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

De Angelis (MAGIC) /25 EGRET : 273 sources above 100 MeV > 30 sources above 100 GeV, 3x larger than before HESS and MAGIC came

De Angelis (MAGIC) /25 SNRs Cold Dark Matter Pulsars GRBs Quantum Gravity effects cosmological  -Ray Horizon AGNs The Physics Program Origin of Cosmic Rays  QSRs

De Angelis (MAGIC) /25 MAGIC Cycle1 (Feb 2005-Apr 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 GRB observations during the primary burst MAGIC Catalog opened (MAGIC Jxxx-yyy)

De Angelis (MAGIC) /25 Galactic Sources I: SNRs “MAGIC observations of VHE  -rays from HESS J ”, ApJ Lett. 637 (2006) 41. Index –2.5 ± cm VLA (green) + MAGIC (bck) + 12CO (black) Source is Extended! “Observation of VHE  radiation from HESS J /W41 with MAGIC”, ApJ Lett. 643 (2006) 53. Index –2.1 ± 0.2

De Angelis (MAGIC) /25 Galactic Sources II:  QSR LS I : 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 AU To observer MAGIC has observed LS I for 54 hours from November 2005 to March 2006 (6 orbital cycles) A point-like source (E>200GeV) detected with significance of ~9  consistent with LSI position  identification of  -ray source

De Angelis (MAGIC) /25 The source is quiet at periastron passage and at relatively high emission level (16% Crab Nebula flux) at later phases [ ] Hint of periodicity Science 312, 1771 (2006)

De Angelis (MAGIC) /25 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 ,1110 Energy [TeV] E 2 dN/dE 15 TeV WIMP 6 TeV WIMP HESS, astro-ph/ Galactic Sources III: the GC “Observation of  rays from the GC with MAGIC”, ApJ L 638 (06) 101.

De Angelis (MAGIC) /25 7 AGNs detected –Markarian 421, z=0.030 –Markarian 501, z=0.034 –1ES , z=0.044 –Markarian 180, z=0.045 –1ES , z=0.047 –1ES , z=0.182 –PG , z~0.3 redshift Extragalactic (AGN)

De Angelis (MAGIC) /25 Mkn 421 (z=0.030) & Mkn 501 (z=0.034) Two very well studied sources, highly variable –>40k excess photons in MAGIC –TeV-X Correlation Mkn421 TeV-X-ray- correlation Mkn421

De Angelis (MAGIC) /25 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) /25 From a phenomenological point of view, the effect can be studied with a perturbative expansion. In first order, the arrival delay of  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  -rays coming from sources at cosmological distances. A nontrivial dispersion relation for light in vacuum (e.g., Quantum Gravity effects?)

De Angelis (MAGIC) /25 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). High time-resolution study of AGN flare MAGIC preliminary

De Angelis (MAGIC) /25 1ES (z=0.044) Clear detection, ~9  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

De Angelis (MAGIC) /25 1ES (z=0.047) MAGIC: Significant signal in only 6h of observation ApJ 639 (2006) 761 Spectral index: 2.72 ± ± 0.2 Upper limits from HEGRA, WHIPPLE MAGIC: DISCOVERY! Jan 2005, 8.2 h 6.4 , index: -3.0 ± 0.4 No signs of variability 1ES (z=0.182) ApJ L 642, L119 (2006)

De Angelis (MAGIC) /25 PG [z~0.3? (>0.09)] Observed 18.8h in H.E.S.S.: 4.0  hint (A&A 448L (2006), 43) MAGIC: ApJL submitted, astro-ph/ , 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)

De Angelis (MAGIC) /25 AGN: conclusions There are 12 blazars 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 PG to z 0.42, first observation of multipeak structure of a blazar above 100 GeV. Variation of spectra with distance. Physics?

De Angelis (MAGIC) /25 AGN at a glance PKS2005PG1553 New Sources 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.) Simulated measurements Mkn 421 Mkn 501 1ES PKS ES ES H PKS H

De Angelis (MAGIC) /25 GRB Positions in Galactic Coordinates, BATSE Acc. by MAGIC During clear nights Only to be seen by all sky monitor detectors DURATION OF GRBs GRBs

De Angelis (MAGIC) /25 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) /25 GRB-alarm from SWIFT MAGIC data-taking We are on the track! GRB observation with MAGIC: GRB050713a ApJ Letters 641, L9 (2006) No VHE  emission from GRB positively detected yet... (all other observed GRB very short or at very high z) MAGIC SWIFT

De Angelis (MAGIC) /25 MAGIC Highlights of the First Year Crab Nebula SZA & LZA Mrk421 (0.031)Galactic CenterHESS J1813HESS J CO cloud 1ES2344 (z=0.044)1ES1218 (z=0.18) New Source 1ES1959 (0.047)PG 1553 (Z>0.25) New source LSI Micro-Quasar New Source Mrk180 (0.045) New source Mrk501 (z=0.034)

De Angelis (MAGIC) /25 MAGIC Cycle2 From May 2006 to May 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 (  neutrinos, …) GRB: >36h ToO – and going towards a further improvement of the response time

De Angelis (MAGIC) /25 The threshold 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

De Angelis (MAGIC) /25 Conclusions 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…

De Angelis (MAGIC) /25 BACKUP

De Angelis (MAGIC) /25 TeV blazars TeV blazars: non-thermal emission, highly variable All but one are HBL (high peaked BL Lacertae) Models: leptonic vs. hadronic origin Kino et al, ApJ, 2002, 564, 97

De Angelis (MAGIC) /25 Any  that crosses cosmological distances through the universe interacts with the EBL Absorption of extragalactic  - rays Attenuated flux function of  -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 Acc. by new detectors 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 EBL

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De Angelis (MAGIC) /25 Constraining the EBL density (and paving the way to a measurement of cosmological parameters) Blanch & Martinez 2004 Simulated measurements Different EBL models Mkn 421 Mkn 501 1ES PKS H PKS ES ES H Simulated measurements Mkn 421 Mkn 501 1ES PKS ES ES H PKS H

De Angelis (MAGIC) /25 Flux time variability Albert et al MAGIC has observed LSI during 6 orbital cycles A variable flux (probability of statistical fluctuation 3  ) detected Marginal detections at phases Maximum flux detected at phase 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) /25 Energy spectrum Albert et al 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