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Debris Disk Science with GMT

Debris Disk Science with GMT. Inseok Song, University of Georgia. Zodiacal light: APOD: 2010 Sep 13, Taken in Namibia after a sunset in June. for “Opening New Frontiers with the Giant Magellan Telescope” in Oct 2010. Why Debris Disks?. NRC Astro2010 Report

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Debris Disk Science with GMT

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  1. Debris Disk Science with GMT Inseok Song, University of Georgia Zodiacal light: APOD: 2010 Sep 13, Taken in Namibia after a sunset in June. for “Opening New Frontiers with the Giant Magellan Telescope” in Oct 2010

  2. Why Debris Disks? • NRC Astro2010 Report Telescopes on the ground and in space have even directly imaged as distinct point sources a few large planets. … we can learn about planetary systems by measuring infrared and radio emission from giant disks of gas out of which planets can form. … Terrestrial planets are relatively small and dim, and are easily lost in the exozodiacal light that is scattered by the dusty disks that typically orbit stars. The observational challenge is great, but armed with new technologies and advances in understanding of the architectures of nearby planetary systems …

  3. Debris Disks and Planets • Debris disks act as indirect evidence of exo-planetary systems. But, at the same time, they are obstacles in direct imaging of Earth-like planets. • Need to understand the architecture of debris disks

  4. Breaking the degeneracy of SEDs large grains at rsmall Debris disk studies are based on Spectral Energy Distribution (SED). same SED with different grain configurations small grains at rlarge grain population over r Need a spatially resolved image of DD

  5. Scattered imaging + thermal imaging • Mplanet=5ME, ap=10AU, β=0.023 • Poynting-Robertson effect caused a grain sorting based on particle size  different appearance at different wavelengths. (Stark et al. 2009) scattered light density 10μm image

  6. Need to spatially resolve Debris Disks • 17 resolved debris disks in scattered light to date (optical and near-IR)

  7. Need to spatially resolve Debris Disks • But only four debris disks imaged in thermal IR To increase the number of spatially resolved debris disks We need 1. Good targets 2. Larger telescope with a better IR imager

  8. Some important facts • Adaptive secondary mirror: • excellent for thermal IR observations  only two warm optics (M1 + M2) • AO corrected mid-IR observations (Strehl ratio > 98%) • Extreme AO : Strehl > 99% • mid-IR imager (MIISE or TIGER): • 5-25mu, • R=5-5000, • FOV=30” • FWHM = 40mas at 5mu, Sun-Earth at 25pc away… 1AU  40mas

  9. Can GMT/TIGER really resolve most Debris Disks? • MMT Adaptive Secondary result as a test case. • Expected Strehl ratio at mid-IR > 98%

  10. Expected performance of TIGER • MMT Adaptive Secondary result as a test case. • Expected Strehl ratio at mid-IR > 98% can do 10-4 suppression Credit: Phil Hinz (Steward Observatory)

  11. Other thermal IR instruments competing w GMT/TIGER • Surface brightness high enough? • Enough targets for statistically meaningful studies? Kuiper Belt Disks

  12. Known Population of Debris Disks from IRAS GMT sensitivity JWST sensitivity currently known debris disk from IRAS (Rhee et al. 2006)

  13. Known Population of Debris Disks from IRAS HIP 7345, 20 Myr old Simulated 1hr 18μm image currently known debris disk from IRAS (Rhee et al. 2006)

  14. GMT/TIGER will image planets also… • Higher exoplanet flux at M and N bands especially for lower mass planets • Typical ages of debris disk stars are < 500 Myr (young, bright planets) Y J H K L N GMT M-band (5σ, 1hr) limit : 5.14 μJy 200 Myr 10MJ planet or 50 Myr 5MJ are about 0.8mJy at M-band detectable in 5min exposure with GMT/TIGER! M 700 K planet 400 K planet

  15. We will image disk together with planets! • GMT/TIGER can detect a 1 MJ planet at various ages. • Expect an image like this!! Composite image of βPictoris disk:10μm, planet:3.6μm

  16. More targets to come! WISE sky coverage as of 2010 Sep Increasing the population of Debris Disks • IRAS fully used • Spitzer being summ. • AKARI wasn’t useful • WISE (about 108 sources) • SPICA (not all-sky)

  17. Anticipated Results • GMT should be able to obtain spatially resolved images of several dozen Debris Disks (both in scattered and thermal light) • Some (or many or most) with embedded planets imaged (both in nearIR and thermal) GMT/TIGER 1hr at M-band 200 Myr F-star @50pc with a 5MJ planet and LIR/Lbol=4x10-4, Tdust=300K

  18. Work To Do: Debris Disk Database To prepare optimal GMT/TIGER debris disk studies, we need a centralportal of debris disk database with a long-term commitment of maintenance (e.g., DwarfsArchive.org) Thanks!!

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