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MAGIC observations of Galactic sources

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1 MAGIC observations of Galactic sources
Theoretical part Technical part Experimental part The Čerenkov technique The MAGIC Telescope Data analysis Barcelona IFAE Barcelona UAB Barcelona UB Inst. Astrofísico Canarias U.C. Davis U. Lodz UCM Madrid MPI Munich INFN/ U. Padua INFN/ U. Siena U. Humboldt Berlin Tuorla Observatory Yerevan Phys. Institute INFN/U. Udine U. Würzburg ETH Zürich INR Sofia Univ. Dortmund MAGIC observations of Galactic sources Diego F. Torres First GLAST Symposium

2 MAGIC-I and -II: the instruments
Summary MAGIC-I and -II: the instruments Description of the instruments Schedule of MAGIC-II MAGIC-I: some Galactic results

3 Analog signal transport >300 MHz digitizers
MAGIC I and II MAGIC-I Latest Results Analog signal transport >300 MHz digitizers 17m Ø reflector Active Mirror Control PMT camera Amplification: Pre-amplification and then In the receivers_ the signal is splitted in 2 branch, one to record the low gain signal and a delayed one to record high gain signal. Carbon fiber structure

4 Description of the instrument
MAGIC I and II MAGIC-I Latest Results Description of the instrument MAGIC is an Imaging Air Cherenkov telescope operating in the energy range E>50 GeV. Located at Roque de Los Muchachos observatory, Canary Islands, Spain, 28.8°N, 17.9°W, ~2200 m a.s.l.. Largest single-dish (17 m Ø)  intends to lower energy threshold PMT camera with 3.5 Ø FOV Angular resolution () ~ 0.1 Energy resolution 20-30% Flux sensitivity: 2.5% Crab Nebula flux with 5s in 50h Fast repositioning (<40s average) for GRB observation 1 Sigma 0.1, Energy resolution 20% a 1 TeV and 30% a 100 GeV, energy threshold (trigger 50 GeV) Moon shine Moon light

5 MAGIC I and II MAGIC-I Latest Results MAGIC-II: schedule Foundation, rails, frame, motors and drive equipment are already in place. Entering production for mirrors and electronics. Expect to start comissioning in Fall 2007, synchronous with GLAST. For DT=60 the sensitivity worses only by 15% (from 2.5% to 2.9% Crab Nebula) Absolute cleaning level Cuanto cambia a maxima iluminacion November 2006

6 MAGIC-II: expected performance
MAGIC I and II MAGIC-I Latest Results MAGIC-II: expected performance Expect a factor 2 better sensitivity. Gain may be larger below 100 GeV, i.e., effectively reduced analysis threshold. For DT=60 the sensitivity worses only by 15% (from 2.5% to 2.9% Crab Nebula) Absolute cleaning level Cuanto cambia a maxima iluminacion

7 The galactic plane: TeV galactic sources
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI The galactic plane: TeV galactic sources HESS SCAN (l=+30,-30) 30o ZA TeV J +180 -180 +90 -90 IC 443 W66 ( Cygni) Gal C Me falta mirar el scan de verano J LSI J SNR PWN unidentified XRB Crab W44

8 SNR Connection: HESS J1813 & HESS J1834
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI SNR Connection: HESS J1813 & HESS J1834 After HESS discovery - X-rays ASCA - INTEGRAL - RADIO VLA (SNR G ) HESS J Associated with the SNR G Radio (20 cm VLA): White et al 2005, Brogan et al 2005 Hard X-rays (Integral): Ubertini et al 2005.

9 SNR Connection: HESS J1813 & HESS J1834
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI SNR Connection: HESS J1813 & HESS J1834 HESS J MAGIC: Section of shell spatially coincident with SNR G Zenith angle: 47°-54° – Threshold: 400 GeV – 25 hours ASCA Associated with the SNR G VLA

10 SNR Connection: HESS J1813 & HESS J1834
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI SNR Connection: HESS J1813 & HESS J1834 HESS J Molecular clouds: CO data [studied in detail for MAGIC paper] VLA: 20 cm radio 70 km/s < v < 85 km/s

11 SNR Connection: HESS J1813 & HESS J1834
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI SNR Connection: HESS J1813 & HESS J1834 HESS J SNR G (W 41) Zenith angle 37°-44° Threshold 150 GeV Existence of dense cloud, also reported by MAGIC (12 and 13CO) Mejor plot

12 Galactic Center MAGIC I and II Extragalactic targets Galactic sources
MAGIC-I Latest Results Extragalactic targets Galactic sources LSI Galactic Center 17.5’ x 14.5’ Chandra X-ray map Sgr A East SNR Sgr A West Sgr A* MAGIC skyplot Radio contours VLA 90 cm Observed for 17h Jul/Aug.05; ZA:58˚-63˚ - 6 σ signal - α = -2.2±0.2 - 600 GeV - 15 TeV - Excellent agreement with H.E.S.S. ; incompatible with CANGAROO

13 MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI PSR /CTB80 Upper limits to the steady emission: below theoretical predictions Upper limits to the pulsed emission imply a cutoff energy <32 GeV

14 LSI +61 303 Detected by MAGIC Detected by HESS MAGIC I and II
MAGIC-I Latest Results Extragalactic targets Galactic sources LSI LSI Detected by MAGIC Detected by HESS

15 LSI +61 303 High Mass X-ray binary at a distance of 2 kpc
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI LSI High Mass X-ray binary at a distance of 2 kpc Optical companion is a B0 Be star of 10.7m 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 0.2 0.1 0.3 0.5 0.9 0.7 0.4 AU To observer

16 MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI LSI MAGIC observed the source for six orbital cycles in Clear detection far from periastron (phases ). Albert et al. 2006

17 LSI +61 303 No significant emission close to periastron.
MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI LSI periastron No significant emission close to periastron. Hint at periodic emission Maximum found for phase Flux at maximum 16% crab. Maximum before periodic radio outburst at phase 0.7 (Ryle telescope). Oct 2005 Nov 2005 Dec 2005 Jan 2006 Feb 2006 Mar 2006 Albert et al, Science Average

18 MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI LSI Average Spectrum: straight power law spectrum from 400 GeV to 4 TeV:  = -2.6  0.2 (stat)  0.2 (syst) Albert et al, Science No evidence for cutoff up to 5 TeV

19 MAGIC I and II MAGIC-I Latest Results Extragalactic targets Galactic sources LSI On the nature of LSI Radio observations resolved a extended structure which was interpreted as a jet  microquasar? BUT! Recent results show that the outflow could be produced by the interaction of a pulsar wind and the companion star’s wind.

20 Conclusions MAGIC is in its second year of regular observations.
It is starting production of major elements of MAGIC-II: aim at completion by Fall 2007. Galactic highlight: variability of g-ray binary LSI Follow up studies conducted in fall 2006 to give precisions on periodicity First MW campaign conducted at the gamma-ray maximum (CHANDRA+MERLIN+VLBA), Second MW campaign -including harder X-rays- programmed for 2007 Reports on newly detected galactic sources waiting forthcoming data release

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