Marco Baldi

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Introduction outline Standard Model and non-standard models of the Universe Dynamic and interacting DE: - constant couplings [MB, V. Pettorino, G. Robbers, V. Springel - 0812.3901 (2010)] - time dependent couplings [MB - 1005.2188] Numerical methods for N-body simulations of interacting dark energy - assumptions, approximations, and their range of validity Results from high-resolution N-body runs: - Large Scale Structure: Halo Mass Function [MB, V. Pettorino - 1006.3761], Bias - Collapsed objects: Density Profiles, Concentrations, Baryon Fraction Next steps in a resurrected topic Tuesday, July 6, 2010 Marco Baldi - MGADS, Strasbourg 16 VI 2010
The beginning of the story: evidence for DE The last decade (well, actually a bit more than that...) has provided us with a hardly doubtable evidence of the existence of some accelerating component in the Universe, dubbed Dark Energy Tuesday, July 6, 2010 Marco Baldi - MGADS, Strasbourg 16 VI 2010
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Page 5 and 6: The beginning of the story: evidenc
Page 7 and 8: Tuesday, July 6, 2010 Standard mode
Page 9 and 10: Standard model and non-standard mod
Page 19 and 20: Why bothering with non-standard mod
Page 25 and 26: Dynamic and interacting Dynamic DE:
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Page 43 and 44: Features of interacting dark energy
Page 45 and 46: m c 1.4 1.3 1.2 1.1 1.0 Features of
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Tuesday, July 6, 2010 How to implem
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Results (I): halo mass function and
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Results (II): bias The fifth-force
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The fifth-force determines an “ef
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Results (III): baryon fraction The
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The first hydrodynamical high-resol
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Resuts (IV): halo density profiles
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The first hydrodynamical high-resol
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Resuts (IV): halo density profiles
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Some first results (IV) The first h
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Some first results (IV) The first h
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Maccio’ et al 2004 Constant β Tu
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Maccio’ et al 2004 Constant β MB
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Tuesday, July 6, 2010 concluding...
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Marco Baldi

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