1. Recent results from MAGIC Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010 Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010 Characteristics of MAGIC A partial summary of physics results MAGIC 2 at work: First physics results with MAGIC 2

2. MAGIC at La Palma the largest reflector in the world (2 x 17 meters diameter telescopes) A European collaboration of 160 scientists from institutes in Germany, Italy, Spain, Switzerland, Finland, Poland, Bulgaria, Croatia MAGIC2 in production (commissioning ended in May). Full stereo data-taking Further upgrade expected in late 2011 (new Magic 1 camera) is on schedule

3. Some strong points of MAGIC Fast repositioning (sensitivity to transients: GRB) Low energy threshold (50 GeV, 25 GeV in sum trigger mode) – Overlapping with Fermi – Deep universe

4. Low threshold: overlap w/ Fermi (IC peak, X-calibration) FERMIMAGIC …and access to pulsars cutoffs, exg Crab (see Thomas Schweizer’s talk)

5. 5 Low threshold: observations at high z (1) n  ( ,z) is the spectral energy density of background photons Finke & Razzaque 09

6. 6 Low threshold: observations at high z (2) Neglecting evolutionary effects for simplicity Coppi & Aharonian, ApJ 1997 Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…) Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…)

7. The VHE Universe far away is populated by many MAGIC objects… 7 39 Sources … 1ES 1011+496z=0.21MAGIC 2007 1ES 0414+009z=0.29 HESS/Fermi 2009 S5 0716+71z=0.31±0.08MAGIC 2009 1ES 0502+675z=0.34VERITAS 2009 PKS 1510-089z=0.36HESS 2010 4C +21.43z=0.43MAGIC 2010 3C 66Az=0.44VERITAS 2009 3C 279 z=0.54 MAGIC 2008

8. Mkn 180 z = 0.045 ToO trigger MAGIC 12.1 h S=5.5 σ March 2006 ToO trigger 1ES 1011+496 z = 0.212 MAGIC 18.7h S=6.2 σ March-May 07 Mostly Apr 08 ApJ, 667 (2007) L21 KVA optIcal telescope at La Palma ApJ, 648 (2006) L105 MAGIC S5 0716+714 z = 0.31 Optical triggers: KVA in the MAGIC team… MAGIC 13.1h S=5.8 σ ApJ 704 (2009) L129

9. 3C 279 observations Jan -April 2006 6.2σ 2.2σ MAGIC: E>100 GeV MAGIC Coll., Science 320 (2008) 1752 The farthest object (z=0.54) Modeling of 3C 279 non-trivial: FSRQ External-Inverse Compton Modeling required, more free parameters than standard SSC VHE provides vital input! MAGIC Index 4.1+-0.68

10. 3C 279 follow-up observations Observation: January 16, 2007 Spectrum: Index 3.5+-0.7 MAGIC Lightcurve Preliminary Detection with 5.6 sigma

11. 3C 279: consequences on EBL The farthest source Pushes the level of EBL to a limit close to the galaxy count Mazin+2007, Mankuzyl+ 2010 Speculation on possible anomalous mechanisms like mixing with an ALP (DeAngelis+ 2007, Hooper+ 2008, Sanchez-Conde+ 2009) EBL spectrum: probing 0.2-2 μ m excluded still allowed At ~0.5 TeV, flux attenuated by 2 orders of magnitude!

12. S5 0716+714 Discovery after an optical ToO with KVA telescope Low-peaked BL Lac z = 0.31±0.08 Detection on 23-25 April 2008 Flux>400GeV = 9% Crab Photon index = 3.45±0.54 X-ray high flux on April 28th (Swift) April 2008 KVA Swift MAGIC fermi

13. Monitoring of bright sources Regular observation of Mrk 421 preliminary Correlation with X-ray Jan 20 th – April 30th 2009 SED Long term monitoring of bright VHE sources: Mrk 421, Mrk 501, 1ES 1959+650, 1ES 2344+514 MWL campaign, ToO

14. Joint HESS-MAGIC-VERITAS campaign of M87 (Science 2009) VHE nucleus Peak flux knot HST-1 nucleus X-ray Radio HST-1 Core Knot D Knot A Colours: 0.2 - 6 keV (Chandra) Contours: 8 GHz radio (VLA) The M87 radio-galaxy Jet Shared monitoring HESS, MAGIC VERITAS Confirmation of day-scale variability at VHE Evidence of correlation with the nucleus in X-ray & Radio. Evidence of central origin of the VHE emission (60Rs to the black hole) Chandra jet

15. Summary of extragalactic sources Detection of 17/40 AGNs Including 10 discoveries: - Mrk 180 - BL Lac - 1ES 1011 - PG 1553 (with HESS) - 3C 279 (z=0.54) - MAGIC J223+430 (3C66A/B) - S5 0716+714 - PKS 1424+240 (preliminary: 4.4σ) - IC310 - 4C +21.35 Other targets: - GRB - Starburst galaxies - Galaxy clusters EXCLUDED STILL ALLOWED Probing EBL spectrum 0.2-2μm Study AGN mechanism constraint from 3C 279

16. Summary of galactic sources Detection of 9 objects including 3 discoveries: - LSI 61+303 - IC 443 - the Crab pulsar Various families of emitters - SNR - PWN - Binary system - Pulsar - micro-quasar MAGIC detection The SNR IC 443 IC 443

17. IC443 (MAGIC J0616) and CR index~3.1 MAGIC J0616 Fermi, Egret Magic, Veritas

18. Cyg X-3

19. Selected new physics results from MAGIC 2

20. Performance of MAGIC stereo (see T. Schweizer’s talk) Angular resolution: 0.08° @ 1 TeV (was 0.12°) MAGIC stereo integral sensitivity now ~ 0.9% Crab in 50h (was 1.5% for MAGIC-I) Will reach 0.7% with the new camera (2 nd half 2011) Energy resolution: 18% @ 400 GeV (was 25%) MAGIC II (Crab data) Efficiency x3 at 100 GeV

21. Crab Nebula with MAGIC stereo: very first results Jan 10. MAGIC stereo (3h) overlaps with Fermi between 50-300 GeV (2 flux points below 100 GeV, statistical errors already smaller) (See T. Schweizer)

22. New source: IC 310 (March 2010) First source detected in stereo Triggered by Fermi Fermi (10-100 GeV)

23. New source: 4C +21.35 (June 2010) ###100### MAGIC reported the detection of a gamma-ray outburst from the Flat Spectrum Radio Quasar 4C +21.35, redshift of z=0.432. The observation was performed in stereoscopic mode during low intensity moon light During only 0.5 hours on June 17, 2010, preliminary results indicate a significant gamma-ray signal of 120 excess events corresponding to >8 sigma level above the background.

24. Where can MAGIC and the Cherenkov make a change? The gamma/cosmic ray connection: – SNR as galactic sources – AGN as sources DM – The photon annihilation channel? But the information from no detection is not as good as for accelerators – Electrons (and positrons?) A few things still not fully understood – Photon propagation The unexpected (Lorentz invariance, exotica, …) Safe fundamental science (and astronomy/astrophysics) from gamma rays: room for improvement in the region around 50 GeV

25. Summary MAGIC is now taking regular stereo data. Stereo observations since summer 2009, end of commissioning a couple of months ago – MAGIC performance in phase II has some new and unique characteristics – New MAGIC–I camera: in schedule, probably installed before Sept 2011 First MAGIC stereo data already make physics (Crab, Mrk421, 3 new sources, electrons) – 0.9% Crab sensitivity in 50 h (increase by 1.6x wrt MAGIC-I; becomes 3x at 100 GeV) – Stable analysis threshold at 50 GeV (clean data with sum trigger above 30 GeV) More scientific results from MAGIC stereo in near future – new objects to come in the next months – Overlap with Fermi. Interesting E < 100 GeV region

26. BACKUP

27. Stereo Analysis M2 M1 Δδ MAGIC-1 MAGIC-2Axis crossing Image cleaning: - Classical threshold method with time constraints Shower direction reconstruction: - Combination of axis crossing and DISP method Energy reconstruction: - Using lookup tables Background rejection: - Based on Random Forest classification + DISP correction

28. Comparison with our competitors Reaching 0.7 with new camera Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…) Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…) Impact on fundamental physics: Morphology of galactic sources (origin of cosmic rays) Impact on fundamental physics: Morphology of galactic sources (origin of cosmic rays) Impact on fundamental physics: DM, the unexpected

29. Much cleaner signal (Crab can be seen without cuts!!!) 6 hours, no cuts: Crab at 25  Stereo Magic I 100 GeV < E < 150 GeV After cuts

30. Crab Nebula: MAGIC - I MAGIC-I overlaps with Fermi between 60-300 GeV (1 flux point below 100 GeV, statistical errors comparable to Fermi) Abdo et al. 2010, ApJ 708, 1254

31. Crab Nebula: MAGIC - I MAGIC-I overlaps with Fermi between 60-300 GeV (1 flux point below 100 GeV, statistical errors comparable to Fermi) Albert et al. 2007 ApJ 674, 1037 Abdo et al. 2010, ApJ 708, 1254

32. Crab preliminary (larger statistics: 16h)

33. Mrk 421 Mrk 421 spectrum, 3 hours of data on Jan 14 th. Wobble. Flux level ~2.5 Crab Spectrum starts at 50 GeV Overlap with Fermi Fitted with power law + exponential cutoff