Multifrequency observations of BL Lacertae in 1988

Creators: Kawai, N.; Matthews, K.; Neugebauer, G.

Abstract

Simultaneous multiwavelength observations of BL Lacertae were performed on two occasions separated by month in 1988 June and July, covering the radio, submillimeter, infrared, optical, ultraviolet, and X-ray wave bands. In the wide-band photon spectra, the X-ray flux lies clearly above the extension of radio ultraviolet continuum as expected. The slope of the X-ray spectra is significantly flatter than that at optical ultraviolet regimes, and its spectral index 0.7-1.0 corresponds to the slope at submillimeter band. Comparison with earlier observations, in fact, indicates that the X-ray flux is correlated with the submillimeter band, and not with the others, and supports the SSC model.

Additional Information

© 1991 American Astronomical Society. Received 1991 April 9; accepted 1991 June 5. The authors would like to thank the telescope scheduling committees and others responsible for accommodating the demands of multifrequency campaigns such as this. In addition, N. K., M. M., and T. O. would like to thank all the members of the Ginga team; reduction of the Ginga data is partly supported by the Data Analysis Center of ISAS; J. N. B. and S. A. B. would like to thank Anne Kinney and Anuradha Koratkar for their assistance in reducing the IUE data; support for this effort was provided to J. N. B. and S. A. B. by NASA through grants NAG 5-1059 and NAGW 2135. Also, radio astronomy at the University of Michigan is supported by the NSF through grant AST-8815678; J. S. M. and R. G. wish to acknowledge Lick Observatory and the NSF for their support; T. J. B. has been aided by the NSF, Colgate, and the NRAO; infrared astronomy at Caltech gratefully acknowledges continued support by the NSF; observations at the University of Florida were supported by the NSF; R. E. C., M. G. H., P. F. R., G. M. S., and V. A. H. would like to thank the staff of the JCMT for their assistance; M. H., and H. A. T. acknowledge the support from the NSF, the University of Wyoming, and the Astrophysical Research Consortium; B. J. W., and D. W. would like to thank the NSF and the University of Texas.

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