1 / 17

The Mid-infrared on ELT’s

The Mid-infrared on ELT’s. (3 – 25µm). MIR recommended to be essential. R~300. Present MIR instruments: <8m. Present MIR instruments: ≥8m. 4. Sensitivity = BLIP x Site x Telescope . A taste of spatial resolution 4m viz 8m AGN viz starburst.

kasi
Télécharger la présentation

The Mid-infrared on ELT’s

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

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

More Related