Hostname: page-component-8448b6f56d-c4f8m Total loading time: 0 Render date: 2024-04-19T22:31:59.317Z Has data issue: false hasContentIssue false
  • English
  • Français

A rocket observation of cosmic X-rays in the energy range between 0.15 and 20 keV

Published online by Cambridge University Press:  14 August 2015

S. Hayakawa ,
T. Kato ,
F. Makino ,
H. Ogawa ,
Y. Tanaka ,
K. Yamashita ,
M. Matsuoka ,
S. Miyamoto ,
M. Oda  and
Y. Ogawara
S. Hayakawa
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
T. Kato
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
F. Makino
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
H. Ogawa
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
Y. Tanaka
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
K. Yamashita
Affiliation:
Dept. of Physics, Nagoya University, Nagoya, Japan
M. Matsuoka
Affiliation:
Institute of Space and Aeronautical Science, University of Tokyo, Tokyo, Japan
S. Miyamoto
Affiliation:
Institute of Space and Aeronautical Science, University of Tokyo, Tokyo, Japan
M. Oda
Affiliation:
Institute of Space and Aeronautical Science, University of Tokyo, Tokyo, Japan
Y. Ogawara
Affiliation:
Institute of Space and Aeronautical Science, University of Tokyo, Tokyo, Japan

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.

Cosmic X-rays were observed with three sets of proportional counters covering the energy range between 0.15 and 20 keV. The detector born on a spinning rocket scanned a celestial region in which the galactic latitude bII changed from 30° to −55° across the galactic plane in the Cygnus-Cassiopeia region. The spectrum of Cyg XR-2 thus obtained is represented by a thermal bremsstrahlung of temperature 3.4 keV modified by the interstellar absorption for the hydrogen column density of 3 × 1021 cm−2. The diffuse component showed an interstellar absorption effect, which was however found much weaker than one would expect if the diffuse component were due entirely to be of extragalactic origin. The spectrum obtained in the highest latitude region is represented approximately by a power law E−1.8 but shows a possible trough at about 1 keV.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 37: Non-Solar X- and Gamma-Ray Astronomy , 1970 , pp. 121 - 129
Copyright
Copyright © Reidel 1970 

References

[1] Gorenstein, P., Gursky, H., and Garmire, G.: 1968, Astrophys. J. 153, 885.CrossRefGoogle Scholar
[2] Giacconi, R.: this volume, p. 107.Google Scholar
[3] Bell, K. L. and Kingston, A. E.: 1967, Monthly Notices Roy. Astron. Soc. 136, 241.Google Scholar
[4] Bunner, A. N., Coleman, P. L., Kraushaar, W. L., McCammon, D., Palmieri, T. M., Shilepsky, A., and Ulmer, M.: 1969, Nature 223, 1222.Google Scholar
[5] Bowyer, C. S., Field, G. B., and Mack, J. E.: 1968, Nature 217, 32.Google Scholar