Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.207..263b&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 207, March 15, 1984, p. 263-286.
Astronomy and Astrophysics
Astronomy
81
Astronomical Photometry, Emission Spectra, Iron, Quasars, Radiant Flux Density, Spectrophotometry, Absorption Spectra, Abundance, H Beta Line, High Temperature Plasmas, Optical Emission Spectroscopy, Red Shift, Ultraviolet Spectra
Scientific paper
From intermediate-resolution spectrophotometry of 33 quasars with redshift less than 0.7, significant statistical differences in the line properties emerge between the radio and radio-quiet objects. Fe II optical emission is rare in radio quasars and less intense on average when present, whereas Fe II UV emission is always detected in both classes. Moreover, for the radio sample, Fe II optical emission is not correlated with the radio morphology, contrary to previous suggestions. Finally, in radio quasars the full-width at half maximum of H-beta and/or Mg II is statistically larger by nearly a factor of two than in radio-quiet ones. The continua as well approximated by a power law. The average spectral index for the whole sample is 0.16 + or - 0.48, significantly smaller than the value found in the sample of higher redshift quasars studied by Richstone and Schmidt (1980). Seven absorption-line systems are present in the sample and, for the first time, Ca II H and K absorptions are identified in two Mg II absorption systems. A model is suggested to account for the differences found between radio and radio-quiet quasars; it involves a hot diffuse plasma which constrains the surface density of the emissive clumps.
Bergeron Jacqueline
Kunth Daniel
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