We report the discovery of 31.18 \mathrm { ms } pulsations from the INTEGRAL source IGR J14003 - 6326 using the Rossi X-ray Timing Explorer ( RXTE ) .
This pulsar is most likely associated with the bright Chandra X-ray point source lying at the center of G310.6 - 1.6 , a previously unrecognised Galactic composite supernova remnant with a bright central non-thermal radio and X-ray nebula , taken to be the pulsar wind nebula ( PWN ) .
PSR J1400 - 6325 is amongst the most energetic rotation-powered pulsars in the Galaxy , with a spin-down luminosity of \dot { E } = 5.1 \times 10 ^ { 37 } erg s ^ { -1 } .
In the rotating dipole model , the surface dipole magnetic field strength is B _ { s } = 1.1 \times 10 ^ { 12 } G and the characteristic age \tau _ { c } \equiv P / 2 \dot { P } = 12.7 kyr .
The high spin-down power is consistent with the hard spectral indices of the pulsar and the nebula of 1.22 \pm 0.15 and 1.83 \pm 0.08 , respectively , and a 2–10 \mathrm { keV } flux ratio F _ { PWN } / F _ { PSR } \sim 8 .
Follow-up Parkes observations resulted in the detection of radio emission at 10 and 20 \mathrm { cm } from PSR J1400 - 6325 at a dispersion measure of \sim 560 cm ^ { -3 } pc , which implies a relatively large distance of 10 \pm 3 \mathrm { kpc } .
However , the resulting location off the Galactic Plane of \sim 280 \mathrm { pc } would be much larger than the typical thickness of the molecular disk , and we argue that G310.6 - 1.6 lies at a distance of \sim 7 \mathrm { kpc } .
There is no gamma-ray counterpart to the nebula or pulsar in the Fermi data published so far .
A multi-wavelength study of this new composite supernova remnant , from radio to very-high energy gamma-rays , suggests a young ( \lesssim 10 ^ { 3 } yr ) system , formed by a sub-energetic ( \lesssim 10 ^ { 50 } ergs ) , low ejecta mass ( M _ { ej } \sim 3 M _ { \odot } ) SN explosion that occurred in a low-density environment ( n _ { 0 } \sim 0.01 cm ^ { -3 } ) .