J/MNRAS/491/5881 Extended size-luminosity relation for the RM AGNs (Yu+, 2020)
An extended size-luminosity relation for the reverberation-mapped AGNs:
the role of the accretion rate.
Yu L.-M., Zhao B.-X., Bian W.-H., Wang C., Ge X.
<Mon. Not. R. Astron. Soc., 491, 5881-5896 (2020)>
=2020MNRAS.491.5881Y 2020MNRAS.491.5881Y (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies, Seyfert ; Accretion ;
Spectra, optical
Keywords: galaxies: active - galaxies: nuclei - quasars: emission lines -
quasars: general - galaxies: Seyfert
Abstract:
For a compiled sample of 120 reverberation-mapped AGNs, the bivariate
correlations of the broad-line region (BLR) size (RBLR) with the
continuum luminosity at 5100Å (L5100) and the dimensionless
accretion rates (dM/dt) are investigated. Using our recently
calibrated virial factor f, and the velocity tracer from the Hβ
full width at half-maximum (FWHM(Hβ)) or the line dispersion
(σHβ) measured in the mean spectra, three kinds of
supermassive black hole (SMBH) masses and dM/dt are calculated. An
extended RBLR(Hβ)-L5100 relation including dM/dt is found to
be stronger than the canonical RBLR(Hβ)-L5100 relation,
showing smaller scatters. The observational parameters, RFe (the
ratio of optical FeII to Hβ line flux) and the line profile
parameter DHβ (DHβ=FWHM(Hβ)/σHβ), have
relations with three kinds of dM/dt. Using RFe and DHβ to
substitute dM/dt, extended empirical RBLR(Hβ)-L5100 relations
are presented. RFe is a better 'fix' for the RBLR(Hβ)-L5100
offset than the Hβ shape DHβ. The extended empirical
RBLR(Hβ)-L5100 relation including RFe can be used to
calculate RBLR, and thus the single-epoch SMBH mass MBH. Our
measured accretion rate dependence is not consistent with the simple
model of the accretion disc instability leading the BLR formation. The
BLR may instead form from the inner edge of the torus, or from some
other means in which BLR size is positively correlated with accretion
rate and the SMBH mass.
Description:
Up to now, there are 120 RM AGNs with measured Hβ lags (e.g.
Bentz et al. 2013ApJ...767..149B 2013ApJ...767..149B; Du et al. 2015ApJ...806...22D 2015ApJ...806...22D, Cat.
J/ApJ/806/22; Grier et al. 2017ApJ...851...21G 2017ApJ...851...21G, Cat. J/ApJ/851/21; Du
et al. 2018ApJ...856....6D 2018ApJ...856....6D, Cat. J/ApJ/856/6). We divide them into
three subsamples. The first subsample has 25 AGNs presented by SEAMBH
collaboration (Du et al. 2015ApJ...806...22D 2015ApJ...806...22D, Cat. J/ApJ/806/22). 24
out of these 25 sources are identified to be super-Eddington accretor
(dM/det≥3) (Du et al. 2018ApJ...856....6D 2018ApJ...856....6D, Cat. J/ApJ/856/6). The
second subsample contains 39 AGNs summarized by Bentz et al.
(2013ApJ...767..149B 2013ApJ...767..149B) (excluding Mrk 335 and Mrk 142 again mapped by
the SEAMBHs project) and 12 other sources published recently
(hereafter BentzSample; Barth et al. 2015ApJS..217...26B 2015ApJS..217...26B, Cat.
J/ApJS/217/26; Bentz et al. 2016ApJ...830..136B 2016ApJ...830..136B; Bentz, Batiste &
Seals 2016ApJ...831....2B 2016ApJ...831....2B; Fausnaugh et al. 2017ApJ...840...97F 2017ApJ...840...97F, Cat.
J/ApJ/840/97; Williams et al. 2018ApJ...866...75W 2018ApJ...866...75W). The third
subsample contains 44 high-z AGNs (z∼0.1-1.0) from SDSS-RM project
which was done by fibre spectrum (hereafter SDSS-RM; Grier et al.
2017ApJ...851...21G 2017ApJ...851...21G, Cat. J/ApJ/851/21). The entire sample includes
120 AGNs with measured Hβ lags. We collect DHβ and RFe
measured from the optical spectrum, which were suggested to be driven
by dM/dt.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 201 181 The properties of 120 RM AGNs
refs.dat 59 29 References for Table 1
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See also:
J/ApJ/851/21 : SDSS RM project first year of observations (Grier+, 2017)
J/ApJ/806/22 : SEAMBHs IV. Hβ time lags (Du+, 2015)
J/ApJ/856/6 : SEAMBHs IX. 10 new Hβ light curves (Du+, 2018)
J/ApJS/217/26 : Lick AGN monitoring 2011: light curves (Barth+, 2015)
J/ApJ/840/97 : Optical reverberation mapping campaign of 5 AGNs
(Fausnaugh+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Sample Sample name (SEAMBH, SDSS-RM or BentzSample)
13- 25 A13 --- Name Source name
27 A1 --- f_Name [*] Flag on Name (1)
29- 33 F5.1 d tau Rest-frame Hβ lag (2)
35- 38 F4.1 d E_tau Upper error on tau
40- 43 F4.1 d e_tau Lower error on tau
45- 50 F6.3 [10-7W] logL5100 Logarithm of the host-corrected
monochromatic luminosity at 5100Å (3)
52- 56 F5.3 [10-7W] e_logL5100 Error on logL5100
58- 62 I5 km/s FWHM Broad Hβ FWHM measured from the mean
spectrum (2)
64- 67 I4 km/s e_FWHM Error on FWHM
69- 72 I4 km/s sigHb Broad Hβ line dispersion
σHβ measured from the mean
spectrum (2)
74- 77 I4 km/s e_sigHb Error on sigHb
79- 82 F4.2 --- DHb Line profile parameter DHβ=FWHM/sigHb
84- 87 F4.2 --- e_DHb Error on DHb
89- 92 F4.2 --- RFe ? Ratio of optical FeII to Hβ line
flux (4)
94- 97 F4.2 --- e_RFe ? Error on RFe
99-102 F4.2 [Msun] logMBHF Logarithm of the black hole mass derived
from the FWHM and fBLR=1
104-107 F4.2 [Msun] E_logMBHF Upper error on logMBHF
109-112 F4.2 [Msun] e_logMBHF Lower error on logMBHF
114-117 F4.2 [Msun] logMBHs Logarithm of the black hole mass derived
from sigHb and fBLR=4.47
119-122 F4.2 [Msun] E_logMBHs Upper error on logMBHs
124-127 F4.2 [Msun] e_logMBHs Lower error on logMBHs
129-132 F4.2 [Msun] logMBHc Logarithm of the black hole mass derived
from FWHM and fBLR∝FWHM-1.11
134-137 F4.2 [Msun] E_logMBHc Upper error on logMBHc
139-142 F4.2 [Msun] e_logMBHc Lower error on logMBHc
144-148 F5.2 [-] logMdotF Logarithm of the accretion rate associated
to logMBHF
150-153 F4.2 [-] E_logMdotF Upper error on logMdotF
155-158 F4.2 [-] e_logMdotF Lower error on logMdotF
160-164 F5.2 [-] logMdots Logarithm of the accretion rate associated
to logMBHs
166-169 F4.2 [-] E_logMdots Upper error on logMdots
171-174 F4.2 [-] e_logMdots Lower error on logMdots
176-180 F5.2 [-] logMdotc Logarithm of the accretion rate associated
to logMBHc
182-185 F4.2 [-] E_logMdotc Upper error on logMdotc
187-190 F4.2 [-] e_logMdotc Lower error on logMdotc
192-199 A8 --- Ref References
201 A1 --- Note [*] Asterisk means that the MCMC black hole
mass is used to calculate the dimensionless
accretion rate
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Note (1): Flag as follows:
* = For a object with multiple measurements, the dimensionless accretion
rate is calculated by the weighted average of the black masses. Lines
flagged with * are the weighted averages of all the measurements.
Note (2): For SDSS-RM sources the values come from Grier et al.
(2017ApJ...851...21G 2017ApJ...851...21G, Cat. J/ApJ/851/21) and for other sources the
values are mainly from Du et al. (2015ApJ...806...22D 2015ApJ...806...22D,
Cat. J/ApJ/806/22; 2016ApJ...818L..14D 2016ApJ...818L..14D, Cat. J/ApJ/818/L14)
Note (3): The L5100 of SDSS-RM sources comes from Shen et al.
(2015ApJ...805...96S 2015ApJ...805...96S, Cat. J/ApJ/805/96) and for other sources the
values are mainly from Du et al. (2015ApJ...806...22D 2015ApJ...806...22D,
Cat. J/ApJ/806/22; 2016ApJ...818L..14D 2016ApJ...818L..14D, Cat. J/ApJ/818/L14)
Note (4): The RFe of SDSS-RM sources is derived from Shen et al.
(2019ApJS..241...34S 2019ApJS..241...34S, Cat. J/ApJS/241/34) and for other sources the
values are mainly from Du et al. (2015ApJ...806...22D 2015ApJ...806...22D,
Cat. J/ApJ/806/22; 2016ApJ...818L..14D 2016ApJ...818L..14D, Cat. J/ApJ/818/L14)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref [1/29] Rference number
4- 22 A19 --- BibCode BibCode
24- 40 A17 --- Aut Author's name
42- 59 A18 --- Com Comments
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 27-Feb-2023