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Recent results from MAGIC. 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. MAGIC at La Palma the largest reflector in the world
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Recent results from MAGIC 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
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
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
Low threshold: overlap w/ Fermi (IC peak, X-calibration) FERMI MAGIC …and access to pulsars cutoffs, exg Crab (see Thomas Schweizer’s talk)
Low threshold: observations at high z (1) • ne (e,z) is the spectral energy density of background photons Finke & Razzaque 09
Low threshold: observations at high z (2) Coppi & Aharonian, ApJ 1997 • Neglecting evolutionary effects for simplicity Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…)
The VHE Universe far away is populatedby many MAGIC objects… 39 Sources … 1ES 1011+496 z=0.21 MAGIC 2007 1ES 0414+009 z=0.29 HESS/Fermi 2009 S5 0716+71 z=0.31±0.08 MAGIC 2009 1ES 0502+675 z=0.34 VERITAS 2009 PKS 1510-089 z=0.36 HESS 2010 4C +21.43 z=0.43 MAGIC 2010 3C 66A z=0.44 VERITAS 2009 3C 279 z=0.54 MAGIC 2008
ToO trigger MAGIC 12.1 h S=5.5 σ ToO trigger MAGIC 18.7h S=6.2 σ March-May 07 Optical triggers: KVA in the MAGIC team… Mostly Apr 08 MAGIC KVA optIcal telescope at La Palma March 2006 Mkn 180 z = 0.045 ApJ, 648 (2006) L105 1ES 1011+496 z = 0.212 ApJ, 667 (2007) L21 MAGIC 13.1h S=5.8 σ S5 0716+714 z = 0.31 ApJ 704 (2009) L129
3C 279 observations Jan -April 2006 MAGIC: E>100 GeV 6.2σ 2.2σ • The farthest object (z=0.54) • Modeling of 3C 279 non-trivial: • FSRQ • External-Inverse ComptonModeling required, morefree parameters than standard SSC • VHE provides vital input! MAGIC MAGIC Coll., Science 320 (2008) 1752 Index 4.1+-0.68
3C 279 follow-up observations • Observation: January 16, 2007 Detection with 5.6 sigma Spectrum: Index 3.5+-0.7 Preliminary Preliminary MAGIC Lightcurve Preliminary
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) At ~0.5 TeV, flux attenuated by 2 orders of magnitude! • excluded • still allowed • EBL spectrum: probing 0.2-2μm
S5 0716+714 Discovery after an optical ToO with KVA telescope April 2008 • 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) KVA MAGIC Swift fermi April 2008
Monitoring of bright sources Long term monitoring of bright VHE sources: Mrk 421, Mrk 501, 1ES 1959+650, 1ES 2344+514 MWL campaign, ToO Regular observation of Mrk 421 Correlation with X-ray Jan 20th – April 30th 2009 SED preliminary
Joint HESS-MAGIC-VERITAS campaign of M87 (Science 2009) The M87 radio-galaxy Jet Colours: 0.2 - 6 keV (Chandra) Contours: 8 GHz radio (VLA) VHE HST-1 Core Knot A Knot D Chandra knot HST-1 X-ray nucleus • 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) nucleus Radio Peak flux jet
Summary of extragalactic sources • STILL ALLOWED • EXCLUDED • 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 Study AGN mechanism • Probing EBL spectrum 0.2-2μm constraint from 3C 279
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 The SNR IC 443 IC 443 MAGIC detection
IC443 (MAGIC J0616) and CR MAGIC J0616 Fermi, Egret Magic, Veritas index~3.1
Performance of MAGIC stereo (see T. Schweizer’s talk) Energy resolution: 18% @ 400 GeV (was 25%) Angular resolution: 0.08° @ 1 TeV (was 0.12°) Efficiency x3 at 100 GeV • MAGIC stereo integral sensitivity now ~ 0.9% Crab in 50h (was 1.5% for MAGIC-I) • Will reach 0.7% with the new camera (2nd half 2011) MAGIC II (Crab data)
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)
New source: IC 310 (March 2010) • First source detected in stereo • Triggered by Fermi Fermi (10-100 GeV)
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.
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
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
MAGIC-1 MAGIC-2 Axis crossing Stereo Analysis Δδ M2 M1 • 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
Comparison with our competitors Impact on fundamental physics: Morphology of galactic sources (origin of cosmic rays) Reaching 0.7 with new camera Impact on fundamental physics: DM, the unexpected Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…)
Much cleaner signal (Crab can be seen without cuts!!!) 6 hours, no cuts: Crab at 25 s 100 GeV < E < 150 GeV Magic I Stereo After cuts
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
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
Mrk 421 • Mrk 421 spectrum, 3 hours of data on Jan 14th. Wobble. • Flux level ~2.5 Crab • Spectrum starts at 50 GeV • Overlap with Fermi • Fitted with power law + exponential cutoff