The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays

By F. Aharonian, A. Akhperjanian, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, Catherine Boisson, O. Bolz, V. Borrel and 89 more. 2005

414 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/04a2f41e7bdeb1f2cd00df10b709d2b9d66f28b0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “…observational evidence for the presence of high-energy particles inside supernova remnants is provided by the detection of non-thermal X-rays (Vink & Laming 2003; Parizot et al. 2006) and TeV gamma rays from a number of supernova remnants (Aharonian et al. 2006, 2008; Albert et al. 2007).”
MILAGRO OBSERVATIONS OF MULTI-TeV EMISSION FROM GALACTIC SOURCES IN THE FERMI BRIGHT SOURCE LIST (2009, background): “The large extent (implying an emission region of some 5 to 10 pc extent) is likely due to the nearness of the source and may arise from a pulsar-driven wind; it is consistent with HESS observation of more distant PWN with an angular size of ∼10 pc.”
2FHL: THE SECOND CATALOG OF HARD FERMI-LAT SOURCES (2015, background): “…field of view of about 5° and an angular resolution of approximately 0°.12, has invested 2800 hr of exposure to survey part81 of the Galactic plane, reaching an average sensitivity of 2% of the Crab Nebula flux (i.e., 4.5× 10−13 ph cm−2 s−1) at 1 TeV (Aharonian et al. 2006b; Carrigan et al. 2013).”
3FHL: The Third Catalog of Hard Fermi-LAT Sources (2017, background): “Transformed to the energy range >1 TeV based on the Crab Nebula spectrum, this corresponds to an energy flux of ∼8× 10−13 erg cm−2 s−1, which is slightly better than the sensitivity of ∼1.4× 10−12 erg cm−2 s−1 reached at >1 TeV by H.E.S.S. in its Galactic plane survey (Aharonian et al. 2006b; Carrig”
DISCOVERY OF TeV GAMMA-RAY EMISSION FROM TYCHO’S SUPERNOVA REMNANT (2011, neutral): “A conservative a priori trials factor was determined by tiling this area with square 0.04◦ bins (Aharonian et al. 2006), and additionally accounting for the two sets of applied cuts.”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “Such emission has been detected at Eγ >500 MeV with EGRET/CGRO (Mayer-Hasselwander et al., 1998) and at TeV energies with various instruments (Aharonian et al., 2004; Aharonian et al., 2006, and references therein).”
The 2HWC HAWC Observatory Gamma-Ray Catalog (2017, methodology): “Source 2HWC J1814−173 is located 0°.54 away from the TeV source HESS J1813−178, which was detected during the first H.E.S.S. Galactic Plane survey (Aharonian et al. 2005a; Aharonian et al. 2006b).”
A census of high-energy observations of Galactic supernova remnants (2012, background): “In particular, we note that several observatories have made surveys of the Galactic plane (ASCA26: Sugizaki et al. 2001, H.E.S.S.: Aharonian et al. 2006, Milagro: Abdo et al. 2007) or even of the whole sky (ROSAT27: Voges 2003, Fermi28: Fermi LAT Collaboration 2011), so that unexploited data might…”
The Youngest Galactic Supernova Remnant: G1.9+0.3 (2008, background): “This is about times below the H.E.S.S. 1 20n0 upper limit in the GC region (Aharonian et al. 2006); with v p and our density estimate of cm , we do not expect 2 30.1 n ∼ 100 a detectable signal.”
The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey (2017, methodology): “(1) H.E.S.S. Collaboration (2012c); Abramowski et al. (2015); (2) extension limit: Aharonian et al. (2004), flux: Aharonian et al. (2006b); (3) Aharonian et al. (2005a); (4) Aleksić et al. (2014); (5) Aliu et al. (2013).”
FERMI-LAT OBSERVATIONS OF HIGH-ENERGY γ-RAY EMISSION TOWARD THE GALACTIC CENTER (2015, methodology): “…by the EGRET instrument on the Compton Gamma-Ray Observatory (MayerHasselwander et al. 1998) and at higher energies by the H.E.S.S. Cherenkov array (Aharonian et al. 2006a,b) the characterisation of the γ-ray emission for < 100 GeV energies in the region surrounding the GC has remained elusive.”
TeV Gamma-Ray Sources from a Survey of the Galactic Plane with Milagro (2007, background): “The diameter of the excess implies an ∼ 8 pc source extent, which is consistent with the observations by HESS of more distant PWN (Aharonian et al. 2005a).”
The AGILE Mission (2003, background): “…photon statistics for blind gamma-ray period searches of pulsar candidates, (3) studying unpulsed gammaray emission from plerions in supernova remnants and studying pulsar wind/nebula interactions, e.g., as in the Galactic sources recently discovered in the TeV range (Aharonian et al. 2006).”