1. Ge/Ay133 Can we study extrasolar Kuiper Belts?  Pic, A5V star AU Mic, M1Ve star

2. Impossible to see any exo-KBOs themselves, but…

5. How do we find debris disks? Model has 0.1 M moon of 30  m size dust grains in a disk from 30–60 AU Bars are 3  Model based on disks around A stars Spitzer Data (FEPS team) Meyer et al., ApJS, 154, 422

6. What have far-IR SED surveys found?: Overall decay consistent with erosional evolution, fluctuations dominated by large collisions? Rieke et al., ApJ, 620, 1010

16. So, when rings are seen around >10 Myr old stars… the dust must be made in place. CSO/HST have reached similar conclusions about structure of the disk around Fomalhaut and how it is generated. Is there a planet required to maintain it (Kalas et al. 2008)? Marsh et al. – ApJ, Feb. 2005 Kalas, Graham, & Clampin – HST, Nature, June 2005

17. Vega arcsec IRAM Plateau de Bure 1.3 mm Wilner et al. 2002

18. Vega simulation – Marc Kuchner (GSFC)

19. What about “exo-zodii’s? That is, dust in ~1 AU range? Rare! Only one convincing case so far, in large aperture searches. Need to get closer to the star…. Beichman et al., ApJ, 626, 1061

22. Keck Interferometer

23. What about gas? -Most searches negative, but “right” tracers (H 2, C II) difficult to observe - Sharp rings suggestive of small amount of gas - Falling evaporative bodies? (next page)

24. FEBs = Falling Evaporative Bodies See transient redshited absoprtion against stellar continuum. Evaporating comets? For the brightest sources (e.g.  Pic), you can actually image things like Na I line emission and map the disk.

25. Next time: What can comets tell us about the early S.S.? Deep Impact (Comet Tempel 1) Comet Hale-Bopp