tokens: The results we obtain span 7 10 7 2 10 9 M . 3.3 X-ray luminosities and Eddington fractions We returned to the Swift XRT X-ray spectra we presented in S11 in light of the new redshift measurements, and fitted each spectrum with an absorbed power-law model in xspec , making use of the most up-to-date Galactic column densities (Willingale etal. 2013 ) and adopting Cash statistics. Swift XRT observations additional to our fill-in programme were available for one source, XMMSL1J002202.9254004. We included these in a combined X-ray spectrum totalling 12ks of exposure, created using the method of Evans etal. ( 2009 ) and after establishing no significant changes in spectral hardness had occurred. From the XRT best fits, we obtained the observed 210keV X-ray luminosities of our AGN. We estimated the Eddington luminosities, L Edd , using our mass estimates in the equation ergs 1 . To obtain the Eddington ratio, the bolometric luminosity is required. Our measured X-ray luminosities significantly underestimate the total output, by an approximate factor of 10 (Elvis etal. 1994 ). Marconi etal. ( 2004 ) derived a bolometric correction to convert from 210keV X-ray luminosity to L Bol (their equation 21), which we adopt here. The resulting bolometric luminosities and Eddington ratios are listed in Table 4 . Table 4. Estimates of black hole mass and Eddington ratio. Optical photometry from USNOB1.0 ( R , I ) or NOMAD ( V ) is given for the observed band closest to rest frame 5100 . Black hole mass estimates use the virial method described in Shen etal. ( 2011 ) and Vestergaard Peterson ( 2006 ) (H linewidth taken from SDSS for this source). Bolometric luminosity estimates, L Bol , use the corrections given in equation 21 of Marconi etal. ( 2004 ). Most of these AGN have X-ray luminosities that imply a bolometric luminosity around a tenth of a per cent Eddington (mean value 0.2). The spread is large, however; our least luminous AGN, XMMSL1J131651.2084915 with L 210keV 510 42 ergs 1 , is emitting at a few hundredths of the Eddington rate, whilst our most distant source, XMMSL1J095336.4161231 at z 0.873, may be emitting at or close to the Eddington rate. 3.4 -ray and radio searches At the hard X-ray/-ray energies of 15150keV, none of our sources are detected in the Swift BAT transient monitoring programme spanning 20052016 May (Krimm, private communication). This supersedes the low-significance detections we tentatively reported in S11 . All of our sources, listed in Table 1 , have coverage in either the NRAO VLA Sky Survey (Condon etal. 1998 ) or Sydney University Molonglo Sky Survey (Mauch etal. 2003 ), three are also covered by the VLA Faint Images of the Radio Sky at Twenty centimeters survey (White etal. 1997 ) and one by the Westerbork Northern Sky Survey (WENSS; Rengelink etal. 1997 ). A search in radio catalogues at these positions results in no spatially coincident radio sources (within 30arcsec radius). However, XMMSL1J164859.4800507 (for which
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