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|Title:||Chandra COSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties||Authors:||Allevato, V.
|Issue Date:||2019||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||632||First Page:||A88||Abstract:||Aims: We perform clustering measurements of 800 X-ray selected Chandra COSMOS Legacy (CCL) Type 2 active galactic nuclei (AGN) with known spectroscopic redshift to probe the halo mass dependence on AGN host galaxy properties, such as galaxy stellar mass M<SUB>star</SUB>, star formation rate (SFR), and specific black hole accretion rate (BHAR; λ<SUB>BHAR</SUB>) in the redshift range z = [0-3]. <BR /> Methods: We split the sample of AGN with known spectroscopic redshits according to M<SUB>star</SUB>, SFR and λ<SUB>BHAR</SUB>, while matching the distributions in terms of the other parameters, including redshift. We measured the projected two-point correlation function w<SUB>p</SUB>(r<SUB>p</SUB>) and modeled the clustering signal, for the different subsamples, with the two-halo term to derive the large-scale bias b and corresponding typical mass of the hosting halo. <BR /> Results: We find no significant dependence of the large-scale bias and typical halo mass on galaxy stellar mass and specific BHAR for CCL Type 2 AGN at mean z ∼ 1, while a negative dependence on SFR is observed, i.e. lower SFR AGN reside in richer environment. Mock catalogs of AGN, matched to have the same X-ray luminosity, stellar mass, λ<SUB>BHAR</SUB>, and SFR of CCL Type 2 AGN, almost reproduce the observed M<SUB>star</SUB> - M<SUB>h</SUB>, λ<SUB>BHAR</SUB> - M<SUB>h</SUB> and SFR-M<SUB>h</SUB> relations, when assuming a fraction of satellite AGN f<SUB>AGN</SUB><SUP>sat</SUP> ∼ 0.15. This corresponds to a ratio of the probabilities of satellite to central AGN of being active Q ∼ 2. Mock matched normal galaxies follow a slightly steeper M<SUB>star</SUB> - M<SUB>h</SUB> relation, in which low mass mock galaxies reside in less massive halos than mock AGN of similar mass. Moreover, matched mock normal galaxies are less biased than mock AGN with similar specific BHAR and SFR, at least for Q > 1.||URI:||http://hdl.handle.net/20.500.12386/28996||URL:||https://www.aanda.org/articles/aa/abs/2019/12/aa36191-19/aa36191-19.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201936191||Bibcode ADS:||2019A&A...632A..88A||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jan 19, 2021
checked on Jan 19, 2021
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