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Protoplanetary worlds at the AU scale

Explore the environment of young stars and the contribution of broadband infrared interferometry to the knowledge of disk structure. Learn about the first steps towards imaging and the future of infrared astronomy.

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Protoplanetary worlds at the AU scale

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  1. Protoplanetary worlds at the AU scale Jean Philippe Berger J. Monnier, R. Millan-Gabet, W. Traub, M. Benisty, F. Malbet, E. Pedretti Visions for infrared astronomy

  2. Outline • A young star’s environment • The contribution of two telescope broadband infrared interferometry to the knowledge of disk structure • First steps towards imaging • Conclusion Visions for infrared astronomy

  3. A young star’s environment Infrared excess Optical(HubbleAO) /mm imaging Presence of a flared disk of gas and dust associated with bipolar mass loss: winds and/or highly collimated jets, Typical disk sizes: 50-1000AU. Visions for infrared astronomy

  4. The standard disk model e.g. Malbet & Bertout (1995, A&AS 113, 369) • Optically thick disk both for inner gas and outer dust • Simple power-lawtemperature distribution (T a r-0.75, T a r-0.5) • Obliquedisk heating • -> fits rather wellspectral energy distributions (SEDs) Visions for infrared astronomy

  5. Natta, 2001 Dullemond et al. 2001 Optically Thin Cavity Optically Thick, Geometrically Thin Disk Tuthill, Monnier & Danchi 2001 2001: important revision of the model Visions for infrared astronomy

  6. 2T interferometry: the near-IR view • PTI, IOTA and Keck have played a major role in near infrared YSO observing during (Malbet& Berger 98, Millan-Gabet 2001,Akeson2000,02 Eisner2002,2004, Monnier) • Authors concluded Herbig AeBe and T Tauri estimated sizes often bigger than predicted with standard disk model. • Signs for disk flattening at the astronomical unit scale. Eisner, 2004 Visions for infrared astronomy

  7. 2T interferometry: the near-IR view Visions for infrared astronomy

  8. 2T interferometry: the near-IR view Evidence for inner rim (Muzerolle 2004) Flared disk can account for some estimated sizes (Lachaume 2003) Fu Orionis stars observations compatible with standard models provided renmant envelopes or putative companions are taken into account (Malbet 2005, Millan-Gabet 20050 TTauris Visions for infrared astronomy

  9. 2T interferometry: the near-IR view Some visibilities observations are compatible with standard disk (Malbet, 2005) Evolutionary status of these stars should be debated (Monnier 2006) Herbig Be Stars Wind Disk Disk Visions for infrared astronomy

  10. 2T interferometry: the near-IR view Presence of resolved Flux (halo, envelop renmant) IntrinsicVariability Visibility modelling is highly sensitive To the knowledge of short baseline incohernet Flux and stellar vs. disk emission ratio Visions for infrared astronomy

  11. 2T interferometry: the midIR view Flaring Sizes consistent with flat self-shadowed / flaring disk model SED classification Sizes consistent with flat self-shadowed / flaring disk model SED classification Self-shadowed Leinert et al. (2004, A&A, 423, 537) Visions for infrared astronomy

  12. First steps towards imaging Isella et al 2005 • This IONIC3/IOTA campaign was aimed at surveying the brightest HerbigAeBe and Ttauri stars in search for any asymetry (departure from zero closure phase) at the astronomical unit scale in order to select candidates for imaging. • Both a flared disk and disk with inner rim generate asymetries. Visions for infrared astronomy

  13. First steps towards imaging Malbet 2001 • This IONIC3/IOTA campaign was aimed at surveying the brightest HerbigAeBe and Ttauri stars in search for any asymetry (departure from zero closure phase) at the astronomical unit scale in order to select candidates for imaging. • Both a flared disk and disk with inner rim generate asymetries. Visions for infrared astronomy

  14. Visions for infrared astronomy

  15. Results • Essentially zero closure phases • Evidence for resolved flux (incoherent)? Visions for infrared astronomy

  16. Interpretation in the inner rim context Visions for infrared astronomy

  17. Interpretation in the inner rim context Visions for infrared astronomy

  18. Parametric imaging Visions for infrared astronomy

  19. Berger et al, 2006 Image reconstruction: Meimon, Mugnier, ONERA Direct imaging Visions for infrared astronomy

  20. Hot accreting planets in disks? Klahr & Kley (2005, A&A in press) Micro-jets Imaging protoplanetary disks • Imaging the inner AU requires a lot of telescopes and (preferably than) or a lot of array configurations • Model ambiguities often vanish at longer baselines • YSO short baselines images (i.e AO), are essential. • Simultaneous photometry is very important • Understanding the disk structure would ideally require joint near and mid-infrared observations • Second generation VLTI instrumentation is more than welcome. IOTA3 @ H Keck-I @ K CHARA @ K 260 m baseline! Visions for infrared astronomy

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