Observations of 3C 279 Observations of 3C 279 with the MAGIC telescope with the MAGIC telescope M.Teshima M.Teshima 1 , E.Prandini , E.Prandini 2 , M.Errand , M.Errand o, o, D. Kranich D. Kranich 4 , P.Majumdar , P.Majumdar 1 , M.Mariot , M.Mariot ti ti 2 2 and V.Scalzotto and V.Scalzotto 2 for the MAGIC collaboration for the MAGIC collaboration 1) Max-Planck-Institute for Physics, Germany 1) Max-Planck-Institute for Physics, Germany 2) Department of Physics, University Padova, INFN, Italy 2) Department of Physics, University Padova, INFN, Italy
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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.
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Observations of 3C 279 with Observations of 3C 279 with the MAGIC telescopethe MAGIC telescope
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
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