The young energetic pulsar J1747–2958 ( \tau = 26 kyr , \dot { E } = 2.5 \times 10 ^ { 36 } erg s ^ { -1 } ) powers the Mouse pulsar wind nebula ( PWN ) , famous for its spectacular tail spanning 45 ^ { \prime \prime } in X-rays and 12 ^ { \prime } in radio ( d \sim 5 kpc ) .
We present the results of Chandra observations of the PWN and the analysis of archival lower-frequency data .
The Chandra HRC image reveals a point-like source at the pulsar position , \approx 1 ^ { \prime } behind the bow shock apex of the PWN .
The flattened appearance of the compact nebula is consistent with an equatorial outflow deformed by the ram pressure , implying that the angle between the pulsar ’ s spin axis and line of sight is \sim 70 ^ { \circ } ( in agreement with the radio and \gamma -ray pulse profiles ) .
The spatially-resolved spectroscopy with Chandra ACIS shows that the power-law ( PL ) spectrum steepens from \Gamma = 1.65 \pm 0.02 to 3.0 \pm 0.1 over the 45 ^ { \prime } extent of the X-ray tail .
However , the tail ’ s X-ray spectrum integrated over its 45 ^ { \prime \prime } length fits a single absorbed PL with \Gamma = 2.09 \pm 0.03 .
We also found the Mouse PWN in 150 MHz GMRT data , and a possible counterpart in 24 { \mu } m Spitzer data .
The multiwavelength data suggest that , at low frequencies , the spectrum of the X-ray-emitting tail region can be described by a broken PL with at least one turnover between radio and X-rays .
This is consistent with synchrotron cooling of electrons injected at the termination shock ( with an SED slope of 2.2 ) in an equipartition magnetic field B \sim 200 { \mu G } and a bulk flow speed v \sim 4000 km s ^ { -1 } .