Recent results from MAGIC Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010...
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Transcript of Recent results from MAGIC Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010...
Recent results from MAGIC
Recent results from MAGIC
• 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)
5
Low threshold: observations at high z (1)
• n (,z) is the spectral
energy density of
background photons
),(emobs )(),( zEeEzE
Finke & Razzaque 09
€
maxσ at ε ≈ 500 GeV
E
⎛
⎝ ⎜
⎞
⎠ ⎟ eV ⇒ EBL
6
Low threshold: observations at high z (2)
• Neglecting evolutionary effects for simplicity
€
Λ∝1
σ
⎛
⎝ ⎜
⎞
⎠ ⎟
Coppi & Aharonian, ApJ 1997
€
(E,D) ≈D
Λ(E)Λ∝
1
σ
⎛
⎝ ⎜
⎞
⎠ ⎟
Φobs(E,D) ≈ Φem (E) × e−D
Λ(E )
Impact on fundamental physics: Photon propagation through large distances (EBL, Lorentz invariance…)
The VHE Universe far away is populatedby many MAGIC objects…
7
39 Sources…1ES 1011+496 z=0.21 MAGIC 20071ES 0414+009 z=0.29 HESS/Fermi 2009S5 0716+71 z=0.31±0.08 MAGIC 20091ES 0502+675 z=0.34 VERITAS 2009PKS 1510-089 z=0.36 HESS 20104C +21.43 z=0.43 MAGIC 20103C 66A z=0.44 VERITAS 2009 3C 279 z=0.54 MAGIC 2008
Mkn 180z = 0.045
ToO trigger
MAGIC12.1 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 13.1hS=5.8 σ
ApJ 704 (2009) L129
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 ComptonModeling required, morefree parameters than standard SSC
• VHE provides vital input!
MAGIC
Index 4.1+-0.68
3C 279 follow-up observations
• Observation: January 16, 2007
Spectrum: Index 3.5+-0.7
MAGIC
Lightcurve
Detection with 5.6 sigma
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 0.2-2μm
At ~0.5 TeV, flux attenuated by 2 orders of
magnitude!
€
m <<10−10eV (maximal mixing)
1011 GeV < M < 1013 GeV
S5 0716+714
Discovery after anoptical 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
April 2008
KVA
SwiftMAGIC
fermi
Monitoring of bright sources
Regular observation of Mrk 421
preliminary
Correlation with X-ray
Jan 20th – April 30th 2009 SED
Long term monitoring of bright VHE sources: Mrk 421, Mrk 501, 1ES 1959+650, 1ES 2344+514
MWL campaign, ToO
Joint HESS-MAGIC-VERITAS campaign of M87 (Science 2009)
VHE
nucleus
Peak flux
knot HST-1
nucleus
X-ray
Radio
HST-1Core
Knot DKnot 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
Summary of extragalactic sources
• Detection of 17/40 AGNsIncluding 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 AGNmechanism
constraint from 3C 279
Summary of galactic sources
• Detection of 9 objectsincluding 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
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 (2nd half 2011)
Energy resolution: 18% @ 400 GeV (was 25%)
MAGIC II(Crab data)
Efficiency x3at 100 GeV
Crab Nebula with MAGIC stereo: very first resultsJan 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
Stereo Analysis
M2
M1
Δδ
MAGIC-1 MAGIC-2 Axis 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
Comparison with our competitors
Reaching 0.7with new camera
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: DM, the unexpected
Much cleaner signal (Crab can be seen without cuts!!!)
6 hours, no cuts: Crab at 25
StereoMagic I
100 GeV < E < 150 GeV
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