Fully relativistic treatment of decaying cold dark matter in <i>N</i>-body simulations

Dakin, Jeppe; Hannestad, Steen; Tram, Thomas

doi:10.1088/1475-7516/2019/06/032

Cited by 18 publications

(19 citation statements)

References 53 publications

(100 reference statements)

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“…Additional non-homogeneous relativistic corrections can, e.g., be absorbed in a similar way as for trans-relativistic massive neutrinos (see Sect. 7.8.2) using linear theory corrections to the gravitational potential (Dakin et al 2019b) or using a gauge approach (Fidler et al 2017b). Beyond a background contribution, dark matter decay and annihilation could also contribute to a heating of the gas in low mass halos (e.g.…”

Section: Self-interacting Dark Matter (Sidm) Decaying and Dissipative...mentioning

confidence: 99%

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: Self-interacting Dark Matter (Sidm) Decaying and Dissipative...mentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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“…where superscripts 'Nb' and 's' indicate the N-body and synchronous gauge respectively, labels the species, ℎ mp is the trace of the metric perturbation in synchronous gauge and tot is the total velocity divergence of all species. Though more complicated, the metric ( , ) transfer function is similarly constructed from various CLASS outputs, some of which are only available in the CLASS version that ships with CON CEPT (see Dakin et al 2019a for more details). We also note that the computation of the DE pressure perturbation within CLASS, needed for metric , is wrong in the standard version of CLASS, but fixed in the version shipping with CON CEPT (see Dakin et al 2019b for details).…”

Section: Pre-processing With Concept: Transfer Functionsmentioning

confidence: 99%

Euclid preparation: IX. EuclidEmulator2 – power spectrum emulation with massive neutrinos and self-consistent dark energy perturbations

Knabenhans

Stadel

Potter

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a new, updated version of the EuclidEmulator (called EuclidEmulator2), a fast and accurate predictor for the nonlinear correction of the matter power spectrum. 2 per cent-level accurate emulation is now supported in the eight-dimensional parameter space of w0waCDM+∑mν models between redshift z = 0 and z = 3 for spatial scales within the range 0.01 h Mpc−1 ≤ k ≤ 10 h Mpc−1. In order to achieve this level of accuracy, we have had to improve the quality of the underlying N-body simulations used as training data: (i) we use self-consistent linear evolution of non-dark matter species such as massive neutrinos, photons, dark energy and the metric field, (ii) we perform the simulations in the so-called N-body gauge, which allows one to interpret the results in the framework of general relativity, (iii) we run over 250 high-resolution simulations with 30003 particles in boxes of 1(h−1 Gpc)3 volumes based on paired-and-fixed initial conditions and (iv) we provide a resolution correction that can be applied to emulated results as a post-processing step in order to drastically reduce systematic biases on small scales due to residual resolution effects in the simulations. We find that the inclusion of the dynamical dark energy parameter wa significantly increases the complexity and expense of creating the emulator. The high fidelity of EuclidEmulator2 is tested in various comparisons against N-body simulations as well as alternative fast predictors like HALOFIT, HMCode and CosmicEmu. A blind test is successfully performed against the Euclid Flagship v2.0 simulation. Nonlinear correction factors emulated with EuclidEmulator2 are accurate at the level of $1{{\ \rm per\ cent}}$ or better for 0.01 h Mpc−1 ≤ k ≤ 10 h Mpc−1 and z ≤ 3 compared to high-resolution dark matter only simulations. EuclidEmulator2 is publicly available at https://github.com/miknab/EuclidEmulator2.

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“…This situation can be contrasted to that in ΛCDM (and its simplest extension that assume a free but constant dark energy equation of state, wCDM), where the modeling of nonlinear matter power spectrum has been extensively studied with N-body simulations [88][89][90] and analytical fits or models [91][92][93][94]. Limited previous studies of the small-scale structure formation in DMDR include simulations of a less general class of decaying dark-matter models than the one we adopt here [40], and the demonstration that relativistic species have negligible contribution to the gravitational physics of the small-scale structure formation [95]. One potentially useful alternative to running simulations is recent work [96] which proposes to accurately model beyond-ΛCDM models by suitably rescaling the ΛCDM result in order to get one into the desired new model.…”

Section: Nonlinear Matter Power Spectrum Strategies and Des-y1 Scales Usedmentioning

confidence: 99%

Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

Chen¹,

Huterer²,

Lee³

et al. 2021

Phys. Rev. D

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We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has

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Fully relativistic treatment of decaying cold dark matter in N-body simulations

Cited by 18 publications

References 53 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

Euclid preparation: IX. EuclidEmulator2 – power spectrum emulation with massive neutrinos and self-consistent dark energy perturbations

Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

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