The Splashback Mass Function in the Presence of Massive Neutrinos

Abstract

We present a complementary methodology to constrain the total neutrino mass, $\sum m_{\nu }$, based on the diffusion coefficient of the splashback mass function of dark matter halos. Analyzing the snapshot data from the Massive Neutrino Simulations, we numerically obtain the number densities of distinct halos identified via the SPARTA code as a function of their splashback masses at various redshifts for two different cases of $\sum m_{\nu }=0.0$ eV and $0.1$ eV. Then, we fit the numerical results to the recently developed analytic formula characterized by the diffusion coefficient that quantifies the degree of ambiguity in the identification of the splashback boundaries. Our analysis confirms that the analytic formula works excellently even in the presence of neutrinos and that the decrement of its diffusion coefficient with redshift is well described by a linear fit, $B(z-z_c)$, in the redshift range of $0.2\le z\le 2$. It turns out that the massive neutrino case yields significantly lower value of $B$ and substantially higher value of $z_c$ than the massless neutrino case, which indicates that the higher masses the neutrinos have, the more severely the splashback boundaries become disturbed by the surroundings. Given our result, we conclude that the total neutrino mass can in principle be constrained by measuring how rapidly the diffusion coefficient of the splashback mass function diminishes with redshifts at $z\ge 0.2$. We also discuss the anomalous behavior of the diffusion coefficient found at lower redshifts for both of the $\sum m_{\nu }$ cases, and ascribe it to the fundamental limitation of the SPARTA code at $z\le 0.13$.

arXiv commentAccepted for publication in ApJ, 5 figures, 1 table

References in corpus (34)

• Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Planck 2013 results. XVI. Cosmological parameters
• Large scale bias and the peak background split
• Toward a halo mass function for precision cosmology: the limits of universality
• Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes
• Mass function of dark matter halos
• The Rockstar Phase-Space Temporal Halo Finder and the Velocity Offsets of Cluster Cores
• Using the Evolution of Clusters to Constrain Omega
• An excursion set model of hierarchical clustering: Ellipsoidal collapse and the moving barrier
• Precision Determination of the Mass Function of Dark Matter Halos
• Rotation-Dependent Catastrophic Disruption of Gravitational Aggregates
• Dependence of the outer density profiles of halos on their mass accretion rate
• A universal model for halo concentrations
• The splashback radius as a physical halo boundary and the growth of halo mass
• Splashback in accreting dark matter halos
• The pseudo-evolution of halo mass
• An efficient implementation of massive neutrinos in non-linear structure formation simulations
• Galaxy evolution near groups and clusters: ejected satellites and the spatial extent of environmental quenching
• Neutrino cosmology and Planck
• The Nonlinear Evolution of Rare Events
• MassiveNuS: Cosmological Massive Neutrino Simulations
• The Halo Mass Function from Excursion Set Theory. II. The Diffusing Barrier
• Collapse Barriers and Halo Abundance: Testing the Excursion Set Ansatz
• A model for the postcollapse equilibrium of cosmological structure: truncated isothermal spheres from top-hat density perturbations
• The splashback radius of halos from particle dynamics. I. The SPARTA algorithm
• Spherical collapse model in dark energy cosmologies
• The distribution of ejected subhalos and its implication for halo assembly bias
• An Efficient and Accurate Hybrid Method for Simulating Non-Linear Neutrino Structure
• Universal at last? The splashback mass function of dark matter halos
• Toward a Universal Formulation of the Halo Mass Function
• Excursion Set Halo Mass Function and Bias in a Stochastic Barrier Model of Ellipsoidal Collapse
• On the Nonspherical Nature of Halo Formation
• Flybys, orbits, splashback: subhalos and the importance of the halo boundary
• The Diffusion Coefficient of the Splashback Mass Function as a Probe of Cosmology

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