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Observations of the AGN 1ES1959+650 with the MAGIC telescope

Observations of the AGN 1ES1959+650 with the MAGIC telescope. Nadia Tonello and David Paneque for the MAGIC collaboration. Max-Planck-Insitut für Physik, München. The MAGIC Telescope 1ES1959+650 Results from the observations Conclusion. The MAGIC Telescope.

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Observations of the AGN 1ES1959+650 with the MAGIC telescope

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  1. Observations of the AGN 1ES1959+650 with the MAGIC telescope Nadia Tonello and David Paneque for the MAGIC collaboration Max-Planck-Insitut für Physik, München The MAGIC Telescope 1ES1959+650 Results from the observations Conclusion

  2. The MAGIC Telescope • Largest Imaging • Air Cherenkov • Telescope • for -ray astronomy • 236 m2 mirror dish • 576 high-QE PMTs • fast repositioning tR<30 s Canary Island La Palma 2200 m asl MAGIC aims to cover the energy range 30 GeV - 30 TeV Regular observations started in September 2004 Status report, Mirzoyan et al., this conference Tonello & Paneque, MPI Munich

  3. About 1ES1959+650 Elliptical galaxy Active Galactic Nucleus (Blazar type) z = 0.047 RA =19h59’59.8” Dec = +6508'54'' Observability from La Palma: May-October 35-54 z.a. • 1998: First  detection: Utah Seven Telescope Array (Nishiyama et al, 1999) • Confirmed in 2002 by WHIPPLE and HEGRA (Holder et al, 2003) (Aharonian et al, 2003) Tonello & Paneque, MPI Munich

  4. About 1ES1959+650 1 - TeV-emission in quiescent state is very low HEGRA System (2000-2001): > 100 h obs. time (Eth > 2TeV); 5.2  , average integral flux ~5.3% Crab (Aharonian et al, A&A 406, 2003) 2 - Orphan flare in TeV-rays in June 2002 (High activity in -rays with low activity in X-rays) Leptonic or hadronic acceleration ?? Hint for neutrino excess recently reported by AMANDA (Paris, 2005) Correlation with position of a UHECR from HiRes (astro-ph/0406654) 3 - Intermediate distance TeV blazar Candidate to disentangle source features from absorption in EBL Tonello & Paneque, MPI Munich

  5. Observation with MAGIC Analysis used was optimized on the Crab Nebula data set, which was obtained during the same period and zenith angle range Tonello & Paneque, MPI Munich

  6. To be compared with Crab at medium/large zenith angle ALPHA PLOT Tonello & Paneque, MPI Munich

  7. X-ray light curve • Low state in X-Ray 5 - 7 Sept 7 -17 Oct RXTE mission day Tonello & Paneque, MPI Munich

  8. MAGIC observations 2004 MAGIC obs. 2005 Optical light curve • Low state in optical Tuorla Observatory Blazar Monitoring Program (http://users.utu.fi/kani/1m/jytable.html) Tonello & Paneque, MPI Munich

  9. Daily integrated flux ( ~1 h bins) Gamma-ray light curve Average integrated photon flux (above 300 GeV) ~15% Crab • No significant variation of -ray activity 1ES1959 detected in quiescent state Tonello & Paneque, MPI Munich

  10. Only statistical errors Preliminary spectrum Spectrum softer than that of Crab Tonello & Paneque, MPI Munich

  11. New energy domain explored for 1ES1959 in quiescent state ~7 h. Obs. >100 h. Obs Preliminary spectrum Peak of Inverse Compton NOT seen down to 200 GeV = 2.9 ± 0.2 = 3.2 ± 0.2 Only statistical errors Tonello & Paneque, MPI Munich

  12. Conclusions • Clear signal (8 ) from 1ES1959+650 in quiescent state with MAGIC in ~7 h. obs. • Integrated flux ~15% Crab (> 300 GeV) • Differential energy spectrum with = 2.9 ± 0.2 • Inverse Compton emission peak not seen down to 200 GeV (PRELIMINARY). Work ongoing. • Performance of the new IACT instruments allow to do VHE -astronomy of blazars in quiescent state Tonello & Paneque, MPI Munich

  13. Shape of image Nature of primary particle Orientation of image Incoming direction of primary particle and bkg rejection Intensity of image Energy of primary particle Imaging Air Cherenkov Telescopes Tonello & Paneque, MPI Munich

  14. Tonello & Paneque, MPI Munich

  15. (Aharonian et al, A&A 406, 2003) Fig. 3 Tonello & Paneque, MPI Munich

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