J/MNRAS/513/4673 Radio quasars study from Radio/X-ray surveys (Bariuan+, 2022)
The Fundamental Planes of black hole activity for radio-loud and radio-quiet
quasars.
Bariuan L.G.C., Snios B., Sobolewska M., Siemiginowska A., Schwartz D.A.
<Mon. Not. R. Astron. Soc. 513, 4673-4681 (2022)>
=2022MNRAS.513.4673B 2022MNRAS.513.4673B (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Black holes ; Radio sources ; X-ray sources ; Redshifts ;
Photometry ; Spectroscopy
Keywords: accretion, accretion discs - galaxies: active - black hole physics -
galaxies: high-redshift
Abstract:
We examine the Fundamental Plane of black hole activity for
correlations with redshift and radio loudness in both radio-loud and
radio-quiet quasar populations. Sources are compiled from archival
data of both radio-loud and radio-quiet quasars over redshifts
0.1 < z < 5.0 to produce a sample of 353 sources with known X-ray,
radio, and black hole mass measurements. A Fundamental Plane of
accretion activity is fit to a sample of radio-loud and radio-quiet
quasars, and we find a dichotomy between radio-loud and radio-quiet
sources. The set of best-fitting equations that best describe the two
samples are
log LR = (1.12 ± 0.06)logLX-(0.20 ± 0.07)logM-(5.64 ± 2.99)
for our radio-loud sample and
logLR = (0.48 ± 0.06)logLX + (0.50 ± 0.08)logM + (15.26 ± 2.66)
for our radio-quiet sample. Our results suggest that the average
radio-quiet quasar emission is consistent with advection-dominated
accretion, while a combination of jet and disc emission dominates in
radio-loud quasars. We additionally examine redshift trends amongst
the radio-loud and radio-quiet samples, and we observe a redshift
dependence for the Fundamental Plane of radio-loud quasars. Lastly, we
utilize the Fundamental Plane as a black hole mass estimation method
and determine it useful in studying systems where standard spectral
modelling techniques are not viable.
Description:
This work complements recent studies of quasar structure and spectra
performed across different wavelengths providing insights into the
properties of black holes that formed at the early epochs of the
Universe as well as the evolution of their accretion properties (i.e
see section Introduction). Previous investigations of quasars have
indicated that radio loudness is inversely dependent to the accretion
rate of the black hole system (Sikora et al. 2007ApJ...658..815S 2007ApJ...658..815S, Cat.
J/ApJ/658/815; Balokovic et al. 2012ApJ...759...30B 2012ApJ...759...30B). It is therefore
plausible that the derived Fundamental Plane of black hole activity
for a sample will be impacted by the radio loudness distribution of
its sources. We therefore require samples of both radio-loud and
radio-quiet quasars with comparable physical properties in order to
investigate dependences on radio loudness in our Fundamental Plane
analysis, (i.e 2 Quasar sample).
Sources with X-ray and radio luminosity measurements were selected
from the radio-loud quasar catalogues of Zhu et al.
(2019MNRAS.482.2016Z 2019MNRAS.482.2016Z), Snios et al. (2020ApJ...899..127S 2020ApJ...899..127S,
2021ApJ...914..130S 2021ApJ...914..130S, Cat. J/ApJ/914/130), and Zhu et al.
(2021MNRAS.505.1954Z 2021MNRAS.505.1954Z, Cat. J/MNRAS/505/1954). Radio fluxes were taken
from the VLA-FIRST radio survey (Becker et al. 1995ApJ...450..559B 1995ApJ...450..559B),
or from independent Very Large Array (VLA) observations when Faint
Images of the Radio Sky at Twenty-cm (FIRST) data of the source was
not available. X-ray luminosities were derived using observations from
Chandra, XMM-Newton, and Swift. A region was defined around the AGN
core, and an emission spectrum was extracted from the source. In the
table1.dat, we synthesized main informations about our sources and
physical properties used the model the fundamental activity plane (see
section 3).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 77 353 Properties of our quasar sample
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See also:
J/ApJ/914/130 : Chandra & VLA obs. of 14 high-redshift QSOs (Snios+, 2021)
J/MNRAS/505/1954 : Properties and X-rays of RLQs and RQQs quasars (Zhu+, 2021)
J/MNRAS/498/4033 : Extreme quasar X-ray variability (Timlin+, 2020)
J/ApJ/914/130 : Chandra & VLA obs. of 14 high-redshift QSOs (Snios+, 2021)
J/ApJS/249/17 : SDSS QSO DR14 spectral properties (Rakshit+, 2020)
J/ApJ/658/815 : Radio loudness of active galactic nuclei (Sikora+, 2007)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- SDSS SDSS designation name
(HHMMSS.ss±DDMMSS.s) (SDSS_Name)
20- 24 F5.3 --- z Redshift (z)
26- 30 F5.3 [-] logR The radio loudness parameter (LogR) (1)
32- 37 F6.3 [10-7W] logLrad The logarithm of 5 GHz rest-frame
radio luminosity (LogLRi)
39- 43 F5.3 [10-7W] e_logLrad Mean error of logLrad (logLrad_error)
45 I1 --- r_logLrad Reference for 5 GHz radio luminosity
(Ref) (2)
47- 51 F5.2 [10-7W] logLX The logarithm of 2-10 keV rest-frame
X-ray luminosity (LogLX)
53- 56 F4.2 [10-7W] e_logLX Mean error of LogLX (LogLXerror)
58 I1 --- r_logLX Reference for LogLX X-ray luminosity
(Ref) (3)
60- 64 F5.2 [Msun] logMBH The logarithm of the black hole mass
(logMBH)
66- 69 F4.2 [Msun] e_logMBH Mean error logMBH (logMBHerror)
71 I1 --- r_logMBH Reference for black hole mass (Ref) (4)
73- 77 F5.2 [-] log(LX/LEdd) Logarithm of the X-ray
luminosity-to-Eddington luminosity
ratio defined as 1.3*1038 M/M☉
erg/s (LogLX/LEdd)
--------------------------------------------------------------------------------
Note (1): Radio loudness parameter is defined as R = f5GHz/f440nm where i
f5GHz and f440nm correspond to the rest-frame flux density
at 5 GHz and 440 nm, respectively, method from Kellermann et al.
(1989AJ.....98.1195K 1989AJ.....98.1195K).
Note (2): Reference for 5 GHz radio luminosity as follows:
1 = Snios et al. 2021ApJ...914..130S 2021ApJ...914..130S, Cat. J/ApJ/914/130,
12 objects in our sample
2 = Snios et al. 2020ApJ...899..127S 2020ApJ...899..127S, 6 objects in our sample
3 = Zhu et al. 2019MNRAS.482.2016Z 2019MNRAS.482.2016Z, 11 objects in our sample
4 = Zhu et al. 2021MNRAS.505.1954Z 2021MNRAS.505.1954Z, Cat. J/MNRAS/505/1954,
204 objects in our sample
5 = Timlin et al. 2020MNRAS.498.4033T 2020MNRAS.498.4033T, Cat. J/MNRAS/498/4033,
120 objects in our sample
Note (3): Reference for LogLX X-ray luminosity are as follows:
1 = Snios et al. 2021ApJ...914..130S 2021ApJ...914..130S, Cat. J/ApJ/914/130,
12 objects in our sample
2 = Snios et al. 2020ApJ...899..127S 2020ApJ...899..127S, 6 objects in our sample
3 = Zhu et al. 2019MNRAS.482.2016Z 2019MNRAS.482.2016Z, 11 objects in our sample
4 = Zhu et al. 2021MNRAS.505.1954Z 2021MNRAS.505.1954Z, Cat. J/MNRAS/505/1954,
324 objects in our sample
Note (4): Reference for black hole mass are as follows:
6 = Rakshit et al. 2020ApJS..249...17R 2020ApJS..249...17R, Cat. J/ApJS/249/17,
353 objects in our sample
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 10-Jan-2025