Notes. Columns are: (1) QSO name; (2) and (3) position in J2000 coordinates; (4) redshift derived from rest-frame UV lines (references listed below); (5) redshift derived from line center of the intermediate width (ILR) Gaussian component of the double Gaussian fit to the Hα profile. The typical error is about 0.0015 (see below); (6) and (7) observed velengths of the line centers of the intermediate width (ILR) and very broad (VBLR) Gaussian components fitted to the Hα line, respectively; typical errors are 10 Å and 20 Å for the intermediate width and very broad Gaussian components, respectively; (8) and (9) fluxes of the intermediate width and very broad Gaussian components fitted to the Hα line, respectively; (10) and (11) FWHM of the intermediate width and very broad Gaussian components fitted to the Hα line, respectively; (12) FWHM of the single Lorentzian component fitted to the Hα line; (13) FWHM of the Hα line as measured from the summed (ILR+VBLR) double Gaussian fit to the Hα line, and used for the black hole mass estimation; (14) continuum flux near 6000 Å, with a K-correction of (1 + z) applied.Wavelengths reported are vacuum wavelengths. The continuum fluxes are in units of erg s^-1 cm^-2 Å^-1, and have been K-corrected by factor (1 + z). Hα line fluxes are in units erg s^-1 cm^-2. Errors in fluxes are 10−20% (see text). An asterisk after the QSO name indicates a 850 μm detection (Priddey et al. 2003b). A double asterisk after the QSO name indicates that the object is detected at 1.2 mm (Omont et al. 2003) but not detected at 850 μm (Priddey et al. 2003b). The first two QSOs in the table were observed in September 2002 with the HK grism and the other QSOs in March 2002 with the Kb grism. Rest-frame UV redshifts are from Hewett et al. (1995; LBQS B0018-0220), Hewitt & Burbidge (1989; [HB89] 0933+733), Stepanian et al. (2001; SBS B1408+567), SDSS (SBS B1542+541, HS B1049+4033 and HS B1103+6416), and from the Hamburg Bright Quasar Survey (remaining four QSOs; Hagen et al. 1999; Engels et al. 1998).