MAGIC Results

Alessandro De Angelis

INFN, IST and University of Udine

ECRS Lisboa, September 2006

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• EGRET : 273 sources above 100 MeV • > 30 sources above 100 GeV, 3x larger than before HESS and MAGIC came

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SNRsSNRs

Cold Cold Dark Dark

MatterMatter

PulsarsPulsars

GRBsGRBs

Quantum Quantum Gravity effectsGravity effects

cosmologiccosmologicalal-Ray -Ray HorizonHorizon

AGNsAGNs

The Physics Program

Origin of Origin of Cosmic Cosmic RaysRays

QSRsQSRs

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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 2006

• 2 GRB observations during the primary burst• MAGIC Catalog opened (MAGIC Jxxx-yyy)

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Galactic Sources I: SNRs• “MAGIC observations of

VHE -rays from HESS J1813-178”, ApJ Lett. 637 (2006) 41.

Index –2.5 ± 0.2

90 cm VLA (green) + MAGIC (bck) + 12CO (black)

Source is Extended!

• “Observation of VHE radiation from HESS J1834-087/W41 with MAGIC”, ApJ Lett. 643 (2006) 53.

Index –2.1 ± 0.2

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Galactic Sources II: QSR 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

0.2

0.1

0.3

0.50

.9

0.7

0.4 AU

To observer

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 ~9consistent with LSI position identification of -ray source

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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)

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Cangaroo spectral indexΓ=-4.6±0.5

HESS spectral indexΓ=-2.63±0.04MAGIC 2005: Γ=-2.3±0.4 flux: ~10% of Crab no apparent variability

10-9

10-8

10-7

0,1 1 10Energy [TeV]

E2

dN

/dE

15 TeV WIMP6 TeV

WIMP

HESS, astro-ph/0408145

Galactic Sources III: the GC“Observation of rays from the GC with MAGIC”, ApJ L 638 (06) 101.

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• 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

Extragalactic (AGN)

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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

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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?

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• 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.

c

L

E

Et

QG

A nontrivial dispersion relation for light in vacuum

(e.g., Quantum Gravity effects?)

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• 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

MAGICpreliminary

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1ES2344+514 (z=0.044)

Clear detection, ~9No 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

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1ES1959+650 (z=0.047)

• MAGIC: Significant signal in only 6h of observationApJ 639 (2006) 761

Spectral index: 2.72 ± 0.14 3.2 ± 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

1ES1218+304 (z=0.182)

ApJ

L 6

42,

L119

(20

06)

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PG1553+113 [z~0.3? (>0.09)]

• 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)

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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 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?

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AGN at a glanceSource Redshift Spectral Index Type Detection (>5) Confimation

M87 0.004 2.9 FR I HESS

Mkn 421 0.031 2.2 BL Lac Whipple Many

Mkn 501 0.034 2.4 BL Lac Whipple Many

1ES 2344+514 0.044 2.9 BL Lac Whipple HEGRA,MAGIC

1ES 1959+650 0.047 2.4 BL Lac Tel. Array Many

PKS 2005-489 0.071 4.0 BL Lac HESS

PKS 2155-304 0.116 3.3 BL Lac Mark VI HESS

H1426+428 0.129 3.3 BL Lac Whipple Many

H2356-309 0.165 3.1 BL Lac HESS

1ES 1218+304 0.182 3.0 BL Lac MAGIC

1ES 1101-232 0.186 2.9 BL Lac HESS

PG 1553 >0.25 4.0 BL Lac MAGIC

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

0 0.1 0.2 0.3 0.4

Redshift Parameter z

Spe

ctra

l Ind

ex

PKS2005 PG1553

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.)

Simulatedmeasurements

Mkn 421Mkn 501

1ES1959+650PKS2005-489 1ES1218+304

1ES1101-232

H2356-309PKS 2155-304H1426+428

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GRB Positions in Galactic Coordinates, BATSE

Acc. by MAGICDuring clear nights

Only to be seen by all sky monitor detectors

DURATION OF GRBs

GRBs

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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

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GRB-alarm from SWIFTGRB-alarm from SWIFTGRB-alarm from SWIFTGRB-alarm from SWIFT

MAGIC data-takingMAGIC data-takingMAGIC data-takingMAGIC data-taking

We are on the track!

GRB observation with MAGIC: GRB050713a ApJ Letters 641, L9 (2006)ApJ Letters 641, L9 (2006)

No VHE No VHE emission from emission from GRB positively detectedGRB positively detectedyet...yet...(all other observed GRB very (all other observed GRB very short or at very high z)short or at very high z)

MAGIC

SWIFT

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MAGIC Highlights of the First Year

Crab NebulaSZA & LZA

Mrk421 (0.031)Galactic Center HESS J1813 HESS J183413CO cloud

1ES2344 (z=0.044) 1ES1218 (z=0.18)New Source

1ES1959 (0.047) PG 1553 (Z>0.25) New source

LSI+61 303Micro-QuasarNew Source

Mrk180 (0.045)New source

Mrk501 (z=0.034)

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MAGIC Cycle2• 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 (neutrinos, …)

GRB: >36h ToO – and going towards a further improvement of the response time

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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

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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…

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BACKUP

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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

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Any that crosses cosmological distances through the universe interacts with the EBL

Absorption of extragalactic - rays

eeEBLHE

E 1 cos 2 mec2 2

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 detectorsBy 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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Constraining the EBL density (and paving the way to a measurement of cosmological parameters)

Blanch & Martinez 2004

Simulatedmeasurements

Different EBL models

Mkn 421Mkn 501

1ES1959+650

PKS 2155-304H1426+428

PKS2005-489

1ES1218+3041ES1101-232H2356-309

Simulatedmeasurements

Mkn 421Mkn 501

1ES1959+650PKS2005-489 1ES1218+304

1ES1101-232

H2356-309PKS 2155-304H1426+428

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Flux time variability

Albert et al. 2006

MAGIC has observed LSI during 6 orbital cycles A variable flux (probability of statistical fluctuation 310-5) 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!

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Energy spectrum

Albert et al. 2006

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