Simulating nonlinear cosmological structure formation with massive neutrinos

Banerjee, Arka; Dalal, Neal

doi:10.1088/1475-7516/2016/11/015

Cited by 138 publications

(128 citation statements)

References 82 publications

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“…Including massive neutrinos in cosmological simulations presents its own set of technical challenges [36][37][38][39][40]. Neutrinos are often included as another species of particle in the simulation alongside the CDM and baryons [41][42][43].…”

Section: Simulationsmentioning

confidence: 99%

Massive neutrinos and degeneracies in Lyman-alpha forest simulations

Pedersen

Font-Ribera²,

Kitching³

et al. 2020

J. Cosmol. Astropart. Phys.

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Using a suite of hydrodynamical simulations with cold dark matter, baryons, and neutrinos, we present a detailed study of the effect of massive neutrinos on the 1-D and 3-D flux power spectra of the Lyman-α (Lyα) forest. The presence of massive neutrinos in cosmology induces a scale-and time-dependent suppression of structure formation that is strongest on small scales. Measuring this suppression is a key method for inferring neutrino masses from cosmological data, and is one of the main goals of ongoing and future surveys like eBOSS, DES, LSST, Euclid or DESI. The clustering in the Lyα forest traces the quasi-linear power at late times and on small scales. In combination with observations of the cosmic microwave background, the forest therefore provides some of the tightest constraints on the sum of the neutrino masses. However there is a well-known degeneracy between Σm ν and the amplitude of perturbations in the linear matter power spectrum. We study the corresponding degeneracy in the 1-D flux power spectrum of the Lyα forest, and for the first time also study this degeneracy in the 3-D flux power spectrum. We show that the non-linear effects of massive neutrinos on the Lyα forest, beyond the effect of linear power amplitude suppression, are negligible, and this degeneracy persists in the Lyα forest observables to a high precision.We discuss the implications of this degeneracy for choosing parametrisations of the Lyα forest for cosmological analysis.

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Section: Simulationsmentioning

confidence: 99%

Massive neutrinos and degeneracies in Lyman-alpha forest simulations

Pedersen

Font-Ribera²,

Kitching³

et al. 2020

J. Cosmol. Astropart. Phys.

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“…The level of complexity of Nbody simulations has been increasing over the years, so that the physical processes included in the simulations and the final results are much closer to the observations than they used to be at the beginning. Recent examples are given by the MassiveNuS [69] suite, based on the Gadget-2 code [70] modified to include the effects of massive neutrinos, the DEMNUni suite [71][72][73], the TianNu simulation [74][75][76], the BAHAMAS project [77], the gevolution simulations [78], and the nuCONCEPT simulations [79] (see also [80] for a method combining the particle and fluid descriptions) 7 . Nevertheless, the uncertainties related to the non-linear evolution of cosmological structures are still higher than those affecting the linear theory, therefore reducing the constraining power coming from the inclusion of those scales in cosmological analysis.…”

Section: Clusteringmentioning

confidence: 99%

Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

2018

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Cosmological observations are a powerful probe of neutrino properties, and in particular of their mass. In this review, we first discuss the role of neutrinos in shaping the cosmological evolution at both the background and perturbation level, and describe their effects on cosmological observables such as the cosmic microwave background and the distribution of matter at large scale. We then present the state of the art concerning the constraints on neutrino masses from those observables, and also review the prospects for future experiments. We also briefly discuss the prospects for determining the neutrino hierarchy from cosmology, the complementarity with laboratory experiments, and the constraints on neutrino properties beyond their mass.

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“…A particular challenge in modeling Warm or Hot Dark Matter with simulations is artificial numerical fragmentation, which has been extensively discussed in the literature (Wang & White 2007;Banerjee & Dalal 2016;Schneider et al 2013;Angulo et al 2013). Shot noise due to initial random thermal velocities can seed unphysical overdensities at small scales, which lead to the formation of spurious structures as the simulation evolves.…”

Section: Simulations and Their Calibrationmentioning

confidence: 99%

Warm Dark Matter and Cosmic Reionization

Villanueva-Domingo

Gnedin

Mena

2018

ApJ

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In models with dark matter made of particles with keV masses, such as a sterile neutrino, small-scale density perturbations are suppressed, delaying the period at which the lowest mass galaxies are formed and therefore shifting the reionization processes to later epochs. In this study, focusing on Warm Dark Matter (WDM) with masses close to its present lower bound, i.e. around the 3 keV region, we derive constraints from galaxy luminosy functions, the ionization history and the Gunn-Peterson effect. We show that even if star formation efficiency in the simulations is adjusted to match the observed UV galaxy luminosity functions in both CDM and WDM models, the full distribution of Gunn-Peterson optical depth retains the strong signature of delayed reionization in the WDM model. However, until the star formation and stellar feedback model used in modern galaxy formation simulations is constrained better, any conclusions on the nature of dark matter derived from reionization observables remain model-dependent.

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Simulating nonlinear cosmological structure formation with massive neutrinos

Cited by 138 publications

References 82 publications

Massive neutrinos and degeneracies in Lyman-alpha forest simulations

Massive neutrinos and degeneracies in Lyman-alpha forest simulations

Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

Warm Dark Matter and Cosmic Reionization

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