisherEDP Scienceses
dc.relation.isversionofinfo:eu-repo/semantics/publishedVersiones
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectGalaxies: activees
dc.subjectGalaxies: evolutiones
dc.subjectGalaxies: ISMes
dc.subjectQuasars: generales
dc.subjectSubmillimeter: ISMes
dc.subjectGalaxies: high redshiftes
dc.titleSUPER IV. CO(J = 3–2) properties of active galactic nucleus hosts at cosmic noon revealed by ALMAes
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidMannucci, F. [0000-0002-4803-2381]-
dc.identifier.doi10.1051/0004-6361/202039270-
dc.identifier.e-issn1432-0746-
dc.contributor.funderScience and Technology Facilities Council (STFC)-
dc.contributor.funderComunidad de Madrid-
dc.description.peerreviewedPeerreviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/100012818-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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