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

M.TeshimaM.Teshima11, E.Prandini, E.Prandini22, M.Errando, , M.Errando, D. KranichD. Kranich44, P.Majumdar, P.Majumdar11, M.Mariotti, M.Mariotti2 2

and V.Scalzottoand V.Scalzotto22

for the MAGIC collaborationfor the MAGIC collaboration

1) Max-Planck-Institute for Physics, Germany1) Max-Planck-Institute for Physics, Germany2) Department of Physics, University Padova, INFN, Italy2) Department of Physics, University Padova, INFN, Italy

3) IFAE Barcelona, Spain3) IFAE Barcelona, Spain4) ETH Zurich, Switzerland4) ETH Zurich, Switzerland

3C 279 (z = 0.538)3C 279 (z = 0.538)EGRET brightest AGNEGRET brightest AGN

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

(Wehrle et al. 1998)(Wehrle et al. 1998)

Typical OVV quasar (Optically violent variable)Typical OVV quasar (Optically violent variable) Categorized as a FSRQCategorized as a FSRQ

Superluminal motion(Wehrle et al 200)Superluminal motion(Wehrle et al 200) ββappapp ~ 4.8~7.5, ~ 4.8~7.5, γγ~ 20~ 20

z = 0.538z = 0.538

Kniffen et al. 1993EGRET 1991

Wehrle et al. 2000

EGRET 1991

3C 279 Flare in 19963C 279 Flare in 1996Wehrle et al. 1998

Wehrle et al. 1998

EGRET

SSC+EC / HadronicSSC+EC / Hadronic

MAGIC

Sikora et al. 1998

Sikora et al. 1998

Wehrle et al. 1998

EBL AbsorptionEBL Absorption

Pair Creation; γHE ＋ γEBL e+ + e-

Stecker et al. 1992

MAGIC TelescopeMAGIC Telescope

New technologiesto lower the threshold energy

17m diameter world largest cherenkov tel.0.1°High resolution cameraHemispherical PMT with enhanced QEAnalogue 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%

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 cameraHemispherical PMT with enhanced QEAnalogue 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 degrees Zenith angle range is between 32 and 40 degrees

relatively high threshold of 120GeVrelatively high threshold of 120GeV

AnalysisAnalysis 4 independent analyses have been done4 independent analyses have been done

Standard analysis and standard quality cutStandard analysis and standard quality cut

Relative time image cleaning (lower threshold)Relative time image cleaning (lower threshold)

All results are consistentAll results are consistent Here, preliminary results will be presentedHere, preliminary results will be presented

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

80-220 GeV

E> 220 GeV

PreliminaryPreliminary

Sky map around 3C279Sky map around 3C279

PreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

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

Intra-night LC

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 FSRQ 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

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 FSRQ 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 3C 279 was discovered VHE gamma-ray emission from 3C 279 was discovered by MAGICby MAGIC

New class of source FSRQ, OVV-quasarNew class of source FSRQ, OVV-quasar

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

6.1 sigma below 220GeV, and 5.1 sigma above 220GeV6.1 sigma below 220GeV, and 5.1 sigma above 220GeV

The survey distance is extended up to z = 0.538 by The survey distance is extended up to z = 0.538 by MAGIC telescopeMAGIC 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 Analysis is ongoing; We need very careful understanding of Analysis is ongoing; We need very careful understanding of

systematic uncertainties in the energy determinationsystematic uncertainties in the energy determination

ThanksThanks

Blazar SequenceBlazar Sequence

Fosatti et al. 1998

HBLs

LBLs

FSRQs

Ghisellini 2003

Collection efficiency for Collection efficiency for VHE Gamma RaysVHE Gamma Rays

Low Energy Bin High Energy Bin

3C 2793C 279

Will not showWill not showEnergy SpectrumEnergy Spectrum