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Perkins, JS and Badran, HM and Blaylock, G and Bradbury, SM and Cogan, P and Chow, YCK and Cui, W and Daniel, MK and Falcone, AD and Fegan, SJ and Finley, JP and Fortin, P and Fortson, LF and Gillanders, GH and Gutierrez, KJ and Grube, J and Hall, J and Hanna, D and Holder, J and Horan, D and Hughes, SB and Humensky, TB and Kenny, GE and Kertzman, M and Kieda, DB and Kildea, J and Kosack, K and Krawczynski, H and Krennrich, F and Lang, MJ and LeBohec, S and Maier, G and Moriarty, P and Ong, RA and Pohl, M and Ragan, K and Rebillot, PF and Sembroski, GH and Steele, D and Swordy, SP and Valcarcel, L and Vassiliev, VV and Wakely, SP and Weekes, TC and Williams, DA and VERITAS Collaboration
TeV gamma-ray observations of the Perseus and Abell 2029 galaxy clusters
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Galaxy clusters might be sources of TeV gamma rays emitted by high-energy protons and electrons accelerated by large-scale structure formation shocks, galactic winds, or active galactic nuclei. Furthermore, gamma rays may be produced in dark matter particle annihilation processes at the cluster cores. We report on observations of the galaxy clusters Perseus and A2029 using the 10 m Whipple Cerenkov telescope during the 2003-2004 and 2004-2005 observing seasons. We apply a two-dimensional analysis technique to scrutinize the clusters for TeV emission. In this paper we first determine flux upper limits on TeVgamma- ray emission from point sources within the clusters. Second, we derive upper limits on the extended cluster emission. We subsequently compare the flux upper limits with EGRET upper limits at 100 MeV and theoretical models. Assuming that the gamma-ray surface brightness profile mimics that of the thermal X-ray emission and that the spectrum of cluster cosmic rays extends all the way from thermal energies to multi-TeV energies with a differential spectral index of similar to 2.1, our results imply that the cosmic-ray proton energy density is less than 7.9\% of the thermal energy density for the Perseus Cluster.
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