We report on 12 years of observations of PSR J1713+0747 , a pulsar in a 68-day orbit with a white dwarf .
Pulse times of arrival were measured with uncertainties as small as 200 ns .
The timing data yielded measurements of the relativistic Shapiro delay , perturbations of pulsar orbital elements due to secular and annual motion of the Earth , and the pulsar ’ s parallax , as well as pulse spin-down , astrometric , and Keplerian measurements .
The observations constrain the masses of the pulsar and secondary star to be m _ { 1 } = 1.3 \pm 0.2 { M } _ { \odot } and m _ { 2 } = 0.28 \pm 0.03 { M } _ { \odot } , respectively ( 68 % confidence ) .
Combining the theoretical orbital period-core mass relation with the observational constraints yields a somewhat higher pulsar mass , m _ { 1 } = 1.53 _ { -0.06 } ^ { +0.08 } { M } _ { \odot } .
The parallax is \pi = 0.89 \pm 0.08 mas , corresponding to a distance of 1.1 \pm 0.1 kpc ; the precision of the parallax measurement is limited by uncertainties in the electron content of the solar wind .
The transverse velocity is unusually small , 33 \pm 3 km s ^ { -1 } .
We find significant timing noise on time scales of several years , but no more than expected by extrapolating timing noise statistics from the slow pulsar population .
With the orientation of the binary orbit fully measured , we are able to improve on previous tests of equivalence principle violations .