1. G. Duchêne (UCB) A.M. Ghez (UCLA), C.E. McCabe (IPAC) C. Pinte, F. Menard, G. Duvert, K. Stapelfeldt, D. Padgett, M. Perrin, H. Bouy, D. Barrado, A. Noriega-Crespo, T. Brooke Keck Science Meeting – Sept 18 2008

2.  Key questions for planet formation: Processes? Timescales? Initial conditions?  Map disk structure/content through time  A complementary set of observations G. Duchêne – Keck Science Meeting – Sept 18 2008 Corder et al. (2005) Fukagawa et al. (2004) Tannirkulam et al. (2008) Mariñas et al. (2006)

3. HST Keck AO McCabe et al. (2002) Duchêne et al. (2004) Krist et al. (2004) G. Duchêne – Keck Science Meeting – Sept 18 2008

4.  PMS system in Taurus (~1 Myr, ~0.5 M  )  Tertiary has an opaque 50AU edge-on disk  V=14.5, R=13.0  Limited NGS correction Stapelfeldt et al. (2003) HST/WFPC2DSS2 blue 1” G. Duchêne – Keck Science Meeting – Sept 18 2008

5.  New images in NGS (55 Hz) and LGS mode L’ (3.78 μm) and M s (4.67 μm) filters Strehl ratios of 70-80% LGS AO dataset deeper and sharper HST/WFPC2Keck LGS-AO Keck NGS-AO 4.7 μm3.8 μm 0.6-0.8 μm G. Duchêne – Keck Science Meeting – Sept 18 2008

6.  JHK images obtained at VLT with NAOS Continuous 0.6-4.7 μm coverage at uniform resolution (~0.1” or better) 2.2 μm G. Duchêne – Keck Science Meeting – Sept 18 2008

7.  From 0.6 to 4.7 μm, distance between nebulae decreases  Over same range, nebulae flux ratio decreases as well  Both phenomena are typical of “small” dust grains (not much larger than 1 μm)  Persistent shear-like asymmetry (warp?) Structural feature on scales of many AUs 1.6μm0.8μm3.8μm 0.1” G. Duchêne – Keck Science Meeting – Sept 18 2008

8.  Panchromatic fit to broad dataset to constrain the disk main properties Disk mass, overall structure Grain size distribution (a max ) Spatial variations in dust properties MCFOST (multi-purpose RT code) Scattered light images (0.8 – 3.8 μm) Thermal emission map (1.3 mm) Overall SED (0.5 μm – 2.7 mm) Grid of ~10 6 independent models; 50,000h of CPU time G. Duchêne – Keck Science Meeting – Sept 18 2008 Pinte et al. (2006)

9.  Each dataset has its own “best fit” Objective is to find the best compromise in the grid Best overall model ISM-like dust model

10.  Keck LGS-AO offers Comparable 3-5 μm resolution as HST (optical) Great sensitivity to disks, even in thermal IR  Detailed model for HV Tau C still needs work  Need to expand sample to find trends! G. Duchêne – Keck Science Meeting – Sept 18 2008 HV Tau CHK Tau B