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Exploring Exozodiacal Disks in Planetary Systems

This panel delves into exozodiacal disks, debris disks, asteroid collisions, and comet outgassing, examining the luminous nature of dust in planetary systems. Observations, simulations, and the significance of exozodi issues in both visible imaging and IR interferometry are explored. The discussion also addresses the tools, sensitivities, and future prospects for studying exozodis and Kuiper belts in different planetary systems.

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Exploring Exozodiacal Disks in Planetary Systems

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  1. P3 panel: exozodiacal disks O. Absil & C. Eiroa with inputs fromA. Roberge, D. Defrère, C. Beichman, W. Danchi, J.-C. Augereau, etc.

  2. Dust in planetary systems • We all live in a debris disk! • Asteroid collisions • Comet outgassing • Dust is luminous (much more than the Earth) • Dust is expected in any planetary system Kuiper belt: 40 K, 50 AU Zodiacal disk: 300 K, 1 AU

  3. Dust not uniformly distributed Observations Simulations Earth at 1 AU Stark & Kuchner 2008

  4. The exozodi issue: visible imaging • 10-100 zoditolerable for closesttargets • Asymmetriesneedthorough investigation 2m 4m 6m 8m 12m

  5. The exozodi issue: IR interferometry • Shot noise: 100 zodi tolerable in average • Preserves 75% of mission outcome • Asymmetries: ~10 zodi tolerable

  6. But ... do we really care? • If Solar system is the rule, “Earth explorer” could just skip unsuitable systems • Can afford to loose some time • EZs interesting on their own • What if EZ mode is around 10 zodi? 100 zodi? • Is the distribution log-normal at all? Bimodal? 100 zodi? Bad systems 10 zodi? < 1 zodi? 0.01 0.1 1 10 100 1000

  7. What we know: exo-Kuiper belts 100 × solar • Detected since 1984 • IRAS, ISO, Spitzer • Sensitivity ~ 100 × solar • Herschel • Down to 1 ×solar • Actual distribution will soon be known for the cold parts • What about warm parts? Bryden et al. 2006

  8. What we want to know: exozodis • Mid-infrared most suited • Photometry • Spitzer: IRS, MIPS • Imaging • 10-m telescopes, (JWST) • Interferometry • Keck Nuller, VLTI/MIDI • Near-infrared can help • Interferometry • CHARA/FLUOR, VLTI/VINCI

  9. Exozodis: where we stand • IRS, MIPS • 1000 zodi at 3-σ • Large sample • ~2% of systems • Keck Interferometer Nuller • 300 zodi at 3-σ • Small sample (on-going) • K-band interferometry • 1000 zodi at 3-σ • Small sample (on-going) • ~20% of MS stars with large amount of hotdust?? • EZs≠ from solar zodi?? KIN 300 zodi 0.01 0.1 1 10 100 1000

  10. Whatneeds to bedone? • Solution #1 • Use models to connect Kuiper beltswithexozodis • Problem: planetary system architecture matters! • Solution #2 • Survey exozodisto buildhistogram • Whatshouldbe the goal sensitivity? • Probablyaround 30 zodi (3-σ) • Solution #3 • Characteriseexozodisaround all identifiedtargets • (need to wait for SIM or RV detections, and to reach 10 zodi)

  11. Whatdoesittake? • LBTI • Expect ~30 zodiat 3-σ • Survey starting> 2012 • 60 targets: sufficient? • Other possible nullers • ALADDIN • Balloon • FKSI/Pegase • Other instruments • Small coronagraphs: needto beinvestigated

  12. Conclusions / recommendations • Invest in modelling • Probability distribution (log-normal? bimodal? other?) • How deep is enough? 30 zodi? • Asymmetries: better predictions needed! • Invest in LBTI • Could greatly reduce the exozodi problem if it lives up to the expectations • Support development of other exozodi finders • ALADDIN, balloon, FKSI (share the same payload) • Small coronagraphs?

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