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Y.C. Lin, B.B. Jones, P.F. Michelson, P.L. Nolan, W.F. Tompkins (Stanford), D.L. Bertsch, J.A. Esposito, R.C. Hartman, S.D. Hunter, P. Sreekumar, D.J. Thompson (NASA/GSFC), G. Kanbach, H.A. Mayer-Hasselwander, O.L. Reimer (MPE), D.A. Kniffen (Hampden-Sydney), E.J. Schneid (Northrop-Grumman), B.L. Dingus (Univ. of Utah), R. Mukherjee (Barnard \& Columbua), M.K. Pohl (Ruhr-Univ.), A. M\"ucke (Adelaide), S.D. Bloom (Cal Tech/IPAC), EGRET Team
In current theoretical models of the blazar subclass of active galaxies, the broadband emission consists of two components: a low frequency synchrotron component with an SED peak in the IR to X-ray band, and a high frequency inverse Compton component with a peak in the gamma-ray band. In such models, the gamma-ray spectral index should be correlated with the location of the low-energy peak, with flatter gamma-ray spectra expected for blazars with synchrotron peaks at higher photon energies. Using the EGRET-detected blazars as a sample, we examine this correlation and possible uncertainties in its construction.