  We report the discovery of PSR J1101-6101, a 62.8 ms pulsar in IGR
J11014-6103, a hard X-ray source with a jet and a cometary tail that strongly
suggests it is moving away from the center of the supernova remnant (SNR) MSH
11-61A at v>1000 km/s. Two XMM-Newton observations were obtained with the EPIC
pn in small window mode, resulting in the measurement of its spin-down
luminosity E_dot = 1.36e36 erg/s, characteristic age Tau_c = 116 kyr, and
surface magnetic field strength B_s = 7.4e11 G. In comparison to Tau_c, the
10-30 kyr age estimated for MSH 11-61A suggests that the pulsar was born in the
SNR with initial period in the range 54 < P_0 < 60 ms. PSR J1101-6101 is the
least energetic of the 15 rotation-powered pulsars detected by INTEGRAL, and
has a high efficiency of hard X-ray radiation and jet power. We examine the
shape of the cometary nebula in a Chandra image, which is roughly consistent
with a bow shock at the velocity inferred from the SNR age and the pulsar's
E-dot. However, its structure differs in detail from the classic bow shock, and
we explore possible reasons for this.
