J/MNRAS/453/1201 Radio properties of brightest cluster galaxies (Hogan+, 2015)
A comprehensive study of the radio properties of brightest cluster galaxies.
Hogan M.T., Edge A.C., Hlavacek-Larrondo J., Grainge K.J.B., Hamer S.L.,
Mahony E.K., Russell H.R., Fabian A.C., McNamara B.R., Wilman R.J.
<Mon. Not. R. Astron. Soc., 453, 1201-1222 (2015)>
=2015MNRAS.453.1201H 2015MNRAS.453.1201H (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, radio
Keywords: galaxies: clusters: general - galaxies: jets -
radio continuum: galaxies
Abstract:
We examine the radio properties of the brightest cluster galaxies
(BCGs) in a large sample of X-ray selected galaxy clusters comprising
the Brightest Cluster Sample (BCS), the extended BCS and ROSAT-ESO
Flux Limited X-ray cluster catalogues. We have multifrequency radio
observations of the BCG using a variety of data from the Australia
Telescope Compact Array, Jansky Very Large Array and Very Long
Baseline Array telescopes. The radio spectral energy distributions of
these objects are decomposed into a component attributed to on-going
accretion by the active galactic nuclei (AGN) that we refer to as 'the
core', and a more diffuse, ageing component we refer to as the
'non-core'. These BCGs are matched to previous studies to determine
whether they exhibit emission lines (principally Hα), indicative
of the presence of a strong cooling cluster core. We consider how the
radio properties of the BCGs vary with cluster environmental factors.
Line emitting BCGs are shown to generally host more powerful radio
sources, exhibiting the presence of a strong, distinguishable core
component in about 60 per cent of cases. This core component more
strongly correlates with the BCG's [OIII] 5007Å line emission. For
BCGs in line emitting clusters, the X-ray cavity power correlates with
both the extended and core radio emission, suggestive of steady
fuelling of the AGN over bubble-rise time-scales in these clusters.
Description:
Our parent sample is drawn from three ROSAT X-ray selected cluster
catalogues - the Brightest Cluster Sample (BCS; Ebeling et al.,
1998, Cat. J/MNRAS/301/881), the extended BCS (eBCS; Ebeling et al.,
2000, Cat. J/MNRAS/318/333) and ROSAT-ESO Flux Limited X-ray (REFLEX;
Bohringer et al., 2004, Cat. J/A+A/425/367) samples, which contain
206, 107 and 447 clusters, respectively. Since publication some
catalogue entries have been reclassified, and there are also a small
number of cross-catalogue duplicates. We therefore remove a minority
of sources, leaving us with a sample of 199, 104 and 417 sources in
the BCS, eBCS and REFLEX samples, respectively. Our total X-ray
selected parent sample therefore consists of 720 clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 160 263 Recovered C-band fluxes
tableb2.dat 160 15 L band fluxes
tableb3.dat 160 81 X band fluxes
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See also:
J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000)
J/A+A/425/367 : REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)
J/MNRAS/453/1223 : BCG high radio-frequency properties (Hogan+, 2015)
Byte-by-byte Description of file: tableb[123].dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Array Array (VLA-A, VLA-C or ATCA-6A)
9- 13 A5 --- PropID Proposal ID
15 A1 --- --- [:]
17- 20 I4 yr Year Year
22 A1 --- --- [:]
24- 59 A36 --- Inst Bandwhith, Core limit, or Upper limits
60- 77 A18 --- Cluster Cluster name
79-103 A25 --- BCG BCG name
105-106 I2 h RAh Right ascension (J2000)
108-109 I2 min RAm Right ascension (J2000)
111-116 F6.3 s RAs Right ascension (J2000)
118 A1 --- DE- Declination sign (J2000)
119-120 I2 deg DEd Declination (J2000)
122-123 I2 arcmin DEm Declination (J2000)
125-129 F5.2 arcsec DEs Declination (J2000)
131 A1 --- l_Fcore Limit flag on Fcore
132-137 F6.2 mJy Fcore Core flux (1)
139 A1 --- l_Ftot Limit flag on Ftot
140-146 F7.2 mJy Ftot Total flux
148-151 F4.2 --- rms RMS
153-158 F6.4 --- z Redshift (2)
160 A1 --- Lines? [YNx] Presence of optical emission lines (3)
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Note (1): peak of the emission if unresolved or the peak of the core component
for resolved sources.
Note (2): Redshifts are from Crawford et al. (1999, Cat. J/MNRAS/306/857)
unless otherwise stated.
Note (3): Flag for presence of lines as follows:
Y = yes
N = no
x = unknown
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 16-Feb-2016