5 12-25 keV band, where the flux initially rose to about 240 mCrab (2009 Oct 25-28), suddenly dropped to non-detectable on 2009 October 29-30, then rose again during the period 2009 October 31 to November 2. As of mid December 2009, the source remains in a high intensity state. The light curve is shown for the pe- riod MJD 54700-55200, again with 1-day resolution, in Fig. 8. The fluxes for XTE J1752-223 in Table 1 are given are for the interval of flaring activity, TJD 55130-55180. 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 Acknowledgments This work is supported by the NASA Fermi Guest Investigator program. At LSU, additional support is provided by NASA/Louisiana Board of Regents Co- operative Agreement NNX07AT62A. FIG. 8: XTEJ1752-223 light curve. Horizontal scale is in modified Julian days. [1] C. Meegan et al., Ap. J. 702 , 791 (2009). [2] C. Wilson-Hodge et al. (2010), these proceedings. [3] B. A. Harmon et al., Ap. J. Suppl. 138 , 149 (2002). [4] B. A. Harmon et al., Ap. J. Suppl. 154 , 585 (2004). [5] G. L. Case et al., in The First GLAST Symposium , edited by S. Ritz, P. Michelson, and C. Meegan (2007), vol. 921 of AIP Conf. Proceedings , p. 538. [6] J. Tueller et al. (2010), ap. J. Suppl., (to be pub- lished), astro-ph/0903.3037. [7] J. C. Ling and W. A. Wheaton, Ap. J. 598 , 334 (2003). [8] E. Jourdain and J. P. Roques, Ap. J. 704 , 17 (2009). [9] H. Steinle et al., Astron. and Astrophys. 330 , 97 [16] C. Wilson-Hodge et al., Astron. Telegram 2280 (2009). [15] G. L. Case et al. (2010), to be submitted. [14] M. C. Bell et al., Ap. J. 659 , 549 (2007). [13] L. Bouchet et al., Ap. J. 693 , 1871 (2009). [12] G. L. Case et al., Chinese J. Astron. Astrophys. Suppl. 5 , 341 (2005). [11] J. C. Ling and W. A. Wheaton, Chinese J. Astron. Astrophys. Suppl. 5 , 80 (2005). [10] M. McConnell et al., Ap. J. 523 , 928 (2000). (1998). eConf C091122