Galaxy rotation curves using a non-parametric regression method: core, cuspy and fuzzy scalar field dark matter models

Fernandez-Hernandez, Lizbeth M.; Montiel, Ariadna; Rodríguez‐Meza, M. A.

doi:10.1093/mnras/stz1969

Cited by 11 publications

(13 citation statements)

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“…For z ≫ 1, x ≪ 1 this expression is quite similar to (35) and for x ≥ 1 it is similar to (36). As is seen from ( 37) for x ≪ 1 we have…”

Section: Evolution Of Massive Halossupporting

confidence: 59%

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The patch like model of galaxies formation: the virial paradox, core-cusp and missing satellite problems

Demiański¹,

Doroshkevich²

2020

Preprint

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The patch like model of the hierarchical galaxy formation in the ΛCDM cosmological model with small damping scale is considered. In this model galaxies and clusters of galaxies are identified with rare high density peaks, what suppresses the action of random factors in the vicinity of peaks and makes the process of halos formation more rapid and regular. High concentration of irregular subhalos surrounding the central peaks and their subsequent merging just after formation allows to consider this medium as a mixture of collisionless dispersed dark matter (DM) particles and collisional subhalos. Merging of these subhalos with the central dominating halo is accompanied by tidal destruction of the central cusp, what progressively shallows the density profile and promotes formation of super massive central black holes. The simulations [1-3] provide some quantitative characteristics of these processes.In the framework of this model we can reproduce the observed correlation of mass and density of virialized galaxies and clusters of galaxies known as the virial paradox [4,5]. These correlations are closely linked with the composition of DM and the shape of the power spectrum of density perturbations what allows to restrict them using already available observations. In particular, these correlations put constraints on the HDM and WDM models and allow to test models of cosmological inflation. We confirm that the missing satellite problem is directly linked with the virial paradox and reheating of the Universe which increases temperature and entropy of the baryons, prevents formation of first stars and divides halos into two populations: the first one includes galaxies formed before reheating which are mainly concentrated in the vicinity of the massive ones while the second population -numerous dark halos formed after reheating -accumulates majority of DM but does not contain stars. Their spatial distribution is more homogeneous.

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“…For z ≫ 1, x ≪ 1 this expression is quite similar to (35) and for x ≥ 1 it is similar to (36). As is seen from ( 37) for x ≪ 1 we have…”

Section: Evolution Of Massive Halossupporting

confidence: 59%

“…This profile reproduces reasonably well the observed one in clusters of galaxies. However in less massive galaxies the density profile is more shallow [33][34][35] and can be expressed by the relation (1) with the power index α ≃ 0.4 ≤ 1. This is the core-cusp problem.…”

Section: Introductionmentioning

confidence: 99%

The patch like model of galaxies formation: the virial paradox, core-cusp and missing satellite problems

Demiański¹,

Doroshkevich²

2020

Preprint

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“…Furthermore, in order to compute the measurement errors of the data we use Simulation and extrapolation method (Simex). The merging of both techniques is the so-called LOESS-Simex reconstruction, which has been used in order to reconstruct the cosmic expansion [32], the Om diagnostic up to first derivative on the Hubble parameter [33] and to reconstruct rotation curves for dark matter profiles [34].…”

Section: Introductionmentioning

confidence: 99%

Performance of Non-Parametric Reconstruction Techniques in the Late-Time Universe

Escamilla-Rivera,

Said,

Mifsud

2021

Preprint

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In the context of a Hubble tension problem that is growing in its statistical significance, we reconsider the effectiveness of non-parametric reconstruction techniques which are independent of prescriptive cosmological models. By taking cosmic chronometers, Type Ia Supernovae and baryonic acoustic oscillation data, we compare and contrast two important reconstruction approaches, namely Gaussian processes (GP) and the Locally weighted Scatterplot Smoothing together with Simulation and extrapolation method (LOESS-Simex or LS). We firstly show how both GP and LOESS-Simex can be used to successively reconstruct various data sets to a high level of precision. We then directly compare both approaches in a quantitative manner by considering several factors, such as how well the reconstructions approximate the data sets themselves to how their respective uncertainties evolve. In light of the puzzling Hubble tension, it is important to consider how the uncertain regions evolve over redshift and the methods compare for estimating cosmological parameters at current times. For cosmic chronometers and baryonic acoustic oscillation compiled data sets, we find that GP generically produce smaller variances for the reconstructed data with a minimum value of σ GP−min = 1.1, while the situation for LS is totally different with a minimum of σ LS−min = 50.8. Moreover, some of these characteristics can be alliviate at low z, where LS presents less underestimation in comparison to GP.

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“…These so called dark matter cores are characterised by a finite central density ρ 0 and a flat density profile within a core radius r 0 , reminiscent of self-gravitating isothermal spheres (e.g. Moore, 1994;Burkert 1995;Gentile et al 2004;de Blok 2010;Pontzen & Governato 2014;Fernández-Hernández et al 2019;Genzel et al 2020; for reviews with references see Weinberg et al 2015and di Paolo & Salucci 2020. Various empirical density distributions have been proposed to fit these cores.…”

Section: Introductionmentioning

confidence: 99%

Fuzzy Dark Matter and Dark Matter Halo Cores

Burkert

2020

Preprint

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Whereas cold dark matter (CDM) simulations predict central dark matter cusps with densities that diverge as ρ(r)∼ 1/r observations often indicate constant density cores with finite central densities ρ 0 and a flat density distribution within a core radius r 0 . This paper investigates whether this core-cusp problem can be solved by fuzzy dark matter (FDM), a hypothetical particle with a mass of order m≈10 −22 eV and a corresponding de Broglie wavelength on astrophysical scales. We show that galaxies with CDM halo virial masses M vir ≤ 10 11 M ⊙ follow two core scaling relations. In addition to the well known universal core column density Σ 0 ≡ ρ 0 ×r 0 = 75 M ⊙ pc −2 core radii increase with virial masses as r 0 ∼ M γ vir with γ of order unity. Using the simulations by Schive et al. ( 2014) we demonstrate that FDM can explain the r 0 -M vir scaling relation if the virial masses of the observed galaxy sample scale with formation redshift z as M vir ∼(1+z) −0.4 . The observed constant Σ 0 is however in complete disagreement with FDM cores which are characterised by a steep dependence Σ 0 ∼r −3 0 , independent of z. More highresolution simulations are now required to confirm the Schive et al. simulations and explore especially the transition region between the soliton core and the surrounding halo. If these results hold, FDM can be ruled out as the origin of observed dark matter cores and other physical processes are required to account for their formation.

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Galaxy rotation curves using a non-parametric regression method: core, cuspy and fuzzy scalar field dark matter models

Cited by 11 publications

References 50 publications

The patch like model of galaxies formation: the virial paradox, core-cusp and missing satellite problems

The patch like model of galaxies formation: the virial paradox, core-cusp and missing satellite problems

Performance of Non-Parametric Reconstruction Techniques in the Late-Time Universe

Fuzzy Dark Matter and Dark Matter Halo Cores

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