First results of Galactic First results of Galactic observations with MAGICobservations with MAGIC

Javier RicoJavier RicoInstitut de Física d’Altes EnergiesInstitut de Física d’Altes Energies

Barcelona, SpainBarcelona, Spain

XII International Workshop on “Neutrino Telescopes”Twenty years after the Supernova 1987A neutrino bursts discovery

March 6-9, 2007“Istituto Veneto di Scienze, Lettere ed Arti”, Palazzo Franchetti - S. Stefano

Venice (Italy)

J. Rico (IFAE)First results of Galactic observations with MAGIC

Su

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Su

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1. TeV gamma-ray astronomy with Cherenkov telescopes

2. MAGIC Technical features Results

3. LS I +61 303

4. MAGIC as a neutrino telecope

5. Conclusions

Gamma-ray

~ 10 kmParticleshower

~ 1o

Che

renk

ov L

ight

~ 120 m

Cherenkov telescopesCherenkov telescopes

Collection area:~ 105 m2

Important sincegamma-rays at theseenergies are rare(1/m2 month)

GLAST(slightly magnified)

Image intensityPrimary energy

Image orientation Prim. direction

Image shape Primary nature

Imaging Imaging

techniquetechnique

StereoscopyStereoscopy

Better determinationPrimary energyPrimary natureBetter signal/backgrounddiscrimination

First results of Galactic observations with MAGIC J. Rico (IFAE)

Get

tin

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nd

(C

R)

Get

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id o

f th

e b

ackg

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(C

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(2) Orientation: -rays point to the source: excess at small alpha

ON: Pointing to source

OFF: Pointing somewhere else

Crab Nebula

Image parameterization

CR

(1) Shape: –rays are narrowerthan cosmic rays.

Cherenkov images are parameterized by the light distribution (shape, position and orientation)

First results of Galactic observations with MAGIC J. Rico (IFAE)

The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:

• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

17 m

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MA

GIC

tel

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pe The existing technology has been carried to the limit to improve sensitiity and lower the

energy threshold:• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:

• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:

• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:

• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:

• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system

MAGIC is located at La Palma, Canary Islands (Northern Hemisphere)

First results of Galactic observations with MAGIC J. Rico (IFAE)

Active Mirror Control

Jupiter before and after focusing

Super-light structure (65 t), to catch GRBs

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MC

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First results of Galactic observations with MAGIC J. Rico (IFAE)

MA

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MA

GIC

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MAGIC-II:• Second telescope, completion in 2007• Stereo high purity gamma samples better physics (lower threshold and better sensitivity)

MAGIC-1.5:• Running since February’07. • 2 GHz readout• Power of timing information under study

First results of Galactic observations with MAGIC J. Rico (IFAE)

Ph

ysic

s w

ith

100

GeV

-10

TeV

P

hys

ics

wit

h 1

00 G

eV-1

0 Te

V

-ray

s-r

ays

SNRsSNRs

Cold Cold Dark Dark

MatterMatter

PWNPWNPulsarsPulsars

GRBsGRBs

Quantum Quantum Gravity effectsGravity effects

cosmologiccosmologicalal-Ray -Ray HorizonHorizon

AGNsAGNs

Origin of Origin of CRsCRs

Astrophysics

Fundamental Physics

BinariesBinariesQSRsQSRs

First results of Galactic observations with MAGIC J. Rico (IFAE)

VH

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VH

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VHE fluxes → upper limits to fluxes (unless strong absorption)

km3 detectors sensitivity: F(>1TeV) = 10-11 /cm2s → Crab nebula -ray flux

Shell type supernova remnants with ~1 Crab flux in -rays: RAJ1713.7-3946 and RAJ0852.0-4622 best explained by hadronic interactions (extension, morphology, hard spectrum up to 100 TeV)

PWN: well explained by leptonic models but room for ions accelerated in the pulsar relativistic wind: Vela-X, Crab

Compact binary systems: LS5039 and LSI+61303. Lower flux F(>1TeV) = 10-12 /cm2s or more depending on -ray production region

VHE ’s messengers of non-thermal processes involving hadronic interactions

Ultimate proof of Galactic CR origin

p

p±

0

+ photo-meson interaction in high magnetic fields

(TeV-PeV)

First results of Galactic observations with MAGIC J. Rico (IFAE)

Ob

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Observations from November 2004 to May 2006

About 25% total observation time for Galactic targets (apart from Crab Nebula)

Targets include: SNR:

Intense EGRET sources HESS galactic scan sources (HESS J1834, HESS

J1813) PWN Pulsars: limits to Crab, PSR B1957, PSR B1951 Binaries/microquasars (low and high mass)

LS I +61 303 variable source Galactic Center HEGRA Unidentified TeV2032 Cataclysmic variable (AE Aquari)

HESS J1834

PSR B1951+32

J. Rico (IFAE)First results of Galactic observations with MAGIC

LS

I +

61 3

03L

S I

+61

303

LS I +61 303: High Mass x-ray binary at a distance of 2 kpc Optical companion is a B0 Ve star of 10.7 mag with a circumstellar disc 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 Secondary modulation of period 4 years attributed to changes in the Be star equatorial disc

0.20.1

0.3

0.5

0.9

0.70.4 AU

To observer

J. Rico (IFAE)First results of Galactic observations with MAGIC

• LSI was temptatively associated to an EGRET source (<10 GeV)

EG

RE

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ou

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EG

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LS5039Detected by HESS

Hartman et al. 1999

LSI +61 303Detected by MAGIC

J. Rico (IFAE)First results of Galactic observations with MAGIC

LS

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03 b

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S I

+61

303

by

MA

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Albert et al. 2006

• We observed LS I +61 303 with MAGIC for 54 horas between November 2005 and March 2006 (6 orbital cycles)

• LS I +61 303 is a VHE gamma-ray emitter:• The flux is variable• It is modulated by the orbital motion (first indication of periodicity) • The peak of intensity is far from periastron

• Results from another 4 orbital cycles obs. during fall 2006 published soon

J. Rico (IFAE)First results of Galactic observations with MAGIC

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Albert et al. 2006

MAGIC has observed LSI during 6 orbital cycles A variable flux above 400 GeV (probability of statistical fluctuation 310-5) detected Marginal detections at phases 0.2-0.4 Maximum flux detected at phase 0.6 with a 16% of the Crab Nebula flux More luminous at these energies than at x-rays Energy spectrum from 200 GeV to 4 TeV is well fitted by a power law with spectral index = -2.6, no cutoff seen

J. Rico (IFAE)First results of Galactic observations with MAGIC

• The broad-band experimental data on LSI may be explained both as produced by

• relativistic jets (microquasar) • interaction of the winds of a young pulsar with that of the companion star.

• In both cases the responsible may be accelerated electrons (Inverse Compton) or protons (pp interaction) → neutrinos!

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J. Rico (IFAE)First results of Galactic observations with MAGIC

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• Ultra-high energy neutrinos (PeV energies or more) can be looked for using MAGIC (Fargion 2002)• lifetime is 50 m at 1 PeV (1015eV) and hundreds of km for 1 EeV (1018eV)• 83% of the times the decay produces air showers observable by MAGIC

• Feasibility studies in MAGIC started this observation cycle• Data taking → background studies (scattered light)• Preliminary Sensitivity studies:

MAGIC not competitive for diffuse neutrinos Identified best source candidates:

LS I +61 303 1ES1959 1ES2344

• No “normal” observation time is lost since it is done when clouds do not allow them

J. Rico (IFAE)First results of Galactic observations with MAGIC

Co

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New generation of Cherenkov telescopes are main actors of the recent burst of VHE astronomy

MAGIC has a major role with already 5 new discoveries and other interesting results

The compact binary system LS I +61 303 has been detected at TeV energies The emission is variable Possible hint of periodicity The maximum of the emission happens 1/3 of

the orbit away from periastron The possibility of using MAGIC as a

telescope for UHE neutrinos is under study