Razmick Mirzoyan Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) Munich, Germany Photo by M. Garczarczyk 11.12.2008 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review The MAGIC Project Laser beams of the Active Mirror Control system become visible on foggy night The collaboration counts > 160 scientists 23 institutions, 10 countries 17 m Ø reflector, Al mirrors CF frame, fast rotation 180°/50s Active mirror control Analogue signal transport via 162m long optical fibres 2 GSample/s readout,... December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review The MAGIC Project MAGIC-I performance : Fast rotation for GRB < 50 secs Trigger threshold ~ 25 (50) GeV Sensitivity ~ 1.6 % Crab (50 h) Angular resolution ~ 0.1° Energy Resolution 20-30 % MAGIC-II: under commissioning, 1st Light in early spring 2009 M-I + M-II: ~2 times higher sensitivity Lower threshold energy of ~40 GeV in “stereo” mode December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Atmospheric Imaging Cherenkov Telescope ~ 10 km Particle shower ~ 1o Cherenkov light ~ 120 m Gamma ray Cherenkov light from g showers: ~10 photons/m2 @ 100 GeV scarce photon statistics MAGIC @ 100 GeV  200p.e. Trigger @ 50 GeV  100 p.e. December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Gamma/Hadron separation Height in km 20 km 1 TeV Angle in degrees Radius in m Proton Gamma MC Simulation of Shower 300 GeV Hadron Rejection by Image Shape + Orientation ~ 99.94 % Hadron Gamma December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Crab Nebula (PWN) Gamma Ray Signals from Crab ~ 0.4Hz Circle containing 64% of events at 250GeV >500GeV Circle Location of Pulsar Extended the spectrum from 400 GeV down to ~ 70-80 GeV (recent data shows excess for energies ≥ 40-50 GeV, under study) Hint on peaked distribution @ 77 ± 45 GeV December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Crab Pulsar Observations Optical light curve of Crab Pulsar observed by MAGIC Central pixel readout optical light intensity (not Cherenkov light) 95% Upper Limit for H.E. Gamma ray pulsed emission from Crab Pulsar Some 2.9 s ‘excess’ at EGRET phase at ~65GeV December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Σ A new technique: Analogue Sum Trigger ... ... Smart combination of several key ideas from different people. A small crew (M. Shayduk, N. Otte, M. Rissi, …) led by T. Schweizer played a decisive role in the design, implementation, data taking and analysis Below 100 GeV also g shower images are “patchy”, frequently consisting of a few “islands” Afterpulsing in a PMT produces a rate ~ 0.3% of the original rate. LONS photons trigger the telescope with a rate 150 MHz => Afterpulsing rate of 0.5 MHz => very high accidental trigger rate FWHM = 2.1 ns Measured in FADC Idea: a) Sum up, analog, ph.e.s from clusters of 18 pixels; b) provide a ring-shape sensitive area in the camera with overlap of patches; c) clip signal amplitudes before they are fed into trigger. Analog sum of 18 pixels Signal Clipper Σ ... ... Signal Clipper Discriminator December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Threshold at 24-27 PhE Thomas Schweizer, Clipped at 6-8 PhE MPI Seminar, October 7, 2008

Single pixel spectrum with afterpulses Standard and Sum triggers Single pixel spectrum with afterpulses Event distribution LONS 25 GeV threshold Sum Trigger Afterpulses 55 GeV threshold Standard Trigger December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

MAGIC discovery of Crab Pulsar > 25 GeV 3.4 sigma SCIENCE 322 (2008) Pulses in phase with EGRET AP1 = AP2 !!! Kuiper et al., 2001 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Comparison with pulsar models Magnetic pair production introduces a super-exponential cutoff at low energies Our superexponential cutoff is 23.2 GeV+-2.9stat GeV+-6.6syst GeV Absorption of g in the magnetic field Assuming a magnetic field of 8.108 T can put a lower limit on the distance of the emitting region of 6.2 +- 0.2stat +- 0.4syst stellar radii The high location of the emission region excludes the classical polar cap model (emission distance < 1 stellar radius) and challenges the slot gap model Baring et al., 2001 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Nearby radio galaxy (16 Mpc) Core: a supermassive black-hole of 3.2.109 MSun; jet morphology resolved, jet seen @ angle 30°, „misaligned Blazar“ Candidate source of UHECR ? Discovered by HEGRA, measured by H.E.S.S., VERITAS MAGIC sees a 8 s signal in February 1st; alerts SWIFT, H.E.S.S., VERITAS 22.8 h total measurements between Jan.30 – Febr.11, also partial moon and twilight measurements, ~10 s Nucleus at historical maximum in X-rays December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review M-87 Multi-l Campaign Simultaneous Multifrequency observations covering 15 orders of magnitude in energy: VHE: VERITAS, HESS, MAGIC X-ray: Suzaku, Swift Optical: KVA Astrophys. J. Lett. 685 (2008) L23 8.3‘ . 6.6‘ 8.6m December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review M-87 Flux in Time Reported flux values in the range of 0.7 – 15 % of Crab Really surprising: Nearly constant flux in E ~ 150 – 350 GeV but Variable for E ≥ 350 GeV Variability scale ~ 1 day Constrain size of emitting region: rSchwarzschield ~ 3 . M / MSun km => 9 . 109 km for M-87 (60 AU) (1 light-day is 173 AU) Multi-wavelength campaigns are planned for future December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Micro-quasar LS I +61 303 Quasar Microquasar X-Ray Binary System, Radio jet; 26.5 days orbital period; d ~2kpc; Galactic prototype of a quasar. Companion star: B0 main sequence star ~18M◎, a Be star with a circumstellar disc. Compact star: Black hole/neutron star < 4M◎ High eccentric orbit (ε~0.7) 3C223 VLA at 1500MHz λ~20cm 1E1740.7-2942 VLA; λ~6cm December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review TeV Binary System LS I +61 303 SCIENCE 312 (2006) Albert et al., SCIENCE 2006 Discovered by MAGIC in 2005 The average emission has a maximum at phase 0.6. No hint for intra-night flux variations (observed in radio and x-rays) Marginal detections occur at lower phases. December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Season II: ~112 hours Season I : ~54 hours MAGIC Oct 2005 Set 2006 Nov 2005 Oct 2006 Dec 2005 Nov 2006 Jan 2006 Feb 2006 Dec 2006 Mar 2006 Average Average ● More complete orbital coverage ● Similar behaviour as before ● Maximum flux detected at phase 0.6-0.7 ● Exception one point at Φ~0.85 ● A variable flux (prob. stat. fluctuation 3×10-5) ● Maximum flux @ phase 0.6-0.7 (16% Crab flux) ● No intra-night flux variations (but seen in radio, & X) December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

A possible scenario comes from the interaction of the relativistic wind from a young pulsar with the wind from its stellar companion, as in PSR B1259-63. A cometary nebula of radio emitting particles is formed. It rotates with the orbital period of the binary system. We see this nebula projected (Dubus 2006, A&A 456, 801). Mirabel 2006, (Perspective) Science 312, 1759 UV photons from the companion star suffer inverse Compton scattering by the same population of non-thermal particles, leading to emission in the GeV-TeV energy range. Dubus 2006, Vulcano Workshop (Dubus 2006, A&A 456, 801; Maraschi & Treves 1981). December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review LSI +61 303 LS I +31 606 VHE emission is periodic P = (26.8 ± 0.2) d compatible with the orbital periodicity found in other wavelengths Highest emission phase 0.6-0.7 Quiet at periastron Second peak in Dec 06 at 0.8-0.9 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review average cycle I cycle II 0.6<Φ<0.7 cycle II 0.5<Φ<0.6 Energy Spectrum The average energy spectrum from 200 GeV to 4 TeV is well fitted by a power law with spectral index  = -2.6 ± 0.2 (stat) ± 0.2 (syst) The luminosity above 200 GeV is ~7 x 1033 erg s-1 (if distance ~2 kpc) It is more luminous at TeV energies than at X-rays Spectral stability: both cycles (over 1 year) / different measured phases / days December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

MAGIC Discoveries due to Optical Triggers from KVA Telescope in LP 12.1 h S=5.5σ March 2006 Trigger point Mkn 180; z = 0.045 Albert et al. 2006 ApJ, 648, L105 Trigger point 1ES 1011+496 z = 0.212 18.7h S=6.2 σ March-May 07 Albert et al. 2007 ApJ, 667, L21 S5 0716+714 PRELIMINARY Significance 6.8 σ S5 0716+714 z = 0.31 (?) December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Aliu et al. 2008 in preparation

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review 3C 279 (z = 0.536) optical EGRET brightest AGN Gamma-ray flares in 1991 and 1996 Apparent luminosity ~ 1048erg/s First time variation △T ~ 6hr in 1996 flare Typical OVV quasar (Optically violent variable) Categorized as a FSRQ (Flat Spectrum Radio Quasar) Superluminal motion, γ~ 20~30 z = 0.538, Ld ~ 3Gpc Radio measurements over 7 years December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review 3C 279 Flare in 1996 3C273 3C279 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review MAGIC Discovery: 3C 279 SCIENCE 320 (2008) With this detection MAGIC has stretched the reach of VHE gama-ray telescopes from the previous z=0.212 to z=0.536 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Simultaneous optical-IR-radio (WEBT) and X-ray (RXTE, SWIFT) data: X-rays follow VHE flare but with 5-7 day delay, high optical level but low variability One-zone SSC ruled out One zone EC: requires too low B-field (B~0.03G) or very high G factor; either X-rays not reproduced or optics Lack of optical g correlation suggests a multi-zone inetrpretation Hadronic models could describe the data, but they require an extreme jet power of ~ Lj~1049 ergs-1 that is ~50 times more compared to leptonic models December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review Observation of GRBs later on we learnt that z = 6.3 December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Summary: coming close to solve the puzzle of cosmic rays ! With the single MAGIC-I telescope we discovered and detected g ray emission from a few tens of sources, a really impressive harvest ! > 35 publications in peer reviewed journals, 3-articles in SCIENCE magazine Crab Pulsar has been discovered at energies ≥ 25 GeV, rejecting polar cap model Most new extra-galactic Blazars show steep spectra Constraints on EBL  Cosmology (star and galaxy formations) With the discovery of 3C 279 MAGIC-I stretched its own reach to z = 0.536 Shown that also Bl-Lac objects are also VHE gamma emitting class … Flaring sources Detail of flare, intra night light curves, evolution of spectra Limit on Quantum Gravity Scale Periodic nature of a binary system LSI +61 303 has been shown Frequently optical triggers for AGN indicate high activity in VHE gammas GRB observations a few tens of GRBs were observed and 2 were in prompt phase, but no positive results yet, continue measuring, one day we are going to “catch” one We are doing research in the golden era of the VHE g astrophysics ! With the operation of MAGIC-II in a few months we will become even more powerful and (~2 times more) sensitive, a unique instrument operating in “stereo” at energies ≥ 40 GeV December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

New Source, BL Lacertae (New class: LBL, z=0.069) 5.1σ ~ 3%Crab Very steep Spectrum December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mrk-501 Flares on June 30 and July 9 in 2005 Intra-night light curve in 2mins bin June 30 July 9 Light curve in May-July 2005 MAGIC X-Ray Energy Spectra in pre-burst state and burst state June 30 July 9 Optical December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

g-Ray Emission Processes A major test on the accelerated particle type and process is to measure the very low energies < 100 GeV where the left 2 mechanisms much differ. December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review

Mrk-501: July 9 outburst Time lag for higher energies 4min bin This time lag may be explained by the particle acceleration process. 30 sec. July 9 Our data provides a stringent lower limit of Q.G. energy scale: MQG > 0.26 . 1018 GeV at 95% CL. The Q.G. energy scale is estimated to be 1017~1019GeV. Mrk501 BH ~ 3x109Msolar  Rsh/c ~3x104sec=10 light hours Order of 100sec time variation requires extreme jet / blob emission of Γ-factor of 100. Perhaps new theory/explanation is necessary. December 15, 2008 Mirzoyan, R.: Gamma Ray Astrophysics With MAGIC-I , MPI Project Review