  We report on the detection of PSR 1706-44 in two ROSAT-PSPC observations. The
recorded source counts are unpulsed with a $2\sigma$ 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 $dN/dE\propto E^{-2.4\pm 0.6}$ 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}_{-1.8} x E-12 erg/ s/ cm^2 within the 0.1-2.4 keV energy range.
An upper limit for the neutron star's surface temperature is put at Log
T_s^\infty \sim 6.03 K for a neutron star with a medium stiff equation of state
(FP-model with M=1.4 Mo, R=10.85 km). Slightly different values for
$T_s^\infty$ 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 G343.1-2.3, proposed to be
associated with PSR 1706-44.
