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(thermal) IR instruments from Antarctica: what can be gained Ralf Siebenmorgen

(thermal) IR instruments from Antarctica: what can be gained Ralf Siebenmorgen. Why ? pwv , T, aerosols IR projects: DomeC and elsewhere Science cases Conclusion: my favoured modes. (thermal) IR := 2-24µm = K,L,M,N,Q . Atmospheric optical thickness spectrum.

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(thermal) IR instruments from Antarctica: what can be gained Ralf Siebenmorgen

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  1. (thermal) IR instruments from Antarctica: what can be gained Ralf Siebenmorgen • Why? pwv, T, aerosols • IR projects: DomeC and elsewhere • Science cases • Conclusion: my favoured modes (thermal) IR := 2-24µm = K,L,M,N,Q

  2. Atmospheric optical thickness spectrum

  3. Atmospheric transmission • 1 - 2.5µm opens up • OH emission remains • Kdark filter Paranal Dome C (30m)

  4. Atmospheric transmission Paranal Dome C (30m)

  5. Atmospheric transmission Paranal Dome C (30m)

  6. Sky background: temperature

  7. Sky background: Burton et al. 2005 - PWV Low: - temperature - aerosol

  8. Seeing at Dome C Beckers’08 8m 30m

  9. AO at Dome C – what is done at E-ELT ? sky coverage 2’ 1’ • 4-6 LGSs (cone effect) • Correction on axis • 1 deformable mirror NGS Single Conjugate AO L T A O

  10. LTAO AO at Dome C – what is done at E-ELT ? G L A O Wide corrected FoV • 5 LGSs/ WFSs • 1 DM • FoV ~ 6’

  11. AO at Dome C – what is done at E-ELT ? PSF uniformity • >6 LGSs/ WFSs • >3 NGS • >2 DM • improve corrected FoV 2’ 1’ GLAO M C A O

  12. AO at Dome C ? GLAO Tower solution • Technical issues • maintenace GLAO -> next talk by MarcellCarbillet

  13. GLAO Tower solution maintenance • Vibration • Footing • Thermal bending • Icing Beckers’08

  14. Dome sizes

  15. Dome sizes

  16. IR projects at Dome C • This session : • IRAIT(International Robotic Antarctic IR Tel.) MaurizoBusso • AMICA(Antarctic Multiband IR Camera ) Mauro Dolci

  17. IR projects at Dome C • WHITE • 2.4m tel. • 0.3” resolution • 0.7deg2fov • 1-5µm ? • Surveys • LMC • weak lensing • SN(z<0.2) PI: Denis Burgarella

  18. IR projects at Dome C

  19. IR projects at Dome C

  20. MIR instrument at Dome C Point source sensitivity 10σ/1h K 2µJy L 80µJy M 200µJy N 8mJy Q 200mJy Burton et al ‘05 N band: pfov 0.5”; 1kx1k detector Mora et al. (this session)

  21. Present MIR instruments: <8m None in the South

  22. Present MIR instruments: ≥8m 4

  23. R~900

  24. flux [ mJy] Dome C: IR sensitivities in context NACO Spitzer NACO Dome C ~VLT 0.1 1 10

  25. Science in the Galaxy Formation of stars in MC: surveys Evolution of proto-planetary & debris disks: spectral index 3-10µm Life cycle of dust Planet: transits in K MIR spectro-polarisation

  26. MIR spectra

  27. MIR spectro-pol IR3481 Wright’08

  28. Monitoring of X-ray flares of the GC at 10µm

  29. MIR surveys Whitney ‘08

  30. SN light curves in K + rapid monitoring GRB at high z Burgarella ‘08

  31. IR instruments from Antarctica: • - 2m telescope (+ tower) • Surveys • wide field imaging: K,L band • SED: K,L,M,N,Q • low resolution spectro-polarisation in N • Monitoring • Sgr A* • SN • GRB

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