Finding the Needle in G18.95-1.1

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Utilizing the Chandra X-ray Observatory, we have pinpointed the location of a faint X-ray point source and an associated diffuse nebula in the composite supernova remnant G18.95-1.1. These objects appear to be the long-sought pulsar and its wind nebula. The X-ray spectrum of the pulsar is best described by an absorbed powerlaw model with Gamma=1.73 and an NH of about 6x1021cm-2. This model predicts a relatively low unabsorbed X-ray luminosity of about Lx=1.1x1031erg/s in the 0.35-8.0keV energy band and 54% of Lx is emitted above 2keV. The spectral characteristics of the pulsar wind nebula are very similar to the pulsar and agree within the uncertainties of the models. Based on a powerlaw model with Gamma=1.66 and an NH of 5x1021cm-2, the X-ray luminosity amounts to 2x1031erg/s with almost an identical fraction of Lx being emitted above 2keV. No radio or X-ray pulsations have been reported for CXO J182913.1-125113 which we associate with the pulsar. If we assume an age of about 4400-6100yr for G18.95-1.1 and use the observed X-ray luminosity for the pulsar and the relationship between spin-down luminosity and period, we expect the pulsar to have a period of 3.1s. Compared to other rotation-powered pulsars, a magnetic field of 2x1014G is implied by its location in the P-Pdot diagram, a value which is well above that of the quantum critical field.

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