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Effect of the Availability of Search Lines in Determining QSO Emission Line Redshift Distribution

Nature Physical Science volume 241, pages 159–160 (1973)Cite this article

Abstract

Karitskaya and Komberg1 have recently explained qualitatively some of the peaks and dips in the distribution of emission line redshifts of QSOs by the presence of four strong lines (Mg II, C III, C IV and Ly α) in the QSO spectrum. Roeder2, on the other hand, has obtained significant correlation between the number of QSOs at intervals of Δz = 0.1 and the average number of lines per object observed at the corresponding intervals. From this he concludes that at some redshifts there are more lines per object to measure.

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References

  1. Karitskaya, E. A., and Komberg, B. V., Soviet Astron.—A.J., 14, 33 (1970).

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  2. Roeder, R. C., Nature Physical Science, 233, 74 (1971).

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  3. De Veny, J. B., Osborn, W. H., and Janes, K., Publ. Astron. Soc. Pac., 83, 611 (1971).

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  4. Croxton, F. E., and Cowden, D. J., Applied General Statistics, 681 (Prentice Hall, New York, 1947).

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Authors and Affiliations

  1. Centro de Radio Astronomia e Astrofisica, Universidade Mackenzie, São Paulo, Brazil

    D. BASU

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  1. D. BASU
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BASU, D. Effect of the Availability of Search Lines in Determining QSO Emission Line Redshift Distribution. Nature Physical Science 241, 159–160 (1973). https://doi.org/10.1038/physci241159a0

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  • DOI: https://doi.org/10.1038/physci241159a0

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