Hostname: page-component-76fb5796d-wq484 Total loading time: 0 Render date: 2024-04-27T00:24:51.862Z Has data issue: false hasContentIssue false
  • English
  • Français

ROSAT Deep Surveys

Published online by Cambridge University Press:  30 March 2016

Günther Hasinger
Günther Hasinger*
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik 8046 Garching, Germany

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.

A series of 20 deep pointed observations with the ROSAT PSPC is discussed. 530 X-ray sources with 0.5-2 keV fluxes down to 3·10-15erg cm-2 s-1 have been discovered in 5.9 deg2. The N(>S) relation of the sources selected in the 0.5-2 keV band shows a density in excess of 200 deg-2 at the faintest fluxes and a flattening below 2·10-14erg cm-2 s-1. The average spectrum of those sources is a power law with energy index 1.2 ±0.1. The absorption column densities are consistent with the galactic HI columns. More than 50% of the 1-2 keV background has been resolved into discrete sources in the deepest field. The total background spectrum shows an emission line feature around 0.65 keV, most probably due to OVII-OVIII from a 2·106K plasma. Above ~ 1 keV the background is dominated by a power law spectrum with a normalization of 13.4 ± 0.2 keV cm-2 s-1 sr-1 keV-1 and a slope 1.2 ± 0.1, i.e. considerably steeper than the extrapolation from higher energies.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 199 - 204
Copyright
Copyright © Kluwer 1992

References

Fink, H.H., Schmitt, J.H.M.M. & Harnden, F.R. Jr. Asir. Astrophys. 193, 345(1988).Google Scholar
Giacconi, R. et al. Astrophys. J. 234, L1 (1979).CrossRefGoogle Scholar
Gioia, I. M. et al. Astrophys. J. suppl. Ser. 72, 567(1990).CrossRefGoogle Scholar
Griffiths, R.E. et al. Astrophys. J. 269, 375(1983).CrossRefGoogle Scholar
Hasinger, G., Schmidt, M. & Trümper, J. Astr. Astrophys. 246, L2 (1991) (paper I).Google Scholar
Inoue, H. et.al Astrophys. J. 238, 886(1980).CrossRefGoogle Scholar
Lockman, F.J., Jahoda, K. & McCammon, D. Astrophys. J. 302, 432(1986).CrossRefGoogle Scholar
Marshall, F.E. et al. Astrophys. J. 235, 4(1980).CrossRefGoogle Scholar
McCammon, D. & Sanders, W.T. Ann. Rev. Astron. Astrophys. 28, 657(1990).CrossRefGoogle Scholar
Primini, F.A. et al. Astrophys. J. 374, 440 CrossRefGoogle Scholar
Pfeffermann, E. et al. Proc. SPIE 733, 519(1986).CrossRefGoogle Scholar
Rocchia, R. et al. Astr.Astrophys. 130, 53(1984).Google Scholar
Snowden, S. et al., Astrophys. J. (submitted) (1991).Google Scholar
Shanks, T. et al., Nature 253, 315(1991).CrossRefGoogle Scholar
Trümper, J. Adv. Space Res. 2, no.4, 241 (1983).CrossRefGoogle Scholar