TeV Gamma-Ray Observations of the Galactic Center

Kosack, K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter‐Lewis, D. A.; Çelik, Ö.; Connaughton, V.; Cui, Wei; Daniel, M. K.; D'Vali, M.; Pérez, I. de la Calle; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Gutierrez, K.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D. B.; Kildea, J.; Knapp, J.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Bohec, S. Le; Linton, E.; Lloyd‐Evans, J.; Milovanovic, A.; McEnery, J. E.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S. J.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.

doi:10.1086/422469

Cited by 164 publications

(89 citation statements)

References 25 publications

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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%

Discovery of very-high-energy γ-rays from the Galactic Centre ridge

Aharonian

Akhperjanian

Bazer‐Bachi

et al. 2006

Nature

488

506

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mentioning

confidence: 80%

Discovery of very-high-energy γ-rays from the Galactic Centre ridge

Aharonian

Akhperjanian

Bazer‐Bachi

et al. 2006

Nature

488

506

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“…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%

Stellar processes near the massive black hole in the Galactic center

2005

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“…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%

CONSTRAINTS ON COSMIC RAYS, MAGNETIC FIELDS, AND DARK MATTER FROM GAMMA-RAY OBSERVATIONS OF THE COMA CLUSTER OF GALAXIES WITH VERITAS ANDFERMI

Arlen

Aune

Beilicke

et al. 2012

ApJ

Self Cite

103

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Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated and, on account of weak energy losses, can accumulate, suggesting that clusters may also be sources of very high energy (VHE; E > 100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cerenkov telescopes, with complementing Fermi Large Area Telescope observations at GeV energies. No significant gamma-ray emission from the Coma Cluster was detected. Integral flux upper limits at the 99% confidence level were measured to be on the order of (2-5) × 10 −8 photons m −2 s −1 (VERITAS, >220 GeV) and ∼2 × 10 −6 photons m −2 s −1 (Fermi, 1-3 GeV), respectively. We use the gamma-ray upper limits to constrain cosmic rays (CRs) and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be <16% from VERITAS data and <1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be <50%. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Assuming that the radio-emitting electrons of the Coma halo result from hadronic CR interactions, the observations imply a lower limit on the central magnetic field in Coma of ∼(2-5.5) μG, depending on the radial magnetic field profile and on the gamma-ray spectral index. Since these values are below those inferred by Faraday rotation measurements in Coma (for most of the parameter space), this renders the hadronic model a very plausible explanation of the Coma radio halo. are dark matter (DM) dominated, the VERITAS upper limits have been used to place constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the DM particles, σ v .

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TeV Gamma-Ray Observations of the Galactic Center

Cited by 164 publications

References 25 publications

Discovery of very-high-energy γ-rays from the Galactic Centre ridge

Discovery of very-high-energy γ-rays from the Galactic Centre ridge

Stellar processes near the massive black hole in the Galactic center

CONSTRAINTS ON COSMIC RAYS, MAGNETIC FIELDS, AND DARK MATTER FROM GAMMA-RAY OBSERVATIONS OF THE COMA CLUSTER OF GALAXIES WITH VERITAS ANDFERMI

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