3 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 FIG. 4: Cyg X-1 light curve. Horizontal scale is in modi- fied Julian days. FIG. 3: Cen A light curve. Horizontal scale is in modified Julian days. to observe these breaks, GBM is able to see significant emission above 300 keV, consistent with the canonical hard spectrum. Cen A (Fig. 3) is a Sy 2 galaxy that is the brightest AGN in hard x-rays/low energy gamma rays. It has a hard spectrum (Γ = 1 . 8) and has been observed at energies > 1 MeV [9]. The GBM results are consis- tent with this hard spectrum, though GBM does not have the sensitivity to determine if the hard spectrum continues beyond 300 keV or if the spectrum cuts off. Cyg X-1 (Fig. 4) is a HMXB and one of the first systems determined to contain a black hole. It has been observed to emit significant emission above 100 keV including a power law tail extending out to greater than 1 MeV [10, 11]. The GBM results show significant emission above 300 keV, consistent with the power law tail observed when Cyg X-1 is in its hard state. GRS 1915+105 (Fig. 5) is a LMXB with the com- pact object being a massive black hole. Evidence for emission above 100 keV has been seen previously [12] with BATSE. The GBM light curve integrated over 490 days shows significant emission above 100 keV. 1E 1740-29 (Fig. 6) is a LMXB very near the Galactic Center. It is a microquasar, and spends most of its time in the low/hard state. Integral observa- tions indicate the presence of a power law tail above 200 keV [13]. The present GBM results are consis- tent with this high energy emission. In the future, we eConf C091122 FIG. 5: GRS 1915+105 light curve. Horizontal scale is in modified Julian days.