J/MNRAS/514/1595 Spectral properties of 105 SDSS-DR7 quasars (Wang+, 2022)
The role of radio loudness in Eigenvector 1 and the Baldwin Effect of [O III]
λ5007.
Wang Y., Shang Z., Brotherton M.S.
<Mon. Not. R. Astron. Soc. 514, 1595-1605 (2022)>
=2022MNRAS.514.1595W 2022MNRAS.514.1595W (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Black holes ; Active gal. nuclei ; Spectroscopy ; Optical ;
Line Profiles ; Equivalent widths
Keywords: galaxies: fundamental parameters - quasars: emission lines -
quasars: general
Abstract:
The radio emission is an important observable of quasars, but its
relationship to Eigenvector 1 and the [O III] λ5007 Baldwin
Effect is not fully understood. We explore these issues based on a
sample of 1800 quasars taken from the Sloan Digital Sky Survey Data
Release 7. We employ a new approach of selecting subsamples in the
plane of fundamental physical parameters of the black hole mass and
Eddington ratio, so as to reduce variables and complexity in analyses.
Based on these subsamples, we investigate the relationship between
radio loudness R and Eigenvector 1 and find that radio loudness is
correlated with [O III] λ5007 emission, but has no clear
relationship with optical Fe II emission, which indicates that the
radio power is probably not a driver of Eigenvector 1 but merely a
secondary process. In addition, we also investigate the impact of
radio loudness on the Baldwin Effect of [O III] λ5007. We find
that when the radio loudness is not strong (log R < 2), the Baldwin
Effect of [O III] λ5007 is clear, while in the samples of
extreme radio loudness (log R => 2), the Baldwin Effect of [O III]
λ5007 becomes weaker or even disappears. We suggest that both
radio loudness and luminosity influence the relative strength of [O III].
Description:
As the most luminous active galactic nuclei (AGNs), distant quasars
may provide important clues for studying the various properties of the
early Universe. The most widely accepted theory on quasar fueling
mechanisms suggests that quasars arise from accreting material on to
their central supermassive black holes (BHs). In this paper, we address
the role of radio loudness on EV 1 and the BE of [O III] using a
sample of 1800 quasars from which subsamples are selected in the
Eddington ratio Lbol/LEdd and MBH plane.
In our work, the sample selection is based on selected quasars from
SDSS-DR7 Shen et al. (2011ApJS..194...45S 2011ApJS..194...45S, Cat. J/ApJS/194/45) matched
on the radio FIRST catalog. We proceed to MBH-Lbol/LEdd plane
selection, focusing on object with FIRST detections, redshift z < 0.8
for SDSS spectral coverage, Median S/N => 5 in the H β spectral
region t oensur good quality on MBH and Lbol/LEdd. Leading us to a
base sample of 1800 quasars. Next, we focus on a subsample of the base
sample. After applying specral and host corrections, we finally get a
subsample of 105 quasars as presented in the table1.dat with the
highest data accuracy. This table includes refined and host/spectral
corected monochromatic luminosity at 5100Å, equivalent width broad
Hβ, virial BH mass and Eddington ratio Lbol/LEdd (i.e see sections
2.2 and 2.3 for details on corrections and MBH-Lbol/LEdd plane
subsample methods/data).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 69 105 The spectral measurements and derived
fundamental physical parameters with and without
refitting for the corrected sources
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See also:
J/MNRAS/477/830 : Radio flux density of extremely red quasars (Hwang+, 2018)
VII/260 : The SDSS-DR7 quasar catalog (Schneider+, 2010)
J/MNRAS/498/1278 : VLA NLS1s southern sample (Chen+, 2020)
J/A+A/630/A110 : SDSS-FIRST quasar sample study (Ganci+, 2019)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name SDSS designation (Jhhmmss.ss+ddmmss.s)
in (J2000) (SDSS_Name)
21- 25 F5.2 [10-7W] logL5100c Monochromatic luminosity at 5100Å
after refitting and correcting as
explained in the section 2.3
(LOGL5100_CORRECTED)
27- 31 I5 km/s FWHM(BHb)c FWHM of broad Hβ after refitting
and correcting as explained in
the section 2.3 Measurement correction
(FWHMBROADHB_CORRECTED)
33- 36 F4.2 [Msun] logMBHc The virial BH mass based on logL5100c
and FWHM(BHb)c (LOGBH_CORRECTED)
38- 42 F5.2 [-] log(Lbol/LEdd)c Eddington ratio Lbol/LEdd as
3.2*104 MBH/M_☉ based on
logL5100c (LOGEDDRATIOCORRECTED)
44- 48 F5.2 [10-7W] logL5100hc ? Monochromatic luminosity at
5100Å from S11 (LOGL5100_S11) (1)
50- 54 I5 km/s FWHM(BHb)S11 FWHM of broad Hβ from Shen et al.
2011ApJS..194...45S 2011ApJS..194...45S, Cat. J/ApJS/194/45
(FWHMBROADHB_S11)
56- 59 F4.2 [Msun] logMBHS11 ? The virial BH mass based on
logL5100hc and FWHM(BHb)S11 (LOGBH_S11)
61- 65 F5.2 [-] log(Lbol/LEdd)hc ? Eddington ratio Lbol/LEdd as
3.2*104 MBH/M_☉ based on
logL5100hc (LOGEDDRATIOS11)
67- 69 A3 --- Flagcor The reason for correction (FLAG) (2)
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Note (1): logL5100hc taken from Shen et al. 2011ApJS..194...45S 2011ApJS..194...45S,
Cat. J/ApJS/194/45 after host-correction as explained in the section
2.2 Host correction.
Note (2): Line correction reasons as fgollows:
1 = FeII line overestimated, 45 cases in our sample
2 = Hβ narrow line overestimated, 71 cases in our sample
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 02-Apr-2025