J/MNRAS/520/2781 SOUX AGN sample with SDSS-XMM-Newton surveys (Kynoch+, 2023)
The SOUX AGN sample SDSS-XMM-Newton optical, ultraviolet, and X-ray selected
active galactic nuclei spanning a wide range of parameter space - sample
definition.
Kynoch D., Mitchell J.A.J., Ward M.J., Done C., Lusso E., Landt H.
<Mon. Not. R. Astron. Soc. 520, 2781-2805 (2023)>
=2023MNRAS.520.2781K 2023MNRAS.520.2781K (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Active gal. nuclei ; Black holes ; Cross identifications ;
Accretion ; Spectroscopy ; Photometry ; Optical ; X-ray sources ;
Radio sources ; Ultraviolet ; Equivalent widths ;
Velocity dispersion ;
Keywords: accretion, accretion discs - black hole physics - galaxies: active -
galaxies: high-redshift - quasars: emission lines -
quasars: supermassive black holes
Abstract:
We assemble a sample of 696 type 1 active galactic nuclei (AGN) up to
a redshift of z = 2.5, all of which have an SDSS spectrum containing
at least one broad emission line (Hα, Hβ, or Mg II) and an
XMM-Newton X-ray spectrum containing at least 250 counts in addition
to simultaneous optical/ultraviolet photometry from the XMM Optical
Monitor. Our sample includes quasars and narrow-line Seyfert 1s: thus
our AGN span a wide range in luminosity, black hole mass, and
accretion rate. We determine single-epoch black hole mass relations
for the three emission lines and find that they provide broadly
consistent mass estimates whether the continuum or emission line
luminosity is used as the proxy for the broad emission line region
radius. We explore variations of the UV/X-ray energy index αox
with the UV continuum luminosity and with black hole mass and
accretion rate, and make comparisons to the physical quasar spectral
energy distribution model QSOSED. The majority of the AGN in our
sample lie in a region of parameter space with 0.02 < L/LEdd < 2 as
defined by this model, with narrow- line type 1 AGN offset to lower
masses and higher accretion rates than typical broad-line quasars. We
find differences in the dependence of αox on UV luminosity
between both narrow/broad-line and radio-loud/quiet subsets of AGN:
αox has a slightly weaker dependence on UV luminosity for
broad-line AGN and radio-loud AGN have systematically harder
αox.
Description:
Obtaining high-quality multiwavelength spectra for high-z AGN
necessarily restricts sample to a small number of bright quasars,
thereby limiting the parameter space which can be explored. An
approach is to sample the far-UV and soft X-ray emission on either
side of the peak and use a physical model to 'bridge the gap' and
recover the intrinsic spectral energy distribution (SED), these models
are based on relatively small number of sources. Studies showed that
the broad-band SEDs of AGN could generally be fit with three
components: a standard accretion disc, a hot corona, and an
intermediate 'warm corona' responsible for the observed excess of soft
X-ray emission. Since a decade, the continuing SDSS and XMM-Newton
surveys have greatly increased the number of AGN with quality
optical/UV and X-ray spectra which allows us to test model predictions
against the observed properties of a large and diverse sample of AGN.
(see more on Introduction section).
A more rigorous understanding of the accretion flow and disc-corona
relationship will also enable us to better understand the origin of
relativistic jets. In this first paper in a series, we make use of
recent optical, UV, and X-ray catalogues to compile a large sample of
AGN with both optical and X-ray spectra in addition to broad
multiwavelength coverage. This new sample has the advantage of being
large enough to investigate population statistics whilst still having
good quality multiwavelength data. It has been selected to probe a
diverse range of AGN properties as we will demonstrate, the sample
spans several orders of magnitude in black hole mass and luminosity
(accretion rate). The sample is a well-suited selection with which to
perform detailed investigations of the evolution of the disc-corona
system with black hole mass and accretion rate. In this paper we make
key measurements of AGN properties and take a preliminary look at the
evolution of the spectral energy distribution with both mass and
luminosity. (see more on Introduction section).
As detailed in section 2, we choose SDSS-DR14Q optical spectra which
also compiled ROSAT, XMM-Newton (also 3XMM-DR7 and OM), GALEX, 2MASS,
WISE, UKIDSS, and FIRST multiwavelength data. For X-ray we
investigated 4XMM-DR9. Finally, we take optical and ultraviolet
photometry from XMM-SUSS4.1. We cross matched optical and X-ray
catalogs to find ∼17000 clean sources. Then we cross-matched our
positions and IDs with OM-EPIC observations, we only select quasar
redshifts with OM photometry not compromised by the strong UV Lyman
α and forest. We also required high-quality spectra with good
number of X-ray counts (~>250) which left 782 quasars. More, to
estimate of the black hole mass, we require spectral coverage of at
least one of (Hα, Hβ, MgII) emission lines that are visible
for z≤2.5 which left 768 sources. At the end, a visual inspection of
all optical spectra to remove low SNR, bad absorption features affect
MBH measurements, a wrong X-ray diffuse emission spectra. These
quality control give rise to unique 696 AGNs of these 636 are from
SDSS-DR14Q, 60 are added from Rakshit et al. (2017ApJS..229...39R 2017ApJS..229...39R,
Cat. J/ApJS/229/39, R17). All their informations and physical
properties are included in table.dat in which we provide spec/phot
UV/X-ray/Optical/Radio rest frame luminosities of continums and lines
(with uncertainties and spectral fits quality flags), line FWHMs and
EWs, radio loudness, ΓX αox indices, MBHs (see
section 2.3, 3, 4 and 5 for respectively spectral fits, luminosities,
MBH and αox index).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 1122 696 Spectroscopic and photometric measurements and
physical quantities of AGN in the SOUX sample
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See also:
J/MNRAS/504/5726 : IR lines of AGNs accretion disk (Fernandez-Ontiveros+, 2021)
J/MNRAS/496/245 : Lx-Luv-Lradio relation in radio-loud quasars
(Zhu+, 2020)
J/MNRAS/422/3268 : Relation between X-ray and optical spectra (Jin+, 2012)
J/MNRAS/383/581 : Broad-line Balmer decrements in blue AGN (Dong+, 2008)
J/ApJ/843/30 : MgII line vs 3000Å continuum analysis in 68 QSOs
(Zhu+, 2017)
J/ApJ/819/154 : SDSS-DR7 QSOs with X-ray and UV luminosities (Lusso+, 2016)
J/ApJ/753/125 : Near-IR spectroscopy follow-up of 60 SDSS-DR7 QSOs
(Shen+, 2012)
J/ApJ/613/682 : AGN central masses and broad-line region sizes
(Peterson+, 2004)
J/ApJS/249/17 : SDSS QSO DR14 spectral properties (Rakshit+, 2020)
J/ApJS/241/34 : The SDSS Reverberation Mapping (SDSS-RM) project
(Shen+, 2019)
J/ApJS/229/39 : Narrow line Seyfert 1 galaxies from SDSS-DR12
(Rakshit+, 2017)
J/ApJS/206/4 : SED and bolometric corrections for luminous QSOs
(Krawczyk+, 2013)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/ApJS/166/128 : Narrow line Seyfert 1 galaxies from SDSS-DR3 (Zhou+, 2006)
J/AJ/130/387 : SDSS-ROSAT AGN data (Strateva+, 2005)
J/A+A/663/L7 : Quasars as high-redshift standard candles (Sacchi+, 2022)
J/A+A/512/A34 : XMM-COSMOS Type 1 AGNs (Lusso+, 2010)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI
(Kalberla+ 2005)
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VII/286 : SDSS quasar catalog, fourteenth data release (Paris+, 2018)
IX/59 : XMM-Newton Serendipitous Source Catalogue 4XMM-DR9
(Webb+, 2020)
II/340 : XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS2.1)
(Page+ 2014)
Byte-by-byte Description of file: table.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- SDSS Unique SDSS spectrum identifier as
PLATE-MJD-FIBER (SDSS_ID)
17- 27 F11.7 deg RAdeg Degrees Right Ascension (J2000) (RA)
29- 41 F13.10 deg DEdeg Degrees Declination (J2000) (DEC)
43- 53 F11.9 --- z Spectroscopic redshift (Z)
55 I1 --- DR14Q [0/1] If source is in SDSS DR14 quasar
from Paris et al. 2018A&A...613A..51P 2018A&A...613A..51P,
Cat. VII/286 636 times (DR14Q)
57 I1 --- R17 [0/1] If source is in R17 NLS1 from
Rakshit et al. 2017ApJS..229...39R 2017ApJS..229...39R,
Cat. J/ApJS/229/39 132 times (R17)
59- 68 F10.7 --- SNRmed Median S/N sampled in emission-line
free windows of the spectrum
(SNRATIOCONT)
70- 78 F9.4 0.1nm WaveMin Shortest rest-frame wavelength covered
in the optical spectrum (MIN_WAVE)
80- 88 F9.4 0.1nm WaveMax Longest rest-frame wavelength covered
in the optical spectrum
90- 100 F11.6 10-7W logL1350 ?=-999 Logarithm of the continuum
luminosity at 1350 Å rest-frame
from the SDSS spectrum (LOG_L1350)
102- 113 E12.10 10-7W e_logL1350 ?=-999 Uncertainty on logL1350
(LOGL1350ERR)
115- 118 I4 --- q_logL1350 ?=-999 Quality flag indicator on
logL1350 (QUALITY_L1350) (1)
120- 128 F9.4 10-7W logL2500sp ?=-999 Logarithm of the continuum
luminosity at 2500 Å rest-frame
from the SDSS spectrum (LOGL2500SPEC)
130- 138 F9.4 10-7W e_logL2500sp ?=-999 Uncertainty on logL2500sp
(LOGL2500SPEC_ERR)
140- 159 F20.15 10-7W logL2500OM ?=-999 Logarithm of the continuum
luminosity at 2500 Å rest-frame
from XMM-Newton OM photometry
(LOGL2500PHOT_OM)
161- 181 E21.19 10-7W e_logL2500OM ?=-999 Uncertainty on logL2500OM
(LOGL2500PHOTOMERR)
183- 202 F20.15 10-7W logL2500ph ?=-999 Logarithm of the continuum
luminosity at 2500 Å rest-frame
from SDSS photometry
(LOGL2500PHOT_SDSS)
204- 227 F24.19 10-7W e_logL2500ph ?=-999 Uncertainty on logL2500ph
(LOGL2500PHOTSDSSERR)
229- 247 A19 --- f_alphaOX The L2500 column measurement used to
calculate UV/X-ray energy index
αox (LOGL2500ALPHA_OX)
249- 259 F11.6 10-7W logL3000 ?=-999 Logarithm of the continuum
luminosity at 3000 Å rest-frame
from the SDSS spectrum (LOG_L3000)
261- 272 E12.10 10-7W e_logL3000 ?=-999 Uncertainty on logL3000
(LOGL3000ERR)
274- 277 I4 --- q_logL3000 ?=-999 Quality flag indicator on
logL3000 (QUALITY_L3000) (2)
279- 298 F20.15 10-7W logL4400sp ?=-999 Logarithm of the continuum
luminosity at 4400 Å rest-frame
from the SDSS spectrum (LOGL4400SPEC)
300- 322 F23.18 10-7W e_logL4400sp ?=-999 Uncertainty on logL4400sp
(LOGL4400SPEC_ERR)
324- 332 F9.4 10-7W logL4400OM ?=-999 Logarithm of the continuum
luminosity at 4400 Å rest-frame
from XMM-Newton OM photometry
(LOGL4400PHOT_OM)
334- 342 F9.4 10-7W e_logL4400OM ?=-999 Uncertainty on logL4400OM
(LOGL4400PHOTOMERR)
344- 363 F20.15 10-7W logL4400ph ?=-999 Logarithm of the continuum
luminosity at 4400 Å rest-frame
from SDSS photometry
(LOGL4400PHOT_SDSS)
365- 388 F24.19 10-7W e_logL4400ph ?=-999 Uncertainty on logL4400ph
(LOGL4400PHOT_SDSS)
390- 408 A19 --- n_RL The L4400 column measurement used to
calculate RL radio loudness energy
index (LOGL4400R_LOUD)
410- 420 F11.6 10-7W logL5100 ?=-999 Logarithm of the continuum
luminosity at 5100 Å rest-frame
from the SDSS spectrum (LOG_L5100)
422- 433 A12 10-7W e_logL5100 Uncertainty on logL5100 (LOGL5100ERR)
435- 438 I4 --- q_logL5100 ?=-999 Quality flag indicator on
logL5100 (QUALITY_L5100) (3)
440- 449 E10.5 km/s FWHMHa ?=-999 Full-width at half-maximum of
the broad Hα emission line
(FWHMHABR)
451- 460 E10.7 km/s e_FWHMHa ?=-999 Uncertainty on FWHMHa
(FWHMHABR_ERR)
462- 470 E9.4 0.1nm WaveHa ?=-999 Peak wavelength of the broad
H α emission line (PEAKHABR)
472- 481 E10.8 0.1nm e_WaveHa ?=-999 Uncertainty on WaveHa
(PEAKHABR_ERR)
483- 492 A10 0.1nm EWHa Equivalent width of the broad
H α emission line (EWHABR)
494- 503 A10 0.1nm e_EWHa Uncertainty on EWHa (EWHABR_ERR)
505- 515 F11.6 10-7W logLHa ?=-999 Logarithm of the luminosity of
the broad H α emission line
(LOGLHABR)
517- 531 F15.10 10-7W e_logLHa ?=-999 Uncertainty on logLHa
(LOGLHABR_ERR)
533- 536 I4 --- q_logLHa ?=-999 Quality flag indicator on
logLHa (QUALITY_HA) (4)
538- 548 F11.5 km/s FWHMHb ?=-999 Full-width at half-maximum of
the broad H {bata} emission line
(FWHMHBBR)
550- 560 F11.6 km/s e_FWHMHb ?=-999 Uncertainty on FWHMHb
(FWHMHBBR_ERR)
562- 570 F9.4 0.1nm WaveHb ?=-999 Peak wavelength of the broad
H β emission line (PEAKHBBR)
572- 584 F13.8 0.1nm e_WaveHb ?=-999 Uncertainty on WaveHb
(PEAKHBBR_ERR)
586- 595 A10 0.1nm EWHb Equivalent width of the broad Hβ
emission line (EWHBBR)
597- 606 A10 0.1nm e_EWHb Uncertainty on EWHb (EWHBBR_ERR)
608- 618 F11.6 10-7W logLHb ?=-999 Logarithm of the luminosity of
the broad H β emission line
(LOGLHBBR)
620- 634 F15.10 10-7W e_logLHb ?=-999 Uncertainty on logLHb
(LOGLHBBR_ERR)
636- 639 I4 --- q_logLHb ?=-999 Quality flag indicator on
logLHb (QUALITY_HB) (5)
641- 643 A3 --- Balmer Flag for Balmer lines as K23 for this
work 60 times and as R20 636 times for
Rakshit et al. 2020ApJS..249...17R 2020ApJS..249...17R,
Cat. J/ApJS/249/17 (BALMER_SOURCE)
645- 653 E9.4 km/s FWHMMgII ?=-999 Full-width at half-maximum of
the broad Mg II emission line
(FWHMMGIIBR)
655- 664 E10.6 km/s e_FWHMMgII ?=-999 Uncertainty on FWHMmgII
(FWHMMGIIBR_ERR)
666- 674 E9.4 0.1nm WaveMgII ?=-999 Peak wavelength of the broad
Mg II emission line (PEAKMGIIBR)
676- 685 E10.8 0.1nm e_WaveMgII ?=-999 Uncertainty on WavemgII
(PEAKMGIIBR_ERR)
687- 696 E10.6 0.1nm EWMgII ?=-999 Equivalent width of the broad
Mg II emission line (EWMGIIBR)
698- 707 E10.8 0.1nm e_EWMgII ?=-999 Uncertainty on EWmgII
(EWMGIIBR_ERR)
709- 719 F11.6 10-7W logLMgII ?=-999 Logarithm of the luminosity of
the broad Mg II emission line
(LOGLMGIIBR)
721- 735 F15.10 10-7W e_logLMgII ?=-999 Uncertainty on logLmgII
(LOGLMGIIBR_ERR)
737- 740 I4 --- q_logLMgII ?=-999 Quality flag indicator on
logLmgII (QUALITY_MGII) (6)
742- 744 A3 --- MgII Flag for Mg II as K23 for this work
100 times and as R20 596 times for
Rakshit et al. 2020ApJS..249...17R 2020ApJS..249...17R,
Cat. J/ApJS/249/17 (MGII_SOURCE)
746 I1 --- SepMgII Flag for modelled MgII region method
(MGII_SEP) (9)
748 A1 --- TypeLine Flag for AGN types 1 broad line as B
595 times and narrow line as N 101
times (LINEWIDTH)
750- 761 E12.9 Msun MBH1 ?=-999 The BH mass estimate from
FWHMHa and logL5100
(MASSHA5100_MR16) (10)
763- 774 E12.9 Msun MBH2 ?=-999 The BH mass estimate from
FWHMHa and logLHa
(MASSHAHA_MR16) (10)
776- 787 E12.9 Msun MBH3 ?=-999 The BH mass estimate from
FWHMHb and logL5100
(MASSHB5100_MR16) (10)
789- 800 E12.9 Msun MBH4 ?=-999 The BH mass estimate from
FWHMHb and logLHb
(MASSHBHB_G10) (11)
802- 814 E13.9 Msun MBH5 ?=-999 The BH mass estimate from
FWHMmgII and logL3000
(MASSMGII3000_MR16) (10)
816- 828 E13.9 Msun MBH6 ?=-999 The BH mass estimate from
FWHMmgII and logLmgII
(MASSMGIIMGII_W18) (12)
830- 841 E12.9 Msun MBH7 ?=-999 The BH mass estimate from
FWHMHa and logL5100 using the
calibrated relation in section 4 of
this work (MASSHA5100_K23)
843- 854 E12.9 Msun MBH8 ?=-999 The BH mass estimate from
FWHMHa and logLHa using the calibrated
relation in section 4 of this work
(MASSHAHA_K23)
856- 867 E12.9 Msun MBH9 ?=-999 The BH mass estimate from
FWHMHb and logLHb using the calibrated
relation in section 4 of this work
(MASSHBHB_K23)
869- 881 E13.9 Msun MBH10 ?=-999 The BH mass estimate from
FWHMmgII and logL3000 using the
calibrated relation in section 4 of
this work (MASSMGII3000_K23)
883- 895 E13.9 Msun MBH11 ?=-999 The BH mass estimate from
FWHMmgII and logLmgII using the
calibrated relation in section 4 of
this work (MASSMGIIMGII_K23)
897- 902 F6.1 --- QHa5100 ?=-999 Quality flag for MBH1 and MBH7
(QMASSHA_5100) (13)
904- 909 F6.1 --- QHB5100 ?=-999 Quality flag for MBH3 and MBH
(QMASSHB_5100) (14)
911- 916 F6.1 --- QMgII3000 ?=-999 Quality flag for MBH5 and MBH10
(QMASSMGII_3000) (15)
918- 936 F19.16 Msun MBH Logarithm of our preferred BH mass
estimate (LOGMASSPREF_VALUE)
938- 955 A18 --- f_MBH Flag for which BH mass estimate is the
preferred one (LOGMASSPREF_SOURCE)
(7)
957- 966 I10 --- ObsID The XMM-Newton obsID for the X-ray and
OM photometric data from 4XMM-DR9 of
Webb et al. 2020A&A...641A.136W 2020A&A...641A.136W,
Cat. IX/59 (XMM_OBSID)
968- 982 I15 --- Source The unique X-ray source number taken
from the 4XMM-DR9 of Webb et al.
2020A&A...641A.136W 2020A&A...641A.136W, Cat. IX/59
(XMM_SRCID)
984- 990 F7.4 10-7W/Hz logL2keV Logarithm of monochromatic X-ray
Lν2keV flux at rest-frame 2 keV
estimated from the XMM-Newton band
fluxes as seen in sect 3.2 (LOG_L2KEV)
992-1001 F10.8 10-7W/Hz e_logL2keV Uncertainty on logL2keV (LOGL2KEVERR)
1003-1013 F11.8 --- GammaX Estimated X-ray photon index as seen
in section 3.2 (GAMMA_X)
1015-1024 F10.8 --- e_GammaX Uncertainty on GammaX (GAMMAXERR)
1026-1038 F13.8 --- alphaOX ?=-999 Optical-X-ray energy index
(ALPHA_OX) (16)
1040-1051 E12.10 --- e_alphaOX ?=-999 Uncertainty on alphaOX
(ALPHAOXERR)
1053-1072 F20.15 W/Hz logL5GHz ?=-999 Logarithm of Lν5GHz flux
estimated from the FIRST radio flux as
explained in section 3.3 (LOG_L5GHZ)
1074-1094 E21.19 W/Hz e_logL5GHz ?=-999 Uncertainty on logL5GHz
(LOGL5GHZERR)
1096-1117 F22.16 --- RL ?=-999 Radio loudness parameter
(R_LOUD) (17)
1119-1122 A4 --- f_RL Flag for RL types (RLOUDFLAG) (8)
--------------------------------------------------------------------------------
Note (1): In this case, for 30 sources with L1350 values, the quality flag 0
indicates no issues are raised and the measurement may be considered
to be reliable.
Note (2): In this case for 586 sources with L3000 values, quality flags are
as follows:
0 = No issues are raised and the measurement may be considered to
be reliable, 582 occurences in our sample
8 = The continuum slope has reached the lower or upper limit in
the fit, 1 occurence in our sample
16 = The uncertainty on the continuum slope >0.3, 3 occurences in
our sample
Note (3): In this case for 451 sources with L5100 values, quality flags are
as follows:
0 = No issues are raised and the measurement may be considered to
be reliable, 476 occurences in our sample
8 = The continuum slope has reached the lower or upper limit in
the fit, 2 occurences in our sample
12 = The continuum slope or its uncertainty are zero, NaN, or
infinite and has reached the lower or upper limit in the fit,
3 occurences in our sample
Note (4): In this case for 220 sources with LHA values, quality flags are
as follows:
0 = No issues are raised and the measurement may be considered to
be reliable, 582 occurences in our sample
1 = S/N in the continuum around the line < 3, 14 occurences in our
sample
4 = Fractional uncertainty of the luminosity >1.5, 1 occurence in
our sample
18 = The FWHM ≤ 910 km/s and the luminosity or its uncertainty are
zero, NaN, or infinite, 9 occurences in our sample
19 = Same quality indicators as 18 plus S/N in the continuum around
the line < 3, 2 occurences in our sample
Note (5): In this case for 482 sources with LHB values, quality flags are
as follows:
0 = No issues are raised and the measurement may be considered to
be reliable, 406 occurences in our sample
1 = S/N in the continuum around the line < 3, 40 occurences in our
sample
16 = The FWHM ≤ 910 km/s, 1 occurence in our sample
18 = The FWHM ≤ 910 km/s and the luminosity or its uncertainty are
zero, NaN, or infinite, 4 occurences in our sample
32 = The fractional uncertainty of the FWHM > 2, 1 occurence in our
sample, 1 occurence in our sample
256 = The uncertainty on the velocity offset > 1000 km/s, 14
occurences in our sample
257 = The uncertainty on the velocity offset > 1000 km/s and S/N in
the continuum around the line < 3, 12 occurences in our sample
274 = The uncertainty on the velocity offset > 1000 km/s, the
FWHM ≤ 910 km/s and the luminosity or its uncertainty are
zero, NaN, or infinite, 1 occurence in our sample
275 = Same quality indicators as 274 plus S/N in the continuum
around the line < 3, 1 occurence in our sample
289 = The uncertainty on the velocity offset > 1000 km/s, the
fractional uncertainty of the FWHM > 2 and S/N in the continuum
around the line < 3, 1 occurence in our sample
314 = The uncertainty on the velocity offset > 1000 km/s, the
fractional uncertainty of the FWHM > 2, FWHM ≤ 910 km/s, its
uncertainty are zero, NaN, or infinite, the luminosity or its
uncertainty are zero, NaN, or infinite, 1 occurence in our
sample
Note (6): In this case for 521 sources with MgII values, quality flags are
as follows:
0 = No issues are raised and the measurement may be considered to
be reliable, 483 occurences in our sample
1 = S/N in the continuum around the line < 3, 40 occurences in our
sample, 34 occurences in our sample
33 = The fractional uncertainty of the FWHM > 2, S/N in the
continuum around the line < 3, 1 occurence in our sample
257 = The uncertainty on the velocity offset > 1000 km/s and S/N in
the continuum around the line < 3, 2 occurences in our sample
289 = The uncertainty on the velocity offset > 1000 km/s, the
fractional uncertainty of the FWHM > 2 and S/N in the continuum
around the line < 3, 1 occurence in our sample
Note (7): Preferred MBH values are as follows:
MASSHA5100_K23 = MBH7, 19 occurences in our sample
MASSHAHA_K23 = MBH8, 1 occurence in our sample
MASSHB5100_MR16 = MBH3, 356 occurences in our sample
MASSHBHB_K23 = MBH9, 5 occurences in our sample
MASSMGII3000_K23 = MBH10, 310 occurences in our sample
MASSMGIIMGII_K23 = MBH11, 5 occurences in our sample
Note (8): The RL types are as follows:
RL = Radio-loud, 68 occurences in our sample
RQd = Radio-detected and radio-quiet, 33 occurences in our sample
RQu = Radio-undetected and radio-quiet, 206 occurences in our sample
RU = Radio-undetected and undetermined radio-loudness,
304 occurences in our sample
-999 = Outside FIRST footprint or no L4400 values, 85 occurences
in our sample
Note (9): As 0 651 times for global fit to full spectrum and 1 45 times for
separately to Balmer line regions as explained in section 2.3.
Note (10): Using the calibrated relation of Mejia-Restrepo et al.
2016MNRAS.460..187M 2016MNRAS.460..187M as explained in section 4.
Note (11): Using the calibrated relation of Greene et al. 2010ApJ...723..409G 2010ApJ...723..409G
as explained in section 4.
Note (12): Using the calibrated relation of Woo et al. 2018ApJ...859..138W 2018ApJ...859..138W
as explained in section 4.
Note (13): As 1 19 times if q_logLHa and q_logL5100 are both in 0 for reliable
data cases otherwise is set to 0 189 times.
Note (14): As 1 73 times if q_logLHb and q_logL5100 are both in 0 for reliable
data cases otherwise is set 0 401 times.
Note (15): As 1 38 times if q_logLmgII and q_logL3000 are both in 0 for
reliable data cases otherwise is set 0 479 times.
Note (16): Calculated with L2500 and logL2keV shows relative power of the
UV-emitting accretion disc to the X-ray emitting corona as
explained in section 5.
Note (17): As L5GHz/L4400 indicates the power of AGN outflows relative to the
accretion flow mostly for radio-loud AGN exhibiting powerful jets
as explained section 3.3.
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License: CC-BY-4.0 [see https://spdx.org/licenses/]
(End) Luc Trabelsi [CDS] 23-Mar-2026