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Are PSR 0656+14, PSR 0950+08, and PSR 1822-09 gamma-ray pulsars?

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Abstract

The possible discovery of three new γ-ray pulsars PSR 0656+14, PSR 0950+08, and PSR 1822-09 (Ma, Lu, Yu, and Young, 1993) in data obtained with the COS-B experiment is reinvestigated using a refined technique for pulsar light curve analysis. The results of this study do not confirm the previously claimed γ-ray pulsar nature of any of these pulsars. Even when using the standard epoch folding technique in conjunction with energy-dependent acceptance cones, we do not detect pulsed γ-ray emission from these sources. We suspect that insufficient position accuracy is the cause for the discrepancy between our results and those of Maet al. (1993). We do not rule out that any one of the three candidates, or all of them, is in fact a γ-ray pulsar, but their spin properties must differ from those derived by Maet al. (1993). More work is needed to determine the correct high-energy properties of these three sources.

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Authors and Affiliations

  1. Department of Physics and Astronomy, Clemson University, Clemson, South Carolina, USA

    Lawrence E. Brown & Dieter H. Hartmann

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  1. Lawrence E. Brown
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  2. Dieter H. Hartmann
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Brown, L.E., Hartmann, D.H. Are PSR 0656+14, PSR 0950+08, and PSR 1822-09 gamma-ray pulsars?. Astrophys Space Sci 209, 285–295 (1993). https://doi.org/10.1007/BF00627448

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  • DOI: https://doi.org/10.1007/BF00627448

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