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A Hard X-ray Observation of CYG X-1 in 1985

Published online by Cambridge University Press:  04 August 2017

Y.Q. Ma ,
G.H. Li ,
C.M. Zhang ,
Q.Y. Xiao ,
Y.M. Qian ,
Z.G. Li ,
M. Wu ,
CJ. Dai ,
Y.D. Gu  and
X.Y. Zhang
...Show all authors
Y.Q. Ma
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
G.H. Li
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
C.M. Zhang
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
Q.Y. Xiao
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
Y.M. Qian
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
Z.G. Li
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
M. Wu
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
CJ. Dai
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
Y.D. Gu
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
X.Y. Zhang
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China
T.P. Li
Affiliation:
Institute of High Energy Physics, Academia Sinica, P.O. Box 918, Beijing, China

Extract

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On September 22, 1985, a hard X-ray observation of Cyg X-1 was performed by using a balloon-borne CsI-NaI phoswich telescope HAPI-2 at Xianghe Balloon Facility in China. The main detector is CsI(T1) with a thickness of 0.4cm and an area of 140cm2. The energy range is 20–200KeV. The telescope reached a float altitude of about 38Km(4g/cm2). The photon's arrival time and energy loss spectrum were measured for both background and active tracking on-source observations.

Type
II. Accretion Powered Pulsars
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 202
Copyright
Copyright © Reidel 1987 

References

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Watanabe, H., RUP 85-2, 1985.Google Scholar