An accurate tool for the fast generation of dark matter halo catalogues

Monaco, Pierluigi; Sefusatti, Emiliano; Borgani, S.; Crocce, M.; Fosalba, P.; Sheth, Ravi K.; Theuns, Tom

doi:10.1093/mnras/stt907

Cited by 138 publications

(143 citation statements)

References 57 publications

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“…Straight N -body simulations are too numerically expensive to be done in mass production, so many semi-analytic approaches such as PThalos [1,2] PINOCCHIO [3][4][5], and COLAR [6], have been developed. These methods rely on Lagrangian perturbation theory (LPT) to displace the particles at large scales.…”

Section: Introductionmentioning

confidence: 99%

Helmholtz decomposition of the Lagrangian displacement

Chan

2014

Phys. Rev. D

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Lagrangian displacement field Ψ is the central object in Lagrangian perturbation theory (LPT). LPT is very successful at high redshifts, but it performs poorly at low redshifts due to severe shell crossing. To understand and quantify the effects of shell crossing, we extract Ψ from N -body simulation and decompose it into scalar and vector parts. We find that at late time the power spectrum of the scalar part agrees with 1-loop results from LPT at large scales, while the power in small scales is much suppressed due to shell crossing. At z = 0, the power spectrum of Ψ is 10% lower than the 1-loop results at k = 0.1 Mpc −1 h. Shell crossing also generates the vector contribution in Ψ, although its effect is subdominant in comparison with the power suppression in the scalar part. At z = 0, the vector part contributes 10% to the total power spectrum of Ψ at k = 1 Mpc −1 h, while only 1% is expected from the vector contribution in LPT. We also examine the standard LPT recipes and some of its variants. In one of the variants, we include a power suppression factor in the displacement potential to take into account the power suppression in small scales after shell crossing. However, these simple phenomenological approaches are found to yield limited improvement compared to the standard LPT after the onset of shell crossing.

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Section: Introductionmentioning

confidence: 99%

Helmholtz decomposition of the Lagrangian displacement

Chan

2014

Phys. Rev. D

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“…The position of dark matter particles after cosmic evolution according to perturbative approaches show a typical uncertainty of roughly a few Mpc, depending on the chosen approximation (e.g., see Monaco et al 2013;Kitaura & Hess 2013). This does not show up so clearly in the correlation function in configuration space, where the small scales are kept separated from the large ones.…”

Section: Discussionmentioning

confidence: 99%

“…However, it does have a very clear impact in the power spectrum, as it does not reproduce the one halo-term, and thus lacks the commonly known non-linear bump towards high ks. Small scale uncertainties propagate in Fourier space having the effect of a convolution (see Tassev & Zaldarriaga 2012;Monaco et al 2013). In this work we have presented two kinds of approaches based on perturbation theory.…”

Section: Discussionmentioning

confidence: 99%

“…17 Monaco et al (2002Monaco et al ( , 2013) is based on the ellipsoidal collapse, solved with the aid of 3rd-order LPT, to compute the time at which mass elements collapse (in the orbit-crossing sense), and Extended Press & Schecther (EPS) to deal with multiple smoothing radii. It starts from the generation of a linear density field on a regular grid in Lagrangian space, in the same way as initial conditions are generated for an N -body simulation.…”

Section: Pinocchiomentioning

confidence: 99%

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nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics

Chuang

Zhao

Prada

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a comparison of major methodologies of fast generating mock halo or galaxy catalogues. The comparison is done for two-point (power spectrum and 2-point correlation function in real-and redshift-space), and the three-point clustering statistics (bispectrum and 3-point correlation function). The reference catalogues are drawn from the BigMultiDark Nbody simulation. Both friend-of-friends (including distinct halos only) and spherical overdensity (including distinct halos and subhalos) catalogues have been used with the typical number density of a large-volume galaxy surveys. We demonstrate that a proper biasing model is essential for reproducing the power spectrum at quasilinear and even smaller scales. With respect to various clustering statistics, a methodology based on perturbation theory and a realistic biasing model leads to very good agreement with N-body simulations. However, for the quadrupole of the correlation function or the power spectrum, only the method based on semi-N -body simulation could reach high accuracy (1% level) at small scales, i.e., r < 25 h −1 Mpc or k > 0.15 h Mpc −1 . Full N -body solutions will remain indispensable to produce reference catalogues. Nevertheless, we have demonstrated that the more efficient approximate solvers can reach a few percent accuracy in terms of clustering statistics at the scales interesting for

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“…In addition to this there is a wealth of alternative methods such as PINOCCHIO (Monaco et al, 2002(Monaco et al, , 2013, Quick Particle Mesh Simulations (QPM; White et al 2014), Augmented lagrangian Perturbation Theory (ALPT; Kitaura & Heß 2013), Effective Zel'dovich approximation mocks (EZmocks; Chuang et al 2015) and the Comoving Lagrangian Acceleration method (COLA; Tassev et al 2013, Tassev et al 2015 which can all be used to produce mock catalogues comparable in accuracy to, if not better than, 2LPT and with similar speed. In this paper we present a stand-alone parallel implementation of the latter of these, with emphasis on maximising speed, memory conservation and ease of use.…”

Section: Introductionmentioning

confidence: 99%

L-PICOLA: A parallel code for fast dark matter simulation

Howlett

Manera

Percival

2015

Astronomy and Computing

154

181

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Robust measurements based on current large-scale structure surveys require precise knowledge of statistical and systematic errors. This can be obtained from large numbers of realistic mock galaxy catalogues that mimic the observed distribution of galaxies within the survey volume. To this end we present a fast, distributed-memory, planar-parallel code, L-PICOLA, which can be used to generate and evolve a set of initial conditions into a dark matter field much faster than a full non-linear N-Body simulation. Additionally, L-PICOLA has the ability to include primordial non-Gaussianity in the simulation and simulate the past lightcone at run-time, with optional replication of the simulation volume. Through comparisons to fully non-linear N-Body simulations we find that our code can reproduce the z = 0 power spectrum and reduced bispectrum of dark matter to within 2% and 5% respectively on all scales of interest to measurements of Baryon Acoustic Oscillations and Redshift Space Distortions, but 3 orders of magnitude faster. The accuracy, speed and scalability of this code, alongside the additional features we have implemented, make it extremely useful for both current and next generation large-scale structure surveys. L-PICOLA is publicly available at https://cullanhowlett.github.io/l-picola.

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An accurate tool for the fast generation of dark matter halo catalogues

Cited by 138 publications

References 57 publications

Helmholtz decomposition of the Lagrangian displacement

Helmholtz decomposition of the Lagrangian displacement

nIFTy cosmology: Galaxy/halo mock catalogue comparison project on clustering statistics

L-PICOLA: A parallel code for fast dark matter simulation

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