Probing particle acceleration in Abell 2256: From 16 MHz to gamma rays

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Table 2.

Flux density measurements and best-fit synchrotron model parameters of the AGN-related sources in Abell 2256.

Source	S_144 MHz	S_46 MHz	S_23 MHz	Model	α_inj^(a)	Break frequency ^(a)	Remnant fraction ^(a)	Age ^(b)
	[Jy]	[Jy]	[Jy]			[MHz]		[Myr]
AG+AH	0.13 ± 0.01	0.47 ± 0.05	0.64 ± 0.08	KGJP	−0.55 ± 0.02	113 ± 12	0.57 ± 0.05	197 ± 10
AI	0.04 ± 0.01	0.15 ± 0.02	0.38 ± 0.06	KGJP	−0.91 ± 0.02	242 ± 82	0.33 ± 0.04	135 ± 30
F1	0.05 ± 0.01	0.26 ± 0.03	0.64 ± 0.07	CI ^(c)	−0.86 ± 0.02	< 23	–	> 437
F2	0.69 ± 0.07	1.96 ± 0.20	2.62 ± 0.26	KGJP	−0.53 ± 0.01	129 ± 22	0.24 ± 0.05	185 ± 15
F3	0.36 ± 0.04	1.06 ± 0.11	1.97 ± 0.20	KGJP	−0.66 ± 0.02	145 ± 24	0.25 ± 0.05	174 ± 14
F4	0.06 ± 0.01	0.56 ± 0.06	1.91 ± 0.19	CI ^(c)	−1.4 ± 0.1	< 23	–	> 437

Notes.

^(a)

The error bars only reflect the statistical uncertainties from the fit.

^(b)

For the age estimate, a conservative magnetic field value of 7 μG was assumed, following Brentjens (2008). For a lower magnetic field strength, the age would increase.

^(c)

F1 and F4 are consistent with a simple power-law spectrum without a break frequency observed.

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