Perturbation theory, effective field theory, and oscillations in the power spectrum

被引:92
|
作者
Vlah, Zvonimir [1 ,2 ,3 ,4 ]
Seljak, Uros [5 ,6 ,7 ]
Chu, Man Yat [7 ]
Feng, Yu [7 ]
机构
[1] Stanford Univ, Stanford Inst Theoret Phys, Stanford, CA 94306 USA
[2] Stanford Univ, Dept Phys, Stanford, CA 94306 USA
[3] SLAC, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA
[4] Stanford Univ, Menlo Pk, CA 94025 USA
[5] Univ Calif Berkeley, Dept Astron, Phys, 601 Campbell Hall, Berkeley, CA 94720 USA
[6] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
[7] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA
关键词
cosmological perturbation theory; dark matter simulations; power spectrum; ANALYTIC MODEL; GALAXY; HALO;
D O I
10.1088/1475-7516/2016/03/057
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We explore the relationship between the nonlinear matter power spectrum and the various Lagrangian and Standard Perturbation Theories (LPT and SPT). We first look at it in the context of one dimensional (1-d) dynamics, where 1LPT is exact at the perturbative level and one can exactly resum the SPT series into the 1LPT power spectrum. Shell crossings lead to non-perturbative effects, and the PT ignorance can be quantified in terms of their ratio, which is also the transfer function squared in the absence of stochasticity. At the order of PT we work, this parametrization is equivalent to the results of effective field theory (EFT), and can thus be expanded in terms of the same parameters. We find that its radius of convergence is larger than the SPT loop expansion. The same EFT parametrization applies to all SPT loop terms and if stochasticity can be ignored, to all N-point correlators. In 3-d, the LPT structure is considerably more complicated, and we find that LPT models with parametrization motivated by the EFT exhibit running with k and that SPT is generally a better choice. Since these transfer function expansions contain free parameters that change with cosmological model their usefulness for broadband power is unclear. For this reason we test the predictions of these models on baryonic acoustic oscillations (BAO) and other primordial oscillations, including string monodromy models, for which we ran a series of simulations with and without oscillations. Most models are successful in predicting oscillations beyond their corresponding PT versions, confirming the basic validity of the model. We show that if primordial oscillations are localized to a scale q, the wiggles in power spectrum are approximately suppressed as exp[-k(2)Sigma(2)(q)/2], where Sigma(q) is rms displacement of particles separated by q, which saturates on large scales, and decreases as q is reduced. No oscillatory features survive past k similar to 0.5h/Mpc at z = 0.
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页数:28
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