ìQ[ËĨ/ĢĔÀ|*1ĩY´ĉĉĉ!

ation measures of radio sources in hot galaxy clustersĉĉ
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Reference

3.64 × 1020
8.54 × 1019
2.49 × 1020
8.33 × 1020
4.79 × 1020
3.51 × 1020
5.96 × 1021
3.99 × 1020
9.88 × 1020
3.78 × 1020
3.04 × 1020
1.93 × 1021

0.6
0.654
0.797
0.534
0.640
0.675
0.601
0.9
0.613
0.591
1.162
0.747

417
245438110
261362226
373
177
114
507
199

0.5
3.5
2.1
2.4
2.8
1.8
2.1
1.2
7.0
18.7
2.3
8.0

0.15
0.44
0.48
0.14
0.40
0.39
0.27
0.17
0.60
0.86
0.39
0.53

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3, 82, 82, 84, 85, 8
6, 94, 84, 84, 82, 8V]

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8Feretti et al.

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28 25

kťÀ|*ĪÀ|*'3ĩ¡Ĩıĳ\ÁĚģčĴĥďĲĵģĐĳĊ¡ĩÅIntraCluster!Medium(ICM)Ĥĩ ĩĒ)ęĵģčĴċRyu!et!al.!(2008)ĨıĴLarge!Scale!
6Structure!(LSS)Q\ŀŏœŗśŀŔŚĨĐčģ ĨıĴ1ĩ
angular to linear conversion; Col. 4: cluster temperature; Col. 5: galactic absorption taken
ctic HI (Kalberla et al. 2005); Cols. 6, 7: β-model parameters (β and core radius); Col. 8:2KĒęĵĝėĥđĲĊÀ|*ĩ¼ĥ1ĩ\ÁĨĪby integrating the
β-model profile over a sphere of 1 Mpc in radius; Col. 10: temperature
Fukazawa et al. (1998); 3 White (2000); 4 Markevitch (1998); 5 Edge & Stewart (1991);
ĲđĩÃĒČĴĥďĲĵĴċ!
al. (2007); 9 Guidetti
et al. (2008).
ťÀ|*ĪXĨıĳIrregularĊRegularĊCool>CoreĩšQ
HťComa!ClusterĤªęĵĝŀŚļŘņŘŚ`DċÀ|*1ĩ=,Ē)ęĵĴŜFereP!!et!al.!2012ŝċ9ťMHDŀŏœŗśFig. S2. Left panel: Time evolution of kinetic and magnetic energies in a three-dimensional,ŀŔŚĨıĴ ĩ½ĹŉŖĻśĥ1ĩĹŉŖĻśĩjÂ¼ċ$ť1P
incompressible simulation of driven MHD turbulencewith very
weak initial magnetic field.
Bĥ»PVĩŊřśŁōļņŖŜRyu!et!al.!2008ŝċ!
The green lines show our fitting for the growth and saturation of magnetic energy. Right panel:Distance [ĨËĤēĴċXĨıĴQ[ËĪÀ|*ĩ¼[ķσS [0.1−2.4] keV
Reference
Power spectra for flow velocity, P , and magnetic fields, P , at a time of saturation. Two[kpc][rad/m ]10 [erg/s cm sterad]presented 7 new candidates from a search in the Westerbork
Sky Survey
straightNorthernlines of slopes−5/3 and −1 are also drawn for comparison.
(WENSS[219])
at
327
MHz;
Rudnick&Lemmerman[226]
searchedfor
Mpc-scale
232 "iĚģčĴ#63
5.75 ± 0.13
1YĒČĳĊ%Q[ĘĥĨ1ĩY´Ĩ¾č
radio emission reprocessing WENSS radio images.
ŠŞXQ[Ë!
50947
1.56 ± 0.03
1XQ[ËĪÀ|*ĩ¼[ķ¢ĚģčĴŦ!
Recently, other extensive radio observations have been published. We note the1556 Ē§ĲĵĴėĥĒmSęĵĴċn±ĤĪXQ[ËĘĥĩ48<1.79
1Giant Metrewave Radio Telescope (GMRT) survey of massive galaxy clusters at z
1654
47
<1.79
1= 0.2 - 0.4 by Venturi and collaborators [265,266], who found diﬀuse sources in 10clusters (out of which 3 new halos, 2 new core-halo sources and 3 new halo or relic
1822
24
<1.79
1
À|*ĩ1ONķx¸ěĴċ!
candidates), the GMRT follow up at low frequencies of all clusters known to contain
51
303
86.74 ± 0.48
2
radio halos and relics up to z = 0.4 200!
[114], and the observing campaign carried out with100!
260!
69124
166
65.22 ± 0.26
2kpc
the WSRT, VLA and GMRT by Van
Weeren et al. [255], who discovery 6 new radiokpckpc
e}ťVLA!archiveĥdĝĨªęĵĝEVLAĩ~ŅśłđĲĉ
relics,including
aprobable
doublesystem,and2radio
halos.
Theabovementioned
372
154
16.37 ± 0.08
2
studies and their follow-ups have produced rich information in a short time in this532
16
6.76 ± 0.05
2field.
9919 XQ[ËĘĥĨÀ|*ĩRotaDon!Measure!(RM)ķzįĴċ
65
0.70 ± 0.01
21250
56–
2
4 Radio halos
1489 zįĝRMĩađĲ1ONķzįĴċ!
37–
2279
79
15.78 ± 0.22
3Radio halos are diﬀuse radio sources of low surface brightness (∼ 1 – 0.1 µJy arcsec
44459
7.86 ± 0.113
at 1.4 GHz) permeating the central volume of a cluster. They are typically extendedpťÀ|*Abell!401AŜAbellĪAĥěŝĊA401BĊA2142Ċ
with sizes of ! 1 Mpc, regular in morphology, and are unpolarized down to a few
1497
420.33 ± 0.01
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40 A2199ĊA2256ĩRM!mapķ\ĚĝċUĲĵĝRMĩađĲĊ120
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4! Irregular(and(Regular(→!X¢È¹NJĩCYĤËŜe.g.,!Akahori!&!Masai!2005ŝ!
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124
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720
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50
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00
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58 30

00

Fig. 2 Diﬀuse radio halo Coma C in the Coma cluster (z = 0.023) at 0.3 GHz obtained with the WSRT,superimposed onto the optical image from the Digitized Sky Survey DSS1. The resolution of the radio
image is 55′′ × 125′′ (FWHM, RA × DEC); contour levels are: 3, 6, 12, 25, 50, 100 mJy/beam.

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