IDENTIFICATION OF LINES IN THE SPECTRUM OF THE QUASAR 0237-233
Varshni,Y.P: 1988, Astrophys.Space Sci. 149, 197.
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Abstract.
The emission and absorption lines (3716-4290 Å) in the spectrum of the
quasar 0237-233 are identified within the framework of the
PLS model.
The available evidence indicates that it is a helium star. Similarities
between the spectral properties of 0237-233 and the star Upsilon
Sagittarii are pointed out. Predictions are made for the absorption-line
spectrum which falls outside 3716-4290 Å and also for an expected
discontinuity at 2600 Å.
- Introduction
- Emission lines
- Absorption-Line Spectrum
- The Discontinuity in the Ultraviolet
- Similarities with Upsilon Sagittarii
Predictions
- In the optical region outside of 3716-4290 Å, many lines due to He I, Ti II, Cr II,
Fe I, and Fe II should be observable, especially those arising from low-lying terms in the
case of Ti II, Cr II, Fe I, and Fe II.
- Narrow-band spectrophotometry would show that the discontinuity in the
ultraviolet is close to 2600 Å. Further if any discontinuity is observed in the ultraviolet
in any of the other quasars listed in
Table I,
it is expected to occur either at 2600 Å or
at 3122 Å (the ionization limit from the 1s2s^1S state of He I).
The crying need in quasar spectral studies is for better resolution, greater accuracy
and the ability to detect weaker lines.
If there should chance to be any mathematicians who, ignorant in
mathematics yet pretending to skill in that science, should dare, upon
the authority of some passage of Scripture wrested to their purpose, to
condemn and censure my hypothesis, I value them not, and scorn their
inconsiderate judgement.
- Nicolaus Copernicus,
De Revolutionibus Coelestibus
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