A deep search for pulsar wind nebulae using pulsar gating

Using the Australia Telescope Compact Array (ATCA) we have imaged the fields around five promising pulsar candidates to search for radio pulsar wind nebulae (PWNe). We have used the ATCA in its pulsar gating mode; this enables an image to be formed containing only off-pulse visibilities, thereby dramatically improving the sensitivity to any underlying PWN. Data from the Molonglo Observatory Synthesis Telescope were also used to provide sensitivity on larger spatial scales. This survey found a faint new PWN around PSR B0906-49; here we report on non-detections of PWNe towards PSRs B1046-58, B1055-52, B1610-50 and J1105-6107. Our radio observations of the field around PSR B1055-52 argue against previous claims of an extended X-ray and radio PWNe associated with the pulsar. If these pulsars power unseen, compact radio PWN, upper limits on the radio flux indicate that less than 1e-6 of their spin-down energy is used to power this emission. Alternatively PSR B1046-58 and PSR B1610-50 may have relativistic winds similar to other young pulsars and the unseen PWN is resolved and fainter than our surface brightness sensitivity threshold. We can then determine upper limits on the local ISM density of 2.2e-3 cm^-3 and 1e-2 cm^-3, respectively. Furthermore we constrain the spatial velocities of these pulsars to be less than ~450 km/s and thus rule out the association of PSR B1610-50 with SNR G332.4+00.1 (Kes 32). Strong limits on the ratio of unpulsed to pulsed emission are also determined for three pulsars.Comment: 10 pages, 5 figures, MNRAS in pres

X-Ray Timing, Spectroscopy and Photometry of the Anomalous X-Ray Pulsar Candidate CXOU J010043.1-721134

We present new X-ray timing and spectral results on the 8.0-second X-ray pulsar CXOU J010043.1-721134 from a series of observations using the Chandra X-ray Observatory. We find a spin period in 2004 January of 8.020392pm0.000009 seconds. Comparison of this to 2001 Chandra observations implies a period derivative dot{P} = (1.88 pm 0.08) times 10^{-11} s s^{-1}, leading to an inferred dipole surface magnetic field of 3.9 times 10^{14} G. The spectrum is well fit to an absorbed blackbody of temperature kT = 0.38pm0.02 keV with a power law tail of photon index Gamma = 2.0pm0.6. We find that the source has an unabsorbed X-ray flux (0.5-10 keV) of 4(+2-1) times 10^{-13} erg cm^{-2} s^{-1} and a corresponding X-ray luminosity of ~2 times 10^{35} erg s^{-1} for a distance of 60 kpc. These properties support classification of CXOU J010043.1-721134 as the seventh confirmed anomalous X-ray pulsar,the eleventh confirmed magnetar, and the first magnetar to be identified in the Small Magellanic Cloud.Comment: 5 pages, plus 1 embedded eps figure. Refined coordinates of source, including typo in declination. ApJ Letters, in pres