1. -Sachindra Naik, Biswajit Paul, and Zulfikar Ali

3. Light curves & other info The XIS detectors cover the 0.2-12 keV range and the HXD/PIN detectors cover 10-70 keV. The end of one eclipse is seen at about 0-50 ks; the beginning of another comes at about 150 ks. These eclipses and other features are present in the data up to about 40 keV; at higher energies, on the other hand, the graph becomes essentially featureless. The graph obviously has many features other than the eclipses at the ends; besides these two, it contains three dips, four egresses, five ingresses, six high-count regions, and two bumps that have different exposure times and count rates.

6.  The X-ray light curve of the system shows a lot of variation  presence of dips.  The dips are due to the presence of dense matter that absorbs the X-ray photons.  Partial covering absorption model  Problem: Iron emission lines

7.  Naik, S., Paul, B., & Ali, Z. (2011). X-RAY SPECTROSCOPY OF THE HIGH-MASS X- RAY BINARY PULSAR CENTAURUS X-3 OVER ITS BINARY ORBIT. The Astrophysical Journal, 737 (79), 1-8.