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LGS-AO observations of the HV Tau C edge-on protoplanetary disk

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. LGS-AO observations of the HV Tau C edge-on protoplanetary disk.

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LGS-AO observations of the HV Tau C edge-on protoplanetary disk

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  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 LGS-AO observations of the HV Tau C edge-on protoplanetary disk Keck Science Meeting – Sept 18 2008

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

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

  4. The HV Tau triple system • 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 DSS2 blue HST/WFPC2 1” Stapelfeldt et al. (2003) G. Duchêne – Keck Science Meeting – Sept 18 2008

  5. Keck AO images • New images in NGS (55 Hz) and LGS mode • L’ (3.78 μm) and Ms (4.67 μm) filters • Strehl ratios of 70-80% • LGS AO dataset deeper and sharper HST/WFPC2 Keck LGS-AO Keck NGS-AO 0.6-0.8 μm 3.8 μm 4.7 μm G. Duchêne – Keck Science Meeting – Sept 18 2008

  6. Additional AO images • 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. Major features 0.8μm 1.6μm 3.8μm • 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 0.1” G. Duchêne – Keck Science Meeting – Sept 18 2008

  8. Modeling strategy • Panchromatic fit to broad dataset to constrain the disk main properties • Disk mass, overall structure • Grain size distribution (amax) • 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) Pinte et al. (2006) Grid of ~106 independent models; 50,000h of CPU time G. Duchêne – Keck Science Meeting – Sept 18 2008

  9. Preliminary results • 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. Summary • 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! HV Tau C HK Tau B G. Duchêne – Keck Science Meeting – Sept 18 2008

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