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Microquasar searches with MAGIC

Microquasar searches with MAGIC. Núria Sidro Institut de Física d’Altes Energies (IFAE) Barcelona. International School of Cosmic Ray Astrophysics Erice, Sicily, 10 July 2004. Double-star system = collapsed object (BH or NS) + normal star. Ejected plasma at apparent Superluminal motion.

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Microquasar searches with MAGIC

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  1. Microquasar searcheswith MAGIC Núria Sidro Institut de Física d’Altes Energies (IFAE) Barcelona International School of Cosmic Ray Astrophysics Erice, Sicily, 10 July 2004

  2. Double-star system = collapsed object (BH or NS) + normal star Ejected plasma at apparent Superluminal motion Mirabel & Rodriguez, Nature 1994 GRS1915+105 Mirabel et al, Nature 1992 1E1740.7-2942 Microquasar = X-ray binary star displaying relativistic Radio-jets. What is a microquasar?

  3. Quasar Microquasar MBH~ 108M T ~ 105K accretion luminosity OPTICAL & UV Radio jets Million LY time scales of years MBH~ 10M T ~ 107K accretion luminosity X RAY Radio jets few LY time scales of minutes Observed Morphological & Physical similarities

  4. multi-wavelength Compact jets Radio & Gamma IR & UV

  5. Radio IR Optical UV X-rays Gamma-rays MAGIC sensitivity • Model: • Leptonic jet • Strong magnetic field • Dominant stellar IC multi-wavelength (Bosch-Ramon et al, A&A 2004)

  6. LSI+61 303 AX J1639.0-4642 LS 5039 168 Unid -> some could be μQ High-massμQ have been proposed as the counterparts of the variable EGRET sources of the galactic plane. (Kaufman Bernadó et al. 2002, Romero et al. 2004) μQ EGRET sources

  7. LSI+61 303 μQ EGRET sources EGRET detection EGRET extrapolation MAGIC sensitivity cut-off Model (Bosch-Ramon et al) For Eth<100GeV  Observation Time for 5σ is < 50 hours

  8. μQ EGRET sources Northern Hemisphere • LSI +61 303 • SS 433 • AX J 1639.0-4642 • Cygnus X1 • Cygnus X3 • GRS 1915+105 • XTE J118+480 130 High 150 Low Mass X-ray binary sources 16 μQ in our Galaxy Being observed by MAGIC May/2004 Flare ASM ( 2-10 KeV)

  9. Summary • μQ present a broad band spectrum. • Gamma-rays can arise in IC processes when the relativistic e- of the jet interact with external photons from the massive companion. • The obtained results for the μQ LS 5039, LSI +61 303 and AX J1639.04642 point towards a population of HMXB μQ, as counterparts of low galactic latitude unidentified EGRET sources. • MAGIC is ready to discover a new population of μQ emitting VHE Gamma-rays.

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