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http://hdl.handle.net/20.500.12386/30313
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Lana Ceraj | en_US |
dc.contributor.author | Vernesa Smolčić | en_US |
dc.contributor.author | DELVECCHIO, IVAN | en_US |
dc.contributor.author | Mladen Novak | en_US |
dc.contributor.author | Giovanni Zamorani | en_US |
dc.contributor.author | Jacinta Delhaize | en_US |
dc.contributor.author | Eva Schinnerer | en_US |
dc.contributor.author | Eleni Vardoulaki | en_US |
dc.contributor.author | Noelia Herrera Ruiz | en_US |
dc.date.accessioned | 2021-02-11T09:56:34Z | - |
dc.date.available | 2021-02-11T09:56:34Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30313 | - |
dc.description.abstract | We study a sample of 1,604 moderate-to-high radiative luminosity active galactic nuclei (HLAGN) selected at 3 GHz within the VLA-COSMOS 3 GHz Large Project. These were classified by combining multiple AGN diagnostics: X-ray data, mid-infrared data and broad-band spectral energy distribution fitting. We decompose the total radio 1.4 GHz luminosity ($\mathrm{L_{1.4\ GHz,TOT}}$) into the emission originating from star formation and AGN activity by measuring the excess in $\mathrm{L_{1.4\ GHz,TOT}}$ relative to the infrared-radio correlation of star-forming galaxies. To quantify the excess, for each source we calculate the AGN fraction ($\mathrm{f_{AGN}}$), the fractional contribution of AGN activity to $\mathrm{L_{1.4\ GHz,TOT}}$. The majority of the HLAGN, $(68.0\pm1.5)\%$, are dominated by star-forming processes ($f_{AGN}\leq0.5$), while $(32.0\pm1.5)\%$ are dominated by AGN-related radio emission ($0.5<f_{AGN}\leq1$). We use the AGN-related 1.4 GHz emission to derive the 1.4 GHz AGN luminosity functions of HLAGN. By assuming pure density and pure luminosity evolution models we constrain their cosmic evolution out to $z\sim6$, finding $\mathrm{\Phi^* (z) \propto (1+z)^{(2.64\pm0.10)+(-0.61\pm0.04) z}}$ and $\mathrm{L^* (z) \propto (1+z)^{(3.97\pm0.15) + (-0.92\pm0.06)z}}$. These evolutionary laws show that the number and luminosity density of HLAGN increased from higher redshifts ($z\sim6$) up to a maximum in the redshift range $ 1<z<2.5$, followed by a decline towards local values. By scaling the 1.4 GHz AGN luminosity to kinetic luminosity using the standard conversion, we estimate the kinetic luminosity density as a function of redshift. We compare our result to the semi-analytic models of radio mode feedback finding that this feedback could have played an important role in the context of AGN-host coevolution in HLAGN which show evidence of AGN-related radio emission ($f_{AGN}>0$). | en_US |
dc.language.iso | eng | en_US |
dc.title | The VLA-COSMOS 3 GHz Large Project: Star formation properties and radio luminosity functions of AGN with moderate-to-high radiative luminosities out to z ∼6 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201833935 | en_US |
dc.identifier.scopus | 2-s2.0-85058861561 | en_US |
dc.identifier.isi | 000453501000002 | en_US |
dc.identifier.url | http://arxiv.org/abs/1811.02966v1 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2018/12/aa33935-18/aa33935-18.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 620 | en_US |
dc.relation.firstpage | A192 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018A&A...620A.192C | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0001-8706-2252 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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