The development of gravitational instabilities - RESCEU

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‣ A lot is known at tree order <strong>The</strong> tree order bispectra B δ (k 1 , k 2 , k 2 ) = 〈δ (1) (k 1 )δ (1) (k 2 )δ (2) (k 3 )〉 + sym. = F (s) 2 (k 1, k 2 ) P (k 1 ) P (k 2 ) + sym. Comparisons <strong>of</strong> poly-spectra (collapsed geometry) with N-body simulations... ... and in observations From FB ‘94 k 1 ≈ 0.3h/Mpc k 1 ≈ 2k 2 From PSCz catalogue, Feldman et al. ‘01 10 Francis Bernardeau IPhT Saclay
• But things get not as nice when one wants to include loops Not necessarily the best way to expand... 11
Page 1: Francis Bernardeau IPhT Saclay, Fra
Page 4 and 5: Which observables ? 〈δ x (k 1 )
Page 6 and 7: A self-gravitating expanding dust f
Page 8 and 9: ‣Motion equations in Fourier spac
Page 12 and 13: A field theory reformulation Scocci
Page 14 and 15: Not a standard quantum field theory
Page 16: The closure theory Valageas P., A&A
Page 19 and 20: One key ingredient : the propagator
Page 21 and 22: ‣ RPT (Scoccimarro and Crocce) co
Page 23 and 24: Insights into higher order propagat
Page 25 and 26: ‣ This suggests another scheme :
Page 27 and 28: Comparison with numerical simulatio
Page 29 and 30: • Does it speed up the convergenc
Page 31 and 32: Using large-scale structure to test
Page 33 and 34: In presence of a dilaton field Brax
Page 35 and 36: Evolution of structure: from GR to
Page 37 and 38: Bispectra (equilateral configuratio

The development of gravitational instabilities - RESCEU

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