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ELLIPTICALS AND HIGH-REDSHIFT UNIVERSE: D iscussion

ELLIPTICALS AND HIGH-REDSHIFT UNIVERSE: D iscussion. Francesco Calura INAF/O. A. Bologna. A few Questions still open, from:. Pagel, B., 2002, ASPC, 253, 509. How do galaxies form? When do the stellar populations of their sub-components form?

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ELLIPTICALS AND HIGH-REDSHIFT UNIVERSE: D iscussion

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  1. ELLIPTICALS AND HIGH-REDSHIFT UNIVERSE:Discussion Francesco Calura INAF/O. A. Bologna

  2. A fewQuestionsstill open, from: Pagel, B., 2002, ASPC, 253, 509

  3. How do galaxies form? • When do the stellar populations of their sub-components form? • What are the principal feedback/quenching mechanisms? • Scaling relations of ETG: can they be reproduced w/in LCDM?

  4. Results from a SAM (FC & Menci, 2011, MNRAS, 413, L1)

  5. Results from a SAM – No AGN Model Slope=-0.02 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)

  6. Results from a SAM – With AGN Model Slope=0.03 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)

  7. Results – No AGN, with ITS Model Slope=0.11 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)

  8. Results – with AGN+ITS Model Slope=0.21 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)

  9. What is the chronology of the Hubble sequence? (And role of Main Sequence galaxies) • What have we learned (and what can we really learn ever) from numerical simulations and SAMs?

  10. ‘Unsatisfied Observers’ (S. Lilly) + Frustrated theoreticians = Lack of trust in ‘physical’ (i.e. fully cosmological) models

  11. Use of ‘Simple’ (i.e. analytical) models to describe galaxy evolution Lilly et al. 2013

  12. Tworegimes of cosmic (s)SFR evolution • Spheroids (at z>2) • Discs (at z<2) Fig. from Pipino et al., 2013, MNRAS, 432, 2541

  13. How do galaxies form? • When do the stellar populations of their sub-components form? • What are the principal feedback/quenching mechanisms? • Scaling relations of ETG: can they be reproduced w/in LCDM? • What is the chronology of the Hubble sequence? (And role of Main Sequence galaxies) • What have we learned (and what can we really learn ever) from numerical simulations and SAMs?

  14. How do metals escape from galaxies (ram pressure, winds…driven by which mechanism (Sne and/or AGN) • Is ICM typical of IGM (as traced by Lya-forest) in general? • Does either the metallicity or abundance pattern vary with z?

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