The semiforbidden C III lambda 1909 effective wavelength-redshift relationship in quasars

Details The semiforbidden C III lambda 1909 effective wavelength-redshift relationship in quasars The semiforbidden C III lambda 1909 effective wavelength-redshift relationship in quasars

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...249...17f&link_type=abstract

Astrophysical Journal, Part 1, vol. 249, Oct. 1, 1981, p. 17-22.

Astronomy and Astrophysics

Astrophysics

39

Carbon, Ion Density (Concentration), Photoionization, Quasars, Red Shift, Ultraviolet Spectra, Astronomical Models, Emission Spectra, Forbidden Bands, Galactic Nuclei, Line Spectra, Radiant Flux Density, Rarefied Gases

Scientific paper

This paper investigates the recently discovered correlation between redshift and the effective wavelength of the semiforbidden C III 1909 emission line in quasars. It is proposed that the delta z = to 0.0005 blueshift discovered in z less than 1.8 objects by Willis (1980) is caused by an unresolved low-density-region component which contributes significant 1906.8 emission. Photoionization calculations are presented which model a typical quasar narrow-line-region (NLR) cloud. These calculations suggest that clouds typically have a density of about 10,000/cu cm and contribute roughly 20-50% of the flux in strong ultraviolet lines. A synthetic semiforbidden C III 1909 line profile is computed, and its centroid is found to be in good agreement with the Wills results. The Wills relationship would suggest that high-redshift (z greater than 1.8) objects tend to have weaker NLR emission, which may mean that these objects are more similar to 3C 273 than to typical low z objects. The importance of a proper accounting of the effects of a sharp component on ultraviolet broad-line profiles is stressed.

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