Low-frequency radio observations of Seyfert galaxies: A test of the unification scheme

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Table 6

Comparison of radio luminosities and spectral indices of Seyfert types 1s and 2s.

Distribution	Statistical parameters								KS test		F.D. Ref.
	Seyfert type 1s				Seyfert type 2s


	min	max	SD	median	min	max	SD	median	D	p-value

logL_240 MHz	28.78	30.90	0.66	30.31	28.87	31.22	0.73	30.18	0.2	0.99	1
logL_610 MHz	28.66	30.62	0.61	29.90	28.92	30.86	0.58	29.83	0.2	0.99	1
logL_1.4 GHz	28.54	30.35	0.55	29.62	28.70	30.64	0.55	29.64	0.3	0.79	2
logL_5.0 GHz	28.10	29.92	0.57	29.19	28.51	30.62	0.63	29.35	0.3	0.79	3
	−1.26	−0.15	0.36	−0.83	−1.13	+0.66	0.50	−0.52	0.3	0.79	1
	−0.94	+0.27	0.31	−0.59	−0.77	−0.07	0.20	−0.59	0.3	0.79	1, 2
	−1.13	−0.49	0.16	−0.77	−1.38	+0.79	0.57	−0.67	0.4	0.42	2, 3
α _Int.	0.88	−0.47	0.12	−0.74	−0.79	−0.14	0.20	−0.72	0.38	0.51	1, 2, 3

Notes.Flux density (F.D.) references: (1) our GMRT observations; (2) NRAO VLA Sky Survey (NVSS); (3) Literature (Gallimore et al. 2006; Edelson 1987; Gregory & Condon 1991; Griffith et al. 1995). The adopted conservative error values of 15%, 10%, 7%, and 7% for S_240 MHz, S_610 MHz, S_1.4 GHz, and S_5.0 GHz, respectively, render ~8%, ~5%, ~4%, and ~7% errors in , , , and α_int, respectively. Radio luminosities are in units of ergs s^-1 Hz^-1. Kolmogorov−Smirnov (KS) two-sample test examines the hypothesis that two samples comes from same distribution. D = Sup x |S1(x) − S2(x)| is the maximum difference between the cumulative distributions of two samples S1(x) and S2(x), respectively.

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