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

C. Y. Osako*, M. P. Ulmer, D. A. Grabelsky, W. R. Purcell, M. S. Strickman, W. N. Johnson, R. L. Kinzer, J. D. Kurfess, G. V. Jung

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

9 Scopus citations


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 × 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 × 10-7 gauss for the ∼5′ radio source centered on NGC 1275.

Original languageEnglish (US)
Pages (from-to)181-184
Number of pages4
JournalAstrophysical Journal
Issue number1
StatePublished - Nov 1 1994


  • Galaxies nuclei
  • Galaxies: individual (NGC 1275)
  • Galaxies: magnetic fields
  • Gamma rays: observations

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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