Is the Compact Source at the Center of Cassiopeia A Pulsed?

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Abstract
A 50 ks observation of the supernova remnant Cas A was taken, using the Chandra X-Ray Observatory High-Resolution Camera (HRC) to search for periodic signals from the compact source located near the center. Using the HRC-S in imaging mode, problems with correctly assigning times to events were overcome, allowing the period search to be extended to higher frequencies than possible with previous observations. In an extensive analysis of the HRC data, several possible candidate signals are found using various algorithms, including advanced techniques recently developed by Ransom to search for low-significance periodic signals. Of these possible periods, none is at a high enough confidence level to be particularly favored over the rest. When combined with other information, however (e.g., spectra, total energetics, and the historical age of the remnant), a 12 ms period seems to be more physically plausible than the others, and we use it for illustrative purposes in discussing the possible properties of a putative neutron star in the remnant. We emphasize that this is not necessarily the true period, and that a follow-up observation, scheduled for the fall of 2001, is required. A 50 ks Advanced CCD Imaging Spectrometer (ACIS) observation was taken, and analysis of these data for the central object shows that the spectrum is consistent with several forms and that the emitted X-ray luminosity in the 0.1-10 keV band is 1033-1035 ergs cm-2 s-1, depending on the spectral model and the interstellar absorption along the line of sight to the source. The spectral results are consistent with those of Pavlov et al. and Chakrabarty et al.
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