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BDRv3 - November 26, 2008 - Markus Kissler-Patig

E-ELT Programme. E-ELT Science Case. Markus Kissler-Patig. BDRv3 - November 26, 2008 - Markus Kissler-Patig. 1. E-ELT Programme. The Science Case against which we evaluate the project resides on three pillars: - contemporary science cases (DRM, instrument teams, DRSP, ...)

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BDRv3 - November 26, 2008 - Markus Kissler-Patig

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  1. E-ELT Programme E-ELT Science Case Markus Kissler-Patig BDRv3 - November 26, 2008 - Markus Kissler-Patig 1

  2. E-ELT Programme The Science Case against which we evaluate the project resides on three pillars: - contemporary science cases (DRM, instrument teams, DRSP, ...) - synergy with other facilities (8m-class telescopes, interferometry, ALMA, JWST, LSST/surveys, SKA, ...) - discovery potential (open unique parameter space, be prepared for the unexpected, ...) BDRv3 - November 26, 2008 - Markus Kissler-Patig 2

  3. Contemporary Science

  4. Planets & Stars Stars & Galaxies Galaxies & Cosmology

  5. Planets & Stars

  6. From giant to terrestrial exo-planets: detection, characterisation and evolution • Circumstellar disks • Young clusters and the Initial Mass Function

  7. Stars & Galaxies

  8. Imaging and spectroscopy of resolved stellar populations in galaxies • Black holes and AGN

  9. Galaxies & Cosmology

  10. First light: the physics of highest-redshift galaxies • IGM, metal enrichment • A dynamical measurement of the expansion history of the universe

  11. Synergy with Large Facilities

  12. The main synergy is expected with: • The 8-10m class Telescopes (VLT/I, ...) • The JWST • ALMA • LSST • SKA / SKA Pathfinders • ...

  13. JWST key science • The End of the Dark Ages: First Light and Reionization • Assembly of Galaxies • ➱ optical/NIR sensitive multi-object spectrographs • The Birth of Stars and Protoplanetary Systems • Planetary Systems and the Origins of Life • ➱mid-IR instrument (high spatial/spectral resolution at 3-15 μm) • ➱ planet-finder (incl. low-resolution spectroscopy and polarimetry)

  14. ALMA key science • Detect spectral line emission from CO or CII in a normal galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours of observation. • ➱ NIR sensitive integral spectrograph and imager • Image the gas kinematics in protostars and in protoplanetary disks around young Sun-like stars at a distance of the nearest star-forming clouds. • ➱ NIR and mid-IR high-spectral resolution instruments • Provide precise images at an angular resolution of 0.1 arcsec.

  15. The Unknown

  16. Enabling discovery is achieved by opening parameter space (see Martin Harwit: “Cosmic Discovery”) The E-ELT excels - in collecting power and - in spatial resolution. These should not be compromised and pushed into a range unattained previously.

  17. E-ELT Programme The End BDRv3 - November 26, 2008 - Markus Kissler-Patig 17

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