OSSE observations of NGC 1275 in the 0.05-10.0 MeV range

Details OSSE observations of NGC 1275 in the 0.05-10.0 MeV range OSSE observations of NGC 1275 in the 0.05-10.0 MeV range

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435..181o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 435, no. 1, p. 181-184

Astronomy and Astrophysics

Astronomy

7

Active Galactic Nuclei, Astronomical Models, Gamma Ray Astronomy, Gamma Ray Spectra, Interstellar Magnetic Fields, Spaceborne Astronomy, Astronomical Spectroscopy, Gamma Ray Observatory, Mathematical Models, Radio Astronomy, Scintillation Counters, Spectrometers, X Ray Astronomy

Scientific paper

We made observations of NGC 1275 with the Compton Gamma-Ray Observatory's Oriented Scintillation Spectrometer Experiment (OSSE) between 1991 November 28 and December 12. We did not detect the source during this viewing period. Our 3 sigma upper limit to a detection in the approximately 50-90 keV range is 6 x 10-6 photons/sq cm/s/keV. This flux is more than 10 times lower than the 3 sigma detection in the same energy range reported by Rothschild et al. for their OSO 7 observations. Our results are discussed in comparison with radio observations and models for the X-ray emission, and we show that it is likely that most of the approx. greater than 10 keV photons come from the nuclear region of NGC 1275. We find no significant correlation between the variable radio intensity and the hard X-ray flux of the entire NGC 1275 source. Simultaneous Very Large Baseline Array and gamma-ray observations are needed to test the self-Compton synchrotron models for gamma-ray emission from the core of NGC 1275. Our results also provide a lower limit to the magnetic field of approximately 2 x 10-7 gauss for the approximately 5 min radio source centered on NGC 1275.

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