Hostname: page-component-745bb68f8f-b6zl4 Total loading time: 0 Render date: 2025-01-10T23:49:31.524Z Has data issue: false hasContentIssue false
  • English
  • Français

Radio Source Counts at Centimetre Wavelengths

Published online by Cambridge University Press:  07 February 2017

I. I. K. Pauliny-Toth  and
K. I. Kellermann
I. I. K. Pauliny-Toth
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn, F.R.G.
K. I. Kellermann
Affiliation:
National Radio Astronomy Observatory, Green Bank, W.Va. 24944, 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.

Counts of radio sources at 5 GHz (6 cm wavelength) have been derived from a number of surveys including a new strong source survey. The source counts do not appear to differ markedly from an integral number-flux relation having a slope of − 1.5 between 5 and 5 × 103 sources per steradian, and show a sharp drop at source densities smaller than 5 sr-1. On the basis of the form of the number counts and the observed anisotropies in the distribution of sources and of their spectra, the cosmological significance of the source counts is questioned. In particular, the evidence for strong cosmic evolution appears weaker than is generally thought unless the cosmological origin of the quasar redshifts is assumed. Measurements of the radio spectra of the sources suggest a dependence of the spectral curvature on flux density.

Type
Part II: The Structure of the Universe
Information
Symposium - International Astronomical Union , Volume 63: Confrontation of Cosmological Theories , 1974 , pp. 111 - 119
Copyright
Copyright © Reidel 1974 

References

Crawford, D. E., Jauncey, D. L., and Murdoch, H. S.: 1970, Astrophys. J. 162, 405.CrossRefGoogle Scholar
Davis, M. M.: 1971, Astron. J. 76, 980.CrossRefGoogle Scholar
Davis, M. M.: 1974, (in preparation).Google Scholar
Davis, M. M. and Kellermann, K. I.: 1974 (in preparation).Google Scholar
Jauncey, D. L.: 1967, Nature 217, 877.CrossRefGoogle Scholar
Kellermann, K. I.: 1972, Astron. J. 77, 531.CrossRefGoogle Scholar
Kellermann, K. I., Davis, M. M., and Pauliny-Toth, I. I. K.: 1971, Astrophys. J. Letters 170, L1.Google Scholar
Kellermann, K. I., Pauliny-Toth, I. I. K., and Davis, M. M.: 1968, Astrophys. Letters 2, 113.Google Scholar
Longair, M. S.: 1974, this volume, p. 93.CrossRefGoogle Scholar
Maslowski, J.: 1972, Astron. Astrophys. 16, 197.Google Scholar
Maslowski, J., Machalski, J., and Zieba, S.: 1973, Astron. Astrophys. 28, 289.Google Scholar
Pauliny-Toth, I. I. K. and Kellermann, K. I.: 1972, Astron. J. 77, 560.CrossRefGoogle Scholar
Pauliny-Toth, I. I. K., Preuß, E., Witzel, A., and Kellermann, K. I.: 1974, (in preparation).Google Scholar
Pauliny-Toth, I. I. K., Kellermann, K. I., Davis, M. M., Fomalont, E., and Shaffer, D.: 1972, Astron. J. 77, 265.CrossRefGoogle Scholar
Pooley, G. G. and Ryle, M.: 1968, Monthly Notices Roy. Astron. Soc. 139, 515.CrossRefGoogle Scholar
Yahil, A.: 1972, Astrophys. J. 178, 45.Google Scholar