Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprn17029g&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
We report the first detection of pulsed X-ray emission from the young, energetic radio and gamma-ray pulsar PSR B1706-44. In a 47 ks observation with the High Resolution Camera on-board the Chandra X-ray Observatory we find a pulsed signal at a frequency consistent with the radio ephemeris, f = 9.7588081 ± 0.0000027 Hz (at epoch 51585.34104 MJD). The broad, single-peaked pulse profile has a pulsed fraction of 23% ± 6%; this is not in conflict with a ROSAT PSPC upper limit of <18% because this instrument could not resolve the pulsar from a surrounding synchrotron nebula. The probability that this pulsed detection is a chance occurrence is 1.8 × 10-4 as judged by the Rayleigh test. We also fitted Chandra spectroscopic data on PSR B1706-44, which require at least two components, e.g., a blackbody of T_∞ = (1.66_-0.15^+0.17) × 10^6 K and a power-law of Γ = 2.0 ± 0.5. The blackbody radius at the nominal 2.5 kpc distance is only R_∞ = 3.6 ± 0.9 km, indicating either a hot region on a cooler surface, or the need for a realistic atmosphere model that would allow a lower temperature and larger area. Because the power-law and blackbody spectra each contribute more than 23% of the observed flux, it is not possible to decide which component is responsible for the modulation in the spectrally unresolved light curve.
Dodson Richard
Gotthelf Eric Van
Halpern Jules P.
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