Table 5:

Bolometric luminosities, black hole masses, and Eddington ratios.

Source		Ref.		Ref.
	( )		()
(1)	(2)	(3)	(4)	(5)	(6)
4C12.03	<42.0	6	8.5	9	<-4.6
3C 015	<42.8	1	8.8	4	<-4.1
3C 029	42.3	3	9.1	3	-4.9
3C 040	<41.5	3	7.9	2	<-4.5
3C 078	43.5	3	8.9	3	-3.5
Fornax A	<41.1	5	8.4	1	<-5.4
3C 093	45.3	3	9.5	6	-2.3
3C 098	<41.5	1	7.9	8	<-4.5
3C 105	43.6	5	7.8	10	-2.3
3C 120	45.3	4	7.4	8	-0.2
3C 135	43.2	1	8.5	7	-3.4
Pictor A	44.3	3	8.7	6	-2.5
3C 198	43.9	1	8.1	4	-2.3
3C 227	44.9	3	8.9	6	-2.1
3C 270	40.4	3	8.6	3	-6.3
Centaurus A	41.1	2	7.7	5	-4.7
PKS1417-19	45.3	3	8.3	6	-1.1
3C 317	42.4	3	9.5	3	-5.2
3C 327	<42.4	1	9.1	4	<-4.8
3C 353	<41.4	1	7.6	4	<-4.3
PKS1839-48	44.5	5	8.7	10	-2.3
3C 403	42.5	1	8.5	4	-4.1
3C 403.1	<42.0	6	8.1	10	<-4.2
3C 424	<42.6	5	7.8	7	<-3.3
PKS2158-380	<42.0	6	8.6	2	<-4.7
3C 445	44.8	3	8.0	6	-1.3
PKS2354-35	<42.0	7	9.2	10	<-5.3

Notes. Columns (2, 3) Logarithm of bolometric luminosity from: 1 = Marchesini et al. (2004), 2 = Meisenheimer et al. (2007), 3 = Sikora et al. (2007), 4 = Woo & Urry (2002), 5 = calculated from bolometric correction (Marchesini et al. 2004; Elvis et al. 1994) to optical nuclear luminosity (Tadhunter et al. 1993; Balmaverde & Capetti 2006), 6 = upper limit from spectral energy distribution fit in Fig. 4 and 5. Columns (4, 5) Logarithm of black hole mass from: 1 = Balmaverde & Capetti (2006), 2 = Bettoni et al. (2003), 3 = Cao & Rawlings (2004), 4 = Marchesini et al. (2004), 5 = Neumayer et al. (2007), 6 = Sikora et al. (2007), 7 = Woo et al. (2005), 8 = Woo & Urry (2002), 9 = calculated from the velocity dispersion (Wold et al. 2007) using the correlation from Tremaine et al. (2002), 10 = calculated from B- or V-band absolute magnitudes (Zirbel & Baum 1995; Wall & Peacock 1985) following the work of Marchesini et al. (2004). Column (6) Efficiency expressed in the logarithm of the bolometric to Eddington luminosity ratio.