Review of solutions to the Cusp-core problem of the $Λ$CDM Model

Popolo, A. Del; Delliou, Morgan Le

doi:10.48550/arxiv.2209.14151

Cited by 3 publications

(3 citation statements)

References 223 publications

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“…The formation of cores at the center of dark matter haloes has been long debated (Bullock & Boylan-Kolchin 2017;Del Popolo & Le Delliou 2022). The tension, named the 'core/cusp problem', comes from observations of present-day dwarf galaxies, in which a constant dark matter density distribution is inferred from measures of central rotation velocities (McGaugh & de Blok 1998;de Blok et al 2003;Gentile et al 2007;Salucci et al 2007;Oh et al 2015), whereas dark matter haloes from early N -body, DMO simulations preferentially form cusps (Dubinski & Carlberg 1991;Navarro et al 1996a).…”

Section: Baryon-driven Flattening Of Cusps In Dark Matter Haloesmentioning

confidence: 99%

“…As mentioned, the presence of cusps or cores of constant densities at the centres of dark matter haloes can also have a significant im-pact in differentiating between cosmological and galaxy evolution models (Bullock & Boylan-Kolchin 2017;Del Popolo & Le Delliou 2022). The contrast between DMO simulations, that predict haloes to accumulate mass in the inner parts following cuspy profiles, and measurements based on observations of rotation curves of local disc galaxies is, indeed, an indication that the effects of baryons may not be negligible on small scale halo structures (Pontzen & Governato 2012) or may alternatively hint that exotic dark matter models / cosmologies may be required (Governato et al 2015).…”

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confidence: 99%

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Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations

Pascale,

Calura,

Lupi

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We use zoom-in, hydrodynamical, cosmological N-body simulations tracing the formation of the first stellar clumps from the SImulating the Environments where Globular clusters Emerged project, to study key structural properties of dark matter haloes when the Universe was only $0.92\, {\rm Gyr}$ old. The very high resolution (maximum physical resolution $0.3\, {h}^{-1}\, {\rm pc}$ at z = 6.14, smallest dark matter particle mass $164\, {\rm M}_{\odot }$) allows us to reach the very low mass end of the stellar-to-halo mass relation ($M_{\rm vir}=10^{7.5{\!-\!}9.5}\, {\rm M}_{\odot }$) to study the processes that mould dark matter haloes during the first stages of structure formation. We investigate the role of baryonic cooling and stellar feedback, modelled from individual stars, in shaping haloes, and of environmental effects as accretion of dark matter along cosmic filaments and mergers. We find that the onset of star formation (typically for $\log M_{\rm vir}/\, {\rm M}_{\odot }\simeq 7.6$) causes the inner cusp in the haloes’ density profile to flatten into a core with constant density and size proportionally to the halo virial mass. Even at these mass scales, we confirm that baryons make haloes that have formed stars rounder in the central regions than haloes that have not formed stars yet, with median minor-to-major 〈q〉 and intermediate-to-major 〈s〉 axes 0.66 and 0.84, respectively. Our morphological analysis shows that, at z = 6.14, haloes are largely prolate in the outer parts, with the major axis aligned along filaments of the cosmic web or towards smaller sub-haloes, with the degree of elongation having no significant dependence on the halo mass.

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Section: Baryon-driven Flattening Of Cusps In Dark Matter Haloesmentioning

confidence: 99%

mentioning

confidence: 99%

Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations

Pascale,

Calura,

Lupi

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…Read et al 2016;Di Cintio et al 2017). For a recent review of cusps and cores see Del Popolo & Le Delliou (2022).…”

Section: Deriving Halo Masses From Measured Dynamical Massesmentioning

confidence: 99%

Globular Clusters in Early-Type Galaxies

Forbes

Eso Astrophysics Symposia

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Do ultra diffuse galaxies with rich globular clusters systems have overly massive haloes?

Forbes,

Gannon

2023

Monthly Notices of the Royal Astronomical Society

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Some Ultra Diffuse Galaxies (UDGs) appear to host exceptionally rich globular cluster (GC) systems compared to normal galaxies of the same stellar mass. After re-examing these claims, we focus on a small sample of UDGs from the literature that have both rich GC systems (NGC >20) and a measured galaxy velocity dispersion. We find that UDGs with more GCs have higher dynamical masses and that GC-rich UDGs are dark matter dominated within their half-light radii. We extrapolate these dynamical masses to derive total halo masses assuming cuspy and cored mass profiles. We find reasonable agreement between halo masses derived from GC numbers (assuming the GC number - halo mass relation) and from cored halo profiles. This suggests that GC-rich UDGs do not follow the standard stellar mass – halo mass relation, occupying overly massive cored halos for their stellar mass. A similar process to that invoked for some Local Group dwarfs, of early quenching, may result in GC-rich UDGs that have failed to form the expected mass of stars in a given halo (and thus giving the appearance of overly an massive halo). Simulations that correctly reproduce the known properties of GC systems associated with UDGs are needed.

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Review of solutions to the Cusp-core problem of the $Λ$CDM Model

Cited by 3 publications

References 223 publications

Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations

Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations

Globular Clusters in Early-Type Galaxies

Do ultra diffuse galaxies with rich globular clusters systems have overly massive haloes?

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