The Crab Nebula and Pulsar between 500 GeV and 80 TeV: Observations with the HEGRA Stereoscopic Air Cerenkov Telescopes

By F. Aharonian, A. Akhperjanian, M. Beilicke, K. Bernlöhr, H. Börst, H. Bojahr, O. Bolz, T. Coarasa, J. Contreras, J. Cortina and 43 more. 2004

212 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/459531c82eff00d1aa1d92bd9a23dee5edeee8ac

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In Astronomy and Astrophysics

1. F. Tavecchio
2. M. Meyer
3. D. Horns
4. D. Mazin
5. J. Hinton
6. I. Grenier
7. William H. Lee
8. H. Zechlin

In Nuclear and High Energy Physics

1. F. Tavecchio
2. M. Meyer
3. D. Horns
4. D. Mazin
5. I. Grenier
6. J. Hinton
7. W. Rhode
8. H. Zechlin

Citations in the corpus

• Discovery of TeV Gamma-Ray Emission from the Cygnus Region of the Galaxy (2006, methodology): “With this technique, the Crab flux at 12 TeV is determined to be consistent with the flux measured by the HEGRA atmospheric Cherenkov telescope (Aharonian et al. 2004).”
• Polarization of the Crab Pulsar and Nebula as Observed by the INTEGRAL/IBIS Telescope (2008, methodology): “The synchrotron radiating electrons traced by IBIS have energies as high as 250-500 TeV in the average 16.2 ± 1.8 nT nebular field (Aharonian et al. 2004).”
• Sensitivity of the high altitude water Cherenkov detector to sources of multi-TeV gamma rays (2013, background): “ due to photon/hadron discrimination. Without improvement to the high-energy effective area, this is a practical limit to the HAWC sensitivity. Also shown, for reference, is the measured Crab flux from [19] and an inferred quarter-decade differential upper limit from the Crab at 141 TeV from the CASA-M”
• Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory (2017, methodology): “It has been observed with imaging atmospheric Cherenkov telescopes (IACTs) over the past two decades(Tanimori et al. 1998; Aharonian et al. 2004, 2006; Celik 2008; Aleksić et al. 2015).”
• The Crab Nebula as a standard candle in very high-energy astrophysics (2010, methodology): “1a, b are taken from Aharonian et al. (2004) and references therein.”
• VHE γ-Ray Observation of the Crab Nebula and its Pulsar with the MAGIC Telescope (2007, methodology): “Studies about the morphology of the γ-ray emitting region of the Crab Nebula have been performed by Aharonian et al. (2000, 2004) for γ-ray energies above 1 TeV.”
• The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey (2017, unknown): “(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).”
• TeV Gamma-Ray Sources from a Survey of the Galactic Plane with Milagro (2007, background): “The source location is consistent with 3EG J2227+6122, GEV J2227+6106, and the SNR G106.”
• Modern Tests of Lorentz Invariance (2005, background): “For recent fits of data to the SSC spectrum see [4].”
• Variable Very High Energy γ-Ray Emission from Markarian 501 (2007, result): “The obtained results were in perfect agreement with data published previously (Hillas et al 1998; Aharonian et al 2004; Wagner et al 2005), which shows that the analysis procedures used produce reliable results.”