1. 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

2. 3C 279 (z = 0.538) EGRET brightest AGN Gamma-ray flares in 1991 and 1996 Gamma-ray flares in 1991 and 1996 Apparent luminosity ~ 10 48 erg/s Apparent luminosity ~ 10 48 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 = 0.538 Kniffen et al. 1993 EGRET 1991 Wehrle et al. 2000 EGRET 1991

3. 3C 279 Flare in 1996 Wehrle et al. 1998 EGRET

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

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

6. 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%

7. 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

8. 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

9. Sky-map and alpha plot on 23 rd Feb 2007 80-220 GeV E> 220 GeV Preliminary Sky map around 3C279 Preliminary Preliminary Preliminary Preliminary

10. 3C279 VHE gamma-ray light curve Intra-night LC Preliminary Preliminary Optical light curve

11. Extragalactic VHE-sources (19) SourceRedshiftSp.TypesDiscoveryObservation M 87 0.0042.9 FR-IHEGRAHESS Mkn 421 0.0312.2 HBLWhipplemany Mkn 501 0.0342.4 HBLWhipplemany 1ES 2344+514 0.0442.9 HBLWhippleMAGIC Mkn 180 0.0453.3 HBLMAGIC 1ES 1959+650 0.0472.4 HBL7TAmany PKS 0548-322 0.069 HBLHESS BL Lac 0.069 3.6LBLMAGIC PKS 2005-489 0.0714.0 HBLHESS PKS 2155-304 0.1163.3 HBLDurhammany 1ES 1426+428 0.1293.3 HBLWhippleHEGRA 1ES 0229+200 0.139 HBLHESS H 2356-309 0.1653.1 HBLHESS 1ES 1218+304 0.1823.0 HBLMAGICVERITAS 1ES 1101-232 0.1862.9 HBLHESS 1ES 0347-121 0.188 HBLHESS 1ES 1011+496 0.212 4.0HBLMAGIC 3C 279 0.538 FSRQMAGIC PG 1553 ?4.0 HBL HESS/MAGIC New HBL 1ES1011+496 See the presentation by D. Mazin Big progress in AGN study from z ~ 0.2 to z = 0.538

12. Extragalactic VHE-sources (19) SourceRedshiftSp.TypesDiscoveryObservation M 87 0.0042.9 FR-IHEGRAHESS Mkn 421 0.0312.2 HBLWhipplemany Mkn 501 0.0342.4 HBLWhipplemany 1ES 2344+514 0.0442.9 HBLWhippleMAGIC Mkn 180 0.0453.3 HBLMAGIC 1ES 1959+650 0.0472.4 HBL7TAmany PKS 0548-322 0.069 HBLHESS BL Lac 0.069 3.6LBLMAGIC PKS 2005-489 0.0714.0 HBLHESS PKS 2155-304 0.1163.3 HBLDurhammany 1ES 1426+428 0.1293.3 HBLWhippleHEGRA 1ES 0229+200 0.139 HBLHESS H 2356-309 0.1653.1 HBLHESS 1ES 1218+304 0.1823.0 HBLMAGICVERITAS 1ES 1101-232 0.1862.9 HBLHESS 1ES 0347-121 0.188 HBLHESS 1ES 1011+496 0.212 4.0HBLMAGIC 3C 279 0.538 FSRQMAGIC PG 1553 ?4.0 HBL HESS/MAGIC New HBL 1ES1011+496 See the presentation by D. Mazin Big progress in AGN study from z ~ 0.2 to z = 0.538

13. 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 2006 6.1 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 = 0.538 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

14. Thanks

15. Blazar Sequence Fosatti et al. 1998 HBLs LBLs FSRQs Ghisellini 2003

16. Collection efficiency for VHE Gamma Rays Low Energy BinHigh Energy Bin

17. 3C 279

18. Will not show Energy Spectrum