A NEW METHOD TO RESOLVE X-RAY HALOS AROUND POINT SOURCES WITH CHANDRA DATA AND ITS APPLICATION TO CYGNUS X-1

摘要

With excellent angular resolution, good energy resolution, and a broad energy band, the Chandra Advanced CCD Imaging Spectrometer (ACIS) is the best instrument for studying the X-ray halos around some Galactic X-ray point sources caused by the dust scattering of X-rays in the interstellar medium. However, the direct images of bright sources obtained with the ACIS usually suffer from severe pileup. Making use of the fact that an isotropic image could be reconstructed from its projection into any direction, we can reconstruct the images of the X-ray halos from the data obtained with the High Energy Transition Grating Spectrometer (HETGS) and/or in continuos clocking (CC) mode. These data have no or less serious pileup and enable us to take full advantage of the excellent angular resolution of Chandra. With the reconstructed high-resolution images, we can probe the X-ray halos as close as 1″ to their associated point sources. Applying this method to Cygnus X-1 observed with the Chandra HETGS in CC mode, we derived an energy-dependent radial halo flux distribution and concluded that in a circular region (2′ in radius) centered at the point source: (1) relative to the total intensity, the fractional halo intensity is about 15% at ～1 keV and drops to about 5% at ～6 keV; (2) about 50% of the halo photons are within the region of a radius less than 40″; and (3) the spectrum of the point source is slightly distorted by the halo contamination.