2001/12/06 by V. M. Kaspi, E. V. Gotthelf, Kaspi, V. M. +5
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0112165
4 pages, incl 2 figures; To appear in "Neutron Stars in Supernova Remnants" (ASP Conference Proceedings), eds P. O. Slane and B. M. Gaensler
arxiv created 2001/12/06 · arxiv updated 2009/12/01
We report the first X-ray detection of the radio pulsar PSR B1757-24 using the Chandra X-ray Observatory. The image reveals point-source emission at the pulsar position, consistent with being magnetospheric emission from the pulsar. In addition, we detect a faint tail extending nearly 20" east of the pulsar, in the same direction and with comparable morphology to the pulsar's well-studied radio tail. The X-ray tail is unlikely to be emission left behind following the passage of the pulsar, but rather is probably from synchrotron-emitting pulsar wind particles having flow velocity ~7000 km/s. Assuming the point-source X-ray emission is magnetospheric, the observed X-ray tail represents only ~0.01% of the pulsar's spin-down luminosity, significantly lower than the analogous efficiencies of most known X-ray nebulae surrounding rotation-powered pulsars.