Photoionization models and diagnosis of physical properties of the broad-line emission gas in quasars and Seyfert nuclei

Details Photoionization models and diagnosis of physical properties of the broad-line emission gas in quasars and Seyfert nuclei Photoionization models and diagnosis of physical properties of the broad-line emission gas in quasars and Seyfert nuclei

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...283...70k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 283, Aug. 1, 1984, p. 70-80.

Astronomy and Astrophysics

Astrophysics

104

Astronomical Spectroscopy, Galactic Nuclei, Photoionization, Quasars, Seyfert Galaxies, Astronomical Models, Correlation, Emission Spectra, H Lines, Iron

Scientific paper

The earlier photoionization calculations of Kwan and Krolik are extended and improved. The present models all pertain to slabs of finite column densities. The 0 Ι and Fe ΙΙ multilevel systems are modeled better, and the dependence of different line ratios on the physical conditions is illustrated graphically. It is found that O Ι λ1304/ 8446 and Fe ΙΙ λλ 2240-2250/λλ4450-4750 are good gauges of the cloud column density. The relative flux of several semiforbidden transitions, namely, N Ιv] λ1486, O Ιv] &lambda1402, and 0 ΙΙΙ] λ 1663, to that of C ΙΙΙ] λ1909 are useful density diagnostic ratios, in addition to C ΙΙΙ] λ1909/C Ιv λ1549. Lyβ/Lyα, Hβ/Hα, Lyα/O Ι λ1304, He Ι λ5876/Hβ, C Ιv λ1549/Mg ΙΙ λ2798, and Fe ΙΙ λλ2240-2650/ Mg ΙΙ λ2798 all depend strongly on the incident continuum flux. The quantitative dependence of all these ratios on the physical parameters will provide tests of the photoionization model, a framework for modeling an individual quasar spectrum, and, in conjunction with kinematic models, allow specific calculations of both the relative intensities and profiles for the different lines.

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