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O I Line Emission in the Quasar PG 1116+215
By observing the near-infrared spectrum of the quasar PG 1116+215 at z =0.176 and combining with the HST/FOS spectrum, we obtained the relativestrengths of three permitted O I lines(λ1304, λ8446, and λ11287) in a quasar for thefirst time. The photon flux ratios of the O I lines of the quasar were compared with those previously measured in a Seyfert 1 and six narrow-line Seyfert 1s. No significant differences were found in the O I line flux ratios between the quasar and the other Seyferts, suggesting that the gas density in the O I and Fe II line-emitting regions in the quasar is of the same order as those in low-luminosity AGNs. It was also found that the line width of O Iλ11287 is significantly narrower than that of Lyα, which isconsistent with O I and Fe II emission occurring in the partly ionized regions at the outermost portion of the broad-line region where velocities are small.
| UvbyHbeta_ photometry of main sequence A type stars.
We present Stroemgren uvby and Hbeta_ photometry for a set of575 northern main sequence A type stars, most of them belonging to theHipparcos Input Catalogue, with V from 5mag to 10mag and with knownradial velocities. These observations enlarge the catalogue we began tocompile some years ago to more than 1500 stars. Our catalogue includeskinematic and astrophysical data for each star. Our future goal is toperform an accurate analysis of the kinematical behaviour of these starsin the solar neighbourhood.
| Photoelectric UBV observations made on the Palomar 20-inch telescope
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973MNRAS.164..133P&db_key=AST
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Observation and Astrometry data
| Constellation: | Leo |
| Right ascension: | 11h24m33.35s |
| Declination: | +21°46'45.6" |
| Apparent magnitude: | 9.526 |
| Proper motion RA: | -11 |
| Proper motion Dec: | -1 |
| B-T magnitude: | 9.68 |
| V-T magnitude: | 9.539 |
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