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The emission spectrum of active galactic nuclei. II - High column density photoionization models and low ionization lines
Current one-component models of the broad line region of quasars fail toexplain the strength of low ionization lines. A two-componentphotoionization model where the high and low ionization lines areallowed to arise from different kinds of clouds is explored. A spectraldistribution of the incident radiation which tends to overestimate theX-ray flux around 3 keV is adopted in order to enhance the extent andthe heating of the excited H I region. After discussing the influence ofseveral parameters, it is concluded that the model is still unable toexplain the observed ratio Fe II/H? and that another kind of cloud,presumably not heated by photoionization, is needed to emit Fe II.
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Observation and Astrometry data
| Constellation: | ぼうえんきょう座 |
| Right ascension: | 19h15m43.94s |
| Declination: | -53°51'42.2" |
| Apparent magnitude: | 8.91 |
| Distance: | 117.925 parsecs |
| Proper motion RA: | 30.8 |
| Proper motion Dec: | -96.1 |
| B-T magnitude: | 9.4 |
| V-T magnitude: | 8.951 |
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