J/MNRAS/455/2551 SDSS/3XMM X-ray-selected LINERs (Nisbet+, 2016)
The mass fraction of AGN and the Fundamental Plane of black hole activity from
a large X-ray-selected sample of LINERs.
Nisbet D.M., Best P.N.
<Mon. Not. R. Astron. Soc., 455, 2551-2566 (2016)>
=2016MNRAS.455.2551N 2016MNRAS.455.2551N (SIMBAD/NED BibCode)
ADC_Keywords: X-ray sources ; Active gal. nuclei ; Radio sources
Keywords: accretion, accretion discs - black hole physics - galaxies: active -
radio continuum: general- X-rays: general
Abstract:
A sample of 576 X-ray-selected LINERs was constructed by combining
data from the 3XMM-DR4 and SDSS-DR7 catalogues. The sample was used to
investigate the fraction of galaxies hosting a LINER, finding that the
fraction is a strong function of both stellar mass and black hole mass
(increasing as fLINER∝M*1.6±0.2 and
fLINER∝MBH0.6±0.1, respectively) and that it rises
close to unity at the highest black hole masses and lowest X-ray
luminosities. After obtaining radio flux densities from the FIRST
survey, the sample was also used to investigate the Fundamental Plane
of black hole activity - a scale-invariant relationship between black
hole mass, X-ray luminosity and radio luminosity that is believed to
hold across at least nine orders of magnitude of mass. There are key
advantages in using only LINERs for the derivation as these are the
counterparts of the 'low-hard' X-ray binaries for which the
relationship is tightest. The Fundamental Plane was found to be
log(LR/(erg/s)) = 0.65(±0.07)log(LX/(1042erg/s)) +
0.69(±0.10)log(MBH/108M☉) + 38.35(±0.10). The scatter
around the plane was 0.73±0.03dex, too large to suggest that the
Fundamental Plane can be used as a tool to estimate black hole mass
from the observables of X-ray and radio luminosity. The black hole
mass scaling is sensitive to the slope of the mass - velocity
dispersion relation and, in order to achieve consistency with X-ray
binaries, the analysis favours a steep gradient for this relationship,
as found in recent research.
Description:
This research has been carried out on a data base of LINERs, for which
both X-ray and radio luminosity information and black hole mass
estimates are available. The sample was constructed by cross-matching
the fourth data release of the 3XMM Serendipitous Source catalogue of
X-ray sources (released by the XMM-Newton Survey Science Centre;
XMM-SSC 2013, Cat. IX/44) with the seventh data release from the
SDSS-DR7; Abazajian et al. (2009ApJS..182..543A 2009ApJS..182..543A) and then adding in
radio luminosity data obtained from the FIRST catalogue (Becker, White
& Helfand, 1995ApJ...450..559B 1995ApJ...450..559B, Cat. VIII/92).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 111 576 Full sample of 576 LINERs
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See also:
IX/44 : XMM-Newton Serendipitous Source Catalogue 3XMM-DR4 (XMM-SSC, 2013)
VIII/92 : The FIRST Survey Catalog, Version 2014Dec17 (Helfand+ 2015)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Id Identifier in this sample of LINERs
5- 8 I4 --- Plate Plate identifier for the SDSS source
in the SDSS-DR7 catalogue
10- 14 I5 d MJD MJD identifier for the SDSS source
in the SDSS-DR7 catalogue
16- 18 I3 --- Fibre Fibre identifier for the SDSS source
in the SDSS-DR7 catalogue
20- 30 F11.7 deg RAdeg Right ascension for the SDSS source (J2000)
32- 40 F9.5 deg DEdeg Declination for the SDSS source (J2000)
42- 47 F6.4 --- z Redshift derived from the SDSS spectra
49- 53 F5.1 km/s sigma Stellar velocity dispersion of the galaxy
bulge, derived from SDSS data
55- 58 F4.2 [Msun] MBH log10 black hole mass (1)
60- 64 F5.2 Msun M* log10 stellar mass derived from the SDSS data
66- 71 I6 --- 3XMM Identifier of X-ray source in the 3XMM-DR4
catalogue
73- 84 E12.7 mW/m2 FX X-ray flux in the 2.0-12.0keV band
86- 91 F6.3 [10-7W] logLX log10 X-ray luminosity corresponding to the
flux in the 2.0-10.0keV band
93-103 E11.6 Jy S1.4GHz Radio flux density at an observing frequency
of 1.4GHz
105 A1 --- l_logL1.4GHz [L] Limit flag on logL1.4GHz (2)
106-111 F6.3 [10-7W] logL1.4GHz log10 radio luminosity from an observing
frequency of 1.4GHz (2)
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Note (1): black hole mass derived from the velocity dispersion using the
McConnell & Ma (2013ApJ...764..184M 2013ApJ...764..184M) relationship (see text).
Note (2): If the radio flux density is under 0.32mJy (2x the FIRST survey rms),
the luminosity is shown as a limit corresponding to a flux density of 0.32mJy.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jul-2016