J/A+A/686/A156 3 main-sequence galaxy systems datacubes (Devereaux+, 2024)
The ALMA-ALPINE CII survey: The sub-kpc morphology of three main sequence
galaxy systems at z∼4.5 revealed by ALMA.
Devereaux T., Cassata P., Ibar E., Accard C., Guillaume C., Bethermin M.,
Dessauges-Zavadsky M., Faisst A., Jones G.C., Zanella A., Bardelli S.,
Boquien M., D'Onghia E., Giavalisco M., Ginolfi M., Gobat R., Hayward C.C.,
Koekemoer A.M., Lemaux B., Magdis G., Mendez-Hernandez H., Molina J.,
Pozzi F., Romano M., Tasca L., Vergani D., Zamorani G., Zucca E.
<Astron. Astrophys. 686, A156 (2024)>
=2024A&A...686A.156D 2024A&A...686A.156D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Millimetric/submm sources
Keywords: galaxies: evolution - galaxies: formation - galaxies: high-redshift -
galaxies: ISM - galaxies: star formation - submillimeter: galaxies
Abstract:
Going from a redshift of 6 down to nearly 4, galaxies grow rapidly
from low-mass galaxies towards the more mature types of massive
galaxies seen at cosmic noon. Growth via gas accretion and mergers
undoubtedly shape this evolution, however, there is considerable
uncertainty at present over the contribution of each of these
processes to the overall evolution of galaxies. Furthermore, previous
characterisations of the morphology of galaxies in the molecular gas
phase have been limited by the coarse resolution of earlier
observations.
In this work, we utilise new high-resolution ALMA [CII] observations
to analyse three main sequence (MS) galaxy systems at a redshift of
z∼4.5 and at resolutions of up to 0.15". This approach enables us to
investigate the morphology and kinematics on a kpc scale and
understand the processes at play as well as the classifications of
galaxies at high resolution. Thanks to this unique window, we are able
to gain insights into the molecular gas of MS galaxies undergoing mass
assembly in the early Universe
We used intensity and velocity maps, position-velocity diagrams, and
radial profiles of [CII] in combination with dust continuum maps to
analyse the morphology and kinematics of the three systems.
In general, we find that the high-resolution ALMA data reveal more
complex morpho-kinematic properties. For one galaxy in our sample, we
identified interaction-induced clumps, demonstrating the profound
effect that mergers have on the molecular gas in galaxies, which is
consistent with what has been suggested by recent simulations. One
galaxy that was previously classified as dispersion-dominated turned
out to show two bright [CII] emission regions, which could either be
classified as merging galaxies or massive star-forming regions within
the galaxy itself. The high-resolution data for the other dispersion
dominated object also revealed clumps of [CII] that had not been
identified previously. Within the sample, we might also detect
star-formation powered outflows (or outflows from active galactic
nuclei) that appear to be fuelling diffuse gas regions and enriching
the circumgalactic medium. The new high-resolution ALMA data we
present in this paper reveal that the galaxies in our sample are much
more complex than they previously appeared in the low-resolution
ALPINE data. In particular, we find evidence of merger induced clumps
in the galaxy DC8187, along with signs of merging components for the
other two objects. This may be evidence that the number of mergers at
high redshift are significantly underestimated at present.
Description:
In this work, we utilise new high-resolution ALMA [CII] observations
to analyse three main sequence (MS) galaxy systems at a redshift of
z∼4.5 and at resolutions of up to 0.15". This approach enables us to
investigate the morphology and kinematics on a kpc scale and
understand the processes at play as well as the classifications of
galaxies at high resolution.
Data cubes at high resolution for the [CII] line for 3 main sequence
galaxies at redshift ∼4.5.
Objects:
-------------------------------------------------------
RA (2000) DE Designation(s)
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10 00 02.719 +02 37 39.990 DC8737 = COSMOS2015 873756
10 01 12.495 +02 18 52.384 VC8326 = VUDS 5101218326
10 01 54.854 +02 32 31.431 DC8187 = COSMOS2015 818760
-------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 146 3 List of fits datacubes
fits/* . 3 Individual fits datacubes
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See also:
J/A+A/643/A2 : ALPINE DR1 merged catalog (Bethermin+, 2020)
J/A+A/643/A4 : ALPINE-ALMA [CII] survey. IR luminosity (Fudamoto+, 2020)
J/A+A/643/A6 : Lyα-[CII] velocity offsets in MS galaxies (Cassata+, 2020
J/A+A/664/A73 : Star-forming galaxies at 4.5 < z < 6.2 (Burgarella+, 2022)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 30 I3 --- Nz Number of pixels along Z-axis
32- 57 A26 "datime" Obs.date Observation date
59- 69 E11.6 Hz bFREQ Lower value of frequency interval
71- 81 E11.6 Hz BFREQ Upper value of frequency interval
83- 92 E10.5 Hz dFREQ Frequency resolution
94- 99 I6 Kibyte size Size of FITS file
101-111 A11 --- FileName Name of FITS file, in subdirectory fits
113-146 A34 --- Title Title of the FITS file
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Acknowledgements:
Toby Devereaux, toby.devereaux(at)studenti.unipd.it
(End) Patricia Vannier [CDS] 03-Jun-2024