J/MNRAS/497/2163 Properties of galaxy group sample (Pasini+, 2020)
The relation between the diffuse X-ray luminosity and the radio power of the
central AGN in galaxy groups.
Pasini T., Bruggen M., de Gasperin F., Borzan L., O'Sullivan E.,
Finoguenov A., Jarvis M., Gitti M., Brighenti F., Whittam I.H.,
Collier J.D., Heywood I., Gozaliasl G.
<Mon. Not. R. Astron. Soc. 497, 2163 (2020)>
=2020MNRAS.497.2163P 2020MNRAS.497.2163P (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radio sources ; X-ray sources
Keywords: galaxies: clusters: general -
galaxies: clusters: intracluster medium - galaxies: groups: general -
radio continuum: galaxies - X-rays: galaxies: clusters
Abstract:
Our understanding of how active galactic nucleus feedback operates in
galaxy clusters has improved in recent years owing to large efforts in
multiwavelength observations and hydrodynamical simulations. However,
it is much less clear how feedback operates in galaxy groups, which
have shallower gravitational potentials. In this work, using very deep
Very Large Array and new MeerKAT observations from the MIGHTEE survey,
we compiled a sample of 247 X-ray selected galaxy groups detected in
the COSMOS field. We have studied the relation between the X-ray
emission of the intra-group medium and the 1.4GHz radio emission of
the central radio galaxy. For comparison, we have also built a control
sample of 142 galaxy clusters using ROSAT and NVSS data. We find that
clusters and groups follow the same correlation between X-ray and
radio emission. Large radio galaxies hosted in the centres of groups
and merging clusters increase the scatter of the distribution. Using
statistical tests and Monte Carlo simulations, we show that the
correlation is not dominated by biases or selection effects. We also
find that galaxy groups are more likely than clusters to host large
radio galaxies, perhaps owing to the lower ambient gas density or a
more efficient accretion mode. In these groups, radiative cooling of
the intra-cluster medium could be less suppressed by active galactic
nucleus heating. We conclude that the feedback processes that operate
in galaxy clusters are also effective in groups.
Description:
The properties of a sample of 247 galaxy groups observed in both radio
(VLA and MeerKAT) and X-ray (XMM-Newton and Chandra) in COSMOS are
reported in the table. The listed properties include X-ray coordinates
of the group, redshift, M200, R200, X-ray luminosity in the 0.1-2.4keV
band, radio coordinates, flux density at 1.4GHz, radio luminosity at
1.4GHz and Largest Linear Size (when resolved). The last column
reports 1 if the radio source was detected with both VLA and MeerKAT,
and 2 if it was detected only by MeerKAT.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 121 173 Properties of the group sample
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See also:
VII/84 : Groups of Galaxies. III. The CfA Survey (Geller+ 1983)
VII/86 : Groups of Galaxies. I. Nearby Groups (Huchra+ 1982)
VII/88 : CEDAG Catalogue of Clusters of Galaxies (Fernandez+ 1984)
VII/89 : Compact groups of compact galaxies (Shakhbazian+ 1973-1979)
VII/196 : Shakhbazian compact groups of galaxies (Stoll+ 1993-97)
VII/213 : Hickson's Compact groups of Galaxies (Hickson+ 1982-1994)
J/A+A/381/420 : Group of Galaxies in the SSRS2 catalog (Adami+, 2002)
J/A+A/391/35 : Compact Groups in the UZC galaxy sample (Focardi+, 2002)
J/A+A/514/A102 : SDSS DR7 groups of galaxies (Tago+, 2010)
J/A+A/565/A25 : Hickson compact groups Herschel observations (Bitsakis+, 2014)
J/A+A/578/A61 : Galaxy groups in the 2M++ (Diaz-Gimenez+, 2015)
J/ApJ/751/50 : Galaxy groups catalog from DEEP2 Redshift Survey (Gerke+ 2012)
J/ApJ/821/113 : HCG and RSCG compact group galaxies with WISE (Zucker+, 2016)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg X-ray right ascension (J2000)
11- 17 F7.5 deg DEdeg X-ray declination (J2000)
19- 23 F5.3 --- z Redshift
25- 29 F5.2 10+13Msun M200 Mass of the cluster within R200
31- 34 F4.2 10+13Msun e_M200 Mass error
36- 42 F7.2 kpc R200 Radius within which the mean density of a
cluster is 200 times of the critical
density of the Universe
44- 50 F7.3 10+35W LX X-ray luminosity (0.1-2.4keV)
in 1042erg/s
52- 57 F6.3 10+35W e_LX X-ray luminosity error in 1042erg/s
59- 60 I2 h RARh Radio right ascension (J2000)
62- 63 I2 min RARm Radio right ascension (J2000)
65- 70 F6.3 s RARs Radio right ascension (J2000)
72 A1 --- DER- Radio declination sign (J2000)
73- 74 I2 deg DERd Radio declination (J2000)
76- 77 I2 arcmin DERm Radio declination (J2000)
79- 83 F5.2 arcsec DERs Radio declination (J2000)
86- 92 F7.3 mJy S1.4GHz 1.4GHz flux density
94- 98 F5.3 mJy e_S1.4GHz Flux density error
100-107 F8.3 10+23W/Hz LR1.4GHz 1.4GHz power in 1030erg/s/Hz
109-112 F4.2 10+23W/Hz e_LR1.4GHz 1.4GHz power error in 1030erg/s/Hz
114-119 F6.2 kpc LLS ? Largest Linear Size
121 I1 --- Det [1/2] Detection flag (1)
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Note (1): Detection flag as follows:
1 = detected by both VLA and MeerKAT
2 = detected only by MeerKAT
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Acknowledgements:
Thomas Pasini, thomas.pasini94(at)gmail.com
(End) Thomas Pasini [Hamburg Univ.], Patricia Vannier [CDS] 18-Aug-2020