Cubic halo bias in Eulerian and Lagrangian space

Abidi, Muntazir; Baldauf, Tobias

doi:10.1088/1475-7516/2018/07/029

Cited by 103 publications

(152 citation statements)

References 42 publications

Supporting

Mentioning

127

Contrasting

Order By: Relevance

“…If the scale R * is larger than the spatial length scale (nonlinear scale) controlling the perturbative expansion, then one can correspondingly include higher-order derivative terms. This might be the case for very massive halos [66][67][68], for example, or due to radiative-transfer effects [69][70][71][72][73][74].…”

Section: Higher Derivativesmentioning

confidence: 99%

An EFT description of galaxy intrinsic alignments

Vlah

Chisari

Schmidt

2020

J. Cosmol. Astropart. Phys.

146

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We present a general perturbative effective field theory (EFT) description of galaxy shape correlations, which are commonly known as intrinsic alignments. This rigorous approach extends current analytical modelling strategies in that it only relies on the equivalence principle. We present our results in terms of three-dimensional statistics for two-and three-point functions of both galaxy shapes and number counts. In case of the two-point function, we recover the well-known linear alignment result at leading order, but also present the full next-to-leading order expressions. In case of the three-point function we present leading order results for all the auto-and cross-correlations of galaxy shapes and densities. We use a spherical tensor basis to decompose the tensor perturbations in different helicity modes, which allows us to make use of isotropy and parity properties in the correlators. Combined with the results on projection presented in a forthcoming companion paper, our framework is directly applicable to accounting for intrinsic alignment contamination in weak lensing surveys, and to extracting cosmological information from intrinsic alignments. 42A.1 Two-point functions 44 A.2 Three-point functions 47 B Fields in Fourier space 50 B.1 Bias expansion and renormalisation of the one-loop power spectrum 55 B.2 Degeneracy of the bias operators 62 B.3 Bias expansion of the tree-level bispectrum 63 C Bias renormalisation for tensor fields 65 1 Explicitly, we writewhere the Dirac delta function ensures the total momentum conservation, and is a consequence of the statistical translation invariance.

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Section: Higher Derivativesmentioning

confidence: 99%

An EFT description of galaxy intrinsic alignments

Vlah

Chisari

Schmidt

2020

J. Cosmol. Astropart. Phys.

146

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“…We shall use the 'natural' smoothing of our simulation grids (0.75 h −1 Mpc), and comment upon this later (see also Aviles 2018). Going to higher order in the bias expansion requires the addition of many more terms, with cubic order already doubling the number of coefficients (Lazeyras & Schmidt 2018;Abidi & Baldauf 2018).…”

Section: The Bias Expansionmentioning

confidence: 99%

“…While values of the derivative bias b∇ will be sensitive to small-scale details such as smoothing and are therefore not expected to be universal, an extensive literature exists studying physical models for b1, b2, bs (see §1 for references). To this end, we have checked that enforcing, to within a few per cent, the peak-background split relations between (b1, b2) from Sheth & Tormen (1999) (keeping ν as a free parameter) and values of bs from Abidi & Baldauf (2018) only degrades our fits at the few (∼ 3) per cent level in P hh and P hm and doesn't significantly alter the range of fit.…”

Section: Fitting Halo Spectramentioning

confidence: 99%

Simulations and symmetries

Modi

Chen

White

2020

Monthly Notices of the Royal Astronomical Society

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We investigate the range of applicability of a model for the real-space power spectrum based on N-body dynamics and a (quadratic) Lagrangian bias expansion. This combination uses the highly accurate particle displacements that can be efficiently achieved by modern N-body methods with a symmetries-based bias expansion which describes the clustering of any tracer on large scales. We show that at low redshifts, and for moderately biased tracers, the substitution of N-body-determined dynamics improves over an equivalent model using perturbation theory by more than a factor of two in scale, while at high redshifts and for highly biased tracers the gains are more modest. This hybrid approach lends itself well to emulation. By removing the need to identify halos and subhalos, and by not requiring any galaxy-formation-related parameters to be included, the emulation task is significantly simplified at the cost of modeling a more limited range in scale.

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“…The relevance of these operators is controlled by the corresponding non-linear bias coefficients. One could try to derive bias parameters analytically or extract them from N-body simulations [33][34][35][36]. In this work we adopt an agnostic approach for the bias expansion.…”

mentioning

confidence: 99%

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

Chudaykin

Ivanov

2019

J. Cosmol. Astropart. Phys.

148

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 ...

show abstract

Cubic halo bias in Eulerian and Lagrangian space

Cited by 103 publications

References 42 publications

An EFT description of galaxy intrinsic alignments

An EFT description of galaxy intrinsic alignments

Simulations and symmetries

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

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