Gamma-Ray Observations of NGC 253 and M82 with OSSE

D. Bhattacharya, L.-S. The, J. D. Kurfess, D. D. Clayton, N. Gehrels, M. D. Leising, D. A. Grabelsky, W. N. Johnson, G. V. Jung, R. L. Kinzer, W. R. Purcell, M. S. Strickman, and M. P. Ulmer

Astrophysical Journal, 437, 173-178, 1994 December 10

Abstract

Gamma-ray observations of the nearby starburst galaxies NGC 253 and M82 over the energy range (0.05--10) MeV have been obtained with the OSSE spectrometer on the Compton Gamma Ray Observatory. The priority of these galaxies as OSSE targets had been established on the grounds that the average supernova rate may be high in starbursts as indicated by infrared and radio observations, and at distances of ~3 Mpc a significant chance of supernova gamma-ray line detection exists. NGC 253 was detected in continuum emission up to 165 keV with a total significance of 4.4 sigma and an estimated luminosity of 3 x 10^40 ergs s^-1. The spectrum is best fit by a power law of photon index ~ 2.5. We consider the possible contribution of different emission mechanisms, including inverse Compton scattering, bremsstrahlung, discrete sources and Type Ia/Ib supernova continuum to the measured flux. No significant continuum flux was observed from M82. A search for the \gamm-ray line from the decay of the most abundant radioactive element produced in supernovae Ni^56 -> Co^56 -> Fe^56 yielded no significant detection: the 3 sigma upper limits to the line fluxes at 0.158, 0.812, 0.847 and 1.238 MeV for both galaxies are obtained. Notes: Figures to be added in near future