Hostname: page-component-54dcc4c588-wlffp Total loading time: 0 Render date: 2025-09-11T21:18:20.919Z Has data issue: false hasContentIssue false
  • English
  • Français

Energy spectra of several discrete X-ray sources in the 20–120 keV range

Published online by Cambridge University Press:  14 August 2015

P. C. Agrawal ,
S. Biswas ,
G. S. Gokhale ,
V. S. Iyengar ,
P. K. Kunte ,
R. K. Manchanda  and
B. V. Sreekantan
P. C. Agrawal
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
S. Biswas
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
G. S. Gokhale
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
V. S. Iyengar
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
P. K. Kunte
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
R. K. Manchanda
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India
B. V. Sreekantan
Affiliation:
Tata Institute of Fundamental Research, Bombay 5, India

Extract

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.

In this paper we report on our observations of hard X-rays from several X-ray sources in the energy range 20–120 keV. The results were obtained from the data collected during two balloon flights made from Hyderabad, India (latitude 17.6°N, longitude 78.5°E). The first flight was made on April 28, 1968, and the balloon reached a ceiling of about 5.3 g cm−2 residual atmosphere and floated from 0230 to 0800 hrs. IST (Indian Standard Time). The second balloon was launched on December 22, 1968 and floated at about 7.5 g cm−2 of residual air from 1000 to 1130 hrs. IST.

Information

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 37: Non-Solar X- and Gamma-Ray Astronomy , 1970 , pp. 94 - 103
Copyright
Copyright © Reidel 1970 

References

[1] Agrawal, P. C., Biswas, S., Gokhale, G. S., Iyengar, V. S., Kunte, P. K., Manchanda, R. K., and Sreekantan, B. V.: 1969, Nature 224, 51.Google Scholar
[2] Chodil, G., Jopson, R. C., Mark, H., Seward, F. D., and Swift, C. D.: 1965, Phys. Rev. Letters 15, 605.Google Scholar
[3] Peterson, L. E. and Jacobson, A. S.: 1966, Astrophys. J. 145, 62.Google Scholar
[4] Lewin, W. H. G., Clark, G. W., and Smith, W. B.: 1967, Astrophys. J. (Letters) 150, L153.Google Scholar
[5] Chodil, G., Mark, H., Rodrigues, R., Seward, F. D., Swift, C. D., Turiel, L., Hiltner, W. A., Wallerstein, G., and Mannery, E. J.: 1968, Astrophys. J. 154, 645.Google Scholar
[6] Buselli, G., Clancy, M. C., Davison, P. J. N., Edwards, P. J., McCracken, K. G., and Thomas, R. M.: 1968, Nature 219, 1124.Google Scholar
[7] Bradt, H., Naranan, S., Rappaport, S., and Spada, G.: 1968, Astrophys. J. 152, 1005.CrossRefGoogle Scholar
[8] Overbeck, J. W. and Tananbaum, H. D.: 1968, Astrophys. J. 153, 899.Google Scholar
[9] Grader, R. J., Hill, R. W., Seward, F. D., and Toor, A.: 1966, Science 152, 1499.CrossRefGoogle Scholar
[10] Clark, G. W., Lewin, W. H. G., and Smith, W. B.: 1968, Astrophys. J. 151, 21.Google Scholar
[11] Peterson, L. E., Jacobson, A. S., Pelling, R. M., and Schwartz, D. A.: 1968, Can. J. Phys. 46, S437.Google Scholar
[12] Bleeker, J. A. M., Burger, J. J., Deerenberg, A. J. M., Scheepmaker, A., Swanenburg, B. N., and Tanaka, Y.: 1967, Astrophys. J. 147, 391.CrossRefGoogle Scholar
[13] Rocchia, R., Rothenflug, R., Boclet, D., and Durochoux, Ph.: 1969, Astron. Astrophys. 1, 48.Google Scholar