VERITAS: the Very Energetic Radiation Imaging Telescope Array System

Weekes, T. C.; Badran, H. M.; Biller, S. D.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.; Carter‐Lewis, D. A.; Catanese, M.; Criswell, S.; Cui, Wei; Dowkontt, P. F.; Duke, C.; Fegan, D. J.; Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gillanders, G. H.; Grindlay, Jonathan E.; Hall, T. A.; Harris, K.; Hillas, A. M.; Kaaret, P.; Kertzman, M.; Kieda, D.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Lessard, R. W.; Lloyd‐Evans, J.; Knapp, J.; McKernan, Barry; McEnery, J. E.; Moriarty, P.; Müller, D.; Ogden, P. A.; Ong, R. A.; Petry, D.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, J.; Salamon, M. H.; Sembroski, G. H.; Sidwell, R. A.; Slane, Patrick; Stanton, N. R.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.

doi:10.1016/s0927-6505(01)00152-9

Cited by 317 publications

(166 citation statements)

References 52 publications

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“…As with the gauge bosons, these SM fermions are taken to be massless, and for generality we say there are n D of them. 7 For the SM doublets, there is a crossed graph, while for the Majorana DM field, there is not, so…”

Section: Results Of the Calculationmentioning

confidence: 99%

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One-loop correction to heavy dark matter annihilation

et al. 2017

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We calculate the one-loop corrections to TeV-scale dark matter annihilation in a model where the dark matter is described by an SUð2Þ L triplet of Majorana fermions, such as the wino. We use this framework to determine the high-and low-scale MS matching coefficients at both the dark matter and weak boson mass scales at one loop. Part of this calculation has previously been performed in the literature numerically; we find our analytic result differs from the earlier work and discuss potential origins of this disagreement. Our result is used to extend the dark matter annihilation rate to next-to-leading logarithmic þ Oðα 2 Þ corrections (NLL 0 ), which enables a precise determination of indirect detection signatures in present and upcoming experiments.

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Section: Results Of the Calculationmentioning

confidence: 99%

“…Correcting this shortcoming is important for determining accurate theoretical predictions for existing and future indirect detection experiments focusing on the TeV mass range, such as H.E.S.S [1,2], HAWC [3][4][5], CTA [6], VERITAS [7][8][9], and MAGIC [10,11].…”

Section: Introductionmentioning

confidence: 99%

One-loop correction to heavy dark matter annihilation

et al. 2017

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“…The VERITAS gamma-ray detector (Weekes et al 2002) is an array of four 12 m diameter IACTs (Holder et al 2006) located at an altitude of ∼1250 m a.s.l. at the Fred Lawrence Whipple Observatory in southern Arizona (31…”

Section: Veritas Observations Analysis and Resultsmentioning

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

102

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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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“…The Very Energetic Radiation Imaging Telescope Array System (VERITAS; Weekes et al 2002) will complement and partially overlap with GLAST by observing in the energy range of 50 GeV -50 TeV. VERITAS enjoys greater flux sensitivity compared to Milagro.…”

Section: Answering the Questions: Observationsmentioning

confidence: 99%

Diffuse gamma rays from the Galactic Plane: Probing the “GeV excess” and identifying the “TeV excess”

Prodanovic

Fields

Beacom

2007

Astroparticle Physics

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Pion decay gamma rays have long been recognized as a unique signature of hadronic cosmic rays and their interactions with the interstellar medium. We present a model-independent way of constraining this signal with observations of the Galactic Plane in diffuse gamma rays. We combine detections by the EGRET instrument at GeV energies and the MilagroČerenkov detector at TeV energies with upper limits from KASCADE and CASA-MIA ground arrays at PeV energies. Such a long "lever arm", spanning at least six orders of magnitude in energy, reveals a "TeV excess" in the diffuse Galactic Plane gamma-ray spectrum. While the origin of this excess is unknown, it likely implies also enhanced TeV neutrino fluxes, significantly improving the prospects for their detection. We show that unresolved point sources are a possible source of the TeV excess. In fact, the spectra of the unidentified EGRET sources in the Milagro region must break between ∼ 10 GeV and ∼ 1 TeV to avoid strongly overshooting the Milagro measurement; this may have important implications for cosmic-ray acceleration.Finally, we use our approach to examine the recent suggestion that darkmatter annihilation may account for the observed excess in diffuse Galactic gamma-rays detected by EGRET at energies above 1 GeV. Within our modelindependent approach, current data cannot rule this possibility in or out; however we point out how a long "lever arm" can be used to constrain the pionic gammaray component and in turn limit the "GeV excess" and its possible sources. Experiments such as HESS and MAGIC, and the upcoming VERITAS and GLAST, should be able to finally disentangle the main sources of the Galactic gamma rays.

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VERITAS: the Very Energetic Radiation Imaging Telescope Array System

Cited by 317 publications

References 52 publications

One-loop correction to heavy dark matter annihilation

One-loop correction to heavy dark matter annihilation

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

Diffuse gamma rays from the Galactic Plane: Probing the “GeV excess” and identifying the “TeV excess”

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