Craig Markwardt writes: This is a summary of the galactic bulge observation on 10 Feb 2000 (day 2231). The scan pattern was primarily in the east-west direction. There are a few interesting things to report, and I apologize for the length of this message. * SAX J1808-368 has faded considerably. I had heard reports from the pointed observations that the source had "gone." In truth the source is there but very weak - about 5 ct/s/5PCU (2-10 keV) above baseline (0.5 mCrab), or around ten sigma. It is not clear whether this was the end of a strong outburst which occurred while the source was behind the sun, or some smaller non-outburst level of activity. * We observed two probable bursts (!). Sharp outbursts are clearly distinguishable from a point source because we almost always cover the same source in multiple scans. When a source is bright in one scan but not the others, then that's pretty strong evidence for a phenomenon lasting less than a few hundred seconds. From there I can do some profile fitting, and sometimes get a rough exponential decay, etc. * One burst is probably from EXO 1722-363, seen near time 192824450 MET (10 Feb 2000 18:20 UT). An extended decay could be seen, which I was able to model with an exponential with folding time ~50 s. It is difficult to pinpoint the onset of the burst, but if it is 192824430, then the peak flux was near 167 ct/s (17 mCrab) - not huge! * Another burst is probably from GRS 1747-312, seen near time 192826450 (10 Feb 2000 18:54 UT). This is potentially significant since no bursts have been seen from this source to date. I can say that the position fit to GRS 1747-312 is very good, of much better quality than that of the nearby SLX 1744-300, from which we have seen bursts in the past. There is however no evidence that either the SLX or GRS source has stronger-than-baseline persistent flux, and thus no strong evidence of enhanced accretion in either. No time evolution model appears to be required, so I modelled it as a constant of about 380 ct/s (38 mCrab). * The faintness of these fluxes is worth pondering. Even at the galactic center these fluxes imply luminosities smaller than Eddington by a factor of ~100. However, we need to consider that we probably did not catch the onset of the burst in either case, which could have occurred 100-200 sec earlier, so I don't there are any terrible problems. * XTE J1710-281 has become detectable again, at a ~typical flux level of 2 mCrab. This is welcome, as I had feared that it had disappeared for good. Craig