We present preliminary results from a Chandra 30 ks observation of the atoll source 4U 1705-44. In particular we concentrate on the study of discrete features in the energy spectrum at energies below similar to 3 keV, as well as the iron Kalpha line, using the HEG spectrometer on board of the Chandra satellite. The iron Ka line at similar to 6.6 keV is found to be intrinsically broad (FWHM similar to 1.7 keV); its width can be explained by reflection from a cold accretion disk extending down to similar to 17 km from the neutron star center or by broadening in the hotter (similar to 3 - 4 keV) Comptonizing corona.
A broad iron line in the Chandra/HETG spectrum of 4U 1705-44
BURDERI, LUCIANO;
2004-01-01
Abstract
We present preliminary results from a Chandra 30 ks observation of the atoll source 4U 1705-44. In particular we concentrate on the study of discrete features in the energy spectrum at energies below similar to 3 keV, as well as the iron Kalpha line, using the HEG spectrometer on board of the Chandra satellite. The iron Ka line at similar to 6.6 keV is found to be intrinsically broad (FWHM similar to 1.7 keV); its width can be explained by reflection from a cold accretion disk extending down to similar to 17 km from the neutron star center or by broadening in the hotter (similar to 3 - 4 keV) Comptonizing corona.
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