-------------------------------------------------------------------------------- Compton Observatory ***************** BATSE Bright Source Report ***************** (Earth Occultation Monitoring) -------------------------------------------------------------------------------- Data for: Apr. 18, 1997 thru Apr. 21, 1997 TJD 10556-10559 Source TJD Flux Spectral Signif** Comments (ph/cm^2 sec, Index* 20-100 keV) (20-100 keV) CRAB 10556 0.34 -2.2 84.9 10557 0.33 71.2 10558 0.32 77.3 10559 0.34 83.0 CYGX-1 10556 0.32 -2.0 76.5 10557 0.27 53.4 10558 0.33 79.4 10559 0.36 80.9 SCOX-1 10556 0.28 -5.0 16.9 10557 0.28 20.2 10558 0.19 15.4 10559 0.14 11.5 GRS1915+105 10556 0.10 -2.8 16.3 10557 0.10 15.8 10558 0.13 22.8 10559 0.12 17.4 GX339-4 10556 0.07 -2.4 10.7 10557 0.06 8.1 10558 0.07 12.6 10559 0.07 6.5 VELAX-1 10556 0.08 -3.7 7.1 10557 0.16 15.4 10558 0.10 8.7 10559 0.11 8.0 4U1700-377 10556 0.05 -3.0 6.0 10557 0.14 17.2 10559 0.05 4.5 GRS1758-258 10556 0.03 -2.0 5.4 10557 0.02 4.1 10558 0.02 5.0 10559 0.02 4.5 NGC4151 10556 0.02 -2.0 5.3 10557 0.02 4.6 1E1740-29 10556 0.07 -2.5 5.1 10557 0.03 3.0 10558 0.04 4.0 10559 0.05 4.8 OAO1657-415 10556 0.05 -3.4 5.0 10558 0.05 5.0 10559 0.09 7.1 CYGX-3 10559 0.06 -3.3 5.7 CEN_A 10559 0.01 -1.9 3.3 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).