OSSE Observations of NGC 1275 in the 0.05--10.0 MeV Range

We made observations of NGC 1275 with the Compton Gamma-Ray Observatory's Oriented Scintillation Spectrometer Experiment between 1991 November 28 and December 12. We did not detect the source during this viewing period. Our 3 σ upper limit to a detection in the ~50-90 keV range is 6 x 10^-6^ photons cm^-2^ s^-1^ keV^-1^. This flux is more than 10 times lower than the 3 σ 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 ~> 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 ~2 x 10^-7^ gauss for the ~5' radio source centered on NGC 1275.