J/MNRAS/427/3103 COSMOS field supermassive black holes (Bongiorno+, 2012)
Accreting supermassive black holes in the COSMOS field and the connection
to their host galaxies.
Bongiorno A., Merloni A., Brusa M., Magnelli B., Salvato M., Mignoli M.,
Zamorani G., Fiore F., Rosario D., Mainieri V., Hao H., Comastri A.,
Vignali C., Balestra I., Bardelli S., Berta S., Civano F., Kampczyk P.,
Le Floc'h E., Lusso E., Lutz D., Pozzetti L., Pozzi F., Riguccini L.,
Shankar F., Silverman J.
<Mon. Not. R. Astron. Soc., 427, 3103-3133 (2012)>
=2012MNRAS.427.3103B 2012MNRAS.427.3103B (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; X-ray sources ; Redshifts
Keywords: catalogues - surveys - galaxies: active - galaxies: evolution -
galaxies: fundamental parameters
Abstract:
Using the wide multiband photometry available in the Cosmic Evolution
Survey (COSMOS) field, we explore the host galaxy properties of a
large sample of active galactic nuclei (AGNs; ∼1700 objects) with
Lbolranging from 1043 to 1047erg/s, obtained by combining
X-ray and optical spectroscopic selections. Based on a careful study
of their spectral energy distributions, which have been parametrized
using a two-component (AGN+galaxy) model fit, we have derived
dust-corrected rest-frame magnitudes, colours and stellar masses of
the obscured and unobscured AGN hosts up to high redshift (z≲3).
Moreover, for the sample of obscured AGNs, we have also derived
reliable star formation rates (SFRs). We find that AGN hosts span a
large range of stellar masses and SFRs. No colour-bimodality is seen
at any redshift in the AGN hosts, which are found to be mainly
massive, red galaxies. Once we have accounted for the colour-mass
degeneracy in well-defined mass-matched samples, we find a residual
(marginal) enhancement of the incidence of AGNs in redder galaxies
with lower specific SFRs. We argue that this result might emerge
because of our ability to properly account for AGN light contamination
and dust extinction, compared to surveys with a more limited
multiwavelength coverage. However, because these colour shifts are
relatively small, systematic effects could still be considered
responsible for some of the observed trends. Interestingly, we find
that the probability for a galaxy to host a black hole that is growing
at any given `specific accretion rate' (i.e. the ratio of X-ray
luminosity to the host stellar mass) is almost independent of the host
galaxy mass, while it decreases as a power law with LX/M*. By
analysing the normalization of such a probability distribution, we
show how the incidence of AGNs increases with redshift as rapidly as
(1 + z)4, which closely resembles the overall evolution of the
specific SFR of the entire galaxy population. We provide analytical
fitting formulae that describe the probability of a galaxy of any mass
(above the completeness limit of the COSMOS) to host an AGN of any
given specific accretion rate as a function of redshift. These can be
useful tools for theoretical studies of the growing population of
black holes within galaxy evolution models. Although AGN activity and
star formation in galaxies do appear to have a common triggering
mechanism, at least in a statistical sense, within the COSMOS sample,
we do not find any conclusive evidence to suggest that AGNs have a
powerful influence on the star-forming properties of their host
galaxies.
Description:
In order to construct a sample of AGNs that is as complete as
possible, including both obscured and unobscured objects, first we
selected XMM-COSMOS point-like sources (Hasinger et al., 2007, Cat.
J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635). To
these, we added a smaller sample of purely optically selected AGNs
from the zCOSMOS bright spectroscopic survey (Lilly et al., 2009, Cat.
J/ApJS/184/218), spanning a lower luminosity range for AGNs (Bongiorno
et al., 2010, Cat. J/A+A/510/A56; Mignoli et al., in preparation).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 84 1702 Source identification
tablec2.dat 69 1702 Parameters derived from the SED fitting
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See also:
J/ApJS/184/218 : The zCOSMOS 10k-bright spectroscopic sample (Lilly+, 2009)
J/A+A/497/635 : XMM-Newton wide-field survey in COSMOS field
(Cappelluti+, 2009)
J/ApJ/690/1236 : COSMOS photometric redshift catalog (Ilbert+, 2009)
J/A+A/510/A56 : zCOSMOS type-2 AGN (Bongiorno, 2010)
J/ApJ/716/348 : The XMM-Newton survey of the COSMOS field (Brusa+, 2010)
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- XMM-ID ?=-1 XMM ID from Cappelluti et al. (2009,
Cat. J/A+A/497/635, XMMC NNNNNN in Simbad)
7- 12 I6 --- zC-ID_BPT ?=-1 zCOSMOS ID (Lilly et al., 2009, Cat.
J/ApJS/184/218) when the object is in the
BPT selected sample (Bongiorno et al.,
2010, Cat. J/A+A/510/A56)
14- 19 I6 --- zC-ID_NeV ?=-1 zCOSMOS ID (Lilly et al., 2009, Cat.
J/ApJS/184/218) when the object is in the
NeV-selected sample
(Mignoli et al., in preparation)
21- 27 I7 --- PHOT-ID ?=-99 Photometric ID from Ilbert et al. (2009,
Cat. J/ApJ/690/1236,
[ICS2009] NNNNNNN in Simbad)
29- 39 F11.7 deg RAdeg Right ascension (J2000)
41- 49 F9.7 deg DEdeg Declination (J2000)
51- 56 F6.2 mag Imag ?=-99 HST F814W filter AB magnitude
58- 64 F7.3 --- zspec ?=-99 Spectroscopic redshift
66- 72 F7.3 --- zphot ?=-99 Photometric redshift when the
spectroscopy is not available (Salvato et
al., 2009ApJ...690.1250S 2009ApJ...690.1250S)
74- 78 F5.1 --- Classsp ?=-99 Classification derived from the
spectra (1)
80- 84 F5.1 --- Classph ?=-99 Classification derived from the SED
(Salvato et al., 2009ApJ...690.1250S 2009ApJ...690.1250S) when
the spectra are not available (2)
--------------------------------------------------------------------------------
Note (1): Classification derived from the spectra, as follows:
1 = unobscured AGNs
2 = obscured AGNs classified from the X-ray
(Brusa et al., 2010, Cat. J/ApJ/716/348 )
22.2 = obscured AGNs selected using the BPT diagram
(Bongiorno et al., 2010, Cat. J/A+A/510/A56)
22.4 = obscured AGNs selected through the [NeV] line
(Mignoli et al., in preparation)
Note (2): Classification derived from the SED (Salvato et al.,
2009ApJ...690.1250S 2009ApJ...690.1250S ) when the spectra are not available as follows:
1 = unobscured AGNs
2 = obscured AGNs
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- XMM-ID ?=-1 XMM ID from Cappelluti et al. (2009,
Cat. J/A+A/497/635, XMMC NNNNNN in Simbad)
7- 12 I6 --- zC-ID_BPT ?=-1 zCOSMOS ID (Lilly et al., 2009, Cat.
J/ApJS/184/218) when the object is in the
BPT selected sample (Bongiorno et al.,
2010, Cat. J/A+A/510/A56)
14- 19 I6 --- zC-ID_NeV ?=-1 zCOSMOS ID (Lilly et al., 2009, Cat.
J/ApJS/184/218) when the object is in the
NeV-selected sample
(Mignoli et al., in preparation)
21- 25 F5.1 mag E(B-V)AGN ?=-99 Extinction E(B-V) of the AGN
component
27- 33 F7.3 mag UMAG ?=-99 Rest-frame absolute U-band magnitude
of the host galaxy not corrected for
extinction
35- 41 F7.3 mag BMAG ?=-99 Rest-frame absolute B-band magnitude
of the host galaxy not corrected for
extinction
43 A1 --- l_logM Limti flag on logM
44- 50 F7.3 [Msun] logM ?=-99 Host galaxy stellar mass
52 I1 --- f_logM [0/2] Flag for logM (1)
54- 61 F8.4 [Msun/yr] logSFR ?=-99 Host galaxy star-formation rate
63 I1 --- f_logSFR [0/3] Flag for logSFR (1)
65- 69 F5.1 mag E(B-V)Gal ?=-99 Extinction E(B-V) of the galaxy
component
--------------------------------------------------------------------------------
Note (1): Flag as follows:
0 = measurement
1 = upper limit
2 = no measurement
3 = no measurement
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Nov-2018