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Table 2

Parameters of the sample galaxies.

Name T D σ ⋆ L x L [O III] Ground measurements HST measurements
F(Hαb) FWHM F(Hαn) F(Hαb) L(Hαb) FWHM
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)
NGC 0315 L 65.8 303.7 41.63 39.43 −13.85 2000 −14.95 <−14.05 <39.66 –
NGC 1052 L 17.8 215.0 41.53 40.10 −12.32 1950 −13.43 <−13.72 <38.86 –
NGC 1275 A 70.1 258.9 42.86 41.61 −12.05 2750 −13.01c <−13.21c <40.56c –
NGC 2787 L 13.0 202.0 38.79 38.37 −13.56 2050 −14.26 <−13.47 <38.83 –
NGC 2985 L 22.4 140.8 39.46a 38.69 −13.98 2050 −14.94 <−14.22 <38.56 –
NGC 3031 L 1.4 161.6 39.38 37.72 −11.94 2650 −13.03 −12.08 38.29 4200
NGC 3227 S 20.6 136.0 41.70 40.68 −11.50 2950 −13.10 −11.87 40.83 2934
NGC 3516 S 38.9 181.0 42.39 40.80 −11.54 3850 – −11.48 41.78 4236
NGC 3642 L 27.5 85.00 39.84 38.96 −13.59 1250 −14.52 <−13.35 <39.61 –
NGC 3982 S 17.0 73.0 38.76 39.83 −13.85 2150 −14.10 <−14.62 <37.92 –
NGC 3998 L 21.6 304.6 41.34 39.62 −12.59 2150 −13.05 −12.48 40.27 5200
NGC 4036 L 24.6 215.1 39.96 39.16 −13.70 1850 −14.64 <−14.26 <38.60 –
NGC 4051 S 17.0 89.0 42.07 40.18 −11.77 1000 – −11.91 40.63 760
NGC 4143 L 17.0 204.9 40.03 38.81 −13.39 2100 −13.99 <−13.31 <39.23 –
NGC 4151 S 20.3 97.0 43.07 41.74 −10.95 3250 −12.40c −10.85c 41.84c 4465
NGC 4203 L 9.7 167.0 39.69 38.53 −13.45 1500 −13.96 −12.86 39.19 7200
NGC 4258 S 6.8 148.0 40.89 38.76 −13.09 1700 −13.87 <−13.14 <38.60 –
NGC 4278 L 9.7 261.0 39.64 38.88 −13.09 1950 −14.32 <−14.07 <37.98 –
NGC 4395 S 3.6 30.0 39.58 38.35 −12.88 442 −13.28c −12.85c 38.34c 786
NGC 4450 L 16.8 135.0 40.02 38.78 −13.70 2300 −13.56 −12.83 39.70 7700
NGC 4579 L 16.8 165.0 41.15 39.42 −13.12 2300 −14.52 −13.03 39.50 8000
NGC 4636 L 17.0 202.7 39.38 38.09 −14.16 2450 −16.32 − – –
NGC 5005 L 21.3 172.0 39.94 39.41 −12.69 1650 −14.57 <−14.11 <38.62 –
NGC 5077 L 40.6 254.6 39.74b 39.52 −14.07 2300 −14.40 <−14.96 <38.33 –

Notes. (1) Object name; (2) spectroscopic classification based on the diagnostic diagram of Kewley et al. (2006) (S = Seyfert, L = Liners, A = ambiguous galaxy); (3) distance of the source in Mpc from Ho et al. (1995); (4) stellar velocity dispersion in km s-1 from Ho et al. (2009); (5) logarithm of the un-absorbed nuclear X-ray luminosity in the 2−10 keV range in erg s-1 from Ho (2009); (6) logarithm of the nuclear [OIII] emission line luminosity in erg s-1 from Ho et al. (1997a); (7) logarithm of the flux of the broad Hα line in erg s-1 cm-2 from Palomar measurement; (8) FWHM in km s-1 from the Palomar measurement (Ho et al. 1997a). (9) Logarithm of the flux of the narrow Hα emission line in erg s-1 cm-2 from this work; for the objects marked with (10) Logarithm of the flux of the broad Hα emission line in erg s-1 cm-2; (11) logarithm of the luminosity of the broad Hα emission line in erg s-1; (12) FWHM in km s-1; the upper limit measurement for the flux of broad Hα emission line reported depends on the assumption about the broad emission line profile (we here assume a Gaussian profile with FWHM reported in Table 4).

(a)

we fitted Chandra data Obs.Id 11669 with the model phabs(powerlaw+mekal), obtaining NH = 2.2e20 cm-2 frozen, Γ = 1.8, kT = 1.1 keV, Cstat = 10.68(9 d.o.f.);

(c)

the Hα luminosities and fluxes are derived from the observed Hβ line.

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