van Eldik C, Bolz O, Braun I, Hermann G, Hinton J, Hofmann W (2007)
Publication Status: Published
Publication Type: Conference contribution, Conference Contribution
Publication year: 2007
Publisher: Universidad Nacional Autonoma de Mexico
Book Volume: 2
Pages Range: 589-592
Event location: Merida, Yucatan
URI: https://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=84899537873&origin=inward
Observations by the H.E.S.S. system of imaging atmospheric Cherenkov telescopes provide the most sensitive measurements of the Galactic Centre region in the energy range 150 GeV - 30 TeV. The vicinity of the kinetic centre of our galaxy harbours numerous objects which could potentially accelerate particles to very high energies (VHE, > 100 GeV) and thus produce the gamma;-ray flux observed. Within statistical and systematic errors, the centroid of the point-like emission measured by H.E.S.S. was found [1] to be in good agreement with the position of the supermassive black hole Sgr A* and the recently discovered PWN candidate G359.95-0.04 [2]. Given a systematic pointing error of about 30", a possible association with the SNR Sgr A East could not be ruled out with the 2004 H.E.S.S. data. In this contribution an update is given on the position of the H.E.S.S. Galactic Centre source using 2005/2006 data. The systematic pointing error is reduced to 6" per axis using guiding telescopes for pointing corrections, making it possible to exclude with high significance Sgr A East as the source of the VHE gamma;-rays.
APA:
van Eldik, C., Bolz, O., Braun, I., Hermann, G., Hinton, J., & Hofmann, W. (2007). Localising the H.E.S.S. Galactic Center point source. In Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007 (pp. 589-592). Merida, Yucatan: Universidad Nacional Autonoma de Mexico.
MLA:
van Eldik, Christopher, et al. "Localising the H.E.S.S. Galactic Center point source." Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007, Merida, Yucatan Universidad Nacional Autonoma de Mexico, 2007. 589-592.
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