Erratum: Cores in warm dark matter haloes: a Catch 22 problem

Macciò, Andrea V.; Paduroiu, Sinziana; Anderhalden, Donnino; Schneider, Aurel; Moore, Ben

doi:10.1093/mnras/sts251

Cited by 24 publications

(15 citation statements)

References 2 publications

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“…This is not valid for radii smaller than some critical value, since WDM predicts the formation of a core beyond a WDM model-dependent density. However, the scales for core formation is less than O(10) pc (Villaescusa- Navarro & Dalal 2011;Macciò et al 2012Macciò et al , 2013, i.e., not an important effect on scales of interest in this study.…”

Section: Internal Structure Of Subhalosmentioning

confidence: 79%

Properties of resonantly produced sterile neutrino dark matter subhaloes

Horiuchi

Bozek

Abazajian

et al. 2016

Mon. Not. R. Astron. Soc.

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The anomalous 3.55 keV X-ray line recently detected towards a number of massive dark matter objects may be interpreted as the radiative decays of 7.1 keV mass sterile neutrino dark matter. Depending on its parameters, the sterile neutrino can range from cold to warm dark matter with small-scale suppression that differs in form from commonly-adopted thermal warm dark matter. Here, we numerically investigate the subhalo properties for 7.1 keV sterile neutrino dark matter produced via the resonant Shi-Fuller mechanism. Using accurate matter power spectra, we run cosmological zoom-in simulations of a Milky Way-sized halo and explore the abundance of massive subhalos, their radial distributions, and their internal structure. We also simulate the halo with thermal 2.0 keV warm dark matter for comparison and discuss quantitative differences. We find that the resonantly produced sterile neutrino model for the 3.55 keV line provides a good description of structures in the Local Group, including the number of satellite dwarf galaxies and their radial distribution, and largely mitigates the too-big-to-fail problem. Future searches for satellite galaxies by deep surveys, such as the Dark Energy Survey, Large Synoptic Survey Telescope, and Wide Field Infrared Survey Telescope, will be a strong direct test of warm dark matter scenarios.

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Section: Internal Structure Of Subhalosmentioning

confidence: 79%

Properties of resonantly produced sterile neutrino dark matter subhaloes

Horiuchi

Bozek

Abazajian

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Some authors have proposed that warm dark matter (WDM), with initial velocities large enough to prevent formation of small dark matter halos, could solve some of these problems. However, that does not appear to work: the systematics of galactic radial density profiles predicted by WDM do not at all match the observed ones (Kuzio de Naray et al, 2010;Macciò et al, 2012aMacciò et al, , 2013. WDM that's warm enough to affect galaxy centers may not permit early enough galaxy formation to reionize the universe (Governato et al, 2015).…”

Section: Review Researchmentioning

confidence: 96%

Cosmological Structure Formation

Primack¹

2017

The Philosophy of Cosmology

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“…For WDM, this is not true: its maximal phase-space density f max is finite at early times and does not increase during halo formation [17]. Usually, density distri-butions with finite f max are derived either from analytical studies of self-gravitating Fermi-Dirac dark matter (see, e.g., [18][19][20][21][22][23][24][25][26][27]) or from N -body simulations imitating initial dark matter velocities (see, e.g., [28][29][30][31][32]).…”

Section: Pacsmentioning

confidence: 99%

New Model of Density Distribution for Fermionic Dark Matter Halos

Rudakovskyi

Savchenko

2018

Ukr. J. Phys.

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PACSIn this paper, we formulate a new model of density distribution for halos made of warm dark matter (WDM) particles. The model is described by a single microphysics parameter the mass (or, equivalently, the maximal value of the initial phase-space density distribution) of dark matter particles. Given the WDM particle mass and the parameters of a dark matter density profile at the halo periphery, this model predicts the inner density profile. In case of initial Fermi-Dirac distribution, we successfully reproduce cored dark matter profiles from N -body simulations. Also, we calculate the core radii of warm dark matter halos of dwarf spheroidal galaxies for particle masses mfd = 100, 200, 300 and 400 eV. K e y w o r d s: Dark matter: warm, cold; dark matter halo profile; cores; Navarro-Frenk-White profileThe nature of dark matter the largest gravitating substance in the Universe is not yet identified. Usual (left-handed) neutrinos the only natural dark matter candidate within the Standard Model of particle physics are too light to form the observed large-scale structure of the Universe [1] and the densest dark matter-dominated objects, dwarf spheroidals (dSphs) [2]. So far, many extensions of the Standard Model containing a viable dark matter candidate have been proposed; see, e.g., reviews [3][4][5][6]. In terms of their initial velocities, valid dark matter candidates can be split in two groups 1 (see, e.g., [9]):• cold dark matter (CDM), composed of particles with small (non-relativistic) initial velocities [10,11]; c A.V. RUDAKOVSKYI, D.O. SAVCHENKO, 2018 1 Note that, for some specific dark matter particle candidates, their initial velocity spectrum can be approximated by a mixture of 'cold ' and 'warm' components [7, 8].• warm dark matter (WDM), composed of particles with large (relativistic) initial velocities [12,13].Density distribution of CDM haloes is often described by the Navarro-Frenk-White (NFW) profile [14,15] ρ nfw (r) = ρ s r s r 1 + r rs 2 . (1) Its parameters ρ s and r s are connected with the halo mass M 200 (the mass within the sphere of radius R 200 , within which the average density is 200 times larger than the critical density ρ crit of the Universe) and halo concentration parameter c 200 = R 200 /r s .The phase-space density for CDM haloes becomes infinite towards the halo centre; see, e.g., [16]. For WDM, this is not true: its maximal phase-space density f max is finite at early times and does not increase during halo formation [17]. Usually, density distri-

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Erratum: Cores in warm dark matter haloes: a Catch 22 problem

Cited by 24 publications

References 2 publications

Properties of resonantly produced sterile neutrino dark matter subhaloes

Properties of resonantly produced sterile neutrino dark matter subhaloes

Cosmological Structure Formation

New Model of Density Distribution for Fermionic Dark Matter Halos

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