J/ApJ/813/77 Galaxy clusters: radio halos, relics and parameters (Yuan+, 2015)
The scaling relations and the fundamental plane for radio halos and relics
of galaxy clusters.
Yuan Z.S., Han J.L., Wen Z.L.
<Astrophys. J., 813, 77 (2015)>
=2015ApJ...813...77Y 2015ApJ...813...77Y (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radio sources
Keywords: galaxies: clusters: general - galaxies: clusters: intracluster medium
Abstract:
Diffuse radio emission in galaxy clusters is known to be related to
cluster mass and cluster dynamical state. We collect the observed
fluxes of radio halos, relics, and mini-halos for a sample of galaxy
clusters from the literature, and calculate their radio powers. We
then obtain the values of cluster mass or mass proxies from previous
observations, and also obtain the various dynamical parameters of
these galaxy clusters from optical and X-ray data. The radio powers of
relics, halos, and mini-halos are correlated with the cluster masses
or mass proxies, as found by previous authors, while the correlations
concerning giant radio halos are in general the strongest. We found
that the inclusion of dynamical parameters as the third dimension can
significantly reduce the data scatter for the scaling relations,
especially for radio halos. We therefore conclude that the
substructures in X-ray images of galaxy clusters and the irregular
distributions of optical brightness of member galaxies can be used to
quantitatively characterize the shock waves and turbulence in the
intracluster medium responsible for re-accelerating particles to
generate the observed diffuse radio emission. The power of radio halos
and relics is correlated with cluster mass proxies and dynamical
parameters in the form of a fundamental plane.
Description:
A large number of radio halos, relics, and mini-halos have been
discovered and measured in recent decades through observations with
VLA (e.g., Giovannini & Feretti 2000NewA....5..335G 2000NewA....5..335G; van Weeren et al.
2011A&A...533A..35V 2011A&A...533A..35V), GMRT (e.g., Venturi et al. 2007A&A...463..937V 2007A&A...463..937V;
Kale et al. 2015A&A...579A..92K 2015A&A...579A..92K), WSRT (e.g., van Weeren et al.
2010Sci...330..347V 2010Sci...330..347V; Trasatti et al. 2015A&A...575A..45T 2015A&A...575A..45T), and also
ATCA (e.g., Shimwell et al. 2014MNRAS.440.2901S 2014MNRAS.440.2901S, 2015MNRAS.449.1486S 2015MNRAS.449.1486S).
We have checked the radio images of radio halos, relics, and
mini-halos in the literature and collected in Table 1 the radio flux
Sν at frequencies within a few per cent around 1.4 GHz, 610 MHz, and
325 MHz; we have interpolated the flux at an intermediate frequency if
measurements are available at higher and lower frequencies. To
establish reliable scaling relations, we include only the very firm
detection of diffuse radio emission in galaxy clusters, and omit
questionable detections or flux estimates due to problematic
point-source subtraction.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 129 101 Radio Flux and Power for Radio Halos, Relics,
and Mini-halos from 75 Galaxy Clusters
table2.dat 127 75 Masses, Mass Proxies, and Dynamical Parameters
for 75 Galaxy Clusters
refs.dat 117 58 References
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See also:
J/MNRAS/281/799 : XBACs, the sample (Ebeling+, 1996)
J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
J/ApJ/519/533 : ROSAT observations of ACO clusters (David+, 1999)
J/ApJS/129/435 : NORAS galaxy cluster survey. I. (Bohringer+, 2000)
J/ApJ/580/774 : X-ray cluster of galaxies behind the Milky way
(Ebeling+, 2002)
J/A+A/423/449 : RASS-SDSS Galaxy Clusters Survey. I. (Popesso+, 2004)
J/A+A/425/367 : REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)
J/ApJ/662/224 : Second CIZA subsample (Kocevski+, 2007)
J/A+A/534/A109 : MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)
J/ApJS/199/34 : Clusters of galaxies in SDSS-III (Wen+, 2012)
J/A+A/551/A24 : GMRT Radio Halo Cluster Survey diffuse sources
(Venturi+, 2013)
J/MNRAS/436/275 : Relaxation parameter of 2092 rich galaxy clusters
(Wen+, 2013)
J/ApJ/807/178 : Newly rich galaxy clusters identified in SDSS-DR12
(Wen+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- Name Cluster name
21- 26 F6.4 --- z Redshift
28- 39 A12 --- Type Type of diffuse radio emission (1)
41- 44 F4.1 arcmin Size Angular size
46- 51 F6.1 mJy S1.4GHz ?=- Flux of halo/relic/mini-halo at 1.4 GHz
53- 57 F5.1 mJy e_S1.4GHz ? Uncertainty in S1.4GHz
58 A1 --- n_S1.4GHz [abc] Note on S1.4GHz (2)
60- 65 F6.1 mJy S610MHz ?=- Flux of halo/relic/mini-halo at 610 MHz
67- 72 F6.2 mJy e_S610MHz ? Uncertainty in S610MHz
73 A1 --- n_S610MHz [c] Note on S610MHz (2)
75- 80 F6.1 mJy S325MHz ?=- Flux of halo/relic/mini-halo at 325 MHz
82- 86 F5.1 mJy e_S325MHz ? Uncertainty in S325MHz
87 A1 --- n_S325MHz [c] Note on S325MHz (2)
89- 96 A8 --- Ref Reference(s) number(s) of these radio
fluxes (see refs.dat file)
98-102 F5.2 [10+24W/Hz] logP1.4 ?=- Log of radio power at 1.4 GHz after
the k-correction
104-107 F4.2 [10+24W/Hz] e_logP1.4 ? Uncertainty in logP1.4
109-113 F5.2 [10+24W/Hz] logP610 ?=- Log of radio power at 610 MHz after
the k-correction
115-118 F4.2 [10+24W/Hz] e_logP610 ? Uncertainty in logP610
120-124 F5.2 [10+24W/Hz] logP325 ?=- Log of radio power at 325 MHz after
the k-correction
126-129 F4.2 [10+24W/Hz] e_logP325 ? Uncertainty in logP325
--------------------------------------------------------------------------------
Note (1): Known "radio Phoenix" looks like it is from a radio galaxy and is not
included in this table.
Note (2): Note as follows:
a = Calculated from fluxes of whole emission region minus relic region;
b = Estimated from flux at a nearby frequency;
c = Uncertainty assumed to be 15%.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Cluster name
18- 22 F5.2 [10+37W] logLX ?=- Log of total X-ray luminosity used as
mass proxy of cluster (in 1044 erg/s)
24- 27 F4.2 [10+37W] e_logLX ? Uncertainty in logLX
28 A1 --- n_logLX [*] Note on logLX (1)
30- 34 F5.2 [10+37W] logL500 ?=- Log of X-ray luminosity within R500
used as mass proxy of cluster
(in 1044 erg/s)
36- 39 F4.2 [10+37W] e_logL500 ? Uncertainty in logL500
41- 44 F4.2 [10+14Msun] logMSZ ?=- Log of cluster mass estimated from
the Sunyaev-Zel'dovich (SZ) effect
46- 49 F4.2 [10+14Msun] e_logMSZ ?=- Uncertainty in logMSZ
51- 54 F4.2 [10+14Msun] logM500 ?=- Log of cluster mass within R500
56- 59 F4.2 [10+14Msun] e_logM500 ? Uncertainty in logM500
61- 71 A11 --- Ref References of mass proxies or mass (2)
73- 77 F5.2 --- Gamma ?=- Optical dynamical parameter
79- 82 F4.2 --- e_Gamma ? Uncertainty in Gamma
84- 88 F5.2 --- logc ?=- Log of X-ray dynamical parameter
90- 93 F4.2 --- e_logc ? Uncertainty in logc
95- 99 F5.2 kpc logomega ?=- Log of centroid shift (in 500 kpc)
101-104 F4.2 kpc e_logomega ? Uncertainty in logomega
106-110 F5.2 kpc logP3/P0 ?=- Log of power ratio (in 500 kpc)
112-115 F4.2 kpc e_logP3/P0 ? Uncertainty in logP3/P0
117-127 A11 --- Ref1 References for dynamical parameters
(2)(3)
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Note (1): Note as follows:
* = For mass proxy is not available from the reference, and 30% of the total
luminosity is taken here
Note (2): Reference as follows:
0 = This paper by the authors;
1 = Ebeling et al. (1998, J/MNRAS/301/881);
2 = Piffaretti et al. (2011, J/A+A/534/A109);
3 = Planck Collaboration et al. (2016, Cat. J/A+A/594/A27);
4 = Bohringer et al. (2004, J/A+A/425/367);
5 = Cassano et al. (2013ApJ...777..141C 2013ApJ...777..141C);
6 = Wen & Han (2015, J/ApJ/807/178);
7 = Zhao et al. (2015ApJ...799...47Z 2015ApJ...799...47Z);
8 = Bohringer et al. (2000, J/ApJS/129/435);
9 = Popesso et al. (2004, J/A+A/423/449);
10 = van Weeren et al. (2011A&A...533A..35V 2011A&A...533A..35V);
11 = David et al. (1999, J/ApJ/519/533);
12 = Ebeling et al. (1996, J/MNRAS/281/799);
13 = Reiprich & Bohringer (2002ApJ...567..716R 2002ApJ...567..716R);
14 = Mantz et al. (2010MNRAS.406.1773M 2010MNRAS.406.1773M);
15 = Feretti et al. (2012A&ARv..20...54F 2012A&ARv..20...54F);
16 = Ebeling et al. (2002, J/ApJ/580/774);
17 = Kocevski et al. (2007, J/ApJ/662/224);
18 = Ebeling et al. (2007ApJ...661L..33E 2007ApJ...661L..33E);
19 = Brown et al. (2011ApJ...727L..25B 2011ApJ...727L..25B);
20 = Bonafede et al. (2014MNRAS.444L..44B 2014MNRAS.444L..44B);
21 = Menanteau et al. (2012ApJ...748....7M 2012ApJ...748....7M);
22 = Bonafede et al. (2012MNRAS.426...40B 2012MNRAS.426...40B);
23 = Bonafede et al. (2012MNRAS.426...40B 2012MNRAS.426...40B);
24 = Bonafede et al. (2009A&A...494..429B 2009A&A...494..429B);
25 = de Gasperin et al. (2014MNRAS.444.3130D 2014MNRAS.444.3130D);
26 = Ebeling et al. (2010MNRAS.407...83E 2010MNRAS.407...83E);
27 = Voges et al. (1999A&A...349..389V 1999A&A...349..389V);
28 = Wen & Han (2013, J/MNRAS/436/275);
29 = Cassano et al. (2010ApJ...721L..82C 2010ApJ...721L..82C).
Note (3): Clusters hosting both radio halo and relic are not listed twice.
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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 [0/57] Reference number
4- 24 A21 --- Aut Author's name(s)
28- 46 A19 --- Bibcode Reference bibcode
50-117 A68 --- Com Comment on reference
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History:
From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 09-Oct-2017