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Maximizing the Mid-Infrared Potential of Extremely Large Telescopes: Resolved Spectroscopy and Imaging for Answering Ast

Explore the importance of mid-infrared (MIR) observations using Extremely Large Telescopes (ELT) for resolving spectroscopy and imaging to tackle various astronomical queries. Learn about MIR instruments, sensitivity, spatial resolution, AGN and starburst observations, HR spectroscopy, black hole mass determination, and MIR science cases. Discover the immense potential of ELT in studying the life cycle of dust, star formation, disk architecture for planet formation, solar system dynamics, and more.

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Maximizing the Mid-Infrared Potential of Extremely Large Telescopes: Resolved Spectroscopy and Imaging for Answering Ast

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Presentation Transcript

  1. The Mid-infrared on ELT’s (3 – 25µm) MIR recommended to be essential

  2. R~300

  3. Present MIR instruments: <8m

  4. Present MIR instruments: ≥8m 4 Sensitivity = BLIP x Site x Telescope

  5. A taste of spatial resolution 4m viz 8m AGNvizstarburst unresolved resolved

  6. HR spectroscopy: velocity field Keplerian gas motion-> black hole mass NGC 7582 NeII (12.8µm) Wold et al. 2006 VLT,JWST, … - ≤ 10m - unresolved ELT - > 30m - resolved

  7. flux [ mJy] Spitzer VISIR METIS

  8. MIR/ELT `galactic’ science cases • Life cycle of dust • Star formation • Governing disk architecture for planet formation • Dynamical history of the solar system • …. MIR/ELT will solve host of astronomical questions by resolved spectroscopy and imaging

  9. Formation of stars in MC Evolution of proto-planetary & debris disks Planetformation Solar system: unique? Building blocks & Origin of life

  10. Richness of MIR +extinction Molecules: ~13µm + solid state + PAH + atoms + ions

  11. MIR spectroscopy in: ISM, disks, comets Resolved lines -> velocity information; density, temperature, abundance Single exposure (not with ALMA) Photoevoparative disk wind TW Hya [NeII] flux N2O j ≤ 46 transitions Pascuci&Sterzik’09 wavelength (nm) v [km/s]

  12. Proto-planetary disks - chemical structure of the disk - velocity field and turbulent disk mixing - probe pathways of planet formation scale: --- ELT ---> <---- ALMA ---

  13. Exo-planets - Ground: RV studies + scattered light imaging -> Orbit parameters (M, r, ε) Transit~> atmosphere • Space: Kepler, SIM • improved statistics • ELT/MIR: • Resolving disk structure • Velocity field • Planet thermal emission • Spectroscopy of bio markers

  14. Origin of life ? In-situ search for prebiotic molecules Delivery to Earth via heavy bombardment? -> ELT provide event Statistics of: 3-5µm: ices in comets (Mumma et al.)

  15. Debris disk structure: theory JWST 30m Disk + planet: possible dust density (Ozernoy et al.) 20µm dust emission at 40pc (Wilner et al)

  16. Debris disks with planet: beta Pic Lagrange et al. 3.6µm Telesco et al. 8-25µm ELT -> Statistics on the debris disk structure

  17. Thermal emission of a planet Pantin et al. ‘08

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