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Antarctic Thermal IR Instruments: Insights & Applications in Astronomy

Explore benefits of thermal IR instruments in Antarctica for studying atmospheric conditions, observing celestial bodies, and conducting IR projects. Learn about DomeC projects, atmospheric optical thickness, atmospheric transmission, advantages of thermal IR modes, and instrumental advancements. Discuss IR projects like IRAIT and AMICA, instrument sensitivities and capabilities, and scientific applications in galaxy formation, planetary studies, and astronomical surveys.

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Antarctic Thermal IR Instruments: Insights & Applications in Astronomy

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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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