Cosmic Background Neutrinos Deflected by Gravity: DEMNUni Simulation Analysis

Hernández, Beatriz López Suevos; Carbone, C.; Jiménez, Raúl; Garay, Carlos Peña

doi:10.48550/arxiv.2301.12430

Cited by 6 publications

(11 citation statements)

References 28 publications

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“…Originally developed for testing different probes in the presence of massive neutrinos and dynamical dark energy, the Dark Energy and Massive Neutrino Universe (DEMNUni) (Carbone et al 2016) experiment is a suite of N-Body simulations (Roncarelli et al 2015;Castorina et al 2015;Moresco et al 2017;Fabbian et al 2018;Ruggeri et al 2018;Kreisch et al 2019;Schuster et al 2019;Verza et al 2019;Parimbelli et al 2021aParimbelli et al , 2022bVerza et al 2022b;Guidi et al 2022;Verza et al 2022a;Hernández-Molinero et al 2023) in ΛCDM, plus different νw 0 w a CDM cosmological scenarios. The largest simulations follow the evolution of 2048 3 CDM and (if present) 2048 3 neutrino particles, in a box of side L = 2 Gpc/h.…”

Section: Demnuni_cov N-body Simulationsmentioning

confidence: 99%

COVMOS: A new Monte Carlo approach for galaxy clustering analysis

Baratta

Bel

Gouyou

et al. 2023

A&A

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We validate the COVMOS method introduced in our previous study allowing for the fast simulation of catalogues of different cosmological field tracers (e.g. dark matter particles, halos, galaxies, etc.). The power spectrum and one-point probability distribution function of the underlying tracer's density field are set as inputs of the method and arbitrarily chosen by the user. To evaluate the validity domain of COVMOS at the level of the produced two-point statistics covariance matrix, we chose to target these two input statistical quantities from realistic N-body simulation outputs. We performed this cloning procedure based on the ΛCDM as well as on a massive neutrino cosmology, for five redshifts in the range of z ∈ [0, 2]. First, we validated the output real-space two-point statistics (both in the configuration and Fourier space) and estimated over 5, 000 COVMOS realisations per redshift and per cosmology, with a volume of 1 [Gpc/h] 3 and 10 8 particles each. This validation was performed against the corresponding N-body measurements, estimated from 50 simulations. We found the method to be valid up to k ∼ 0.2h/Mpc for the power spectrum and down to r ∼ 20 Mpc/h for the correlation function. Then, we extended the method by proposing a new modelling of the peculiar velocity distribution, aimed at reproducing the redshift-space distortions both in the linear and mildly non-linear regimes. After validating this prescription, we finally compared and validated the resulting redshift-space two-point statistics covariance matrices in the same range of scales. We released the Python code associated with this method on a public repository, which allows for the production of tens of thousands of realisations in record time. In particular, COVMOS is intended for any study involving large-scale galaxy-survey science that requires a large number of mock realisations.

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Section: Demnuni_cov N-body Simulationsmentioning

confidence: 99%

COVMOS: A new Monte Carlo approach for galaxy clustering analysis

Baratta

Bel

Gouyou

et al. 2023

A&A

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“…For this study, we use the "Dark Energy and Massive Neutrino Universe" (DEMNUni) suite of large N-body simulations [72]. The DEMNUni simulations have been produced with the aim of investigating the large-scale structure of the Universe in the presence of massive neutrinos and dynamical DE, and they were conceived for the nonlinear analysis and modelling of different probes, including dark matter, halo, and galaxy clustering [73][74][75][76][77][78][79][80][81][82], weak lensing, CMB lensing, Sunyaev-Zel'dovich and integrated Sachs-Wolfe effects [72,[83][84][85], cosmic void statistics [17,23,25,86], as well as cross-correlations among these probes [87,88]. The DEMNUni simulations combine a good mass resolution with a large volume to include perturbations both at large and small scales.…”

Section: Simulations and Void Findermentioning

confidence: 99%

DEMNUni: disentangling dark energy from massive neutrinos with the void size function

Verza,

Carbone,

Pisani

et al. 2023

J. Cosmol. Astropart. Phys.

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Cosmic voids, the underdense regions in the Universe, are impacted by dark energy and massive neutrinos. In this work, relying on the DEMNUni suite of cosmological simulations, we explore the void size function in cosmologies with both dynamical dark energy and massive neutrinos. We investigate the impact of different choices of dark matter tracers on the void size function and study its sensitivity to the joint effect of several dark energy equations of state and total neutrino masses. In particular, we find that for all the combinations of neutrino mass and dark energy equation of state considered, the differences between the corresponding void size functions are larger than the associated Poisson noise, and therefore can be all distinguished. This looks very promising considering that forthcoming surveys, as the Euclid satellite, will be characterised by a void statistics with similar number densities and volumes as for the DEMNUni suite. These findings show that the use of the void size function in forthcoming large galaxy surveys will be extremely useful in breaking degeneracies among these cosmological parameters.

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“…This field of cosmology is rapidly advancing thanks to the improvement in the modeling of large-scale structure and the proliferation of computational facilities, as well as an ever-increasing number of codes for cosmological simulations including neutrinos (see [14] for an extensive code comparison). There has been growing interest in using cosmological simulations to study a variety of properties concerning relic neutrinos, such as, e.g., their helicity composition [15,16] or the radial density profile of neutrino halos [17][18][19]. To specifically determine the local number density one needs to accurately model the gravitational potential of the local neighbourhood (and potentially beyond), which can cause relic neutrinos to cluster and form regions of varying density.…”

Section: Jcap11(2023)038mentioning

confidence: 99%

“…This means that the maximum velocity in our simulations is ∼22% the speed of light. 16 We chose this upper limit to guarantee sufficient coverage of the momentum distribution for the lightest neutrino mass of 0.01 eV we considered. However, the rescaling is only effective for this range of neutrino masses.…”

Section: Jcap11(2023)038mentioning

confidence: 99%

“…All the gravitational effects described in this work will also alter the helicity composition of the CNB, as they can cause the direction of the neutrino momentum to change. There have been several works investigating the helicity flipping rate due to gravitational potentials and the resulting changes in the helicity composition of the CNB today [15,16,60,67]. The amount of fully clustered neutrinos is a proxy for the percentage of the CNB, which has equal amounts of left-and right-helical neutrinos.…”

Section: Jcap11(2023)038mentioning

confidence: 99%

See 1 more Smart Citation

Influence of local structure on relic neutrino abundances and anisotropies

Zimmer,

Correa,

Ando

2023

J. Cosmol. Astropart. Phys.

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Gravitational potentials of the Milky Way and extragalactic structures can influence the propagation of the cosmic neutrino background (CNB). Of particular interest to future CNB observatories, such as PTOLEMY, is the CNB number density on Earth. In this study, we have developed a simulation framework that maps the trajectories of relic neutrinos as they move through the local gravitational environment. The potentials are based on the dark matter halos found in state-of-the-art cosmological N-body simulations, resulting in a more nuanced and realistic input than the previously employed analytical models. We find that the complex dark matter distributions, along with their dynamic evolution, influence the abundance and anisotropies of the CNB in ways unaccounted for by earlier analytical methods. Importantly, these cosmological simulations contain multiple instances of Milky Way-like halos that we employ to model a variety of gravitational landscapes. Consequently, we notice a variation in the CNB number densities that can be primarily attributed to the differences in the masses of these individual halos. For neutrino masses between 0.01 and 0.3 eV, we note clustering factors within the range of 1 + 𝒪(10-3) to 1 + 𝒪(1). Furthermore, the asymmetric nature of the underlying dark matter distributions within the halos results in not only overdense, but intriguingly, underdense regions within the full-sky anisotropy maps. Gravitational clustering appears to have a significant impact on the angular power spectra of these maps, leading to orders of magnitude more power on smaller scales beyond multipoles of ℓ = 3 when juxtaposed against predictions by primordial fluctuations. We discuss how our results reshape our understanding of relic neutrino clustering and how this might affect observability of future CNB observatories such as PTOLEMY.GitHub: our simulation code will be made visiblehere.

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Cosmic Background Neutrinos Deflected by Gravity: DEMNUni Simulation Analysis

Cited by 6 publications

References 28 publications

COVMOS: A new Monte Carlo approach for galaxy clustering analysis

COVMOS: A new Monte Carlo approach for galaxy clustering analysis

DEMNUni: disentangling dark energy from massive neutrinos with the void size function

Influence of local structure on relic neutrino abundances and anisotropies

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