ROSAT observations of the unusual supernova remnant CTB 80 containing the pulsar PSR 1951 + 32

Details ROSAT observations of the unusual supernova remnant CTB 80 containing the pulsar PSR 1951 + 32 ROSAT observations of the unusual supernova remnant CTB 80 containing the pulsar PSR 1951 + 32

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...439..722s&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 439, no. 2, p. 722-729

Astronomy and Astrophysics

Astronomy

58

Interstellar Matter, Pulsars, Supernova Remnants, X Ray Astronomy, Brightness, Data Reduction, Flux Density, Radio Observation, Rosat Mission, X Ray Spectra

Scientific paper

The unusal supernova remnant CTB, 80 containing the 39.5 ms pulsar PSR 1951 + 32, has been observed with the Position Sensitive Proportional Counter (PSPC) and the High Resolution Imager (HRI) aboard ROSAT. The HRI image, centered on the pulsar, is composed of a bright compact core of approximately 1 arcminute radius containing the pulsar and a compact nebula, as well as a diffuse nebula extending approximately 5 arcminutes eastward of the pulsar. The PSPC allowed us to model the spectra of the point source, the compact nebula and the 5 arcminute diffuse nebula. For a power-law spectrum with photon index Gamma approximately 2 and an interstellar column density of NH approximately 3 x 1021/cm21 the derived luminosities are approximately 2.3 x 1033 d2.52 ergs/s from the pointlike source, approximately 3.9 x 1033 d2.52 ergs/s from the compact nebula, and approximately 1.8 x 1033 d2.52 ergs/s from the 5 arcminutes diffuse nebula. In addition, the 2 deg diameter circular field of view of the PSPC reveals a hard emission feature southeast of the pulsar with a conical geometry extending out to the edge of the detector. The spectrum from this region is well described by a two-temperature Raymond-Smith thermal plasma with an average temperature of approximately 107 K and a luminosity of approximately 1034d2.52 ergs/s. Pulsations from the 39.5 ms pulsar, PSR 1951 + 32, are detected at the 99% confidence level. The implied pulsed fration is approximately 35% with a complicated energy-dependent behavior. The compact core and the extended diffuse nebula can be explained as synchrotron radiation from the relativistic pulsar wind confined by the ram pressure of the surrounding inhomgeneous medium. The conelike feature detected southeast of PSR 1951 + 32 is consistent with emission from an optically thin SNR in the radiative cooling phase of its evolution.

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