First results of Galactic observations with MAGIC Javier Rico Institut de Física d’Altes Energies Barcelona, 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 Summary 1. TeV gamma-ray astronomy with Cherenkov telescopes 2. MAGIC Technical features Results 3. LS I MAGIC as a neutrino telecope 5. Conclusions

Gamma-ray ~ 10 km Particle shower ~ 1 o Cherenkov Light ~ 120 m Cherenkov telescopes Collection area: ~ 10 5 m 2 Important since gamma-rays at these energies are rare (1/m 2 month) GLAST (slightly magnified)

Image intensity  Primary energy Image orientation  Prim. direction Image shape  Primary nature Imagingtechnique

Stereoscopy Better determination  Primary energy  Primary nature Better signal/background discrimination

First results of Galactic observations with MAGICJ. Rico (IFAE) Getting rid of the background (CR) (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 narrower than cosmic rays. Cherenkov images are parameterized by the light distribution (shape, position and orientation)

First results of Galactic observations with MAGICJ. 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 The MAGIC telescope 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 MAGICJ. Rico (IFAE) Active Mirror Control Jupiter before and after focusing Super-light structure (65 t), to catch GRBs AMC and fast movement

First results of Galactic observations with MAGICJ. Rico (IFAE) MAGIC near future 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 MAGICJ. Rico (IFAE) Physics with 100 GeV-10 TeV  -rays SNRs Cold Dark Matter PWNPulsars GRBs Quantum Gravity effects cosmological  -Ray Horizon AGNs Origin of CRs Astrophysics Fundamental Physics Binaries  QSRs

First results of Galactic observations with MAGICJ. Rico (IFAE) VHE  connection VHE  fluxes → upper limits to fluxes (unless strong absorption) km 3 detectors sensitivity: F(>1TeV) = /cm 2 s → Crab nebula  -ray flux Shell type supernova remnants with ~1 Crab flux in  - rays: RAJ and RAJ 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 Lower flux F(>1TeV) = /cm 2 s 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0      + photo-meson interaction in high magnetic fields (TeV-PeV)

First results of Galactic observations with MAGICJ. Rico (IFAE) Observation cycle I 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 variable source Galactic Center HEGRA Unidentified TeV2032 Cataclysmic variable (AE Aquari) HESS J1834 PSR B

J. Rico (IFAE) First results of Galactic observations with MAGIC LS I LS I : 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 AU To observer

J. Rico (IFAE) First results of Galactic observations with MAGIC LSI was temptatively associated to an EGRET source (<10 GeV) EGRET sources LS5039 Detected by HESS Hartman et al LSI Detected by MAGIC

J. Rico (IFAE) First results of Galactic observations with MAGIC LS I by MAGIC Albert et al We observed LS I with MAGIC for 54 horas between November 2005 and March 2006 (6 orbital cycles) LS I 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 Flux time variability Albert et al MAGIC has observed LSI during 6 orbital cycles A variable flux above 400 GeV (probability of statistical fluctuation 3  ) detected Marginal detections at phases 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! Emission models

J. Rico (IFAE) First results of Galactic observations with MAGIC MAGIC as a neutrino telescope   Ultra-high energy  neutrinos (PeV energies or more) can be looked for using MAGIC (Fargion 2002)  lifetime is 50 m at 1 PeV (10 15 eV) and hundreds of km for 1 EeV (10 18 eV) 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 ES1959 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 Conclusions 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 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