The status of the HESS project

By J. Hinton. 2004

323 citations recorded by the source corpus.

Abstract The High Energy Stereoscopic System (HESS) is a system of four, 107 m2 mirror area, imaging Cherenkov telescopes under construction in the Khomas Highland of Namibia (1800 m asl). The HESS system is characterised by a low threshold (∼100 GeV) and a ∼1% Crab flux sensitivity resulting from the good angular resolution and background rejection provided by the stereoscopic technique. The first two telescopes are operational and first results are reported here. The remaining two telescopes (of HESS Phase-I) will be commissioned early in 2004.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/120c50d5210f819b76a40cc074e6c3d510f625cf

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Citations in the corpus

Quantum-Spacetime Phenomenology (2008, background): “In particular, studies of TeV flares from Mk 501 and PKS 2155–304 performed by the MAGIC [233] and HESS [285] observatories have established [218, 29, 226, 18, 10, 129] bounds on the scale of dispersion, for the linear-effects (“n = 1”) scenario, at about 1/10 of the Planck scale.”
New limits on the density of the extragalactic background light in the optical to the far-infrared from the spectra of all known TeV blazars (2007, methodology): “While for the H.E.S.S. limit comparable exclusion criteria for the spctra were used, a fixed reference shape scaled in the level of the EBL density was used to calculate the EBL limit3, which presumably causes the differences at smaller wavelengths.”
Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S. (2012, methodology): “The Cherenkov light emitted by VHE-particleinduced showers in the atmosphere is focussed with 13 m diameter optical reflectors onto ultra fast cameras (Bernlöhr et al. 2003; Hinton 2004).”
Dark Matter Searches with Astroparticle Data (2011, methodology): “The HESS experiment in Namibia (Hinton, 2004) and the VERITAS experiment in Arizona (Weekes et al., 2002) are similar but complement each other by being in opposite hemispheres.”
The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays (2005, background): “Until the completion of H.E.S.S. (Hinton 2004) in early 2004, noVHEgamma-ray survey of comparable sensitivity of the southern sky or of the central region of the Galaxy had been performed.”
Semi-analytic modeling of the EBL and consequences for extragalactic gamma-ray spectra (2011, background): “…(IACTs) including the Very Energetic Radiation Imaging Telescope Array System (VERITAS; Maier et al. 2008), High Energy Stereoscopic System (HESS; Hinton 2004) and Major Atmospheric Gamma-Ray Imaging Cherenkov (MAGIC; Cortina 2005) experi- ments, and by the Large Area Telescope (LAT) instrument…”
THE FIRST FERMI-LAT CATALOG OF SOURCES ABOVE 10 GeV (2013, background): “The most advanced IACTs are currently H.E.S.S. and VERITAS (arrays of four ∼12 m telescopes; Hinton 2004; Weekes et al. 2002), and MAGIC (two telescopes of ∼17 m diameter; Lorenz 2004).”
An Exceptional Very High Energy Gamma-Ray Flare of PKS 2155–304 (2007, methodology): “The High Energy Stereoscopic System (H.E.S.S.; Hinton 2004) is used to study VHE γ-ray emission from wide variety of astrophysical objects.”
2FHL: THE SECOND CATALOG OF HARD FERMI-LAT SOURCES (2015, methodology): “All-sky surveys at γ-ray energies are instrumental for ground-based imaging atmospheric Cherenkov telescopes (IACTs) such as H.E.S.S., MAGIC, and VERITAS (Holder et al. 2009; Lorenz 2004; Hinton 2004, respectively) in order to find new sources because of their limited fields of view.”
Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S. (2009, background): “H.E.S.S. (Hinton 2004) is a system of four imaging atmospheric Cherenkov telescopes in Namibia.”
Gamma-Ray Bursts in the Swift Era (2007, background): “Complemented by other space- and ground- based high energy photon detectors (e.g., Dingus et al. 2004; Horan et al. 2005; Pittori & Tavani 2004; Hinton 2004; Lorenz 2004; Kubo et al. 2004), GLAST will unveil the last spectral window of GRB observations.”