Berlin 2005 – scientific programme

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T: Teilchenphysik

T 201: Kosmische Strahlung I

T 201.5: Talk

Friday, March 4, 2005, 15:00–15:15, TU H105

Advanced observation strategy and source position reconstruction for the MAGIC telescope. — •Daniel Mazin¹, Hendrik Bartko¹, Eva Domingo², and Abelardo Moralejo³ — ¹Max-Planck-Institut für Physik, Föhringer Ring 6, 80805 München — ²IFAE, Edifici C, 08193 Bellaterra, Spain — ³INFN, Via Marzolo, 8. Padova 35131, Italy

The 17m diameter MAGIC Cherenkov telescope on the Canary island La Palma measures very high energy cosmic rays through Cherenkov light from atmospheric air showers. For the measurement of γ-ray sources the γ-showers have to be separated efficiently from the much more abundant hadronic showers. The latter background is usually determined from OFF data, which are taken from a neighbouring to the source region in the sky not containing the γ-sources.

A way to assure that ON and OFF data are taken under same conditions (light of the night sky, weather, etc.) is the wobble mode. Thereby the telescope is directed to a sky point at a fixed offset from the γ-source, such that the source location is well inside the field of view of the camera. Both ON and OFF data can be obtained from the same data sample. For analyzing the wobble data it is necessary to estimate the direction of every individual shower. This is achieved by the so-called DISP method. Knowing this direction allows one to classify a shower as an ON or OFF event.

A comparison between the standard observation mode and the wobble mode will be presented and discussed here.