2004
DOI: 10.1086/422469
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TeV Gamma-Ray Observations of the Galactic Center

Abstract: We report a possible detection of TeV gamma rays from the Galactic center by the Whipple 10 m gammaray telescope. Twenty-six hours of data were taken over an extended period from 1995 through 2003 resulting in a total significance of 3.7 j. The measured excess corresponds to an integral flux of Ϫ8 1.6 # 10 ‫ע‬ 0.5 # above an energy of 2.8 TeV, roughly 40% of the flux from the10 (stat) ‫ע‬ 0.3 # 10 (sys) photons m s Crab Nebula at this energy. The 95% confidence region has an angular extent of about 15Ј and inc… Show more

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Cited by 164 publications
(89 citation statements)
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“…Early H.E.S.S. observations of the GC region led to the detection of a point-like source of VHE γ-rays at the gravitational centre of the Galaxy (HESS J1745−290) [6], compatible with the positions of the supermassive black hole Sagittarius A ⋆ , the supernova remnant (SNR) Sgr A East, and a GC source reported by other groups [7,8]. A more sensitive exposure of the region in 2004 revealed a second source: the supernova remnant/pulsar wind nebula G 0.9+0.1 [9].…”
mentioning
confidence: 80%
“…Early H.E.S.S. observations of the GC region led to the detection of a point-like source of VHE γ-rays at the gravitational centre of the Galaxy (HESS J1745−290) [6], compatible with the positions of the supermassive black hole Sagittarius A ⋆ , the supernova remnant (SNR) Sgr A East, and a GC source reported by other groups [7,8]. A more sensitive exposure of the region in 2004 revealed a second source: the supernova remnant/pulsar wind nebula G 0.9+0.1 [9].…”
mentioning
confidence: 80%
“…The possibility that a steep, high density ρ∼ρ h (r/r h ) −α cusp of self-interacting dark matter particles could form under the dynamical influence of the MBH ( §3.1.3) was investigated in the hope that the enhanced particle annihilation rate (∝ ρ 2 ) could produce a detectable signal (Gondolo & Silk 1999; but see opposing conclusions by Merritt 2004b). The detection of strong TeV emission from the vicinity of Sgr A ⋆ (Kosack et al 2004;Aharonian et al 2004), further adds to the interest in this possibility. However, with a (very uncertain) normalization of only ρ h ∼ 100 M ⊙ pc −3 (Gnedin & Primack 2004), the mass in the dark matter particles is too small relative to the stellar cusp (Eq.…”
Section: Extended Dark Mass Around the Mbhmentioning
confidence: 93%
“…As already mentioned, about 80% of the cluster mass is in the form of DM, which makes galaxy clusters interesting targets for DM searches (Evans et al 2004;Bergström & Hooper 2006;Pinzke et al 2009;Cuesta et al 2011) despite their large distances compared to other common targets for DM searches, such as dwarf spheroidal galaxies (Strigari et al 2007;Acciari et al 2010;Aliu et al 2009) or the Galactic center (Kosack et al 2004;Aharonian et al 2006Aharonian et al , 2009aAbramowski et al 2011).…”
Section: Introductionmentioning
confidence: 99%