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The Magellanic Clouds and dSph satellites. Vienna, April 10-12

Ram pressure induced star formation. Chiara Mastropietro LMU Munich A. Burkert (LMU) & B.Moore (UniZH). The Magellanic Clouds and dSph satellites. Vienna, April 10-12. LMC Parkes HI survey (Stavely-Smith et al. 2003). HI TIDAL FEATURES ??. 20 kpc. 20 kpc.

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The Magellanic Clouds and dSph satellites. Vienna, April 10-12

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  1. Ram pressure induced star formation Chiara Mastropietro LMU Munich A. Burkert (LMU) & B.Moore (UniZH) The Magellanic Clouds and dSph satellites. Vienna, April 10-12

  2. LMC Parkes HI survey (Stavely-Smith et al. 2003)

  3. HI TIDAL FEATURES ?? 20 kpc 20 kpc Smooth old stars distribution (near IR) out to 9 kpc No signs of spiral arms (van der Marel 2001)

  4. Age < 0.5 Gyr Age < 1 Gyr Cioni et al. 2000 (DENIS survey)

  5. Age < 25 Myr

  6. X-ray emission (ROSAT) Blondiau et al. 1997 De Boer et al. 1997Bow shock induced star formation

  7. NGC 5746 Chandra X-ray detection T~0.4 keV (Pedersen et al. 2006) OVI absorption lines through the Galactic halo (Sembach et al. 2002)

  8. Mastropietro et al. 2004

  9. Mastropietro et al. 2004 Putman et al. 2002

  10. Mastropietro, Burkert & Moore in prep. c = 9.5 v200 = 40 km/s  = 0.074 Mdisk/Mdark = 0.1 Mgas = 0.5 Mdisk RHI = 8 Rd Q = 3 Npart = 750000 Nhot =2e6

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