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Table 6

Signal-to-noise results for halo.

ASTRO-H 100 ks 500 ks 1 Ms
Cluster sr ν r F 20−80 keVa F 20−80 keVa F 20−80 keVa
[mJy] [MHz] [μG] [μG] [μG]

Bullet 52 1340 0.84 0.42 1.18 0.18 1.37 0.13
A0520 85 325 0.26 0.40 0.39 0.17 0.46 0.12
A0521 328 153 0.61 0.28 0.83 0.12 0.94 0.08
A0665 197 327 0.25 0.72 0.38 0.31 0.45 0.22
A0697 135 153 0.25 0.85 0.35 0.37 0.40 0.26
A0754 86 1365 0.27 0.97 0.40 0.42 0.48 0.30
A1300 130 325 0.74 0.28 1.02 0.12 1.16 0.08
Coma* 640 1400 0.20 1.88 0.29 0.83 0.34 0.59
** 0.54 0.79 0.93
*** " " 0.25 1.11 0.37 0.49 0.44 0.34
A1758 146 325 0.55 0.38 0.78 0.16 0.90 0.11
A1914 64 1465 1.18 0.53 1.57 0.23 1.77 0.16
A2163* 861 325 0.46 1.08 0.67 0.47 0.79 0.33
** " " 0.51 0.75 0.88
A2219 232 325 0.19 0.66 0.31 0.28 0.38 0.20
A2255 536 330 0.61 0.64 0.84 0.28 0.96 0.20
A2256* 6600 63 0.41 0.87 0.58 0.38 0.68 0.27
* " " 0.48 0.68 0.79
A2319* 1450 408 0.56 1.20 0.77 0.53 0.88 0.37
** " " 0.79 " 1.08 1.23
A2744 218 325 0.32 0.55 0.49 0.23 0.59 0.16
A3562 20 1400 0.26 0.55 0.38 0.24 0.44 0.17
CL0217+70a 326 325 0.33 0.68 0.48 0.29 0.56 0.21
MACSJ0717.5+3745 493 235 0.91 0.37 1.35 0.15 1.58 0.11
MACSJ1752.0+4440a 164 323 0.73 0.34 1.02 0.14 1.17 0.10
PLCK G171.9-40.7a 483 235 0.98 0.26 1.33 0.11 1.52 0.08
RXCJ1514.9-1523a 102 327 0.46 0.44 0.63 0.19 0.73 0.13
RXCJ2003.5-2323a 360 240 0.64 0.35 0.93 0.15 1.09 0.10

Notes. For each halo, we show the radio data values sr and νr used in Eq. (7) to calculate . We show the latter for 100 ks, 500 ks and, 1 Ms of ASTRO-H observations, together with the corresponding flux in the 20−80 keV energy band in units of 10-12 erg cm-2 s-1. Within a few percent error, the fluxes and magnetic fields scale with observation time according to Eq. (9).

(*)

In this case, the source is larger than the HXI FoV of 9 × 9 = 81 arcmin2. In our work, for simplicity, we assumed a uniform surface brightness, therefore, sr was scaled by a factor 81 /x where x arcmin2 is the size that a source covers in the sky (see Tables 1 and 2). This estimate results in slightly conservative predictions since halos and relics are non-uniform sources.

(**)

This gives results that assume all radio emission is coming from an area equal to the HXI FoV, so sr was not scaled. This can be considered an optimistic estimate for the detectable magnetic field.

(***)

Additional analysis for Coma. Since the Coma radio halo is extremely large in the sky, we estimated the thermal ICM emission only in the HXI FoV, integrating Eq. (4) out to ~ 180 kpc, which roughly corresponds to the HXI FoV, rather than over the full halo size.

(a)

Thermal ICM emission computed using the model by Zandanel et al. (2014) for the gas density.

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