Possible Evidence for Pulsed Emission of High-Energy Gamma Rays by PSR B0656+14

Details Possible Evidence for Pulsed Emission of High-Energy Gamma Rays by PSR B0656+14 Possible Evidence for Pulsed Emission of High-Energy Gamma Rays by PSR B0656+14

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...458..755r&link_type=abstract

Astrophysical Journal v.458, p.755

Astronomy and Astrophysics

Astronomy

77

Gamma Rays: Observations, Stars: Pulsars: Individual Alphanumeric: Psr 0656+14

Scientific paper

We present here possible evidence for a seventh high-energy gamma-ray pulsar, PSR B0656 + 14, pulsating in gamma rays at E ≥ 50 MeV with the same 384.9 ms periodicity as in radio, using the data obtained during 1991 April to 1993 December by the Energetic Gamma-Ray Experiment Telescope (EGRET) aboard the Compton Gamma Ray Observatory. Since the pulsed flux is very low, we adapted a weighting method in our analysis of the data to detect the pulsar. With this technique, we found that the null hypothesis (viz., that it is not a pulsar) is probable only at a level of < 2.6 x 10-7. The phase-selected data corresponding to the peak seen in the events light curve reveals the existence of a high-energy gamma-ray source positionally consistent with the pulsar. We found that the phase-averaged high-energy gamma-ray pulsed flux from PSR B0656 + 14 is (4.1±1.4) x 10-8 photons cm s at E > 100 MeV, and the exponent of the differential photon number spectrum -2.8±0.3. The pulsar appears to have an efficiency of approximately 0.001 in converting its spindown energy-loss rate into high-energy gamma-rays at E ≥ 100 MeV.

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