-------------------------------------------------------------------------------- Compton Observatory ***************** BATSE Bright Source Report ***************** (Earth Occultation Monitoring) -------------------------------------------------------------------------------- Data for: Oct. 19, 1997 thru Oct. 22, 1997 TJD 10740-10743 Source TJD Flux Spectral Signif** Comments (ph/cm^2 sec, Index* 20-100 keV) (20-100 keV) CYGX-1 10740 0.33 -2.0 89.2 10741 0.36 103.4 10742 0.36 99.8 10743 0.31 84.4 CRAB 10740 0.31 -2.2 79.0 10741 0.31 79.3 10742 0.31 76.4 10743 0.32 78.7 1E1740-29 10740 0.08 -2.5 13.0 Possible source 10741 0.07 9.1 interference 10742 0.06 8.8 10743 0.04 5.0 SCOX-1 10740 0.21 -5.0 13.0 10741 0.16 8.6 10742 0.17 11.1 10743 0.23 13.0 4U1700-377 10740 0.09 -3.0 11.2 GRS1915+105 10740 0.09 -2.8 10.6 10741 0.06 5.9 10742 0.07 7.7 10743 0.10 9.5 GX339-4 10740 0.07 -2.4 9.8 10741 0.06 8.4 10742 0.07 10.7 10743 0.08 6.4 VELAX-1 10740 0.14 -3.7 8.6 10743 0.07 3.4 HERX-1 10740 0.10 -4.4 7.3 10741 0.07 5.1 10743 0.07 3.5 GRS1758-258 10740 0.05 -2.0 5.6 Possible source 10741 0.03 5.1 interference 10742 0.03 5.4 10743 0.03 4.3 CYGX-3 10740 0.03 -3.3 3.9 10741 0.04 3.4 10743 0.11 3.7 CEN_A 10741 0.02 -1.9 4.5 10742 0.02 4.6 NGC4151 10742 0.02 -2.0 3.8 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).