A high precision semi-analytic mass function

Popolo, A. Del; Pace, Francesco; Delliou, Morgan Le

doi:10.1088/1475-7516/2017/03/032

Cited by 38 publications

(50 citation statements)

References 166 publications

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“…More precise predictions are actively being sought (e.g. Pace et al 2014;Pace, Batista & Del Popolo Rei;Del Popolo et al 2017). Eventually we will converge towards an ultimate physical model for the halo mass function.…”

Section: Halo Mass Functionmentioning

confidence: 99%

“…Hopefully such an exercise will be repeated with current and future simulations to reach a better empirical halo definition. About the theoretical halo definition, it seems recent investigations on the extended spherical collapse models by Del Popolo et al (2017) point towards a modification of the Sheth & Tormen (1999) along the lines of the modifications made by Bhattacharya et al (2011). So there might be a physical reason behind the fact that the Bhattacharya et al (2011) is a better description of the data than Sheth & Tormen (1999).…”

Section: Halo Finding Processmentioning

confidence: 99%

See 1 more Smart Citation

Accurate mass and velocity functions of dark matter haloes

Comparat¹,

Prada²,

Yepes³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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N-body cosmological simulations are an essential tool to understand the observed distribution of galaxies. We use the MultiDark simulation suite, run with the Planck cosmological parameters, to revisit the mass and velocity functions. At redshift z = 0, the simulations cover four orders of magnitude in halo mass from ∼ 10 11 M with 8,783,874 distinct halos and 532,533 subhalos. The total volume used is ∼515 Gpc 3 , more than 8 times larger than in previous studies. We measure and model the halo mass function, its covariance matrix w.r.t halo mass and the large scale halo bias. With the formalism of the excursion-set mass function, we explicit the tight interconnection between the covariance matrix, bias and halo mass function. We obtain a very accurate (< 2% level) model of the distinct halo mass function. We also model the subhalo mass function and its relation to the distinct halo mass function. The set of models obtained provides a complete and precise framework for the description of halos in the concordance Planck cosmology. Finally, we provide precise analytical fits of the V max maximum velocity function up to redshift z < 2.3 to push for the development of halo occupation distribution using V max . The data and the analysis code are made publicly available in the Skies and Universes database.

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Section: Halo Mass Functionmentioning

confidence: 99%

Section: Halo Finding Processmentioning

confidence: 99%

Accurate mass and velocity functions of dark matter haloes

Comparat¹,

Prada²,

Yepes³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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show abstract

“…The quoted problems are interconnected, and a unified solution can be obtained taking into account the role of baryons in the central parts of haloes Del Popolo and Le Delliou 2014). …”

Section: Introductionmentioning

confidence: 99%

On the dark matter haloes inner structure and galaxy morphology

Popolo

2016

Astrophys Space Sci

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In the present paper, we extend the study of Del Popolo (Mon. Not. R. Astron. Soc. 408:1808 to determine the slope of the inner density profile of galaxy haloes with different morphologies.We study how galaxy morphology changes the relation between the inner slope of the galaxy halo density profile, α, and the stellar mass, M * , or rotation velocity, V rot . For this, we use the model of Del Popolo (Astrophys. J. 698:293, 2009) in combination with observed data from the Romanowsky and Fall (Astrophys. J. Suppl. Ser. 203:17, 2012) sample of elliptical and spiral galaxies, the Local Group sample compiled by McConnachie (Astrophys. J. 144:4, 2012), and the simulation results by Cloet-Osselaer et al. (Mon. Not. R. Astron. Soc. 442:2909, 2014).We find that the slope α flattens monotonically, from α −1 at V rot 250 km/s, to α 0. After V rot 25 km/s the slope starts to steepen. The steepening happens in the mass range dominated by non-rotationally supported galaxies (e.g., dSphs) and depends on the level of offset in the angular momentum of rotationally and non-rotationally dominated galaxies. The steepening is a consequence of the decrease in baryons content, and angular momentum in spheroidal dwarf galaxies.We finally compare our result to the SPH simulations of Di Cintio. Our result is in qualitative agreement with their simulations, with the main difference that the inner slope α at small stellar masses (M * 10 8 M ) is flatter than that in their simulations.As a result, the claim that finding a core in dwarf galaxies with masses slightly smaller than 10 6 M (as in the Di Cintio, or Governato, supernovae feedback mechanism) would be a problem for the CDM model which should probably be revised.

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“…Unified baryonic solutions to the quoted problems, and others mentioned above have been proposed. They are based on the action of baryons located in the inner parts of the haloes (Zolotov et al 2012;Del Popolo 2014a, 2014b. Hence it is clear from the present work that a constant density core of the halos of dwarf galaxies are strongly preferred but the nature of this DM halo still remains to be explored in greater detail in future.…”

Section: Resultsmentioning

confidence: 78%

“…The cusp-core problem is not only typical of galaxies but there are evidences (e.g., Newman et al 2013aNewman et al , 2013bMartizzi et al 2012;Del Popolo 2012a, 2014a) that the inner DM profiles of clusters are flatter than those predicted by the -CDM model.…”

Section: Introductionmentioning

confidence: 99%

Study of the nature of dark matter in halos of dwarf galaxies

Karmakar

Chattopadhyay

2015

Astrophys Space Sci

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The kinematics of dwarf galaxies are strongly influenced by dark matter down to small galactocentric radii. So they are good candidates to investigate the nature of Dark Matter. In the present work we have carried out mass modeling of a number of recently observed dwarf galaxies Swaters et al. in Astron. Astrophys. 493:871, 2009. We have used a Navarro-Frenk-White (NFW) halo, Freeman disc along with a gaseous disc for modeling the observed rotation curves of those dwarf galaxies. For comparison we also used a Burkert halo, Freeman disc and gaseous disc. For both the scenario we have performed Kolmogorov-Smirnov (KS) test between the observed and predicted rotational velocity profiles. The tests are rejected for NFW halo almost in 50 per cent cases but they are accepted almost for all cases for Burkert halo, preferring a Burkert halo model generally for dwarf galaxies. The above results reveal a constant density core of dark matter (DM) in the halos of dwarf galaxies compared to a cuspy nature of NFW halo and a possible challenge to -CDM scenario for the nature of dark matter in most of the dwarf galaxies.

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A high precision semi-analytic mass function

Cited by 38 publications

References 166 publications

Accurate mass and velocity functions of dark matter haloes

Accurate mass and velocity functions of dark matter haloes

On the dark matter haloes inner structure and galaxy morphology

Study of the nature of dark matter in halos of dwarf galaxies

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