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MAGIC Results

MAGIC Results. Alessandro De Angelis INFN, IST and University of Udine ECRS Lisboa, September 2006. EGRET : 273 sources above 100 MeV. > 30 sources above 100 GeV, 3x larger than before HESS and MAGIC came. The Physics Program. m QSRs. AGNs. Pulsars. GRBs. SNRs.

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MAGIC Results

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  1. MAGIC Results Alessandro De Angelis INFN, IST and University of Udine ECRS Lisboa, September 2006

  2. De Angelis (MAGIC) 2006 • EGRET : 273 sources above 100 MeV • > 30 sources above 100 GeV, • 3x larger than before HESS and MAGIC came

  3. The Physics Program De Angelis (MAGIC) 2006 mQSRs AGNs Pulsars GRBs SNRs Origin of Cosmic Rays cosmological g-Ray Horizon Quantum Gravity effects Cold Dark Matter

  4. MAGIC Cycle1 (Feb 2005-Apr 2006) De Angelis (MAGIC) 2006 • Statistics of physics runs for Cycle1: • 1070 hours dark time out of 1714, plus 150 h “good technical runs”, and 212 hours moon • Moon time increasing to an asymptotical value ~1/3 • ~100 hours ToO (with some important results) • will increase with the increased number of collaborations • Suzaku, Swift, GLAST, AGILE, … • All data analyzed • Papers published or submitted for all positive signals, but 5 (Crab, Mkn501, x, y, z) • 10 papers published or under publication in 2006 • 2 GRB observations during the primary burst • MAGIC Catalog opened (MAGIC Jxxx-yyy)

  5. Galactic Sources I: SNRs Source is Extended! Index –2.5 ± 0.2 90 cm VLA (green) + MAGIC (bck) + 12CO (black) De Angelis (MAGIC) 2006 • “MAGIC observations of VHE g -rays from HESS J1813-178”, ApJ Lett. 637 (2006) 41. Index –2.1 ± 0.2 • “Observation of VHE g radiation from HESS J1834-087/W41 with MAGIC”, ApJ Lett. 643 (2006) 53.

  6. Galactic Sources II: mQSR 0.4 AU 0.7 0.5 0.3 To observer 0.9 0.2 0.1 • LS I +61 303: • High Mass x-ray binary at a distance of 2 kpc • Compact object probably a neutron star • High eccentricity or the orbit (0.7) • Modulation of the emission from radio to x-rays with period 26.5 days attributed to orbital period De Angelis (MAGIC) 2006 • MAGIC has observed LS I +61 303 for 54 hours from November 2005 to March 2006 (6 orbital cycles) • A point-like source (E>200GeV) detected with significance of ~9s • consistent with LSI position  identification of g-ray source

  7. De Angelis (MAGIC) 2006 • The source is quiet at periastron passage and at relatively high emission level (16% Crab Nebula flux) at later phases [0.5-0.7] • Hint of periodicity Science 312, 1771 (2006)

  8. Galactic Sources III: the GC -7 10 E2 dN/dE -8 10 15 TeV WIMP 6 TeV WIMP -9 10 0,1 1 10 Energy [TeV] “Observation of g rays from the GC with MAGIC”, ApJ L 638 (06) 101. De Angelis (MAGIC) 2006 Cangaroo spectral index Γ=-4.6±0.5 HESS spectral index Γ=-2.63±0.04 MAGIC 2005: Γ=-2.3±0.4 flux: ~10% of Crab no apparent variability HESS, astro-ph/0408145

  9. Extragalactic (AGN) De Angelis (MAGIC) 2006 • 7 AGNs detected • Markarian 421, z=0.030 • Markarian 501, z=0.034 • 1ES2344+514, z=0.044 • Markarian 180, z=0.045 • 1ES1959+650, z=0.047 • 1ES1218+304, z=0.182 • PG1553+113, z~0.3 redshift

  10. Mkn 421 (z=0.030) & Mkn 501 (z=0.034) Mkn421 TeV-X-ray-correlation De Angelis (MAGIC) 2006 • Two very well studied sources, highly variable • >40k excess photons in MAGIC • TeV-X Correlation Mkn421

  11. Mkn 501 giant flare • Flare on 9 July 2005 • Doubling time~ 5 min. • Spectrum shape changes within minutes • Implications on the dispersion relation for light, see later • IC peak detected? De Angelis (MAGIC) 2006

  12. A nontrivial dispersion relation for light in vacuum(e.g., Quantum Gravity effects?) De Angelis (MAGIC) 2006 • From a phenomenological point of view, the effect can be studied with a perturbative expansion. In first order, the arrival delay of g-rays emitted simultaneously from a distant source should be proportional to their energy difference and the path L to the source: • The expected delay is very small and to make it measurable one needs to observe very high energy g-rays coming from sources at cosmological distances.

  13. High time-resolution study of AGN flare De Angelis (MAGIC) 2006 • Huge Mkn 501 flare in July 2005: 4 Crab intensity, signal more than doubled wrt baseline • Intensity variation recorded in 2 minute bins => new, much stronger, constraints on emission mechanism and light-speed dispersion relations (effective quantum gravity scale). MAGIC preliminary

  14. 1ES2344+514 (z=0.044) De Angelis (MAGIC) 2006 Clear detection, ~9s No variability Mkn 180 (z=0.045) • Upper limits from HEGRA, WHIPPLE • MAGIC: DISCOVERY! • April 2006, 11.1 h -Triggered by optical flare • 5.5 , index: -3.3 ± 0.7

  15. 1ES1959+650 (z=0.047) Spectral index: 2.72 ± 0.143.2 ± 0.2 • MAGIC: Significant signal in only 6h of observation • ApJ 639 (2006) 761 De Angelis (MAGIC) 2006 1ES1218+304 (z=0.182) • Upper limits from HEGRA, WHIPPLE • MAGIC: DISCOVERY! • Jan 2005, 8.2 h • 6.4 , index: -3.0 ± 0.4 • No signs of variability ApJ L 642, L119 (2006)

  16. PG1553+113 [z~0.3? (>0.09)] De Angelis (MAGIC) 2006 • Observed 18.8h in 2005-06 • H.E.S.S.: 4.0 hint • (A&A 448L (2006), 43) • MAGIC: ApJL submitted,astro-ph/0606161 • 8.8, firm detection. • If (a) intrinsic slope not harder than 1.5 (b) intrinsic spectrum has just one peak • => z < 0.78 (MAGIC only) or z < 0.42 (MAGIC+HESS)

  17. AGN: conclusions De Angelis (MAGIC) 2006 • There are 12blazars above 100 GeV established • MAGIC detected 7 of them; 2 of them discovered by MAGIC, 1 co-discovered with HESS • Fast, giant flare of Mkn501 recorded with unprecedented time resolution. Physics? • Hard constraint on the redshift of PG1553+113 to z<0.42 in case there is one peak above 100 GeV. If z>0.42, first observation of multipeak structure of a blazar above 100 GeV. • Variation of spectra with distance. Physics?

  18. AGN at a glance PKS 2155-304 H1426+428 H2356-309 PKS2005-489 1ES1218+304 1ES1101-232 1ES1959+650 Mkn 421 Mkn 501 PKS2005 PG1553 Simulated measurements New Sources De Angelis (MAGIC) 2006 At least a handle on EBL, but also the possibility of accessing cosmological constants (Martinez et al.) could become reality soon (maybe including X-ray obs.)

  19. GRBs Only to be seen by all sky monitor detectors De Angelis (MAGIC) 2006 Acc. by MAGIC During clear nights GRB Positions in Galactic Coordinates, BATSE DURATION OF GRBs

  20. GRBs and MAGIC • MAGIC is the right instrument, due to its fast movement & low threshold • MAGIC is in the GCN Network • GRB alert active since Apr 2005 De Angelis (MAGIC) 2006

  21. GRB observation with MAGIC: GRB050713a MAGIC data-taking GRB-alarm from SWIFT ApJ Letters 641, L9 (2006) De Angelis (MAGIC) 2006 SWIFT No VHE g emission from GRB positively detected yet... (all other observed GRB very short or at very high z) MAGIC We are on the track!

  22. MAGIC Highlights of the First Year Crab Nebula SZA & LZA LSI+61 303 Micro-Quasar New Source Galactic Center HESS J1813 HESS J1834 13CO cloud Mrk421 (0.031) 1ES2344(z=0.044) Mrk180 (0.045) New source 1ES1959 (0.047) 1ES1218(z=0.18) New Source PG 1553 (Z>0.25) New source Mrk501 (z=0.034) De Angelis (MAGIC) 2006

  23. MAGIC Cycle2 De Angelis (MAGIC) 2006 • From May 2006 to May 2007 • 840 dark time hours recommended for observation time in Class A, plus a maximum (?) of 236h for ToO • 46% to AGN • 28% to Galactic Sources • 9% to Pulsars • 14% to DM, including M87 + Special projects (t neutrinos, …) GRB: >36h ToO – and going towards a further improvement of the response time

  24. The threshold De Angelis (MAGIC) 2006 • We are publishing with a threshold of 70 GeV • We detect significant signal above 40 GeV • Understanding our efficiency towards the goal of 40 GeV. A special task force (UHU) has been set up; preliminary physics results at 50 GeV. • Substantial improvement on DM studies and determination of cosmological constants Secret 

  25. Conclusions De Angelis (MAGIC) 2006 • MAGIC is close to the design performance for 1 telescope • Threshold of 70 GeV for physics analysis; close to understand down to 50 GeV, and signal from 40 GeV • MAGIC is delivering very good physics results • In 2006, 7 papers published (one in Science) and 3 submitted, with 4 new sources; 6 papers in the pipeline, with 2-3 additional new sources • Cycle 2: important commitment to test more fundamental physics (DM, Lorentz violation, …) • And the second telescope will see the first light soon…

  26. BACKUP De Angelis (MAGIC) 2006

  27. TeV blazars Kino et al, ApJ, 2002, 564, 97 De Angelis (MAGIC) 2006 • TeV blazars: non-thermal emission, highly variable • All but one are HBL (high peaked BL Lacertae) • Models: leptonic vs. hadronic origin

  28. Absorption of extragalactic  - rays Any  that crosses cosmological distances through the universe interacts with the EBL De Angelis (MAGIC) 2006 Attenuated flux function of g-energy and redshift z. For the energy range of IACTs (10 GeV-10 TeV), the interaction takes place with the infrared (0.01 eV-3 eV, 100 m-1 m). Star formation, Radiation of stars, Absorption and reemission by ISM EBL By measuring the cutoffs in the spectra of AGNs, any suitable type of detector can help in determining the IR background-> needs good energy resolution Acc. by new detectors

  29. De Angelis (MAGIC) 2006

  30. Constraining the EBL density (and paving the way to a measurement of cosmological parameters) PKS 2155-304 H1426+428 H2356-309 PKS2005-489 1ES1218+304 1ES1101-232 1ES1959+650 Mkn 421 Mkn 501 Simulated measurements De Angelis (MAGIC) 2006 Blanch & Martinez 2004 Different EBL models Simulated measurements Mkn 421 Mkn 501 1ES1959+650 PKS2005-489 PKS 2155-304 H1426+428 1ES1218+304 1ES1101-232 H2356-309

  31. Flux time variability • MAGIC has observed LSI during 6 orbital cycles • A variable flux (probability of statistical fluctuation 310-5) detected • Marginal detections at phases 0.2-0.4 • Maximum flux detected at phase 0.6-0.7 with a 16% of the Crab Nebula flux • Strong orbital modulation  the emission is produced by the interplay of the two objects in the binary • No emission at periastron, two maxima in consecutive cycles at similar phases  hint of periodicity! De Angelis (MAGIC) 2006 Albert et al. 2006

  32. Energy spectrum • The absence of a spectral feature between 10 and 100 keV goes against an accretion scenario • Contemporaneous multiwavelength observations are needed to understand the nature of the object De Angelis (MAGIC) 2006 Albert et al. 2006

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