Observations of 3C 279 with the MAGIC telescope M.Teshima 1, E.Prandini 2, M.Errando, D. Kranich 4, P.Majumdar 1, M.Mariotti 2 and V.Scalzotto 2 for the MAGIC collaboration 1) Max-Planck-Institute for Physics, Germany 2) Department of Physics, University Padova, INFN, Italy 3) IFAE Barcelona, Spain 4) ETH Zurich, Switzerland

3C 279 (z = 0.538) EGRET brightest AGN Gamma-ray flares in 1991 and 1996 Gamma-ray flares in 1991 and 1996 Apparent luminosity ~ erg/s Apparent luminosity ~ erg/s Fast time variation △ T ~ 6hr in 1996 flare (Wehrle et al. 1998) Fast time variation △ T ~ 6hr in 1996 flare (Wehrle et al. 1998) Typical OVV quasar (Optically violent variable) Categorized as a FSRQ Categorized as a FSRQ Superluminal motion(Wehrle et al 200) β app ~ 4.8~7.5, γ~ 20 β app ~ 4.8~7.5, γ~ 20 z = Kniffen et al EGRET 1991 Wehrle et al EGRET 1991

3C 279 Flare in 1996 Wehrle et al EGRET

SSC+EC / Hadronic MAGIC Sikora et al Wehrle et al. 1998

EBL Absorption Pair Creation; γ HE ＋ γ EBL  e + + e - Stecker et al. 1992

MAGIC Telescope New technologies to lower the threshold energy 17m diameter world largest cherenkov tel. 0.1°High resolution camera Hemispherical PMT with enhanced QE Analogue signal fiber transmission Current MAGIC-I Performance Fast rotation for GRB < 40secs Trigger threshold ~50GeV Sensitivity ~2% of Crab (50hrs) Angular resolution ~0.1 degrees Energy Resolution 20-30%

MAGIC Telescope MAGIC-II is under construction and will be completed in the fall of the next year Improve sensitivity by a factor of three Effectively lower the threshold energy New technologies to lower the threshold energy 17m diameter world largest cherenkov tel. 0.1°High resolution camera Hemispherical PMT with enhanced QE Analogue signal fiber transmission Current MAGIC-I Performance Fast rotation for GRB < 40secs Trigger threshold ~50GeV Sensitivity ~2% of Crab (50hrs) Angular resolution ~0.1 degrees Energy Resolution 20-30% 85m

Observation of 3C 279 with MAGIC Observation In the period of January - April 2006 In the period of January - April 2006 Observation of 9.5hrs Observation of 9.5hrs Zenith angle range is between 32 and 40 degrees  relatively high threshold of 120GeV Zenith angle range is between 32 and 40 degrees  relatively high threshold of 120GeVAnalysis 4 independent analyses have been done 4 independent analyses have been done Standard analysis and standard quality cut Relative time image cleaning (lower threshold) All results are consistent Here, preliminary results will be presented Here, preliminary results will be presented

Sky-map and alpha plot on 23 rd Feb GeV E> 220 GeV Preliminary Sky map around 3C279 Preliminary Preliminary Preliminary Preliminary

3C279 VHE gamma-ray light curve Intra-night LC Preliminary Preliminary Optical light curve

Extragalactic VHE-sources (19) SourceRedshiftSp.TypesDiscoveryObservation M FR-IHEGRAHESS Mkn HBLWhipplemany Mkn HBLWhipplemany 1ES HBLWhippleMAGIC Mkn HBLMAGIC 1ES HBL7TAmany PKS HBLHESS BL Lac LBLMAGIC PKS HBLHESS PKS HBLDurhammany 1ES HBLWhippleHEGRA 1ES HBLHESS H HBLHESS 1ES HBLMAGICVERITAS 1ES HBLHESS 1ES HBLHESS 1ES HBLMAGIC 3C FSRQMAGIC PG 1553 ?4.0 HBL HESS/MAGIC New HBL 1ES See the presentation by D. Mazin Big progress in AGN study from z ~ 0.2 to z = 0.538

Extragalactic VHE-sources (19) SourceRedshiftSp.TypesDiscoveryObservation M FR-IHEGRAHESS Mkn HBLWhipplemany Mkn HBLWhipplemany 1ES HBLWhippleMAGIC Mkn HBLMAGIC 1ES HBL7TAmany PKS HBLHESS BL Lac LBLMAGIC PKS HBLHESS PKS HBLDurhammany 1ES HBLWhippleHEGRA 1ES HBLHESS H HBLHESS 1ES HBLMAGICVERITAS 1ES HBLHESS 1ES HBLHESS 1ES HBLMAGIC 3C FSRQMAGIC PG 1553 ?4.0 HBL HESS/MAGIC New HBL 1ES See the presentation by D. Mazin Big progress in AGN study from z ~ 0.2 to z = 0.538

Summary VHE gamma-ray emission from 3C 279 was discovered by MAGIC New class of source FSRQ, OVV-quasar New class of source FSRQ, OVV-quasar The VHE flare at 100GeV was observed on 23 February in sigma below 220GeV, and 5.1 sigma above 220GeV 6.1 sigma below 220GeV, and 5.1 sigma above 220GeV The survey distance is extended up to z = by MAGIC telescope Big jump toward the deep Universe! Big jump toward the deep Universe! Study of Energy spectrum may deliver a stringent constraint on EBL and acceleration model may deliver a stringent constraint on EBL and acceleration model Analysis is ongoing; We need very careful understanding of systematic uncertainties in the energy determination Analysis is ongoing; We need very careful understanding of systematic uncertainties in the energy determination

Thanks

Blazar Sequence Fosatti et al HBLs LBLs FSRQs Ghisellini 2003

Collection efficiency for VHE Gamma Rays Low Energy BinHigh Energy Bin

3C 279

Will not show Energy Spectrum