Luminosity effects and the emission-line properties of quasars with 0 less than Z less than 3.8

Details Luminosity effects and the emission-line properties of quasars with 0 less than Z less than 3.8 Luminosity effects and the emission-line properties of quasars with 0 less than Z less than 3.8

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..678o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 436, no. 2, p. 678-695

Astronomy and Astrophysics

Astronomy

104

Astronomical Catalogs, Emission Spectra, Line Spectra, Quasars, Radio Astronomy, Stellar Luminosity, Stellar Spectra, Ultraviolet Astronomy, Iue, Radio Sources (Astronomy), Red Shift, Spaceborne Astronomy

Scientific paper

We present data and a spectral atlas for 76 quasars with 2.97 less than z less than 3.80 and for 33 quasars with z approximately 2, together with measures of 73 quasars from the IUE archives that mostly have z less than 1. The quasars provide a sampling of the luminosity-redshift plane at constant luminosity for 0 less than z less than 3.8, a range of a factor of 40 in luminosity for 3 less than z less than 3.8, and a range of 103 in luminosity for z less than 1. We investigate the behavior of the principle emission lines from 1200-2000 A and find: (1) The Baldwin effect at z greater than 3 is definitely present in the C IV lambda 1549 line and in the other strong emission lines in varying degrees except for N v lambda-lambda(1240) and 1400, where the effect is very weak. (2) The component that varies with luminosity has a narrower full width at half maximum (FWHM) than the average line width and appears consistent with the first component of the principal component analysis of the Large Bright Quasar Survey sample by Francis et al. (1992). (3) There is no evidence for redshifted-dependent spectral changes, Baldwin or otherwise, in quasars of the same luminosity in the z approximately 2 and z greater than 3 samples. (4) The Baldwin effect in the IUE, z approximately 2, and z greater than 3 subsamples joins smoothly, although the slope of the effect steepens with increasing luminosity. (5) The results are consistent with the ionization parameter decreasing with increasing luminosity. (6) The large ratio of N v to Ly-alpha and its small change with luminosity are consistent with the arguments of Hamann & Ferland (1993a, b) that the N/C ratio is enhanced in high-luminosity quasars with z greater than 3.

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