2015MNRAS.453.1990Y

Query : 2015MNRAS.453.1990Y

2015MNRAS.453.1990Y - Mon. Not. R. Astron. Soc., 453, 1990-1998 (2015/October-3)

Optical inverse-Compton emission from clusters of galaxies.

YAMAZAKI R. and LOEB A.

Abstract (from CDS):

Shocks around clusters of galaxies accelerate electrons which upscatter the cosmic microwave background photons to higher energies. We use an analytical model to calculate this inverse-Compton (IC) emission, taking into account the effects of additional energy losses via synchrotron and Coulomb scattering. We find that the surface brightness of the optical IC emission increases with redshift and halo mass. The IC emission surface brightness, 32-34 mag/arcsec2, for massive clusters is potentially detectable by the newly developed Dragonfly Telephoto Array.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): acceleration of particles - radiation mechanisms: non-thermal - galaxies: clusters: general - intergalactic medium

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 ACO 2744 ClG 00 14 20.03 -30 23 17.8           ~ 812 0
2 NAME XMMU J0044.0-2033 ClG 00 44 05.20 -20 33 59.7           ~ 37 0
3 ACT-CL J0102-4915 ClG 01 02 52.50 -49 14 58.0           ~ 229 0
4 XLSSU J021744.1-034536 ClG 02 17 44 -03 45.6           ~ 12 0
5 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2257 1
6 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 963 1
7 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 454 0
8 MCS J1206.2-0847 ClG 12 06 12.2 -08 48 02           ~ 246 0
9 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 4798 2
10 IDCS J1426.5+3508 ClG 14 26.5 +35 08           ~ 55 0
11 ACT-CL J2106.0-5844 ClG 21 06 04.3 -58 44 32           ~ 90 0
12 ACO 2390 ClG 21 53 37.4 +17 41 46           ~ 688 2
13 ACT-CL J2337.4-5942 ClG 23 37 24.2 -59 42 17           ~ 45 0
14 ACT-CL J2344.7-4243 ClG 23 44 43.9 -42 43 11           ~ 189 0

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