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X-ray Observations of Blazars with Ginga and ASCA

Published online by Cambridge University Press:  19 July 2016

M. Tashiro ,
K. Makishima ,
Y. Kohmura ,
T. Ohashi ,
C. Otani ,
T. Kii ,
R. Fujimoto ,
F. Makino ,
Ginga Team  and
ASCA Team
M. Tashiro
Affiliation:
The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan
K. Makishima
Affiliation:
The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan
Y. Kohmura
Affiliation:
The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan
T. Ohashi
Affiliation:
Tokyo Mitropolitan University, 1-1 Minami-Osawa, Hachioji, Tokyo, Japan
C. Otani
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan
T. Kii
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan
R. Fujimoto
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan
F. Makino
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan

Extract

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Among 13 BL Lacs observed with Ginga, 1H 0323+022, Mkn 421 and PKS 2155-304 exhibited significant variablity during each (typically one day) observation. On the flux-hardness plane, the data points obtained from each source draw a sort of clockwise hysteresis motion. It means that the spectrum hardens before the source gets brighter, while the spectrum softens before the source becomes fainter. Such a soft-lag behavior, first pointed out for PKS2155-304 by Sembay et al. These properties were also confirmed with the discrete cross correlation function technique.

Type
Poster Contributions: X-Rays and Higher Energies
Information
Symposium - International Astronomical Union , Volume 159: Multi-Wavelength Continuum Emission of AGN , 1994 , pp. 383
Copyright
Copyright © Kluwer 1994 

References

1. Tashiro, M.: 1993, Ph. D. Thesis, the University of Tokyo Google Scholar
2. Sembay, S. et al.: 1993, ApJ 404, pp. 112–123 Google Scholar