Files Summary: table1.dat List of the 180 objects and spectra table3.dat Continuum parameters table4.dat Emission line measurements Byte-by-byte Description of file: table1.dat ------------------------------------------------------------------------------- Bytes Format Units Label Explanations ------------------------------------------------------------------------------- 1- 9 A9 --- Name Object designation (1) 10 A1 f_Name [*] See note (3) 12- 25 A14 --- CName Common name 27- 31 A5 --- Type AGN type (2) 33- 37 F5.3 --- z Redshift 39- 43 F6.2 10+20/cm2 NH Neutral hydrogen column density 45- 55 A11 --- NSpect Spectrum name (G1) ------------------------------------------------------------------------------- Note (1):Based on the equinox J2000 position (in standard IAU format consisting of HHMM+/-DDMM). Note (2): AGN type: Q = QSO Sy1 = Seyfert 1 Sy2 = Seyfert 2 NLS1 = Narrow Line Seyfert 1 NLRG = Narrow Line Radio Galaxy Note (3): We include this BL Lac object as it shows weak emission lines. ------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat ------------------------------------------------------------------------------- Bytes Format Units Label Explanations ------------------------------------------------------------------------------- 1- 11 A11 --- Nspect Spectrum name (G1) 12 A1 --- f_Nspect [*] See notes on spectra in Appendix 14- 18 F5.2 --- GammaUV UV power law continuum slope (2) 20- 23 F4.2 --- E_GammaUV ? Upper 2{sigma} error in GammaUV 25- 29 F5.2 --- e_GammaUV ? Lower 2{sigma} error in GammaUV 31- 36 F6.3 10-13mW/m2/nm Norm Normalization of UV power law in units of 10^-14^erg/cm^2^/s/Angstroems 38- 42 F5.3 10-13mW/m2/nm E_Norm Upper 2{sigma} error in Norm 44- 48 F5.3 10-13mW/m2/nm e_Norm Lower 2{sigma} error in Norm 50- 55 F6.1 0.1nm Wave Observed wavelength in Angstroems 57- 61 F5.2 --- GammaOpt ? Optical power law continuum slope (3) 63- 68 F6.2 --- E_GammaOpt ? Upper 2{sigma} error in GammaOpt 70- 74 F5.2 --- e_GammaOpt ? Lower 2{sigma} error in GammaOpt ------------------------------------------------------------------------------- Note (2): Defined as f_{lambda}_ {prop to} {lambda}^-GammaUV^. GammaUV is fitted at {lambda}_rest_<4200{AA}. Slopes with no listed errors show the assumed slope value in cases where only a single continuum window was available. Note (3): Defined as f_{lambda}_ {prop to} {lambda}^-GammaOpt^. GammaOpt is fitted at {lambda}_rest_>4200{AA}. ------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat ------------------------------------------------------------------------------- Bytes Format Units Label Explanations ------------------------------------------------------------------------------- 1- 11 A11 --- NSpect Spectrum name (G1) 13- 20 F8.5 --- z Redshift 22- 38 A17 --- Line Emission line identification 40- 44 I5 km/s FWHM Rest frame Full Width at Half Maximum 47- 51 I5 km/s E_FWHM Upper 2{sigma} error limit on FWHM 53- 58 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM 61- 65 I5 km/s VPeak Gaussian emission line model peak offset from expected position based on tabulated redshift 69- 72 I4 km/s E_VPeak Upper 2{sigma} error limit on VPeak 74- 79 I6 km/s e_VPeak Lower 2{sigma} error limit on VPeak 82- 88 F7.2 0.1nm EW Rest frame equivalent width in Angstroms 92- 97 F6.2 0.1nm E_EW Upper 2{sigma} error limit on EW (1) 100-106 F7.2 0.1nm e_EW Lower 2{sigma} error limit on EW (1) 109-115 F7.2 10-14mW/m2 Flux Observed flux in units of 10^-14^erg/s/cm^2^ 119-124 F6.2 10-14mW/m2 E_Flux Upper 2{sigma} error limit on Flux (1) 127-133 F7.2 10-14mW/m2 e_Flux Lower 2{sigma} error limit on Flux (1) 135-136 I2 --- NAbs Number of narrow absorption features used in the emission line modeling ------------------------------------------------------------------------------- Note (1): Based on the uncertainties in the amplitude and FWHM of the Gaussian model and do not include an error from an uncertainty in the underlying continuum flux level which we estimate to be about 10%. For emission lines where only an upper limit on Flux and EW is available, no values for the VPeak are quoted as the position of the line was fixed at the line's expected wavelength. Also, the FWHM value in this case was set to the median value for the LBQS sample (see Table 3, Paper~II) with no associated errors. ------------------------------------------------------------------------------- Global notes: Note (G1): Based on the equinox J2000 position (in standard IAU format consisting of HHMM+/-DDMM). In addition to this, a two letter designation is used for the spectra indicating that the spectra are from a post-COSTAR observation (o) and whether there is more than one spectrum of the same object (a-z). A capital letter at the end of the name indicates that the object is a gravitational lens and that separate spectra of each lensed component were observed and analyzed. -------------------------------------------------------------------------------