The MUSE-Faint survey. II. The dark matter-density profile of the ultra-faint dwarf galaxy Eridanus 2

Zoutendijk, Sebastiaan L.; Brinchmann, Jarle; Bouché, Nicolas; Brok, Mark den; Krajnović, Davor; Kuijken, K.; Maseda, Michael V.; Schaye, Joop

doi:10.1051/0004-6361/202040239

Cited by 25 publications

(16 citation statements)

References 119 publications

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“…The dark photon exchange, on the other hand, causes the velocity independent self-interaction cross section σ 0 /m DM ∼ 4πα 2 D m DM /m 4 γ , which is of O(0.01-0.1) cm 2 /g. This cross section is consistent with the constraints, σ 0 /m DM 0.1-1cm 2 /g, obtained from the galaxy clusters [61][62][63][64][65][66][67][68][69], and, σ 0 /m DM 0.01-0.1cm 2 /g, obtained from the ultra-faint dwarf galaxies [70,71]. 15 14 Here, we assume that there is no asymmetry between the dark pion and the dark anti-pion, which is justified in the appendix B.…”

Section: Jhep07(2021)220supporting

confidence: 84%

Chiral composite asymmetric dark matter

Ibe

Kobayashi

Watanabe

2021

J. High Energ. Phys.

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The asymmetric dark matter (ADM) scenario solves the baryon-dark matter coincidence problem when the dark matter (DM) mass is of $$ \mathcal{O}(1) $$ O 1 GeV. Composite ADM models based on QCD-like strong dynamics are particularly motivated since the strong dynamics naturally provides the DM mass of $$ \mathcal{O}(1) $$ O 1 GeV and the large annihilation cross-section simultaneously. In those models, the sub-GeV dark photon often plays an essential role in transferring the excessive entropy in the dark sector into the visible sector, i.e., the Standard Model sector. This paper constructs a chiral composite ADM model where the U(1)D gauge symmetry is embedded into the chiral flavor symmetry. Due to the dynamical breaking of the chiral flavor symmetry, the model naturally provides the masses of the dark photon and the dark pions in the sub-GeV range, both of which play crucial roles for a successful ADM model.

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Section: Jhep07(2021)220supporting

confidence: 84%

Chiral composite asymmetric dark matter

Ibe

Kobayashi

Watanabe

2021

J. High Energ. Phys.

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“…There is a long history of performing this type of analysis in local dwarfs (e.g. Kravtsov et al 1998;de Blok et al 2001;Goerdt et al 2006;Oh et al 2011Oh et al , 2015Read et al 2016bRead et al , 2018Read et al , 2019Karukes & Salucci 2017;Zoutendijk et al 2021), in spiral galaxies (e.g. Gentile et al 2004;Spano et al 2008;Donato et al 2009;Martinsson et al 2013a;Allaert et al 2017;Katz et al 2017;Korsaga et al 2018;Di Paolo et al 2019) or in massive early type galaxies often aided by gravitational lensing (e.g.…”

Section: Dm Halos Properties With Core or Cuspy Profilesmentioning

confidence: 99%

The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies atz≃ 1

Bouché

Bera

Krajnović

et al. 2022

A&A

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Context. Disc-halo decompositions z = 1 − 2 star-forming galaxies (SFGs) at z > 1 are often limited to massive galaxies (M⋆ > 1010 M⊙) and rely on either deep integral field spectroscopy data or stacking analyses. Aims. We present a study of the dark-matter (DM) content of nine z ≈ 1 SFGs selected among the brightest [O II] emitters in the deepest Multi-Unit Spectrograph Explorer (MUSE) field to date, namely the 140 h MUSE Extremely Deep Field. These SFGs have low stellar masses, ranging from 108.5 to 1010.5 M⊙. Methods. We analyzed the kinematics with a 3D modeling approach, which allowed us to measure individual rotation curves to ≈3 times the half-light radius Re. We performed disk-halo decompositions on their [O II] emission line with a 3D parametric model. The disk-halo decomposition includes a stellar, DM, gas, and occasionally a bulge component. The DM component primarily uses the generalized α, β, γ profile or a Navarro-Frenk-White profile. Results. The disk stellar masses M⋆ obtained from the [O II] disk-halo decomposition agree with the values inferred from the spectral energy distributions. While the rotation curves show diverse shapes, ranging from rising to declining at large radii, the DM fractions within the half-light radius fDM(< Re) are found to be 60% to 95%, extending to lower masses (densities) recent results who found low DM fractions in SFGs with M⋆ > 1010 M⊙. The DM halos show constant surface densities of ∼100 M⊙ pc−2. For isolated galaxies, half of the sample shows a strong preference for cored over cuspy DM profiles. The presence of DM cores appears to be related to galaxies with low stellar-to-halo mass ratio, log M⋆/Mvir ≈ −2.5. In addition, the cuspiness of the DM profiles is found to be a strong function of the recent star-formation activity. Conclusions. We measured the properties of DM halos on scales from 1 to 15 kpc, put constraints on the z > 0 cvir − Mvir scaling relation, and unveiled the cored nature of DM halos in some z ≃ 1 SFGs. These results support feedback-induced core formation in the cold dark matter context.

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“…With MUSE-Faint (Zoutendijk et al 2020; hereafter Paper I), a survey of UFDs with MUSE (Bacon et al 2010), we are observing the spectroscopically unexplored centres of faint and ultra-faint satellites of the Milky Way. Previously, we have derived constraints on the dark-matter density profile of Eridanus 2 (Eri 2) and on the properties of self-interacting and fuzzy dark matter (Zoutendijk et al 2021; hereafter Paper II). While we could not resolve a core, we found that a core in Eri 2 must be smaller than ≈100 pc (95% confidence level), which is smaller than the cores found in larger dwarf galaxies.…”

Section: Introductionmentioning

confidence: 99%

The MUSE-Faint survey. III. No large dark-matter cores and no significant tidal stripping in ultra-faint dwarf galaxies

Zoutendijk¹,

Júlio²,

Brinchmann³

et al. 2021

Preprint

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Aims. The lowest-mass galaxies, ultra-faint dwarf galaxies, promise unparalleled constraints on how feedback regulates galaxy formation, and on the small-scale matter power spectrum. Their inner dark-matter densities can also be used to constrain dark-matter models and to determine the most promising targets for potential signals from dark-matter annihilation or decay. However, these goals are limited by the current large uncertainties on the properties of the dark-matter haloes that these galaxies inhabit. In this paper, we present 201 new stellar line-of-sight velocities from the MUSE-Faint survey for the faint and ultra-faint dwarf galaxies Antlia B, Leo T, Hydra II, and Grus 1. Combining these with literature data, we obtain the tightest constraints to date on their dark-matter halo masses and inner dark-matter densities. Methods. We use the Jeans equations implemented in CJAM to model the density profiles and constrain the presence of dark-matter cores and solitons (a prediction of fuzzy dark-matter models). Further modelling is done with GravSphere to test the influence of the choice of modelling tool. We calculate masses, concentrations, and circular velocities from the profiles, include results for Eridanus 2 from our previous work, and compare these properties to theoretical scaling relations, deriving constraints on tidal stripping in the process.Results. We find that dark-matter cores as large as those of more massive dwarf galaxies are ruled out for our galaxies (core radius r c < 66-95 pc at the 68% confidence level). We constrain the soliton radii to r sol < 13-112 pc (68% confidence level). We find that the galaxies are consistent with not having been significantly tidally stripped within their half-light radii. The virial masses and concentrations are sensitive to the choice of dynamical modelling tool: GravSphere produces results consistent with M 200 ∼ 10 9 M , as expected from models in which ultra-faint dwarf galaxies are re-ionization fossils, while CJAM prefers haloes that are less massive.

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The MUSE-Faint survey. II. The dark matter-density profile of the ultra-faint dwarf galaxy Eridanus 2

Cited by 25 publications

References 119 publications

Chiral composite asymmetric dark matter

Chiral composite asymmetric dark matter

The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies atz≃ 1

The MUSE-Faint survey. III. No large dark-matter cores and no significant tidal stripping in ultra-faint dwarf galaxies

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