MUSE-ALMA Haloes XV: Cold molecular, ionised, and stellar kinematics of HI-rich galaxies at z ∼ 0.5
Abstract
Spatially resolved galaxy kinematics are well studied at z ∼ 0 and z > 1, revealing that disks are common out to z ∼3−6, albeit with higher velocity dispersions. z ∼ 0.5 marks a key transition in the drivers of disk turbulence and baryonic-dark matter mass budgets, yet multi-tracer resolved kinematic studies remain rare beyond the local Universe. We exploit a unique dataset combining ALMA CO observations with MUSE ionised gas and stellar continuum data to study the resolved kinematics of six galaxies at 0.43 < z < 0.83, part of the MUSE-ALMA Haloes program, selected via their association with H I absorption systems and spanning stellar masses from log(M⋆/M⊙) = 10.1 − 11.8. Combining new ALMA/CO data with existing MUSE Hβ kinematics and HST morphologies, we classify galaxies using morpho-kinematic criteria. For rotating disks, we jointly model Hβ and CO(2-1) kinematics with DYSMALPY and compare results to theoretical predictions for pressure support, while pPXF is used to fit stellar absorption features. Four of the six galaxies are classified as disks, with two having known group members. These disks show elevated gas velocity dispersions relative to z ∼ 0 disks, consistent with interpolated trends between z ∼ 0 and z > 1. The results support marginally stable gaseous disks where gravitational instability still contributes alongside stellar feedback, with tentative evidence for a dynamically hotter warm ionised phase relative to cold gas (σ0, Hβ ∼ 1.7 × σ0, CO). We derive an average dark matter fraction ⟨ fDM ⟩ = 0.42±0.14, consistent with observations at similar redshifts, stellar masses, and surface densities. This work demonstrates the value of self-consistent, multi-wavelength analyses for probing disk settling physics in a relatively unexplored redshift range.
Versions
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BibTeX
@misc{barfety2026musealma,
title = {{MUSE-ALMA Haloes XV: Cold molecular, ionised, and stellar kinematics of HI-rich galaxies at z $\sim$ 0.5}},
author = {C. Barfety and N. M. Förster Schreiber and C. Péroux and L. J. Tacconi and J. Chen and S. Weng and V. Bollo and T. O'Beirne and M. Zwaan and R. Augustin and B. Casavecchia and L. Chemin and A. L . Danhaive and N. Guerra-Varas and V. Kulkarni and R. Potlia},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.10113},
eprint = {2610.10113},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.10113},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - MUSE-ALMA Haloes XV: Cold molecular, ionised, and stellar kinematics of HI-rich galaxies at z ∼ 0.5
AU - C. Barfety
AU - N. M. Förster Schreiber
AU - C. Péroux
AU - L. J. Tacconi
AU - J. Chen
AU - S. Weng
AU - V. Bollo
AU - T. O'Beirne
AU - M. Zwaan
AU - R. Augustin
AU - B. Casavecchia
AU - L. Chemin
AU - A. L . Danhaive
AU - N. Guerra-Varas
AU - V. Kulkarni
AU - R. Potlia
PY - 2026
DA - 2026/10/07
PB - arXiv
DO - 10.48550/arxiv.2610.10113
UR - https://arxiv.org/abs/2610.10113
AB - Spatially resolved galaxy kinematics are well studied at z ∼ 0 and z > 1, revealing that disks are common out to z ∼3−6, albeit with higher velocity dispersions. z ∼ 0.5 marks a key transition in the drivers of disk turbulence and baryonic-dark matter mass budgets, yet multi-tracer resolved kinematic studies remain rare beyond the local Universe. We exploit a unique dataset combining ALMA CO observations with MUSE ionised gas and stellar continuum data to study the resolved kinematics of six galaxies at 0.43 < z < 0.83, part of the MUSE-ALMA Haloes program, selected via their association with H I absorption systems and spanning stellar masses from log(M_⋆/M_⊙) = 10.1 − 11.8. Combining new ALMA/CO data with existing MUSE Hβ kinematics and HST morphologies, we classify galaxies using morpho-kinematic criteria. For rotating disks, we jointly model Hβ and CO(2-1) kinematics with DYSMALPY and compare results to theoretical predictions for pressure support, while pPXF is used to fit stellar absorption features. Four of the six galaxies are classified as disks, with two having known group members. These disks show elevated gas velocity dispersions relative to z ∼ 0 disks, consistent with interpolated trends between z ∼ 0 and z > 1. The results support marginally stable gaseous disks where gravitational instability still contributes alongside stellar feedback, with tentative evidence for a dynamically hotter warm ionised phase relative to cold gas (σ_0, Hβ ∼ 1.7 × σ_0, CO). We derive an average dark matter fraction ⟨ f_DM ⟩ = 0.42±0.14, consistent with observations at similar redshifts, stellar masses, and surface densities. This work demonstrates the value of self-consistent, multi-wavelength analyses for probing disk settling physics in a relatively unexplored redshift range.
ER -