J/MNRAS/511/5436 Study of massive SMBHs hosted by FSRQs (Diana+, 2022)
The evolution of the heaviest supermassive black holes in jetted AGNs.
Diana A., Caccianiga A., Ighina L., Belladitta S., Moretti A.,
Della Ceca R.
<Mon. Not. R. Astron. Soc. 511, 5436-5447 (2022)>
=2022MNRAS.511.5436D 2022MNRAS.511.5436D (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; QSOs ; Black holes ; Radio sources ;
Radio continuum ; Line Profiles ; Photometry ; Spectroscopy ;
Ultraviolet ; Optical ; Extinction ; Velocity dispersion
Keywords: galaxies: active - galaxies: high-redshift - galaxies: evolution -
(galaxies:) quasars: supermassive black holes
Abstract:
We present the space density evolution, from z = 1.5 up to z = 5.5, of
the most massive (M => 109 M☉) black holes hosted in jetted
active galactic nuclei (AGNs). The analysis is based on a sample of
380 luminosity- selected (λL1350 => 1046 erg/s and
P5GHz => 1027 W/Hz) flat spectrum radio quasars (FSRQs) obtained
from the Cosmic Lens All Sky Survey (CLASS). These sources are known
to be face-on jetted AGNs (i.e. blazars) and can be exploited to infer
the abundance of all the (misaligned) jetted AGNs, using a geometrical
argument. We then compare the space density of the most massive
supermassive black holes hosted in jetted AGNs with those present in
the total population (mostly composed by non-jetted AGNs). We find
that the space density has a peak at z ∼ 3, which is significantly
larger than the value observed in the total AGN population with
similar optical/UV luminosities (z ∼ 2.2), but not as extreme as the
value previously inferred from X-ray-selected blazars (z ~> 4). The
jetted fraction (jetted AGNs/total AGNs) is overall consistent with
the estimates in the local Universe (10-20 per cent) and at high
redshift, assuming Lorentz bulk factors Γ ~= 5. Finally, we find
a marginal decrease in the jetted fraction at high redshifts (by a
factor of ∼2). All these evidences point towards a different
evolutionary path in the jetted AGNs compared to the total AGN
population.
Description:
In this paper, we will use the Cosmic Lens All Sky Survey (CLASS) to
build one of the largest radio flux-limited samples of blazars,
covering a large fraction of the sky and that includes sources up to
z ∼ 5.5. In particular, we are interested in tracing the evolution of
the most massive SMBHs where a large difference in the evolutionary
properties has been recently reported. Although for some objects in
our sample, the estimate masses are recomputed here following a single
coherent method. In this way, our analysis should be free from
possible biases that can derive from using different techniques for
sources located at different redshifts. The CLASS a radio survey of
FSRQ contains ∼ 11000 sources. This catalogue was built by combining
the NRAO Very Large Array Sky Survey (NVSS), at 1.4 GHz, with the
Green-Bank Survey (GB6) at 5 GHz and by selecting only the objects
with a flat spectrum between 1.4 and 5 GHz with a final follow-up at
8.4 GHz using the Very Large Array (VLA) that granted an angular
resolution of ∼0.2 arcsec, (i.e see section Introduction).
We have recently carried out a specific search for blazars with
redshift above 4 in the CLASS survey by efficiently pre-selecting
candidates from the Pan-STARRS1 using the so-called drop-out technique
(see Caccianiga et al. 2019MNRAS.484..204C 2019MNRAS.484..204C, C19). The spectroscopic
data are gathered from the SDSS survey, SDSS-I/II and the BOSS survey.
The analysis of the radio spectra and of the X-ray data have then
confirmed the blazar nature for 22 of these objects, we restrict the
search area to the high Galactic latitudes where resulting 19 objects
constituting our high- z complete sample. To extend this sample at
lower redshifts (1 < z < 4), we have considered the CLASS sources
falling in the sky area covered by the large spectroscopic data SDSS
DR14. We have thus cross-correlated CLASS with the SDSS DR14
photometric catalogue, using a 1 arcsec positional tolerance to
guarantee that all the counterparts are recovered. More, in order to
select sources with the same radio and optical luminosities as in the
C19, we can translate the radio and optical flux limits of the high-z
sample of C19 (mAB ≤ 21 and S5GHz => 30 mJy) into luminosity
lower limits at lower redshifts. We also decided to consider only
sources with z > 1.5. We want to analyse a flat spectrum radio quasars
(FSRQ) sample, hence we exclude BL Lac objects. Finally, we exclude
the objects with low Galactic latitudes by analogy with C19. The
resulting 1.5 < z < 4 sub-sample contains 361 objects, with a sky
coverage area ∼ 10700 deg2, to finally get a sample of 380 sources
with z between 1.5 ≤ z < 5.5.
Hereafter, as explained in the sections 3 SMBHs masses estimating and
3.1 Spectral analysis we obtain masses, luminosities and Eddington
ratios from line dispersion and FWHM of C IVλ1549 computation
methods. We present results in tablea1.dat contains also all
redshifts, V-band extinctions, r-band magnitudes, radio 5GHz flux
densities, line dispersions/FWHMs.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 144 380 Physical properties of the FSRQs in our sample
--------------------------------------------------------------------------------
See also:
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/ApJ/699/603 : Evolution of Swift/BAT blazars (Ajello+, 2009)
VIII/72 : CLASS survey of radio sources (Myers+, 2003)
IX/58 : 2SXPS Swift X-ray telescope point source catalogue
(Evans+, 2020)
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16)
(Ahumada+, 2020)
VIII/40 : GB6 catalog of radio sources (Gregory+ 1996)
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Source name (name)
19- 22 F4.2 --- z Spectroscopic redshift (z)
24- 28 F5.3 mag AV Total extinction in the V-band (AV)
30- 34 F5.2 mag rmag Apparent magnitude in the r-filter
(r-mag) (1)
36- 40 I5 mJy S5GHz Radio flux density measured at 5GHz
(S5GHz) (2)
42- 45 I4 km/s sigCIV ? CIVλ1549 line dispersion
σl (σl)
47- 50 I4 km/s e_sigCIV ? Mean error of sigCIV (errσl)
52- 56 I5 km/s FWHMCIV ? CIVλ1549 line FWHM full width
at half-maximum (FWHM)
58- 61 I4 km/s e_FWHMCIV ? Mean error of FWHMCIV (errFWHM)
63- 68 F6.3 [10-7W] LoglL1350 ? Logarithm of the continuum luminosity
at 1350 Å source rest frame
(LogλL1350)
70- 74 F5.3 [10-7W] e_LoglL1350 ? Mean error of LoglL1350
(errLogλL1350)
76- 81 F6.3 [10-7W] LogLCIV ? Logarithm of the CIV1549 line
luminosity (LogLCIV)
83- 87 F5.3 [10-7W] e_LogLCIV ? Mean error of LogLCIV (errLogLCIV)
89- 94 F6.3 [10-7W] LogLbol ? Logarithm of the bolometric luminosity
total energy (LogLbol) (3)
96- 100 F5.3 [10-7W] e_LogLbol ? Mean error of LogLbol (errLogLbol)
102- 106 F5.2 [Msun] LogMsig ? Logarithm of the SMBH mass
(LogMσ) (4)
108- 111 F4.2 [Msun] e_LogMsig ? Mean error of LogMsig
(errLogMσ)
113- 117 F5.2 [Msun] LogMFWHM ? Logarithm of the SMBH mass
(LogMFWHM) (5)
119- 122 F4.2 [Msun] e_LogMFWHM ? Mean error of LogMFWHM (errLogMFWHM)
124- 128 F5.2 [-] LoglEddsig ? Logarithm of the Eddington ratio
(LogλEddσl) (6)
130- 133 F4.2 [-] e_LoglEddsig ? Mean error of LoglEddsig
(errLogλEddσl)
135- 139 F5.2 [-] LoglEddFWHM ? Logarithm of the Eddington ratio
(LogλEddFWHM) (7)
141- 144 F4.2 [-] e_LoglEddFWHM ? Mean error of LoglEddFWHM
(errLogλEddFWHM)
--------------------------------------------------------------------------------
Note (1): The r-band limit magnitude is expressed as the equation 3 of the
section 2 The sample.
Note (2): The S5GHz limit flux is expressed as the equation 4 of the section 2
The sample.
Note (3): This luminosity is produced by the AGN per unit of time integrated
on all the wavelengths calculated assuming a bolometric correction
Kbol described in the section 3.2 Eddington ratio.
Note (4): SMBH mass is estimated using equation 6 of the section 3 Estimating
the masses of the SMBHs where sigCIV is used, expression taken from
Vestergaard & Peterson (2006ApJ...641..689V 2006ApJ...641..689V).
Note (5): SMBH mass is estimated using equation 7 of the section 3 Estimating
the masses of the SMBHs where FWHMCIV is used, expression taken from
Vestergaard & Peterson (2006ApJ...641..689V 2006ApJ...641..689V).
Note (6): Eddington ratio is expressed as Lbol/L_Edd with
LEdd = 1.26*1038 Msig/M☉ taken from the section 3.2
Eddington ratio.
Note (7): Eddington ratio is expressed as Lbol/L_Edd with
LEdd = 1.26*1038 MFWHM/M☉ taken from the section 3.2
Eddington ratio.
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 03-Feb-2025