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

2. ICRC 2005, PuneTonello & Paneque, MPI Munich2 The MAGIC Telescope Canary Island La Palma 2200 m asl Canary Island La Palma 2200 m asl Largest Imaging Air Cherenkov Telescope for  -ray astronomy 236 m 2 mirror dish 576 high-QE PMTs fast repositioning t R <30 s MAGIC aims to cover the energy range 30 GeV - 30 TeV Regular observations started in September 2004 Status report, Mirzoyan et al., this conference

3. ICRC 2005, PuneTonello & Paneque, MPI Munich3 About 1ES1959+650  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)  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) Elliptical galaxy Active Galactic Nucleus Active Galactic Nucleus (Blazar type) (Blazar type) z = 0.047 z = 0.047 RA =19h59’59.8” Dec = +65  08'54'' Observability from La Palma: May-October 35  -54  z.a. May-October 35  -54  z.a.

4. ICRC 2005, PuneTonello & Paneque, MPI Munich4 About 1ES1959+650 1 - TeV-emission in quiescent state is very low HEGRA System (2000-2001): > 100 h obs. time (E th > 2TeV); 5.2 , average integral flux ~5.3% Crab (Aharonian et al, A&A 406, 2003) 1 - TeV-emission in quiescent state is very low HEGRA System (2000-2001): > 100 h obs. time (E th > 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

5. ICRC 2005, PuneTonello & Paneque, MPI Munich5 Observation with MAGIC DaysObs. TimeZA range September 2004 06, 07 October 2004 07, 10, 15, 16, 17 6 h 55 m 4.4 M events min = 36  max = 47  Analysis used was optimized on the Crab Nebula data set, which was obtained during the same period and zenith angle range

6. ICRC 2005, PuneTonello & Paneque, MPI Munich6 ALPHA PLOT To be compared with Crab at medium/large zenith angle

7. ICRC 2005, PuneTonello & Paneque, MPI Munich7 X-ray light curve  Low state in X-Ray 5 - 7 Sept 7 -17 Oct RXTE mission day

8. ICRC 2005, PuneTonello & Paneque, MPI Munich8 Optical light curve Tuorla Observatory Blazar Monitoring Program (http://users.utu.fi/kani/1m/jytable.html)  Low state in optical MAGIC observations 2004 MAGIC obs. 2005

9. ICRC 2005, PuneTonello & Paneque, MPI Munich9 Gamma-ray light curve  No significant variation of  -ray activity Average integrated photon flux (above 300 GeV) ~15% Crab Daily integrated flux ( ~1 h bins) 1ES1959 detected in quiescent state

10. ICRC 2005, PuneTonello & Paneque, MPI Munich10 Only statistical errors Preliminary spectrum Spectrum softer than that of Crab

11. ICRC 2005, PuneTonello & Paneque, MPI Munich11 Preliminary spectrum Only statistical errors  = 3.2 ± 0.2  = 2.9 ± 0.2 ~7 h. Obs.>100 h. Obs Peak of Inverse Compton NOT seen down to 200 GeV New energy domain explored for 1ES1959 in quiescent state

12. ICRC 2005, PuneTonello & Paneque, MPI Munich12  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  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 Conclusions

13. ICRC 2005, PuneTonello & Paneque, MPI Munich13 Imaging Air Cherenkov Telescopes 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

14. ICRC 2005, PuneTonello & Paneque, MPI Munich14 Preliminary analysis Random Forest MC  noise tuned to september off data sample. Hadrons randomly chosen from real on data (25 k events). Parameters: Width, Length, Size, Dist, Conc, logLength(logSize), logWidth(logSize), M3Long Cut in MHadronness chosen from Crab: Maximum significance: had = 0.1 Maximum excess events: had = 0.5 Cuts applied to 1ES1959 without any further optimization. Random Forest MC  noise tuned to september off data sample. Hadrons randomly chosen from real on data (25 k events). Parameters: Width, Length, Size, Dist, Conc, logLength(logSize), logWidth(logSize), M3Long Cut in MHadronness chosen from Crab: Maximum significance: had = 0.1 Maximum excess events: had = 0.5 Cuts applied to 1ES1959 without any further optimization. SignificanceExcess events

15. ICRC 2005, PuneTonello & Paneque, MPI Munich15

16. ICRC 2005, PuneTonello & Paneque, MPI Munich16 (Aharonian et al, A&A 406, 2003) Fig. 3