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Gamma-ray observations of Co-56 in SN 1987A
Mahoney, W. A.; Varnell, L. S.; Jacobson, A. S.; Ling, J. C.; Radocinski, R. G.; Wheaton, Wm. A.
AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 334, Nov. 15, 1988, p. L81-L85. (ApJL Homepage)
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NASA/STI Keywords:
Cobalt Isotopes, Gamma Ray Astronomy, Supernova 1987a, Balloon Flight, Gamma Ray Spectrometers, Line Spectra, Supernova Remnants
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During observations of SN 1987A 286 days after the supernova explosion using a JPL high-resolution gamma-ray spectrometer, a line feature was found in the net supernova spectrum at an energy of 1240.8 + or - 1.7 keV, with an intrinsic width of 8.2 + or - 3.4 keV FWHM, and a net flux of 0.0021 + or - 0.0007 photons/sq cm per s. This feature is interpreted as the 1238 keV line from the decay of Co-56 in the supernova remnant. The blueshift and intrinsic broadening of the 1238 keV line are consistent with models incorporating mixing of the radioactive cobalt in the expanding eject.

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