J/ApJ/895/114 Optical, radio and X-ray properties for 113 QSOs (Huang+, 2020)
On the Relation between the Hard X-Ray Photon Index and Accretion Rate for
Super-Eddington Accreting Quasars.
Huang J., Luo B., Du Pu, Hu C., Wang J.-M., Li Y.-J.
<Astrophys. J., 895, 114 (2020)>
=2020ApJ...895..114H 2020ApJ...895..114H
ADC_Keywords: QSOs; X-ray sources; Black holes; Redshifts; Optical;
Radio sources
Keywords: Accretion ; X-ray quasars ; Supermassive black holes
Abstract:
We investigate whether the correlation between the hard X-ray photon
index (Γ) and accretion rate for super-Eddington accreting
quasars is different from that for sub-Eddington accreting quasars. We
construct a sample of 113 bright quasars from the Sloan Digital Sky
Survey Data Release 14 quasar catalog, with 38 quasars as the
super-Eddington subsample and 75 quasars as the sub-Eddington
subsample. We derive black hole masses using a simple-epoch virial
mass formula based on the Hβ lines, and we use the standard thin
disk model to derive the dimensionless accretion rates (M) for our
sample. The X-ray data for these quasars are collected from the
Chandra and XMM-Newton archives. We fit the hard X-ray spectra using a
single power-law model to obtain Γ values. We find a
statistically significant (RS=0.43, p=7.75x10-3) correlation
between Γ and M for the super-Eddington subsample. The Γ-M
correlation for the sub-Eddington subsample is also significant, but
weaker (RS=0.30, p=9.98x10-3). Linear regression analysis shows
that Γ=(0.34±0.11)log(M)+(1.71±0.17) and
Γ=(0.09±0.04)log(M)+(1.93±0.04) for the super- and
sub-Eddington subsamples, respectively. The Γ-M correlations of
the two subsamples are different, suggesting different disk-corona
connections in these two types of systems. We propose one qualitative
explanation of the steeper Γ-M correlation in the
super-Eddington regime that involves larger seed photon fluxes
received by the compact coronae from the thick disks in
super-Eddington accreting quasars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 84 113 Optical and radio properties for the final sample
table2.dat 90 113 X-ray properties for the final sample
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See also:
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VIII/51 : the FIRST Survey, version 1998Feb (White+ 1998)
VIII/59 : the FIRST Survey, version 1999Jul (White+ 1999)
VIII/71 : The FIRST Survey Catalog, Version 03Apr11 (Becker+ 2003)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
VIII/90 : The FIRST Survey Catalog, Version 12Feb16 (Becker+ 2012)
VII/286 : SDSS quasar catalog, fourteenth data release (Paris+, 2018)
J/AJ/131/2766 : Quasar luminosity function from SDSS-DR3 (Richards+, 2006)
J/ApJS/165/1 : BAL QSOs from SDSS DR3 (Trump+, 2006)
J/ApJ/687/78 : FeII emission in quasars (Hu+, 2008)
J/ApJ/692/758 : BAL QSOs in SDSS-DR5 (Gibson+, 2009)
J/A+A/493/339 : XMM-Newton serendipitous Survey. V. (Watson+, 2009)
J/MNRAS/410/860 : Redshift dependence of BAL QSOs (Allen+, 2011)
J/ApJ/736/86 : FeII emission in SDSS type 1 AGNs (Dong+, 2011)
J/ApJ/726/20 : X-ray emission from quasars (Miller+, 2011)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/ApJ/756/52 : R-band light curve of QSO J0158-4325 images (Morgan+, 2012)
J/ApJ/782/45 : SEAMBHs. I. Mrk 142, Mrk 335, and IRAS F12397+3333 (Du+,2014)
J/ApJ/793/108 : SEAMBHs. II. Continuum and Hbeta LCs (Wang+, 2014)
J/ApJ/805/122 : X-ray properties of PHL1811 analogs and WLQs (Luo+, 2015)
J/ApJ/825/126 : SEAMBHs. V. The third year (Du+, 2016)
J/ApJ/886/42 : Reverberation mapping & opt. spectra data of AGNs (Du+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Object name
20- 24 F5.3 --- z [0.06/0.69] Spectroscopic redshift
26- 31 F6.2 mag iMAG [-26.9/-20.7] Absolute i band magnitude at z=2
33- 36 F4.2 [km/s] FWHM [3.14/4.23] log broad Hβ FWHM
38- 42 F5.2 [10-7W] LHb [41.32/44] log broad Hβ luminosity (1)
44- 48 F5.2 [10-7W] LFe [10.2/44]?=-1.00 log optical FeII luminosity (1)
50- 54 F5.2 [10-7W] L5100 [43.49/45.79] log rest-frame 5100A continuum
luminosity (1)
56- 60 F5.2 [10-7W] LBol [44.19/46.71] log bolometric luminosity (2)
62- 65 F4.2 Msun M [6.69/9.93] log blackhole mass from equ. 2
67- 71 F5.2 [-] lambda [-2.28/0.5] log Eddington ratio
73- 77 F5.2 [-] Mdot [-3.1/2.45] log dimensionless accretion rate
79- 79 A1 --- l_R Upper limit flag on R
80- 84 F5.2 --- R [0.25/13.56] Radio loudness parameter
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Note (1): In units of erg/s.
Note (2): Derived from integrating the SED.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Object identifier
20- 24 F5.3 --- z [0.06/0.69] Spectroscopic redshift
26- 26 A1 --- Obs X-ray observatory code (1)
28- 37 I10 --- OID [865/790181301] Observation identifier
39- 43 F5.1 ks Texp [2.3/167.8] Cleaned exposure time
45- 51 F7.1 ct Net [203/11733] Net source counts in
observed-frame (2)
53- 56 F4.2 10+20/cm2 NH [0.67/7.25] Galactic HI column density
58- 61 F4.2 --- Gamma [1.44/2.6] Hard X-ray photon index
63- 66 F4.2 --- e_Gamma [0.02/0.33] Lower uncertainty in Gamma
68- 71 F4.2 --- E_Gamma [0.02/0.43] Upper uncertainty in Gamma
73- 78 F6.2 [mW/m2] logF [-13.38/-11.14] log observed-frame 2-10keV
flux; erg/s/cm2
80- 85 F6.1 --- Wstat [82/1164] W statistic value
87- 90 I4 --- DoF [116/1171] Degrees of Freedom
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Note (1): Codes as follows:
C = Chandra (43 occurrences)
X = XMM-Newton (70 occurrences)
Note (2): Where 2/(1+z)-7keV band for Chandra and
2/(1+z)-10keV band for XMM-Newton, excluding the Fe K complex.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-Sep-2021