1995A&A...298..528B

We report on the detection of PSR 1706-44 in two ROSAT-PSPC observations. The recorded source counts are unpulsed with a 2σ pulsed fraction upper limit of 18%. Spectral analysis did not distinguish between black-body and power law models; however, we argue that the lack of pulsations and the similarity in the pulsar's spin parameters to those of the Vela pulsar favour a power law model dN/dE∝E^–2.4±0.6 and indicate synchrotron emission from a pulsar-powered nebula as the origin of the detected X-radiation. The X-ray flux derived for the power law model is f_x=3.2^+6.5_–1.8x10^–12erg/s/cm² within the 0.1-2.4keV energy range. An upper limit for the neutron star's surface temperature is put at LogT_s^∞∼6.03K for a neutron star with a medium stiff equation of state (FP-model with M=1.4M_☉, R=10.85km). Slightly different values for T_s^∞ are computed for the various neutron star models available in the literature, reflecting the difference in the equation of state. No soft X-ray emission is detected from the supernova remnant G 343.1-2.3, proposed to be associated with PSR 1706-44.