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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:Discussion Francesco Calura INAF/O. A. Bologna
A fewQuestionsstill open, from: Pagel, B., 2002, ASPC, 253, 509
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?
Results from a SAM (FC & Menci, 2011, MNRAS, 413, L1)
Results from a SAM – No AGN Model Slope=-0.02 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)
Results from a SAM – With AGN Model Slope=0.03 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)
Results – No AGN, with ITS Model Slope=0.11 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)
Results – with AGN+ITS Model Slope=0.21 Obs. Slope=0.38 (FC & Menci, 2011, MNRAS, 413, L1)
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?
‘Unsatisfied Observers’ (S. Lilly) + Frustrated theoreticians = Lack of trust in ‘physical’ (i.e. fully cosmological) models
Use of ‘Simple’ (i.e. analytical) models to describe galaxy evolution Lilly et al. 2013
Tworegimes of cosmic (s)SFR evolution • Spheroids (at z>2) • Discs (at z<2) Fig. from Pipino et al., 2013, MNRAS, 432, 2541
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?
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?