O I lambda 8446 and NA I lambda 5893 in the quasar 3C 273

Details O I lambda 8446 and NA I lambda 5893 in the quasar 3C 273 O I lambda 8446 and NA I lambda 5893 in the quasar 3C 273

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.206p...5w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 206, Jan. 1, 1984, p. 5P-11P.

Astronomy and Astrophysics

Astronomy

6

Astronomical Spectroscopy, D Lines, Emission Spectra, Oxygen Spectra, Quasars, Sodium, Charge Coupled Devices, Helium, Infrared Spectra

Scientific paper

Although the quasar 3C 273 is often used as an example of a 'typical' quasar, it has also some atypical properties. Thus, it is a powerful radio emitter and its optical spectrum has strong permitted iron emission lines. The present investigation is concerned with a critical examination of the evidence for the presence of the emission line O I lambda 8446 in the spectrum of 3C 273. New CCD observations are presented, taking into account the wavelength range from 6200 A to 1 micron. The line O I lambda 8446 was first reported by Oke and Shields (1976). It is found that the widely quoted flux of this line is not consistent with more recent estimates of its strength. It is also found that, after correction for strong atmospheric B band absorption, the feature usually associated with He I lambda 5876 is actually closer in wavelength to NaD lambda 5893.

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