Effective field theory of large scale structure at two loops: The apparent scale dependence of the speed of sound

Baldauf, Tobias; Mercolli, Lorenzo; Zaldarriaga, Matías

doi:10.1103/physrevd.92.123007

Cited by 135 publications

(189 citation statements)

References 54 publications

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“…Ref. [18] also obtained results at various redshifts quoting, e.g. a value of 0.98 (Mpc/h) 2 at z = 0.…”

Section: Effective Matter Sound Speedmentioning

confidence: 95%

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A robust measurement of the first higher-derivative bias of dark matter halos

Lazeyras

2019

J. Cosmol. Astropart. Phys.

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We present a new simulation technique in which any chosen mode k of the density contrast field can be amplified by an amplitude ∆. These amplified-mode simulations allow us to study the response of the halo density field to a long-wavelength mode other than the DC mode. In this sense they are a generalization of the separate-universe simulations to finitewavelength modes. In particular, we use these simulations to obtain robust measurements of the first higher-derivative bias of dark matter halos b ∇ 2 δ . We find a negative bias at all mass considered, roughly following the −R 2 L (M ) relation, the Lagrangian radius of halos squared, as naively expected. We compare our results with those obtained from a fit to the 1-loop halo-matter power spectrum, as well as with the recent results from Abidi and Baldauf (2018), and to the prediction from the peak theory.

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“…Ref. [18] also obtained results at various redshifts quoting, e.g. a value of 0.98 (Mpc/h) 2 at z = 0.…”

Section: Effective Matter Sound Speedmentioning

confidence: 95%

“…There are several terms to consider and we will discuss them one after the other. They are shown in figure 1 of [18] and we will follow the same nomenclature as that reference. The first one is the (3 − 3) I contribution (i.e.…”

Section: Higher Order Correctionsmentioning

confidence: 99%

A robust measurement of the first higher-derivative bias of dark matter halos

Lazeyras

2019

J. Cosmol. Astropart. Phys.

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“…As for the higher-derivative bias coefficient, the measurements from N-body simulations [34,78,101] suggest that it is an order-one quantity in units of [Mpc/h] 2 . Thus, we adopt the following fiducial value along with the time-dependence that corresponds to the one-loop contribution,…”

Section: Parameter Definition Fiducial Value Hmentioning

confidence: 99%

Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

Chudaykin

Ivanov

2019

J. Cosmol. Astropart. Phys.

144

171

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We present a Markov-Chain Monte-Carlo (MCMC) forecast for the precision of neutrino mass and cosmological parameter measurements with a Euclidlike galaxy clustering survey. We use a complete perturbation theory model for the galaxy one-loop power spectrum and tree-level bispectrum, which includes bias, redshift space distortions, IR resummation for baryon acoustic oscillations and UV counterterms. The latter encapsulate various effects of short-scale dynamics which cannot be modeled within perturbation theory. Our MCMC procedure consistently computes the non-linear power spectra and bispectra as we scan over different cosmologies. The second ingredient of our approach is the theoretical error covariance which captures uncertainties due to higher-order non-linear corrections omitted in our model. Having specified characteristics of a Euclid-like spectroscopic survey, we generate and fit mock galaxy power spectrum and bispectrum likelihoods. Our results suggest that even under very agnostic assumptions about non-linearities and short-scale physics a future Euclid-like survey will be able to measure the sum of neutrino masses with a standard deviation of 28 meV. When combined with the most recent Planck likelihood, this uncertainty decreases to 19 meV. Reducing the theoretical error on the bispectrum down to the two-loop level marginally tightens the bound to 17 meV. 1 chudy@ms2.inr.ac.ru 2 mi1271@nyu.edu arXiv:1907.06666v1 [astro-ph.CO] 15 Jul 2019 exploit the potential of upcoming surveys will strongly depend on the understanding on these effects, which is not yet complete.Fortunately, the bulk of information about the neutrino free-streaming is encoded in mildly non-linear scales which can be robustly and systematically described within perturbation theory. One of the most popular approaches is Eulerian standard cosmological perturbation theory (SPT) [14]. The basic formulation of SPT, however, does not correctly capture the non-linear evolution of baryon acoustic oscillations (BAO) [15] and short-scale physics beyond the single-stream pressureless perfect fluid hydrodynamics [16][17][18]. These problems have been intensely studied in the recent years.First, it has been shown that the non-linear suppression and distortion of the BAO can be captured by a resummation of contributions describing the tidal effects of large-scale bulk flows. This procedure, called infrared (IR) resummation, is essential for an accurate description of the BAO and has been formulated within various theoretical frameworks [19][20][21][22][23][24][25]. We will adopt a systematic approach of [22,24] streamlined in the context of time-sliced perturbation theory [26].Second, we will use the effective field theory of large-scale structure (EFT) to account for the back-reaction of small scale nonlinearities on larger scales [17,27,28]. This approach removes the unphysical UV sensitivity of perturbation theory loop integrals and parameterizes the ignorance about short scale-dynamics by various effective operators in the equations of motion for ...

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“…The linear relation is reliable as long as the matter overdensity δ is much smaller than unity. In this regime, one can solve the (Newtonian) dynamical equations perturbatively (see [127] for a review and [128][129][130][131][132][133][134][135][136][137][138][139][140][141][142] for an approach using effective field theory). Even pushing perturbation theories to their limits, theoretical predictions describing the evolution of matter are valid only in the weakly nonlinear regime, that is for k 0.2 h/Mpc at redshift 0, even in the case of Gaussian initial conditions.…”

Section: From Primordial Interactions To Matter Overdensitiesmentioning

confidence: 99%

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

Biagetti

2019

Galaxies

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The understanding of the primordial mechanism that seeded the cosmic structures we observe today in the sky is one of the major goals in cosmology. The leading paradigm for such a mechanism is provided by the inflationary scenario, a period of violent accelerated expansion in the very early stages of evolution of the universe. While our current knowledge of the physics of inflation is limited to phenomenological models which fit observations, an exquisite understanding of the particle content and interactions taking place during inflation would provide breakthroughs in our understanding of fundamental physics at high energies. In this review, we summarize recent theoretical progress in the modeling of the imprint of primordial interactions in the large-scale structures of the universe. We focus specifically on the effects of such interactions on the statistical distribution of dark-matter halos, providing a consistent treatment of the steps required to connect the correlations generated among fields during inflation all the way to the late-time correlations of halos.

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Effective field theory of large scale structure at two loops: The apparent scale dependence of the speed of sound

Cited by 135 publications

References 54 publications

A robust measurement of the first higher-derivative bias of dark matter halos

A robust measurement of the first higher-derivative bias of dark matter halos

Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

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