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Francisco Javier Castander Serentill

Exploiting the Mid-InfraRed to understand galaxies Extragalactic research from Dome C. Francisco Javier Castander Serentill. Institut d’Estudis Espacials de Catalunya (IEEC) Institut de Ci ències de l’Espai (ICE /CSIC) Barcelona.

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Francisco Javier Castander Serentill

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  1. Exploiting the Mid-InfraRed to understand galaxies Extragalactic research from Dome C Francisco Javier Castander Serentill Institut d’Estudis Espacials de Catalunya (IEEC) Institut de Ciències de l’Espai (ICE/CSIC) Barcelona

  2. What can we measure about galaxies? • How many photons: Flux: colours, SED, luminosity • How photons are distributed spatially: Morphology: size, shape • How photons are distributed in λ: SED: redshift, stellar population & gas: Z, t, SFR, IMF • How photons are distributed in λ: kinematics

  3. Understanding galaxies Properties distribution functions: mass, luminosity, morphology, kinematics, colour, metallicity Correlations Environment Evolution

  4. Surveys to unveil properties of galaxies • Galaxy properties are diverse, complex and depend on many parameters => Need large number to characterize variance & evolution => Need large volumes at different z • Large Surveys required

  5. Surveys to characterize Large Scale Structure • Matter difficult to trace. Galaxies (and clusters) best tracers but biased • Typical distances few Mpc & cosmic variance => Need large volumes • Large Surveys required

  6. Surveys to characterize Cosmology • Dark Matter and Dark Energy • Dependency: expansion rate H(z) & growth rate of perturbations D(z) => Need large volumes • Probes: Clustering (BAO), Weak Lensing, Cluster abundances, SNIa • Large Surveys required

  7. Extragalactic Surveys A compromise between area and depth taking into account time and facilities constraints and science goals

  8. Where do we stand? Low redshift • SDSS • 2dFGRS • 2MASS, DENIS

  9. Blanton et al 2003

  10. Blanton et al 2003

  11. Brinchmann et al 04

  12. Where do we stand? Intermediate redshift • VVDS • DEEP2 • COMBO-17, ALHAMBRA • CFHTLS

  13. Where do we stand? High redshift Deep Surveys • HST • Spitzer • (Chandra, XXM-Newton, GALEX)

  14. What is coming next? • CFHT-LS • VST/VISTA/UKIDSS • DES/PanStarrs • WFMOS • KMOS/EMIR • LST • ELT • JDEM, JWST, Herschel, WISE,….

  15. VISTA Dark Energy Survey Baryon Acoustic Oscillations

  16. What is needed next or what is missing currently? Can Dome C play a role in this game? • Spectroscopy: highly multiplexing? • Imaging?

  17. Area-depth-wavelength coverage parameter space

  18. What would we learn if we try to fill the gap? • Modeling & simulations • Spitzer experience

  19. Davoodi et al 2006

  20. Davoodi et al 2006

  21. Mid-IR Band information • L: stellar mass • N: PAH • Q: dust

  22. Is it feasible? • For a 3-m type telescope in the L band it could be possible to reach galaxies to z~0.5 • M band, to z~0.1 • N and Q only local strong emitters

  23. Other possible advantages of Dome C • Seeing: (Busarella’s talk yesterday) • Synergies with SZ surveys • Photo-z

  24. Conclusions Possibilities for extragalactic studies at Dome C • Hard to compete with other observatories in wide field surveys • Low thermal background: Limited gain in mid-IR • Seeing: possible gains • Time monitoring: strong lensed QSOs

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