TY - JOUR
T1 - The ALMA-ALPAKA survey
T2 - I. High-resolution CO and [CI] kinematics of star-forming galaxies at z = 0.5- 3.5
AU - Rizzo, F.
AU - Roman-Oliveira, F.
AU - Fraternali, F.
AU - Frickmann, D.
AU - Valentino, F. M.
AU - Brammer, G.
AU - Zanella, A.
AU - Kokorev, V.
AU - Popping, G.
AU - Whitaker, K. E.
AU - Kohandel, M.
AU - Magdis, G. E.
AU - Di Mascolo, L.
AU - Ikeda, R.
AU - Jin, S.
AU - Toft, S.
N1 - Publisher Copyright:
© The Authors 2023.
PY - 2023
Y1 - 2023
N2 - Context. Spatially resolved studies of the kinematics of
galaxies provide crucial insights into their assembly and evolution,
enabling one to infer the properties of the dark matter halos, derive
the impact of feedback on the interstellar medium (ISM), as well as
measure and characterize the outflow motions. To date, most of the
kinematic studies at z = 0.5 − 3.5 have been obtained using emission lines tracing the warm, ionized gas (e.g., Hα,
[OII], and [OIII]). 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 into the cold gas
kinematics are therefore needed.
Aims. We present the Archival Large Program to Advance
Kinematic Analysis (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 Atacama Large
Millimeter Array (ALMA) public archive. With ≈147 h of total integration
time, ALPAKA assembles ∼0.25″ observations for 28 star-forming
galaxies, which is the largest sample with spatially resolved cold gas
kinematics as traced by either CO or [CI] at z ≳ 0.5, spanning 7
Gyr of cosmic history. A large fraction of ALPAKA galaxies (19 out of
28) lie in overdense regions (clusters, groups, and protoclusters).
Methods. By combining multiwavelength ground- and space-based ancillary data, we derived the stellar masses (M⋆)
and star-formation rates (SFRs) for the ALPAKA targets. We exploited
the ALMA data to infer the dynamical state of the ALPAKA galaxies and
derive their rotation curves and velocity dispersion profiles using 3DBAROLO.
Results. ALPAKA probes the massive (M⋆ ≳ 1010 M⊙), actively star-forming (SFR ≈ 10 − 3000 M⊙ yr−1) part of the population of galaxies at z ∼ 0.5 − 3.5.
Based on our kinematic classification, we find that 19 out of 28 ALPAKA
galaxies are rotating disks, two are interacting systems, while for the
remaining seven 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 35−9+11 km s−1. Despite the
bias of our sample toward galaxies hosting very energetic mechanisms,
the ALPAKA disks have high ratios of ordered-to-random motion (V/σ) with a median value of 9−2+7.
AB - Context. Spatially resolved studies of the kinematics of
galaxies provide crucial insights into their assembly and evolution,
enabling one to infer the properties of the dark matter halos, derive
the impact of feedback on the interstellar medium (ISM), as well as
measure and characterize the outflow motions. To date, most of the
kinematic studies at z = 0.5 − 3.5 have been obtained using emission lines tracing the warm, ionized gas (e.g., Hα,
[OII], and [OIII]). 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 into the cold gas
kinematics are therefore needed.
Aims. We present the Archival Large Program to Advance
Kinematic Analysis (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 Atacama Large
Millimeter Array (ALMA) public archive. With ≈147 h of total integration
time, ALPAKA assembles ∼0.25″ observations for 28 star-forming
galaxies, which is the largest sample with spatially resolved cold gas
kinematics as traced by either CO or [CI] at z ≳ 0.5, spanning 7
Gyr of cosmic history. A large fraction of ALPAKA galaxies (19 out of
28) lie in overdense regions (clusters, groups, and protoclusters).
Methods. By combining multiwavelength ground- and space-based ancillary data, we derived the stellar masses (M⋆)
and star-formation rates (SFRs) for the ALPAKA targets. We exploited
the ALMA data to infer the dynamical state of the ALPAKA galaxies and
derive their rotation curves and velocity dispersion profiles using 3DBAROLO.
Results. ALPAKA probes the massive (M⋆ ≳ 1010 M⊙), actively star-forming (SFR ≈ 10 − 3000 M⊙ yr−1) part of the population of galaxies at z ∼ 0.5 − 3.5.
Based on our kinematic classification, we find that 19 out of 28 ALPAKA
galaxies are rotating disks, two are interacting systems, while for the
remaining seven 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 35−9+11 km s−1. Despite the
bias of our sample toward galaxies hosting very energetic mechanisms,
the ALPAKA disks have high ratios of ordered-to-random motion (V/σ) with a median value of 9−2+7.
KW - Galaxies: evolution
KW - Galaxies: high-redshift
KW - Galaxies: ISM
KW - Galaxies: kinematics and dynamics
KW - Galaxies: photometry
KW - Galaxies: structure
U2 - 10.1051/0004-6361/202346444
DO - 10.1051/0004-6361/202346444
M3 - Journal article
AN - SCOPUS:85179131745
SN - 0004-6361
VL - 679
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A129
ER -