Observation of VHE Gamma Rays from the Remnant of SN 1006 with HEGRA CT1

Details Observation of VHE Gamma Rays from the Remnant of SN 1006 with HEGRA CT1 Observation of VHE Gamma Rays from the Remnant of SN 1006 with HEGRA CT1

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....4.2389v&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

The HEGRA collab oration observed the shell-type remnant SN1006 with the telescope CT1 for 219 h. For the observations we pointed the telescope towards the SNR center. An excess is observed from NE part of the rim with a statistical significance of ≈ 5 σ . Only large zenith angle (ZA) observations ( >70° ) are possible from the telescope site. The energy threshold is ≈ 18 TeV. We discuss the analysis and the problems related to large ZA observations. 2. Introduction supernova remnants (SNRs) are considered as the most likely sources of galactic cosmic ray. The shell type remnant G327.6+14.6 is originated from the SN 1006. This remnant is nearly circular (angular diameter ≈ 0.5° , radius of 9.5 pc, distance 2.18 ± 0.08 Kp c )[1], limb-brightened and shows the NE and SW regions significantly brighter than the rest of the shell (bip olar or barrelshaped)[1]. The shell expands with velocity 2890 ± 100 km/s [2] into a low density ISM. ASCA and ROSAT detected non-thermal X rays from the NE (the brighter one) and SW regions [5],[6]; while Cangaro o [7] detected TeV γ rays only from the NE part of the rim. Non-thermal X rays were explained as synchrotron emission from 10-100 TeV electrons . The possible origins of the TeV radiation are : 1) the above electron population, which can produce TeV γ rays via inverse Compton scattering on the CMBR and local IR photons ; 2) a possible contribution from accelerated hadrons (π0 ⇒ γ γ )[6]. 3. Observations and Analysis We observed SN 1006 for 219 hours from 1999 to 2001 with the HEGRA telescope CT1. CT1 is part of the HEGRA cosmic ray detector complex on La Palma (28.75° N, 17.9° W, 2225 m asl). SN 1006 (Ra 15:02:48.8, Dec -41:54:42) culminates at less than 20° elevation when observed from La Palma. Therefore only large zenith angle (ZA) observations are possible. We collected in total 346000 so-called ON-source events restricting observations to a narrow zenith range between 71-73° ZA as well as a small set of OFF-source data at the same

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