Introduction Data analyzed Analysis method Preliminary results Nadia Tonello, Max-Planck-Insitut für Physik, München First 1ES1959+650 observations with the MAGIC telescope and comparison with Crab Nebula at 40 ZA Introduction Data analyzed Analysis method Preliminary results

Nadia Tonello, MPI Munich What is 1ES1959+650? Elliptical galaxy Active Galactic Nucleus z = 0.047 RA =19h59m59.8s Dec = +6508'54'' Observability from La Palma: May-October 35-54 z.a. 1998: First  detection: Utah Seven Telescope Array Weak source Confirmed in 2002 by WHIPPLE and HEGRA Most interesting aspect: orphan flare in June 2002. Candidate source for south neutrino telescopes Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich The MAGIC Telescope Canary Island La Palma 2200 m asl Largest Imaging Air Cherenkov Telescope for -ray astronomy 17 m mirror dish 3.5 field of view 576 high-QE PMTs Design optimized for: low energy threshold E = 30 GeV fast repositioning tR<30 sec Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Imaging Air Cherenkov Telescopes Gamma ray Cherenkov light Image of particle shower in telescope camera reconstruct: arrival direction, energy reject hadron background ~ 10 km Particle shower ~ 1o Cherenkov light ~ 120 m Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Standard Analysis gamma shower Shower reconstruction and background rejection based on image shape analysis raw image cleaned image Hillas parameters: Length, width, distance, alpha hadron shower (background) Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich MAGIC raw data Source Days Obs. Time ZA range Azimuth 1ES1959+650 September 06, 07 October 07, 10,14,15,16,17 6 h 55 m 4.4 M events min = 35 max = 47 min = -26 max = 2 Crab Nebula September 13, 14, 15, 16,21,22,23 2 h 17 m 1.7 M events max = 46 (selected) min= 85 max = 94 Off data September 8, 10, 11, 12, 13, 14, 16, 17 2 h 49 m 2.3 M events Cuts optimized on Crab Nebula and applied to 1ES1959 and Off data Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Preliminary analysis Extract pedestals from data Image cleaning : Pedestal RMS levels: 4 sigma, 2 sigma (5 rings) Absolute number of photons: 40 ph, 25 ph Image parameters distributions have been compared for the 3 data sets. Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich 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. Significance Excess events Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Signal above 2000 ph. Crab Nebula: Size >2000 ph Significance: 26.4  Excess events: 529 ± 20 1ES 1959 + 650: Size >2000 ph Significance: 7.0  Excess events: 165 Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Time analysis Binning in about 2 h data No substantial variation of activity Days Obs time Significance Excess Rate (phot/min) September 6,7 121 min 3.6 42.8 ± 11.8 0.35 ± 0.09 October 7,10,15 110 min 4.0 49.5 ± 12.3 0.45 ±0.11 October 16, 17 137 min 5.0 64.0 ± 12.8 0.46 ± 0.09 Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich X-ray light curve Activity not particularly high 5 - 7 Sept 7 -17 Oct RXTE mission day Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Optical light curve Quiescent state Tuorla Observatory Blazar Monitoring Program Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Crab-1ES1959 comparison Same cuts applied to Crab and 1ES1959 for each size bin Size (ph) Significance Excess events 1000<S<2000 10.2  296 ± 29 2000<S<4000 18  258 ± 14 4000<S<8000 17.3  166 ± 10 8000<S<16000 4.8  71 ± 15 CRAB 1000<S<2000 5.0  364 ± 73 2000<S<4000 4.9  87 ± 20 4000<S<8000 4.2  42 ± 10 8000<S<16000 1.5  29 ± 19 1ES1959 Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Crab-1ES1959 comparison Excess events/(obs. time * size bin width) Softer spectrum? HEGRA System Results (2000-2001): 94 h obs. Time. Energy threshold: 2TeV Significance 5.4 = 3.3 ±0.7 8% Crab flux 43% 12% 9% 14% Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Nadia Tonello, MPI Munich Conclusions 1ES1959 has been observed with MAGIC for ~7 h. Crab and OFF data (~ 2h each) have been selected to match ZA range: 40 deg. Data have been analyzed with cuts optimized on Crab. We have a signal from 1ES1959+650 when there was no high activity in X-rays No variation of state, observations are fragmented in time. Comparison with Crab in size bins: 1ES1959 ~40% to ~10% of Crab, compatible with HEGRA System flux measurements at high energies. Work in progress: Energy spectrum. Rencontres de Moriond 2005 Nadia Tonello, MPI Munich

Energy distribution of MC  1000< s< 2000 ph ~180 GeV 2000< S < 4000 ph ~300 GeV 4000<s <8000 ph ~500 GeV 8000 <s< 16000 ph ~900 GeV Rencontres de Moriond 2005 Nadia Tonello, MPI Munich