Observations of 3C 279 with Observations of 3C 279 with the MAGIC telescopethe MAGIC telescope

M. TeshimaM. TeshimaMax-Planck-Institute for PhysicsMax-Planck-Institute for Physics

for the MAGIC collaborationfor the MAGIC collaboration

at ICRC2007at ICRC2007

3C 2793C 279EGRET brightest AGN (LBL)EGRET brightest AGN (LBL)

Gamma-ray flares in 1991 and 1996Gamma-ray flares in 1991 and 1996 Apparent luminosity ~ 10Apparent luminosity ~ 104848erg/serg/s First time variation First time variation T ~ 6hr in 1996 flare△T ~ 6hr in 1996 flare△

Typical OVV (Optically violent variable)Typical OVV (Optically violent variable)

Superluminal motion Superluminal motion γγ~ 20~30, B ~ 0.3Gauss~ 20~30, B ~ 0.3Gauss

z = 0.538, Lz = 0.538, Ldd ~ 3Gpc ~ 3Gpc

3C 279 Flare in 19963C 279 Flare in 1996

SSC+EC / HadronicSSC+EC / Hadronic

MAGIC

EBL AbsorptionEBL Absorption

Pair Creation; γHE ＋ γEBL e+ + e-

MAGIC TelescopeMAGIC Telescope

MAGIC-II is under construction and will becompleted in the fall of the next year

Improve sensitivity by a factor of threeEffectively lower the threshold energy

New technologiesto lower the threshold energy

17m diameter world largest cherenkov tel.0.1°High resolution cameraAnalogue signal fiber transmission

Current MAGIC-I Performance

Fast rotation for GRB < 40secsTrigger threshold ~50GeVSensitivity ~2% of Crab (50hrs)Angular resolution ~0.1 degreesEnergy Resolution 20-30%

85m

Observation of 3C 279 Observation of 3C 279 with MAGICwith MAGIC

ObservationObservation In the period of January - April 2006In the period of January - April 2006 Observation of 9.5hrsObservation of 9.5hrs Zenith angle range is between 32 and 40 Zenith angle range is between 32 and 40

degreesdegrees

AnalysisAnalysis 3 independent analysis have been done3 independent analysis have been done Standard analysis and standard quality cutStandard analysis and standard quality cut Preliminary results will be presented herePreliminary results will be presented here

Sky-map and alpha plotSky-map and alpha ploton 23on 23rdrd Feb 2007 Feb 2007

80-220 GeV

E> 220 GeV

PreliminaryPreliminaryPreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

3C279 VHE gamma-ray 3C279 VHE gamma-ray light curvelight curve

Intra-night

PreliminaryPreliminary

PreliminaryPreliminary

Optical light curve

Extragalactic Extragalactic VHE-sources (19)VHE-sources (19)

Source Redshift Sp. Types Discovery Observation

M 87 0.004 2.9 FR-I HEGRA HESS

Mkn 421 0.031 2.2 HBL Whipple many

Mkn 501 0.034 2.4 HBL Whipple many

1ES 2344+514 0.044 2.9 HBL Whipple MAGIC

Mkn 180 0.045 3.3 HBL MAGIC

1ES 1959+650 0.047 2.4 HBL 7TA many

PKS 0548-322 0.069 HBL HESS

BL Lac 0.069 3.6 LBL MAGIC

PKS 2005-489 0.071 4.0 HBL HESS

PKS 2155-304 0.116 3.3 HBL Durham many

1ES 1426+428 0.129 3.3 HBL Whipple HEGRA

1ES 0229+200 0.139 HBL HESS

H 2356-309 0.165 3.1 HBL HESS

1ES 1218+304 0.182 3.0 HBL MAGIC VERITAS

1ES 1101-232 0.186 2.9 HBL HESS

1ES 0347-121 0.188 HBL HESS

1ES 1011+496 0.212 4.0 HBL MAGIC

3C 279 0.538 LBL MAGIC

PG 1553 ? 4.0 HBL HESS/MAGIC

New HBL 1ES1011+496 See the presentation by D. Mazin

Big progress in AGN studyfrom z ~ 0.2 to z = 0.538

SummarySummary

VHE gamma-ray emission from 3C279 was discovered by VHE gamma-ray emission from 3C279 was discovered by MAGICMAGIC

Second LBL after BL-LacerteuSecond LBL after BL-Lacerteu

The VHE flare at 100GeV was observed on 23 February iThe VHE flare at 100GeV was observed on 23 February in 2006 n 2006

6 sigma below 220GeV, and 5 sigma above 220GeV6 sigma below 220GeV, and 5 sigma above 220GeV

The survey distance is extended up to z = 0.538 by MAGIThe survey distance is extended up to z = 0.538 by MAGIC telescopeC telescope

Big jump toward the deep universe!Big jump toward the deep universe!

Study of Energy spectrumStudy of Energy spectrum may deliver a stringent constraint on EBL and acceleration modelmay deliver a stringent constraint on EBL and acceleration model

ThanksThanks