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http://hdl.handle.net/20.500.12386/28982
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Viitanen, A. | en_US |
dc.contributor.author | Allevato, V. | en_US |
dc.contributor.author | Finoguenov, A. | en_US |
dc.contributor.author | BONGIORNO, ANGELA | en_US |
dc.contributor.author | Cappelluti, N. | en_US |
dc.contributor.author | GILLI, Roberto | en_US |
dc.contributor.author | Miyaji, T. | en_US |
dc.contributor.author | Salvato, M. | en_US |
dc.date.accessioned | 2020-12-18T09:23:22Z | - |
dc.date.available | 2020-12-18T09:23:22Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28982 | - |
dc.description.abstract | Aims: We study the spatial clustering of 632 (1130) XMM-COSMOS active galactic nuclei (AGNs) with known spectroscopic or photometric redshifts in the range z = [0.1-2.5] in order to measure the AGN bias and estimate the typical mass of the hosting dark matter (DM) halo as a function of AGN host galaxy properties. <BR /> Methods: We created AGN subsamples in terms of stellar mass, M<SUB>*</SUB>, and specific black hole accretion rate, L<SUB>X</SUB>/M<SUB>*</SUB>, to study how AGN environment depends on these quantities. Further, we derived the M<SUB>*</SUB>-M<SUB>halo</SUB> relation for our sample of XMM-COSMOS AGNs and compared it to results in literature for normal non-active galaxies. We measured the projected two-point correlation function w<SUB>p</SUB>(r<SUB>p</SUB>) using both the classic and the generalized clustering estimator, based on photometric redshifts, as probability distribution functions in addition to any available spectroscopic redshifts. We measured the large-scale (r<SUB>p</SUB> ≳ 1 h<SUP>-1</SUP> Mpc) linear bias b by comparing the clustering signal to that expected of the underlying DM distribution. The bias was then related to the typical mass of the hosting halo M<SUB>halo</SUB> of our AGN subsamples. Since M<SUB>*</SUB> and L<SUB>X</SUB>/M<SUB>*</SUB> are correlated, we matched the distribution in terms of one quantity and we split the distribution in the other. <BR /> Results: For the full spectroscopic AGN sample, we measured a typical DM halo mass of log (M<SUB>halo</SUB>/h<SUP>-1</SUP> M<SUB>☉</SUB>) = 12.79<SUB>-0.43</SUB><SUP>+0.26</SUP>, similar to galaxy group environments and in line with previous studies for moderate-luminosity X-ray selected AGN. We find no significant dependence on specific accretion rate L<SUB>X</SUB>/M<SUB>*</SUB>, with log (M<SUB>halo</SUB>/h<SUP>-1</SUP> M<SUB>☉</SUB>) = 13.06<SUB>-0.38</SUB><SUP>+0.23</SUP> and log (M<SUB>halo</SUB>/h<SUP>-1</SUP> M<SUB>☉</SUB>) = 12.97<SUB>-1.26</SUB><SUP>+0.39</SUP> for low and high L<SUB>X</SUB>/M<SUB>*</SUB> subsamples, respectively. We also find no difference in the hosting halos in terms of M<SUB>*</SUB> with log (M<SUB>halo</SUB>/h<SUP>-1</SUP> M<SUB>☉</SUB>) = 12.93<SUB>-0.62</SUB><SUP>+0.31</SUP> (low) and log (M<SUB>halo</SUB>/h<SUP>-1</SUP> M<SUB>☉</SUB>) = 12.90<SUB>-0.62</SUB><SUP>+0.30</SUP> (high). By comparing the M<SUB>*</SUB>-M<SUB>halo</SUB> relation derived for XMM-COSMOS AGN subsamples with what is expected for normal non-active galaxies by abundance matching and clustering results, we find that the typical DM halo mass of our high M<SUB>*</SUB> AGN subsample is similar to that of non-active galaxies. However, AGNs in our low M<SUB>*</SUB> subsample are found in more massive halos than non-active galaxies. By excluding AGNs in galaxy groups from the clustering analysis, we find evidence that the result for low M<SUB>*</SUB> may be due to larger fraction of AGNs as satellites in massive halos. | en_US |
dc.language.iso | eng | en_US |
dc.title | The XMM-Newton wide field survey in the COSMOS field: Clustering dependence of X-ray selected AGN on host galaxy properties | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201935186 | en_US |
dc.identifier.scopus | 2-s2.0-85071781381 | en_US |
dc.identifier.isi | 000482764800001 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2019/09/aa35186-19/aa35186-19.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 629 | en_US |
dc.relation.firstpage | A14 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | DEU | 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 | 2019A&A...629A..14V | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | 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. Roma | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0002-0101-6624 | - |
crisitem.author.orcid | 0000-0001-8121-6177 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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Viitanen1906.07911.pdf | postprint | 1.12 MB | Adobe PDF | Visualizza/apri |
aa 629 A14.pdf | Pdf editoriale | 1.49 MB | Adobe PDF | Visualizza/apri |
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