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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28982
Title: The XMM-Newton wide field survey in the COSMOS field: Clustering dependence of X-ray selected AGN on host galaxy properties
Authors: Viitanen, A.
Allevato, V.
Finoguenov, A.
BONGIORNO, ANGELA 
Cappelluti, N.
GILLI, Roberto 
Miyaji, T.
Salvato, M.
Issue Date: 2019
Journal: ASTRONOMY & ASTROPHYSICS 
Number: 629
First Page: A14
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.
URI: http://hdl.handle.net/20.500.12386/28982
URL: https://www.aanda.org/articles/aa/abs/2019/09/aa35186-19/aa35186-19.html
ISSN: 0004-6361
DOI: 10.1051/0004-6361/201935186
Bibcode ADS: 2019A&A...629A..14V
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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