2009 Fermi Symposium, Washington, D.C., Nov. 2-5 4 TABLE I: Fluxes and Significance in High Energy Bands 50 - 100 keV 100 - 300 keV 300 - 500 keV Flux Error Signif. Flux Error Signif. Flux Error Signif. (mCrab) (mCrab) ( σ ) (mCrab) (mCrab) ( σ ) (mCrab) (mCrab) ( σ ) Crab 1000 3 336 1000 6 182 1000 47 21.2 Cen A 72 4 18 108 7 15 42 47 0.9 Cyg X-1 1130 4 283 1094 8 137 474 50 9.5 GRS 1915+105 121 4 30 49 7 7 41 52 0.8 1E 1740-29 113 5 23 96 10 10 97 68 1.4 SWIFT 1753.5-0127 135 5 27 151 9 17 131 64 2.0 XTE J1752-223 770 16 48 622 30 21 132 218 0.6 source while it is in the hard state, with longer obser- vations potentially verifying significant emission above 300 keV. will use the GBM CSPEC data with their finer energy bins to obtain a fit to the spectrum and compare the power law index to that measured by Integral. FIG. 7: SWIFTJ1753.5-0127 light curve. Horizontal scale is in modified Julian days. FIG. 6: 1E1740-29 light curve. Horizontal scale is in mod- ified Julian days. The new transient black hole candidate XTE J1752-223 rose from undetectable on 2009 October 24 to 511 ± 50 mCrab (12 - 25 keV), 570 ± 70 mCrab (25 - 50 keV), 970 ± 100 mCrab (50 - 100 keV), and 330 ± 100 mCrab (100 - 300 keV) on 2009 November 2 [2, 16]. The light curve is variable, especially in the SWIFT J1753.5-0127 (Fig. 7) is a LMXB with the compact object likely being a black hole. Swift discovered this source when it observed a large flare in July of 2005. The source did not return to qui- escence but settled into a low intensity hard state [14]. BATSE occultation measurements from 1991- 2000 showed no significant emission from this source above 25 keV [15]. The GBM results show that this source is still in a hard state, with significant emis- sion above 100 keV. We will continue to monitor this B. Transient Source eConf C091122