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ABSTRACT THERE appears to be continuing confusion as to whether or not counts of extragalactic radio sources are compatible with the steady state theory. Ryle and Clarke1 found considerable
discrepancies between the observed counts and those predicted on the basis of steady state. Hoyle2 argues that the source counts are in agreement with the steady state theory except for a
deficiency of only 5 sources per steradian at the bright end. I present here an explicit derivation of source counts expected in the steady state on the basis of identifications and
redshifts of a complete sample of radio galaxies and quasi-stellar sources. Access through your institution Buy or subscribe This is a preview of subscription content, access via your
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article * Purchase on SpringerLink * Instant access to full article PDF Buy now Prices may be subject to local taxes which are calculated during checkout ADDITIONAL ACCESS OPTIONS: * Log in
* Learn about institutional subscriptions * Read our FAQs * Contact customer support SIMILAR CONTENT BEING VIEWED BY OTHERS THE DIFFUSE GAMMA-RAY FLUX FROM CLUSTERS OF GALAXIES Article Open
access 29 April 2023 THE DIFFUSE Γ-RAY BACKGROUND IS DOMINATED BY STAR-FORMING GALAXIES Article 15 September 2021 SELECTION BIAS OBFUSCATES THE DISCOVERY OF FAST RADIO BURST SOURCES Article
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134, 916 (1961). Article ADS MathSciNet Google Scholar Download references AUTHOR INFORMATION AUTHORS AND AFFILIATIONS * Hale Observatories, California Institute of Technology, Carnegie
Institution of Washington, M. SCHMIDT Authors * M. SCHMIDT View author publications You can also search for this author inPubMed Google Scholar RIGHTS AND PERMISSIONS Reprints and
permissions ABOUT THIS ARTICLE CITE THIS ARTICLE SCHMIDT, M. Radio Source Counts and Redshifts in Steady State Cosmology. _Nature_ 240, 399–400 (1972). https://doi.org/10.1038/240399a0
Download citation * Received: 29 September 1972 * Issue Date: 15 December 1972 * DOI: https://doi.org/10.1038/240399a0 SHARE THIS ARTICLE Anyone you share the following link with will be
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