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Cross-Correlation Techniques for the determination of Galaxy Redshifts

  • R. W. Hunstead (a1)

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Most of the galaxy redshifts currently available in the literature have been measured from photographic spectra and are generally based on subjective estimates of the position of the narrow absorption features. In using only the few prominent absorption lines, most of the light from the galaxy is discarded. With the advent of digital linear-response detectors it is possible to obtain accurate and objective redshifts by cross-correlating all or part of the galaxy spectrum with a template galaxy of known redshift (Tonry and Davis 1979, Kelton 1980 and references therein).

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References

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Brault, J. M., and White, O. R., Astron. Astrophys., 13, 169 (1971).
Burbidge, E. M., and Burbidge, G. R., Astrophys. J., 172, 37 (1972).
de Vaucouleurs, G., de Vaucouleurs, A. and Corwin, H. G., Second Reference Catalogue of Bright Galaxies, (Univ. of Texas Press) (1976).
Kelton, P. W., Astron. J., 85, 89 (1980).
Sandage, A., Astrophys. J., 202, 563 (1975).
Shobbrook, R. R., Mon. Not. Astron. Soc., 131, 293 (1966).
Tonry, J., and Davis, M., Astron. J., 84, 1511 (1979).

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