Johan Olofsson MPIA Heidelberg

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The power of interferometry ‣ Near- & mid-IR interferometry at the VLTI ‣ High angular resolution: few milli-arcsec (1 mas, 0.1 AU @ 100 pc) ‣ Near-IR: sensitive to warm dust ‣ Let’s use all possible VLTI facilities ! ‣ AMBER (<strong>Olofsson</strong> et al. 2011) ‣ PIONIER, MIDI, NaCo/SAM (<strong>Olofsson</strong> et al. 2013a) ‣ MCFOST = SED + raytraced images (V 2 , closure phases) ‣ Multi-techniques, multi-wavelength, multi-resolution
The inner disk ‣ Narrow disk: 0.07-0.11 AU ‣ High temperatures: sublimation of smallest silicates (1500 K) ‣ Large scale height: H/R = 0.2 ‣ High temperature gas ‣ (Thi et al. 2011) ‣ Warped disk (optical variability ‣ Schisano et al. 2009) ‣ ISAAC proposal: time monitoring
Page 1 and 2: Planetary formation in transition a
Page 3 and 4: Giant & telluric planetary formatio
Page 5: The transition disk around TCha ‣
Page 9 and 10: The outer disk ‣ Most likely narr
Page 11 and 12: A candidate companion ‣ Huélamo
Page 13 and 14: Hints for a companion ‣ Large gap
Page 16 and 17: Debris disk Final product of star f
Page 18 and 19: Warm debris disk around HD 113766 A
Page 20 and 21: One or two dust belts ‣ One dust
Page 22 and 23: Origin of the dust ‣ Massive coll
Page 24 and 25: Origin of the dust ‣ HD 113766 A:
Page 26: Take away messages ‣ SED modeling

Johan Olofsson MPIA Heidelberg

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