Cosmic-variance limited Baryon Acoustic Oscillations from the DEUS-FUR ΛCDM simulation

Rasera, Yann; Corasaniti, Pier-Stefano; Alimi, Jean‐Michel; Bouillot, Vincent; Reverdy, Vincent; Balmès, Irène

doi:10.1093/mnras/stu295

Cited by 50 publications

(55 citation statements)

References 57 publications

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“…Several processes have been proposed that could displace the BAO feature, the most important being non-linearities, bias e.g., [75,76] and non-zero baryon-dark matter relative velocity [77][78][79]. These effects however have been found to be below current errors [80][81][82] and below the 1% level.…”

Section: Discussionmentioning

confidence: 99%

The trouble with H₀

Bernal

Verde

Riess

2016

J. Cosmol. Astropart. Phys.

761

691

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Abstract. We perform a comprehensive cosmological study of the H 0 tension between the direct local measurement and the model-dependent value inferred from the Cosmic Microwave Background. With the recent measurement of H 0 this tension has raised to more than 3 σ. We consider changes in the early time physics without modifying the late time cosmology. We also reconstruct the late time expansion history in a model independent way with minimal assumptions using distance measurements from Baryon Acoustic Oscillations and Type Ia Supernovae, finding that at z < 0.6 the recovered shape of the expansion history is less than 5% different than that of a standard ΛCDM model. These probes also provide a model insensitive constraint on the low-redshift standard ruler, measuring directly the combination r s h where H 0 = h × 100 Mpc −1 km/s and r s is the sound horizon at radiation drag (the standard ruler), traditionally constrained by CMB observations. Thus r s and H 0 provide absolute scales for distance measurements (anchors) at opposite ends of the observable Universe. We calibrate the cosmic distance ladder and obtain a model-independent determination of the standard ruler for acoustic scale, r s . The tension in H 0 reflects a mismatch between our determination of r s and its standard, CMB-inferred value. Without including high-Planck CMB polarization data (i.e., only considering the "recommended baseline" low-polarisation and temperature and the high temperature data), a modification of the early-time physics to include a component of dark radiation with an effective number of species around 0.4 would reconcile the CMB-inferred constraints, and the local H 0 and standard ruler determinations. The inclusion of the "preliminary" high-Planck CMB polarisation data disfavours this solution.arXiv:1607.05617v2 [astro-ph.CO]

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Section: Discussionmentioning

confidence: 99%

The trouble with H₀

Bernal

Verde

Riess

2016

J. Cosmol. Astropart. Phys.

761

691

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“…The code is mainly used for hydrodynamical simulations in a cosmological context [17,18] but it has also been employed for pure dark matter N -body runs in the past [19,20]. For the comparison, we apply a coarse-level grid with refinement level min = 12, corresponding to 2048 3 coarse cells.…”

Section: N -Body Codesmentioning

confidence: 99%

Matter power spectrum and the challenge of percent accuracy

Schneider

Teyssier

Potter

et al. 2016

J. Cosmol. Astropart. Phys.

208

229

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Abstract. Future galaxy surveys require one percent precision in the theoretical knowledge of the power spectrum over a large range including very nonlinear scales. While this level of accuracy is easily obtained in the linear regime with perturbation theory, it represents a serious challenge for small scales where numerical simulations are required. In this paper we quantify the precision of present-day N -body methods, identifying main potential error sources from the set-up of initial conditions to the measurement of the final power spectrum. We directly compare three widely used N -body codes, Ramses, Pkdgrav3, and Gadget3 which represent three main discretisation techniques: the particle-mesh method, the tree method, and a hybrid combination of the two. For standard run parameters, the codes agree to within one percent at k ≤ 1 h Mpc −1 and to within three percent at k ≤ 10 h Mpc −1 . We also consider the bispectrum and show that the reduced bispectra agree at the sub-percent level for k ≤ 2 h Mpc −1 . In a second step, we quantify potential errors due to initial conditions, box size, and resolution using an extended suite of simulations performed with our fastest code Pkdgrav3. We demonstrate that the simulation box size should not be smaller than L = 0.5 h −1 Gpc to avoid systematic finite-volume effects (while much larger boxes are required to beat down the statistical sample variance). Furthermore, a maximum particle mass of M p = 10 9 h −1 M is required to conservatively obtain one percent precision of the matter power spectrum. As a consequence, numerical simulations covering large survey volumes of upcoming missions such as DES, LSST, and Euclid will need more than a trillion particles to reproduce clustering properties at the targeted accuracy.arXiv:1503.05920v3 [astro-ph.CO]

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“…So far, the biggest efforts were focused into two, somewhat complementary approaches. The first is represented by simulations like Millennium (MS; Springel et al 2005), Millennium II (MS-II; Boylan-Kolchin et al 2009), Millennium XXL (MXXL; Angulo et al 2012), Bolshoi (Klypin et al 2011), MultiDark (Prada et al 2012), Horizon Run I-III (Kim et al 2009(Kim et al , 2011, Horizon-4π (Prunet et al 2008;Teyssier et al 2009), MareNostrum Universe (Gottloeber et al 2006), Jubilee project (Watson et al 2014), Coyote Universe (Heitmann et al 2010), DEUS simulation (Alimi et al 2012;Rasera et al 2014) or MICE suite (Fosalba et al 2015). These follow structure formation in a large cosmological volume at the expense of having a medium or a low-mass resolution.…”

Section: Introductionmentioning

confidence: 99%

The Copernicus Complexio: a high-resolution view of the small-scale Universe

Hellwing¹,

Frenk²,

Cautun³

et al. 2016

Mon. Not. R. Astron. Soc.

119

136

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We introduce Copernicus Complexio (COCO), a high-resolution cosmological N-body simulation of structure formation in the ΛCDM model. COCO follows an approximately spherical region of radius ∼ 17.4h −1 Mpc embedded in a much larger periodic cube that is followed at lower resolution. The high resolution volume has a particle mass of 1.135 × 10 5 h −1 M (60 times higher than the Millennium-II simulation). COCO gives the dark matter halo mass function over eight orders of magnitude in halo mass; it forms ∼ 60 haloes of galactic size, each resolved with about 10 million particles. We confirm the power-law character of the subhalo mass function, N (> µ) ∝ µ −s , down to a reduced subhalo mass M sub /M 200 ≡ µ = 10 −6 , with a best-fit power-law index, s = 0.94, for hosts of mass M 200 = 10 12 h −1 M . The concentration-mass relation of COCO haloes deviates from a single power law for masses M 200 < a few×10 8 h −1 M , where it flattens, in agreement with results by Sanchez-Conde et al. The host mass invariance of the reduced maximum circular velocity function of subhaloes, ν ≡ V max /V 200 , hinted at in previous simulations, is clearly demonstrated over five orders of magnitude in host mass. Similarly, we find that the average, normalised radial distribution of subhaloes is approximately universal (i.e. independent of subhalo mass), as previously suggested by the Aquarius simulations of individual haloes. Finally, we find that at fixed physical subhalo size, subhaloes in lower mass hosts typically have lower central densities than those in higher mass hosts.

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Cosmic-variance limited Baryon Acoustic Oscillations from the DEUS-FUR ΛCDM simulation

Cited by 50 publications

References 57 publications

The trouble with H₀

The trouble with H₀

Matter power spectrum and the challenge of percent accuracy

The Copernicus Complexio: a high-resolution view of the small-scale Universe

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Cosmic-variance limited Baryon Acoustic Oscillations from the DEUS-FUR ΛCDM simulation

Cited by 50 publications

References 57 publications

The trouble with H0

The trouble with H0

Matter power spectrum and the challenge of percent accuracy

The Copernicus Complexio: a high-resolution view of the small-scale Universe

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The trouble with H₀

The trouble with H₀