Detection of pulsed MeV emission from PSR B1951+32 by COMPTEL

Details Detection of pulsed MeV emission from PSR B1951+32 by COMPTEL Detection of pulsed MeV emission from PSR B1951+32 by COMPTEL

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...337..421k&link_type=abstract

Astronomy and Astrophysics, v.337, p.421-432 (1998)

Astronomy and Astrophysics

Astrophysics

18

Gamma Rays: Observations, Pulsars: Individual: Psr B1951+32

Scientific paper

We report on the detection at MeV energies of the radio pulsar PSR B1951+32 by the Compton telescope {COMPTEL } aboard the COMPTON Gamma Ray Observatory (CGRO). Folding the event arrival times with the radio ephemerides, gives for the data collected during CGRO-mission Cycles I+II a pulsar-phase distribution with two peaks, consistent in phase with the pulses measured by {EGRET } for energies above 100 MeV. The overall significance is ga 4.1sigma . For Cycle III-VI data, with similar exposure, no indication was found in the phase distribution. Assuming that the source is not variable, simulations show that fluctuations in the dominating background distribution at significance levels la 3sigma can explain the non-detection. In addition, evidence for the presence of the pulsar in the skymaps for energies above 3 MeV is found for all Cycles of the CGRO mission. Below 3 MeV the skymaps are dominated by the strong, soft-spectrum gamma-ray source Cyg X-1, located at only ~ 2fdg 6 from PSR B1951+32. The flux (7.7+/-4.6) x 10(-7) \ ph/cm(2*) s* MeV measured by {COMPTEL } between 0.75 and 30 MeV is consistent with the measured {EGRET } spectrum. A single power-law fit to the combined EGRET-COMPTEL data (0.75 MeV - 30 GeV) gives an good fit with spectral index -1.89+/-0.07. Furthermore, a break in the pulsar spectrum at MeV energies appears to be required to reconcile the {COMPTEL } flux with upper limits reported below 1 MeV by OSSE and RXTE.

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