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

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

doi:10.1051/0004-6361/202040239

paper

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

arXiv:2101.00253 · doi:10.1051/0004-6361/202040239

Abstract

Aims. We use stellar line-of-sight velocities to constrain the dark matter-density profile of Eridanus 2, an ultra-faint dwarf galaxy ( $M_{V} = - 7.1$ , $M_{*} \approx 9 \times 1 0^{4} M_{⊙}$ ). We furthermore derive constraints on fundamental properties of self-interacting and fuzzy dark matter scenarios. Methods. We present new observations of Eridanus 2 from MUSE-Faint, a survey of ultra-faint dwarf galaxies with MUSE on the Very Large Telescope, and determine line-of-sight velocities for stars inside the half-light radius. Combined with literature data, we have 92 stellar tracers out to twice the half-light radius. We constrain models of cold dark matter, self-interacting dark matter, and fuzzy dark matter with these tracers, using CJAM and pyGravSphere for the dynamical analysis. Results. We find substantial evidence for cold dark matter over self-interacting dark matter and weak evidence for fuzzy dark matter over cold dark matter. We find a virial mass $M_{200} \sim 1 0^{8} M_{⊙}$ and astrophysical factors $J (α_{c}^{J}) \sim 1 0^{11} M_{⊙}^{2} kpc^{- 5}$ and $D (α_{c}^{D}) \sim 1 0^{2}$ - $1 0^{2.5} M_{⊙} kpc^{- 2}$ . We do not resolve a core ( $r_{c} < 47 pc$ , 68-% level) or soliton ( $r_{sol} < 7.2 pc$ , 68-% level). These limits are equivalent to an effective self-interaction coefficient $f Γ < 2.2 \times 1 0^{- 29} cm^{3} s^{- 1} eV^{- 1} c^{2}$ and a fuzzy-dark-matter particle mass $m_{a} > 4.0 \times 1 0^{- 20} eV c^{- 2}$ . The constraint on self-interaction is complementary to those from gamma-ray searches. The constraint on fuzzy-dark-matter particle mass is inconsistent with those obtained for larger dwarf galaxies, suggesting that the flattened density profiles of those galaxies are not caused by fuzzy dark matter. (Abridged)

arXiv comment24 pages, 14 figures, 8 tables. Minor changes, electronic table moved to appendix. Version as accepted on 2021-04-24 for publication in A&A

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

Abstract

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