The properties of non-thermal X-ray filaments in young supernova remnants

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Table 2

Constraints on the downstream magnetic-field strength, cut-off energy of the electron spectrum, photon spectral index of the filament, and the difference between the photon indices of the spectra of filament and plateau at three different photon energies, E_ν, for four young SNRs.

SNR	B	E _cut	Γ_f			Γ_p−Γ_f

	[μG]	[TeV]	E_ν = 0.1 keV	E_ν = 1 keV	E_ν = 10 keV	E_ν = 0.1 keV	E_ν = 1 keV	E_ν = 10 keV

SN 1006^a	130	36	1.81	2.33	2.71	0.31	0.07	0.02
	(110)	(23)	(1.99)	(2.49)	(2.94)	(0.25)	(0.05)	(0.01)
Cas A	520	19	1.83	2.33	2.70	0.31	0.06	0.01
Tycho	310	24	1.82	2.33	2.71	0.32	0.06	0.01
Kepler^b	250	26	1.81	2.32	2.70	0.31	0.07	0.01
	(230)	(37)	(1.75)	(2.23)	(2.61)	(0.34)	(0.08)	(0.02)

Notes. These values are calculated using the energy-loss model and the parameters given in Table 1.

^(a)

The values in brackets were calculated using the shock velocity v_s = 2900 km s^-1 as measured in the northwestern limb.

^(b)

The values in brackets were calculated using the upper limit of 6.4 kpc to the distance.

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