-------------------------------------------------------------------------------- Compton Observatory ***************** BATSE Bright Source Report ***************** (Earth Occultation Monitoring) -------------------------------------------------------------------------------- Data for: Jan. 13, 1997 thru Jan. 16, 1997 TJD 10461-10464 Source TJD Flux Spectral Signif** Comments (ph/cm^2 sec, Index* 20-100 keV) (20-100 keV) CRAB 10461 0.31 -2.2 78.8 10462 0.32 77.0 10463 0.31 74.1 10464 0.32 68.8 CYGX-1 10461 0.28 -2.0 36.6 10462 0.33 34.7 10463 0.30 43.0 10464 0.29 30.1 GROJ1744-28 10461 0.44 -4.2 22.7 10462 0.48 17.4 10463 0.41 27.1 10464 0.48 29.2 GX301-2 10461 0.20 -4.4 15.7 10462 0.13 9.5 10463 0.14 8.6 GRS1915+105 10461 0.13 -2.8 11.7 Possible source 10463 0.10 6.8 confusion 10464 0.14 14.7 SCOX-1 10461 0.19 -5.0 10.0 10462 0.18 9.9 10463 0.16 8.3 10464 0.19 13.0 HERX-1 10461 0.10 -4.4 8.3 10462 0.08 6.8 10463 0.15 12.3 10464 0.09 6.8 4U1700-377 10461 0.10 -3.0 6.2 10464 0.26 22.9 VELAX-1 10461 0.05 -3.7 5.7 10462 0.09 9.8 CEN_A 10463 0.02 -1.9 3.5 NGC4151 10463 0.01 -2.0 3.4 10464 0.01 3.8 CENX-3 10464 0.06 -4.5 4.9 GX339-4 10464 0.06 -2.4 4.9 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 data are of a preliminary nature and should only be used for planning observational programs, and are not intended for publication. Please do not distribute this report beyond your local team. For additional information, contact B. A. Harmon (harmon@ssl.msfc.nasa.gov).