Hostname: page-component-8448b6f56d-sxzjt Total loading time: 0 Render date: 2024-04-23T07:15:23.165Z Has data issue: false hasContentIssue false
  • English
  • Français

The Redshifts of Extragalactic Objects

Published online by Cambridge University Press:  14 August 2015

Wallace L. W. Sargent
Wallace L. W. Sargent*
Affiliation:
Hale Observatories, California Institute of Technology, Carnegie Institution of Washington, U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We review the evidence for a general shift-distance law for galaxies. This is shown directly by a redshift-distance diagram recently prepared by Sandage and Tammann for Sc I galaxies. The distances are measured from H II region diameters and from the diameters of the Sc 1 galaxies themselves for the more distant systems. We also show the redshift-apparent magnitude diagrams for several objects which are identifiable over a large range in distance and which prove to have a small range in absolute magnitude: these are supernovae of type I (Kowal and Sargent, 1973, unpublished), brightest cluster galaxies (Sandage, 1972a), and radio galaxies (excluding N-type galaxies) (Sandage, 1972b). Plots of redshift versus angular size for brightest cluster galaxies (Sandage, 1972c) also have the correct slope for this to be a distance effect. In summary, the tightness of the correlations for the various diagrams listed implies that there is a very close correlation between distance and redshift for galaxies out to at least z = Δλ/λ~0.2 and that there is no evidence for redshift anomalies among the objects in these diagrams.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 58: The Formation and Dynamics of Galaxies , 1974 , pp. 195 - 198
Copyright
Copyright © Reidel 1974 

References

Arp, H. C.: 1970, Astron. J. 75, 1.Google Scholar
Arp, H. C.: 1971, Nature Phys. Sci. 231, 103.Google Scholar
Burbidge, G. R.: 1973, Mitt. Astron. Gesellsch., Nr. 34, p. 19.Google Scholar
Holmberg, E.: 1961, Astron. J. 66, 620.CrossRefGoogle Scholar
Hubble, E. and Tolman, R. C.: 1935, Astrophys. J. 82, 302.CrossRefGoogle Scholar
Kristian, J.: 1973, Astrophys. J. Letters 179, L61.Google Scholar
Lewis, B. M.: 1971, Nature Phys. Sci. 231, 13.CrossRefGoogle Scholar
Lynds, C. R.: 1972, in Evans, D. S. (ed.), ‘External Galaxies and Quasi-Stellar Objects’, IAU Symp. 44, 376.Google Scholar
Peebles, P. J. E.: 1971, Comments Astrophys. Space Sci. 3, 173.Google Scholar
Sandage, A. R.: 1972a, Astrophys. J. 178, 1.Google Scholar
Sandage, A. R.: 1972b, Astrophys. J. 178, 25.CrossRefGoogle Scholar
Sandage, A. R.: 1972c, Astrophys. J. 173, 485.Google Scholar
Sandage, A. R.: 1973, Astrophys. J. 180, 687.Google Scholar
Tammann, G.: 1972, Astron. Astrophys. 21, 355.Google Scholar
Tifft, W. G.: 1972a, in Evans, D. S. (ed.), ‘External Galaxies and Quasi-Stellar Objects’, IAU Symp. 44, 367.Google Scholar
Tifft, W. G.: 1972b, Astrophys. J. 175, 613.Google Scholar
Wampler, E. J., Robinson, E. L., Baldwin, J. A., Hazard, C., and Jauncey, D. L.: 1973, Nature 246, 203.CrossRefGoogle Scholar
Wills, D.: 1972, Nature Phys. Sci. 238, 70.Google Scholar