1. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de The MAGIC view of our Galaxy Tobias Jogler for the MAGIC Collaboration

2. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de The MAGIC Telescope La Palma, asl. 2200m 17 m diameter mirror 3.5 ° FoV camera Trigger threshold of E = 50 GeV Sensitivity of 1.6 % Crab flux Can operate under moonlight conditions Very sensitive instrument to study faint VHE gamma ray sources

3. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de MAGIC II 2nd MAGIC telescope under constructionIn stereo observation mode with both telescopes we will have a 3 times better sensitivity than MAGIC I MAGIC II 7-5 cleaning T 75.1 Dedicated talk

4. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Galactic Source Targets MAGIC mainly pointed at candidate sources Globular ClusterSNRPWNPulsars Microquasar, HMXB SNRs

5. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Casiopeia A Historic supernova around 1680 Distance ~ 3.4 kpc Shelltype SNR Prominent at X-ray and radio wavelength Discovered by HEGRA in VHE after 232 h of observation Most likely a core collapse Supernova Extension in optical, X-ray, radio ~ 4’ Chandra

6. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Cassiopeia A MAGIC Observation: T obs = 47 h 86% under moonlight conditions 29° < ZA < 45° Point-like excess at the position of Cas A with 5.2 σ significance Position is coinciding within the errors with the HEGRA measurements

7. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Cas A Interpretation MAGIC extends the spectrum down to 250 GeV Very good agreement with HEGRA spectrum Theoretical model by Berezhko can describe the measured spectral energy distribution Good candidate for proton accelerator

8. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de IC 443 VLA 20cm NVSS survey XMM: Troja (2006) Radio, shows MASER emissionHigh soft X-ray flux (no shell) Asymmetric shell-type SNR, 45’ diameter (distance ~1.5 kpc) Complex morphology at different wavelength Unidentified EGRET source inside Only upper limits in VHE gamma rays

9. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de MAGIC J0616+225 Point-like source at (RA, DEC) = (06h16m43s, +22 ° 31’48”) statistical position error: 1.5’ and systematic error 1’ Significance: 5.7 σ

10. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de MAGIC J0616+225 Spectrum Flux of MAGIC J0616+225: above 100 GeV ~ 6.5% Crab above 300 GeV ~ 2.8% Crab Acceleration process in MAGIC J0616+225 is currently unknown

11. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Galactic Source Targets MAGIC mainly pointed at candidate sources Globular ClusterSNRPWNPulsars Microquasar, HMXB Binaries / Microquasars

12. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de LS I +61 303 Gamma ray binary discovered by MAGIC Compact object unknown B0Ve star as optical companion Highly eccentric orbit e = 0.72 Periodic emission with orbital Period (P = 26.496 d) in Optical, Radio and X-ray VHE emission strongly variable T 75.1 Dedicated talk

13. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de LS I +61 303 Discovery: T obs = 54 h Broad emission peak around phase 05-07 System is quite at periastron Periastron Deep exposure in fall 2006 T obs = 112 h Highest emission phase 0.6-0.7 Preliminary Albert et al Science 2006

14. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de LS I +61 303 Spectrum in phase 0.6-0.7 consistent with a power law of spectral index Γ = 2.6 +/- 0.2 stat Spectral photon index seems to be constant during orbit and within one year Preliminary Stable spectral index Variable flux levels Phase 0.6 - 0.7 Phase 0.5 - 0.6 Phase 0.4 - 0.7 (Science)

15. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Cygnus X-1 Cygnus X-1 most famous HMXB BH – O-type binary One of the strongest galactic X-ray sources Microquasar (one sided jet) Circular orbit of 5.6 day period Mirabel 2006

16. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Evidence for VHE emission Out of 26 nights one night shows significant signal Dividing night into half yield 4.1 σ evidence

17. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Microquasars GRS 1915 +105 (T obs = 13.4 h ToO) BHB with M BH ~ 14 M Sol Period 33.5 days Companion M star ~ 1 M Sol Superluminal ejection (radio) Distance 6 – 11 kpc Cyg X-3 (T obs = 25.3 h ToO) BHB candidate Period 0.2 days (very compact) Companion WR star 2 sided Jets Distance ~ 10 kpc Preliminary

18. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de HEGRA Whipple Milagro & Tibet EXTENDED with radius ~ (6.2  1.2  0.9) arcmin HARD SPECTRUM with index -1.9  0.1 stat  0.3 sys INTEGRAL FLUX > 1 TeV at the level of ~ 5% Crab DEEP EXPOSURE : 278 h (Aharonian et al, 2005) ‏ 1989-1990: 3.3  12% Crab at 600 GeV 2003-2005: 6.1  pre-trial 8% Crab, 9' apart! ( Lang et al., 2004 )‏ ( Konopelko et al., 2005 )‏ Very extended region! 20 TeV Flux above HEGRA but contribution of diffuse emission? TeV J2032 +4130

19. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de MAGIC View of TeV J2032 +4130 Observation in 2005-2007 yield ~ 94 hours data (moonlight observation) Extension 5.0 +/- 1.7 stat +/- 0.6 syst arcmin (assuming gaussian shape) 5.6 σ significance

20. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de TeV J2032 +4130 Spectrum Integral flux F (E > 1 TeV) ~ 3 % of Crab Nebula flux Spectrum: dF/dE = 4.5 +/- 0.3 x 10 -13 (E/ 1TeV)^-2.0 +/- 0.3 Source type unknown “Dark accelerator” Spectrum and flux compatible with HEGRA measurements

21. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Summary of Observations MAGIC confirms Cas A as VHE source and extends spectrum TeV J2032 is detected and compatible with HEGRA measurement New source discovered MAGIC J0616 +225 in the SNR IC443 LS I +61 303 is studied detailed with a lot of new insights Evidence for VHE emission from Cyg X-1 in an “outburst” Upper Limits to other microquasars GRS 1915 and Cyg X-3

22. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Binary Summary LS I is regularly detected and detailed studied Evidence of VHE gamma rays from Cyg X-1 No detection of GRS 1915 and Cyg X-3 Transient sources (Cyg X-1) Still unknown mechanism which produces VHE gamma rays Very interesting topic since many open questions

23. Tobias Jogler Max – Planck Institut für Physik jogler@mppmu.mpg.de Imaging Air Cherenkov Telescopes ~ 10 km Particle shower ~ 1 o Cherenkov light ~ 120 m γ Cherenkov light image of particle shower in telescope camera Reconstruction of: arrival direction, energy reject hadron background