The ALMA-ALPAKA survey I: high-resolution CO and [CI] kinematics of star-forming galaxies at z = 0.5-3.5
A&A 679, A129 (2023) Spatially-resolved studies of the kinematics of galaxies provide crucial insights into their assembly and evolution, enabling to infer the properties of the dark matter halos, derive the impact of feedback on the ISM, characterize the outflow motions. To date, most of the ki...
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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Journal Article |
| Language: | English |
| Published: |
13-08-2023
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| Subjects: | |
| Online Access: | Get full text |
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| Summary: | A&A 679, A129 (2023) Spatially-resolved studies of the kinematics of galaxies provide crucial
insights into their assembly and evolution, enabling to infer the properties of
the dark matter halos, derive the impact of feedback on the ISM, characterize
the outflow motions. To date, most of the kinematic studies at z=0.5-3.5 were
obtained using emission lines tracing the warm, ionized gas. However, whether
these provide an exhaustive or only a partial view of the dynamics of galaxies
and of the properties of the ISM is still debated. Complementary insights on
the cold gas kinematics are therefore needed. We present ALPAKA, a project
aimed at gathering high-resolution observations of CO and [CI] emission lines
of star-forming galaxies at z=0.5-3.5 from the ALMA public archive. With 147
hours of total integration time, ALPAKA assembles ~0.25'' observations for 28
star-forming galaxies, the largest sample with spatially-resolved cold gas
kinematics as traced by either CO or [CI] at z>0.5. By combining
multi-wavelength ancillary data, we derive the stellar masses ($M_{\star}$) and
star-formation rates (SFR) for our targets, finding values of $M_{\star}\gtrsim
10^{10}$ M$_{\odot}$ and SFR of 10-3000 M$_{\odot}$/yr. A large fraction of
ALPAKA galaxies (19/28) lie in overdense regions (clusters, groups, and
protoclusters). We exploit the ALMA data to infer their dynamical state and we
find that 19/28 ALPAKA galaxies are rotating disks, 2 are interacting systems,
while for the remaining 7 sources the classification is uncertain. The disks
have velocity dispersion values that are typically larger in the innermost
regions than in the outskirts, with a median value for the entire disk sample
of 35$^{+11}_{-9}$ km/s. Despite the bias of our sample towards galaxies
hosting very energetic mechanisms, the ALPAKA disks have high ratios of
ordered-to-random motion ($V/\sigma$) with a median value of 9$^{+7}_{-2}$. |
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| DOI: | 10.48550/arxiv.2303.16227 |