On the non-linear scale of cosmological perturbation theory

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Standard Perturbation Theory100Plin1-loop2-loopP(k,z=0) [(h/Mpc) -3 ]1010.10.010.001 0.01 0.1 1 10k [h/Mpc]SPT breaks down at small scales / late times [P L−loop ∝ D 2L+2+ ∼ ( 11+z) 2L+2]initial spectrum from CAMB (ΛCDM - WMAP5)Mathias Garny (DESY Hamburg / CERN)On the non-linear scale of cosmological perturbation theory
Standard Perturbation TheoryMany approaches have been developed to improve behaviour at large k(closure, LPT, RPT, eikonal, ...) see e.g. Carlson, White, Padmanabhan 0905.0479Enhanced contributions (∝ k 2n , n ≤ L) related to interaction with softmodes cancel out completely in equal-time correlators (like the PS), asexpected from Galilean invariancesee e.g. Bertschinger, Jain 95; Frieman, Scoccimarro 95; Anselmi, Pietroni 12; Pietroni, Peloso 13;Sugiyama, Futamase 13; Blas, MG, Konstandin 13; Carrasco, Foreman, Green, Senatore 13; . . .Mathias Garny (DESY Hamburg / CERN)On the non-linear scale of cosmological perturbation theory
Page 1: On the non-linear scale of cosmolog
Page 4 and 5: Standard Perturbation TheoryPoisson
Page 8 and 9: Standard Perturbation TheoryMany ap
Page 10 and 11: Loop expansion of PS in the limit o
Page 16 and 17: Padé ansatzGoal: improve convergen
Page 18 and 19: Result for Padé resummed small-k l
Page 20 and 21: Padé improved PT vs N-body1.4z⩵0
Page 22 and 23: ConclusionThree loop larger than on
Page 24 and 25: Expansion parameter∫ kσl 2 (k, z
Page 26 and 27: Padé improved PT vs N-body1.4z⩵0

On the non-linear scale of cosmological perturbation theory

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