-------------------------------------------------------------------------------- Compton Observatory ***************** BATSE Bright Source Report ***************** (Earth Occultation Monitoring) -------------------------------------------------------------------------------- Data for: Jan. 25, 1998 thru Jan. 28, 1998 TJD 10838-10841 Source TJD Flux Spectral Signif** Comments (ph/cm^2 sec, Index* 20-100 keV) (20-100 keV) CRAB 10838 0.31 -2.2 66.6 10839 0.32 74.2 10840 0.32 72.0 10841 0.32 66.1 CYGX-1 10838 0.19 -2.0 12.7 10839 0.26 36.5 10840 0.24 20.7 10841 0.24 57.4 VELAX-1 10838 0.38 -3.7 36.4 very large 10839 0.03 2.9 outburst 10841 0.04 3.9 SCOX-1 10838 0.22 -5.0 14.7 10839 0.22 16.0 10840 0.17 13.4 10841 0.11 9.1 1E1740-29 10838 0.10 -2.5 10.7 10839 0.05 4.3 10840 0.07 8.6 10841 0.07 9.0 GRS1915+105 10838 0.10 -2.8 10.6 10839 0.08 8.9 10840 0.12 15.5 10841 0.08 8.8 3C273 10838 0.02 -1.6 7.7 GRS1758-258 10838 0.05 -2.0 6.0 10839 0.04 3.3 10841 0.05 4.3 4U1700-377 10839 0.21 -3.0 14.2 10840 0.21 9.5 10841 0.08 6.9 OAO1657-415 10839 0.09 -3.4 5.1 NGC4151 10839 0.02 -2.0 4.1 10840 0.01 3.3 10841 0.01 2.4 CYGX-3 10840 0.05 -3.3 3.8 10841 0.03 3.2 GX1+4 10841 0.03 -3.0 3.1 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).