The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies at z=1

Bouché, Nicolas F.; Bera, Samuel; Krajnovic, Davor; Emsellem, Eric; Mercier, Wilfried; Schaye, Joop; Épinat, Benoît; Richard, Johan; Zoutendijk, Sebastiaan L.; Abril-Melgarejo, Valentina; Brinchmann, Jarle; Bacon, Roland; Contini, Thierry; Boogaard, Leindert; Wisotzki, Lutz; Maseda, Michael; Steinmetz, Matthias

doi:10.48550/arxiv.2109.07545

Cited by 5 publications

(6 citation statements)

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“…Some authors also implement an asymmetric drift correction to take into account the impact of gas pressure on its dynamics (e.g. Meurer et al 1996;Übler et al 2017;Abril-Melgarejo et al 2021;Bouché et al 2021). Evaluated at R 22 , the gas pressured corrected circular velocity for a double exponential density profile with a constant thickness writes (Meurer et al 1996;Bouché et al 2021)…”

Section: Impact Of the Environment On The Tfrmentioning

confidence: 99%

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Scaling relations of z ∼ 0.25–1.5 galaxies in various environments from the morpho-kinematics analysis of the MAGIC sample

Mercier

Épinat

Contini

et al. 2022

A&A

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Context. The evolution of galaxies is influenced by many physical processes, which may vary depending on their environment. Aims. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic Explorer (MUSE) data of galaxies at 0.25 z 1.5 to probe the impact of environment on the size-mass relation, the main sequence (MS) relation, and the Tully-Fisher relation (TFR). Methods. We perform a morpho-kinematics modelling of 593 [O ii] emitters in various environments in the COSMOS area from the MUSE-gAlaxy Groups In Cosmos survey. The HST F814W images are modelled with a bulge-disk decomposition to estimate their bulge-disk ratio, effective radius, and disk inclination. We use the [O ii]λλ3727, 3729 doublet to extract the galaxies' ionised gas kinematics maps from the MUSE cubes, and we model those maps for a sample of 146 [O ii] emitters, including bulge and disk components constrained from morphology and a dark matter halo. Results. We find an offset of 0.03 dex (1σ significant) on the size-mass relation zero point between the field and the large structure sub-samples, with a richness threshold of N = 10 to separate between small and large structures, and of 0.06 dex (2σ) with N = 20. Similarly, we find a 0.1 dex (2σ) difference on the MS relation with N = 10 and 0.15 dex (3σ) with N = 20. These results suggest that galaxies in massive structures are smaller by 14% and have star formation rates reduced by a factor of 1.3 − 1.5 with respect to field galaxies at z ≈ 0.7. Finally, we do not find any impact of the environment on the TFR, except when using N = 20 with an offset of 0.04 dex (1σ). We discard the effect of quenching for the largest structures, which would lead to an offset in the opposite direction. We find that, at z ≈ 0.7, if quenching impacts the mass budget of galaxies in structures, these galaxies would have been affected quite recently and for roughly 0.7 − 1.5 Gyr. This result holds when including the gas mass but vanishes once we include the asymmetric drift correction.

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Section: Impact Of the Environment On The Tfrmentioning

confidence: 99%

“…Meurer et al 1996;Übler et al 2017;Abril-Melgarejo et al 2021;Bouché et al 2021). Evaluated at R 22 , the gas pressured corrected circular velocity for a double exponential density profile with a constant thickness writes (Meurer et al 1996;Bouché et al 2021)…”

Section: Impact Of the Environment On The Tfrmentioning

confidence: 99%

Scaling relations of z ∼ 0.25–1.5 galaxies in various environments from the morpho-kinematics analysis of the MAGIC sample

Mercier

Épinat

Contini

et al. 2022

A&A

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“…Indeed, there seems to be mounting observational evidence for this scenario (e.g. Bouché et al 2021;Sharma et al 2021).…”

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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“…A potential solution to resolve the mismatch between the ΛCDM prediction and observations is the dynamical heating caused by the potential fluctuation of the galactic gas driven by supernova feedback and radiative cooling (e.g., Pontzen & Governato 2012;Ogiya & Mori 2014;Read et al 2016). Observations showed that star formation induced cores can be formed in the centre of galaxies at 𝑧 ∼ 1 (Bouché et al 2021). However, supernova feedback would not be powerful enough to expel the gas from the centre of massive galaxies, and thus this process does not work to alter the central DM density structure of massive systems (Silk & Mamon 2012;Di Cintio et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Dark matter cores in massive high-$z$ galaxies formed by baryonic clumps

Ogiya,

Nagai

2022

Preprint

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The rotation curves of some star forming massive galaxies at redshift two decline over the radial range of a few times the effective radius, indicating a significant deficit of dark matter (DM) mass in the galaxy centre. The DM mass deficit is interpreted as the existence of a DM density core rather than the cuspy structure predicted by the standard cosmological model. A recent study proposed that a galaxy merger, in which the smaller satellite galaxy is significantly compacted by dissipative contraction of the galactic gas, can heat the centre of the host galaxy and help make a large DM core. By using an 𝑁-body simulation, we find that a large amount of DM mass is imported to the centre by the merging satellite, making this scenario an unlikely solution for the DM mass deficit. In this work, we consider giant baryonic clumps in high redshift galaxies as alternative heating source for creating the baryon dominated galaxies with a DM core. Due to dynamical friction, the orbit of clumps decays in a few Gyr and the baryons condensate at the galactic centre. As a back-reaction, the halo centre is heated up and the density cusp is flattened out. The combination of the baryon condensation and core formation makes the galaxy baryon dominated in the central 2-5 kpc, comparable to the effective radius of the observed galaxies. Thus, the dynamical heating by giant baryonic clumps is a viable mechanism for explaining the observed dearth of DM in high redshift galaxies.

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The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies at z=1

Cited by 5 publications

References 162 publications

Scaling relations of z ∼ 0.25–1.5 galaxies in various environments from the morpho-kinematics analysis of the MAGIC sample

Scaling relations of z ∼ 0.25–1.5 galaxies in various environments from the morpho-kinematics analysis of the MAGIC sample

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

Dark matter cores in massive high-$z$ galaxies formed by baryonic clumps

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