Accurate emulator for the redshift-space power spectrum of dark matter halos and its application to galaxy power spectrum

Kobayashi, Yosuke; Nishimichi, Takahiro; Takada, Masahiro; Takahashi, Ryuichi; Osato, Ken

doi:10.1103/physrevd.102.063504

Cited by 62 publications

(79 citation statements)

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“…Emulators also have the advantage of being able to model complex trends in the data, so that they are being progressively constructed for many more kinds of large-scale structure statistics. For instance, emulators have been used in modelling the nonlinear matter power spectrum (Heitmann et al 2009;Lawrence et al 2017;DeRose et al 2019;Euclid Collaboration 2019;Angulo et al 2021) even beyond KCDM (Winther et al 2019;Ramachandra et al 2021;Arnold et al 2021) and for baryonic effects (Arico `et al 2021b;Giri and Schneider 2021), the galaxy power spectrum and correlation function (Kwan et al 2015;Zhai et al 2019), weak lensing peak counts and power spectra (Liu et al 2015;Petri et al 2015), the 21-cm power spectrum (Jennings et al 2019), the halo mass function (McClintock et al 2019;Bocquet et al 2020), halo clustering statistics (Nishimichi et al 2019;Kobayashi et al 2020). Traditionally, emulators have been built with Gaussian processes (GP), but more recently feed forward neural networks are gaining popularity as they allow to deal with larger datasets and a high number of dimensions.…”

Section: Emulators and Interpolatorsmentioning

confidence: 99%

“…The second challenge is that numerical simulations are intrinsically noisier for discrete objects than for field quantities due to the shot noise associated with the latter. Nevertheless, recently, some progress towards emulators for dark matter haloes has been achieved (Valcin et al 2019;Kobayashi et al 2020). An interesting possibility will be to combine emulators with perturbative expansions of galaxy bias, such as those proposed by Modi et al (2020a), Kokron et al (2021), Zennaro et al (2021), which has been recently applied to data from the Dark Energy Survey (Hadzhiyska et al 2021b).…”

Section: Emulators and Interpolatorsmentioning

confidence: 99%

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Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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Section: Emulators and Interpolatorsmentioning

confidence: 99%

Section: Emulators and Interpolatorsmentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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“…As an alternative approach, in this paper we use a simulation-based theoretical template, the emulator, which enables fast and accurate computation of the redshift-space power spectrum of "halos" in the flat ΛCDM framework, developed in our previous paper [36]. Dark matter halos are the places where galaxies likely form.…”

Section: Introductionmentioning

confidence: 99%

“…It is relatively straightforward to accurately simulate the formation and evolution processes of halos using N -body simulations and then have an accurate prediction of their clustering properties including the redshiftspace power spectrum [19,37]. Kobayashi et al [36] developed an emulator by training a feed-forward neural network with a dataset of the redshift-space power spectra of halos measured from halo catalogs in an ensemble set of N -body simulations for 80 models within flat wCDM framework in the Dark Quest campaign [38]. The emulator was validated using the test dataset consisting of 20 cosmological models that are not in training, and it was shown that the power spectra are sufficiently accurate up to k = 0.6 h Mpc −1 .…”

Section: Introductionmentioning

confidence: 99%

Full-shape cosmology analysis of SDSS-III BOSS galaxy power spectrum using emulator-based halo model: a $5\%$ determination of $σ_8$

Kobayashi,

Nishimichi,

Takada

et al. 2021

Preprint

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We present the results obtained from the full-shape cosmology analysis of the redshift-space power spectra for 4 galaxy samples of the SDSS-III BOSS DR12 galaxy catalog over 0.2 < z < 0.75. For the theoretical template, we use an emulator that was built from an ensemble set of N -body simulations, which enables fast and accurate computation of the redshift-space power spectrum of "halos". Combining with the halo occupation distribution to model the halo-galaxy connection, we can compute the redshift-space power spectrum of BOSS-like galaxies in less than a CPU second, for an input model under flat ΛCDM cosmology. In our cosmology inference, we use the monopole, quadrupole and hexadecapole moments of the redshift-space power spectrum and include 7 nuisance parameters, with broad priors, to model uncertainties in the halo-galaxy connection for each galaxy sample, but do not use any information on the abundance of galaxies. We demonstrate a validation of our analysis pipeline using the mock catalogs of BOSS-like galaxies, generated using different recipes of the halo-galaxy connection and including the assembly bias effect. Assuming weak priors on cosmological parameters, except for the BBN prior on Ω b h 2 and the CMB prior on ns, we show that our model well reproduces the BOSS power spectra. Including the power spectrum information up to kmax = 0.25 h Mpc −1 , we find Ωm = 0.300±0.011, H0 = 68.35 +1.21 −1.39 km s −1 Mpc −1 , and σ8 = 0.742 +0.035 −0.036 , for the mode and 68% credible interval, after marginalization over nuisance parameters including the halo-galaxy connection parameters. We find little improvement in the cosmological parameters beyond a maximum wavelength kmax 0.2 h Mpc −1 due to the shot noise domination and marginalization of the halo-galaxy connection parameters. Our results show a nice agreement with the Planck CMB results for Ωm and H0, but indicate a slight tension for σ8.

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“…Recent works have been taking another route, using different computational methods (e.g. : neural networks, gaussian processes, polynomial chaos expansions) to emulate dark matter statistics from sets of N-Body simulations; this allows one to obtain spectra which are accurate up to k ≈ 1h/Mpc at a negligible computational cost (Heitmann et al, 2013;Kobayashi et al, 2020;Euclid Collaboration et al, 2020;Angulo et al, 2020;Zennaro et al, 2021). N-Body simulations are unmatched in their accuracy, especially at the small scales.…”

Section: Chapter Introductionmentioning

confidence: 99%

Statistical and Numerical Methods for Precision Cosmology

Maion¹

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Accurate emulator for the redshift-space power spectrum of dark matter halos and its application to galaxy power spectrum

Cited by 62 publications

References 70 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

Full-shape cosmology analysis of SDSS-III BOSS galaxy power spectrum using emulator-based halo model: a $5\%$ determination of $σ_8$

Statistical and Numerical Methods for Precision Cosmology

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