The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies at z ≃ 1¹

¹ Univ. Lyon, Univ. Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon (CRAL) UMR5574, 69230 Saint-Genis-Laval, France
e-mail: nicolas.bouche@univ-lyon1.fr
² Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
³ European Southern Observatory (ESO), Karl-Schwarzschild-Strasse 2, 85748 Garching b. München, Germany
⁴ Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, 31400 Toulouse, France
⁵ Leiden Observatory, Leiden University, PO Box 9513 2300 RA Leiden, The Netherlands
⁶ Aix Marseille Univ., CNRS, CNES, LAM, Marseille, France
⁷ Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
⁸ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany

Received: 9 July 2021
Accepted: 23 October 2021

Abstract

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 10^8.5 to 10^10.5 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 R_e. 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 f_DM(< R_e) 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_⋆/M_vir ≈ −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 c_vir − M_vir 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.