Open AccessO i Line Emission in the Quasar PG 1116+215
Author(s) -
Yoshiki Matsuoka,
Shinki Oyabu,
Y. Tsuzuki,
Kimiaki Kawara,
Yuzuru Yoshii
Publication year - 2005
Publication title -
publications of the astronomical society of japan
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.99
H-Index - 110
eISSN - 2053-051X
pISSN - 0004-6264
DOI - 10.1093/pasj/57.4.563
Subject(s) - quasar , physics , astrophysics , lambda , line (geometry) , emission spectrum , luminosity , flux (metallurgy) , infrared , ionization , spectral line , line width , photon flux , astronomy , photon , optics , galaxy , ion , quantum mechanics , geometry , mathematics , materials science , metallurgy
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 OI lines ({lambda}1304, {lambda}8446, and{lambda}11287) in a quasar for the first time. The photon flux ratios of the OIlines of the quasar were compared with those previously measured in a Seyfert 1and six narrow-line Seyfert 1s. No significant differences were found in the OIline flux ratios between the quasar and the other Seyferts, suggesting that thegas density in the OI and FeII line-emitting regions in the quasar is of thesame order as those in low-luminosity AGNs. It was also found that the linewidth of OI {lambda}11287 is significantly narrower than that of Ly{alpha},which is consistent with OI and FeII emission occurring in the partly ionizedregions at the outermost portion of the broad-line region where velocities aresmall.Comment: 6 pages, 2 figures, accepted by PASJ; minor wording changes (01/07/2005
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