Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...204..330s&link_type=abstract
Astrophysical Journal, vol. 204, Mar. 1, 1976, pt. 1, p. 330-336.
Astronomy and Astrophysics
Astrophysics
65
Abundance, Emission Spectra, Nitrogen, Quasars, Seyfert Galaxies, Carbon, Galactic Nuclei, Line Spectra, Oxygen Spectra
Scientific paper
Ionization and temperature structure models of quasar emission-line regions are used to predict the intensities of the most promising UV emission lines of C, N, and O, and also to examine the sensitivity of the relevant line ratios to physical conditions in those regions. These results are then employed to derive the N/C ratio from observations of two quasars. It is found that the N/O abundance ratio can be derived to an accuracy better than a factor of 2 from the N IV/O III intercombination-line ratio, if the ratio of the C III intercombination line to the C IV ionic line is also measured. The N/C ratio can then be determined from the N IV (intercombination)/C IV intensity ratio or the N III/C III intercombination-line intensity ratio. The observed N III/C III intercombination ratios in the quasars PHL 957 and PKS 1756+237 are found to imply N/C ratios that are 5 and 3 to 12 times larger than the solar value, respectively. It is inferred that these quasars share the large N/O ratios and metal abundances found in Seyfert nuclei as well as in the nuclei and inner regions of normal galaxies.
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