------------------------------------------------------------------------------- Compton Observatory ***************** BATSE Bright Source Report ***************** (Earth Occultation Monitoring) ------------------------------------------------------------------------------- Data for: Jul. 17, 1997 thru Jul. 20, 1997 TJD 10646-10649 Source TJD Flux Spectral Signif** Comments (ph/cm^2 sec, Index* 20-100 keV) (20-100 keV) CYGX-1 10646 0.36 -2.0 91.3 10647 0.31 70.3 10648 0.29 78.4 10649 0.30 75.2 CRAB 10646 0.32 -2.2 74.0 10647 0.33 61.5 10648 0.33 77.1 10649 0.32 68.3 SCOX-1 10646 0.23 -5.0 16.3 10647 0.26 18.8 10648 0.15 9.0 10649 0.14 7.5 1E1740-29 10646 0.08 -2.5 13.8 10647 0.09 14.5 10648 0.08 12.0 10649 0.07 11.3 VELAX-1 10646 0.18 -3.7 11.9 10647 0.10 6.6 10648 0.08 5.9 10649 0.08 5.9 4U1700-377 10646 0.09 -3.0 9.5 10648 0.11 12.1 10649 0.08 8.4 GX1+4 10646 0.06 -3.0 8.0 10647 0.05 5.4 10648 0.06 5.5 10649 0.05 3.3 GX339-4 10646 0.05 -2.4 7.5 10647 0.05 5.1 10648 0.06 5.1 10649 0.03 4.1 GRS1915+105 10646 0.04 -2.8 6.9 10648 0.03 5.5 NGC4151 10646 0.02 -2.0 5.1 10649 0.01 3.1 CYGX-3 10646 0.05 -3.3 4.5 10647 0.05 4.9 10648 0.06 6.8 10649 0.07 7.5 OAO1657-415 10646 0.05 -3.4 3.2 CEN_A 10646 0.01 -1.9 3.1 10648 0.02 3.9 GX301-2 10648 0.04 -4.4 3.6 10649 0.06 4.7 Notes: * Spectral index for power law fit to photon number spectrum (photons/cm^2-s) in 20-100 keV band **Detection Significance, = Flux/Sigma ------------------------------------------------------------------------------- The information given above comes from the quick-look analysis performed daily on data obtained from the Burst and Transient Source Experiment (BATSE). The typical sensitivity of these measurements using the Earth occultation technique (one-day integration) is ~100 mCrab. Be aware that sources within about 22 degrees of the orbital poles are not occulted by the Earth; therefore, some bright sources may not show up in the daily averages. These quick-look science results are freely available, but should be considered preliminary. Please use with caution. For additional information, contact B.A. Harmon (harmon@sslmor.msfc.nasa.gov).