予稿集 - 天文・天体物理若手の会

Z T.Tanimori et al. New Astronomy Reviews 48 (2004)263 (1983)G.F.Knoll 3 (2001)----C. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .08a 7 29 15:45 CANGAROO-III ANGAROO TeV 10m 3 S/N I. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .09a 7 29 16:00 IceCube ceCube 1 10 20 eV 10 (EHE) GZKGZK IceCube (PMT) http://icecube.wisc.edu/. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .01cW The Blazar Sequence and The CosmicGamma-ray Background Radiatione present a study of the blazar gamma-ray luminosityfunction (GLF) and their contributionto extragalactic gamma-ray background (EGRB) radiationbased on the unified blazar spectral energy distribution(SED) sequence. Previously power-law SEDmodels are simply assumed to construct GLF and calculateEGRB spectrum. The blazar SED, however, hasa unique sequence feature that synchrotron and Comptonpeak energy increase as the bolometric luminositydecreases. Using such SED sequence, we reconstructthe blazar GLF with the luminosity dependent densityevolution model, which is favored by the X-ray luminosityfunction of active galactic nuclei (AGNs). We thenfind that 50% - 70% of the EGRB spectrum above 100MeV can be explained by blazars. Furthermore, the originof cosmic MeV gamma-ray background has recentlybeen explained by Seyfert class of AGNs, which composethe cosmic X-ray background, with the expectednon-thermal tail in AGN spectrum model. From theseresults, we also find that the cosmic X-ray to gammaraybackground up to 1 GeV will be explained by theemission from Seyfert and blazar type of AGNs. Predictionsfor GLAST mission are also made, and we findthat GLAST will reveal about 2000-5000 blazars in thesky.Donato, D., Ghisellini, G., Tagliaferri, G., & Fossati, G.2001, A&A, 375, 739Inoue Y., Totani T., Ueda Y., 2008, ApJ 672, L5Narumoto T., Totani T., 2006, ApJ 643, 81. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38 | 49