On March 20, 1969, we scanned the Southern sky for 8 hours in a manner similar to that during our October 15, 1967 observations. A quick look at the data shows clearly that the brightness of Cen XR-2 in the energy range above 20 keV has significantly decreased since our first observation. At this stage of the data analysis we can put an upper limit on the intensity of Cen XR-2 which is 1/3 the intensity observed by us on October 15, 1967. From further data analyses we will be able to determine the intensity of the source more precisely.
During the same flight we observed Sco X-l, Nor XR-2, and the sources M-l, M-2, M-3, and M-4. Results on these observations will become available by May 1970.