A Two-Fluid Treatment of the Effect of Neutrinos on the Matter Density

Farshad, Kamalinejad,; Slepian, Zachary

doi:10.48550/arxiv.2203.13103

Cited by 3 publications

(8 citation statements)

References 23 publications

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“…However, due to time-evolution associated with this parameter, the background evolution and hence the above set of perturbation equations are significantly different from EDS. Our analysis thus extends the work done in [38] from theoretical perspectives with distinctive features of the realistic observable universe. As remarked earlier, we will mostly focus on the ΛCDM (and beyond) case in the subsequent analysis.…”

Section: Jcap12(2023)004supporting

confidence: 69%

“…(2.8). The validity of the approximation has been explored in detail in [17,38] at late time, particularly in matter dominated era. Here we have analysed the validity of the approximation in generalised background cosmology in a perturbative fashion in the followed sections.…”

Section: Jcap12(2023)004mentioning

confidence: 99%

“…Having the stage set up, we proceed with our analysis to solve the coupled fluid equations in ΛCDM universe in the following subsection. The evolution of neutrino overdensity and velocity divergence in matter-only Einstein-de Sitter (EDS) universe has been explored to a considerable extent in [27,38]. However, in order to corroborate with observations, one needs to go beyond a matter-only Universe and develop a consistent framework in background ΛCDM (and possibly, evolving DE) cosmology.…”

Section: Jcap12(2023)004mentioning

confidence: 99%

“…Finding a fully analytic solution to the coupled two-fluid equations including the aforementioned generalizations is somewhat difficult. However one can still make progress by treating the neutrino mass fraction (f ν ) as a small parameter, a strategy that was advocated recently in [38] and has also been followed in the present work. In this approach, we provide solutions in terms of numerical integrals for the coupled two-fluid system in ΛCDM background and compute the resulting suppression in the total matter and velocity power spectrum.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Revisiting coupled CDM-massive neutrino perturbations in diverse cosmological backgrounds

Pal,

Samanta,

Pal

2023

J. Cosmol. Astropart. Phys.

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Massive neutrinos are well-known to cause a characteristic suppression in the growth of structures at scales below the neutrino free-streaming length. A detailed understanding of this suppression is essential in the era of precision cosmology we are entering into, enabling us to better constrain the total neutrino mass and possibly probe (beyond)-ΛCDM cosmological model(s). Instead of the usual N-body simulation or Boltzmann solver, in this article we consider a two-fluid framework at the linear scales, where the neutrino fluid perturbations are coupled to the CDM (+ baryon) fluid via gravity at redshifts of interest. Treating the neutrino mass fraction f ν as a perturbative parameter, we find solutions to the system with redshift-dependent neutrino free-streaming length in ΛCDM background via two separate approaches. The perturbative scale-dependent solution is shown to be in excellent agreement with numerical solution of the two-fluid equations valid to all orders in f ν, and also agrees with results from CLASS to a good accuracy. We further generalize the framework to incorporate different evolving dark energy backgrounds and found sub-percent level differences in the suppression, all of which lie within the observational uncertainty of BOSS-like surveys. We also present a brief discussion on the prospects of the current analysis in the context of upcoming missions.

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Section: Jcap12(2023)004supporting

confidence: 69%

Section: Jcap12(2023)004mentioning

confidence: 99%

Section: Jcap12(2023)004mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Revisiting coupled CDM-massive neutrino perturbations in diverse cosmological backgrounds

Pal,

Samanta,

Pal

2023

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…[168][169][170][171][172][173][174][175][176][177]), as well as related cosmological observables (see e.g. [178][179][180][181][182][183][184][185][186][187][188][189][190]).…”

Section: Introductionmentioning

confidence: 99%

Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements

Tanseri,

Hagstotz,

Vagnozzi

et al. 2022

Preprint

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We revisit cosmological constraints on the sum of the neutrino masses Σm ν from a combination of full-shape BOSS galaxy clustering [P (k)] data and measurements of the crosscorrelation between Planck Cosmic Microwave Background (CMB) lensing convergence and BOSS galaxy overdensity maps [C κg ], using a simple but theoretically motivated model for the scale-dependent galaxy bias in auto-and cross-correlation measurements. We improve upon earlier related work in several respects, particularly through a more accurate treatment of the correlation and covariance between P (k) and C κg measurements. When combining these measurements with Planck CMB data, we find a 95% confidence level upper limit of Σm ν < 0.14 eV, while slightly weaker limits are obtained when including small-scale ACTPol CMB data, in agreement with our expectations. We confirm earlier findings that (once combined with CMB data) the full-shape information content is comparable to the geometrical information content in the reconstructed BAO peaks given the precision of current galaxy clustering data, discuss the physical significance of our inferred bias and shot noise parameters, and perform a number of robustness tests on our underlying model. While the inclusion of C κg measurements does not currently appear to lead to substantial improvements in the resulting Σm ν constraints, we expect the converse to be true for near-future galaxy clustering measurements, whose shape information content will eventually supersede the geometrical one.

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Two-loop power spectrum with full time- and scale-dependence and EFT corrections: impact of massive neutrinos and going beyond EdS

Garny

Taule

2022

J. Cosmol. Astropart. Phys.

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We compute the density and velocity power spectra at next-to-next-to-leading order taking into account the effect of time- and scale-dependent growth of massive neutrino perturbations as well as the departure from Einstein-de-Sitter (EdS) dynamics at late times non-linearly. We determine the impact of these effects by comparing to the commonly adopted approximate treatment where they are not included. For the bare cold dark matter (CDM)+baryon spectrum, we find percent deviations for k ≳ 0.17h Mpc-1, mainly due to the departure from EdS. For the velocity and cross power spectrum the main difference arises due to time- and scale-dependence in presence of massive neutrinos yielding percent deviation above k ≃ 0.08, 0.13, 0.16h Mpc-1 for ∑mν = 0.4, 0.2, 0.1 eV, respectively. We use an effective field theory (EFT) framework at two-loop valid for wavenumbers k ≫ k FS, where k FS is the neutrino free-streaming scale. Comparing to Quijote N-body simulations, we find that for the CDM+baryon density power spectrum the effect of neutrino perturbations and exact time-dependent dynamics at late times can be accounted for by a shift in the one-loop EFT counterterm, Δγ̅1 ≃ - 0.2 Mpc2/h 2. We find percent agreement between the perturbative and N-body results up to k ≲ 0.12h Mpc-1 and k ≲ 0.16h Mpc-1 at one- and two-loop order, respectively, for all considered neutrino masses ∑mν ≤ 0.4 eV.

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A Two-Fluid Treatment of the Effect of Neutrinos on the Matter Density

Cited by 3 publications

References 23 publications

Revisiting coupled CDM-massive neutrino perturbations in diverse cosmological backgrounds

Revisiting coupled CDM-massive neutrino perturbations in diverse cosmological backgrounds

Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements

Two-loop power spectrum with full time- and scale-dependence and EFT corrections: impact of massive neutrinos and going beyond EdS

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