TY - JOUR
T1 - MIDIS
T2 - JWST/MIRI Reveals the Stellar Structure of ALMA-selected Galaxies in the Hubble Ultra Deep Field at Cosmic Noon
AU - Boogaard, Leindert A.
AU - Gillman, Steven
AU - Melinder, Jens
AU - Walter, Fabian
AU - Colina, Luis
AU - Östlin, Göran
AU - Caputi, Karina I.
AU - Iani, Edoardo
AU - Pérez-González, Pablo
AU - van der Werf, Paul
AU - Greve, Thomas R.
AU - Wright, Gillian
AU - Alonso-Herrero, Almudena
AU - Álvarez-Márquez, Javier
AU - Annunziatella, Marianna
AU - Bik, Arjan
AU - Bosman, Sarah
AU - Costantin, Luca
AU - Crespo Gómez, Alejandro
AU - Dicken, Dan
AU - Eckart, Andreas
AU - Hjorth, Jens
AU - Jermann, Iris
AU - Labiano, Alvaro
AU - Langeroodi, Danial
AU - Meyer, Romain A.
AU - Moutard, Thibaud
AU - Peißker, Florian
AU - Pye, John P.
AU - Rinaldi, Pierluigi
AU - Tikkanen, Tuomo V.
AU - Topinka, Martin
AU - Henning, Thomas
N1 - Publisher Copyright:
© 2024. The Author(s). Published by the American Astronomical Society.
PY - 2024
Y1 - 2024
N2 - We present deep James Webb Space Telescope (JWST)/Mid-Infrared
Instrument (MIRI) F560W observations of a flux-limited, Atacama Large
Millimeter/submillimeter Array (ALMA)-selected sample of 28 galaxies at z
= 0.5–3.7 in the Hubble Ultra Deep Field (HUDF). The data from the MIRI
Deep Imaging Survey (MIDIS) reveal the stellar structure of the HUDF
galaxies at rest-frame wavelengths of λ > 1 μm for the
first time. We revise the stellar mass estimates using new JWST
photometry and find good agreement with pre-JWST analyses; the few
discrepancies can be explained by blending issues in the earlier
lower-resolution Spitzer data. At z ∼ 2.5, the resolved rest-frame near-infrared (1.6 μm)
structure of the galaxies is significantly more smooth and centrally
concentrated than seen by the Hubble Space Telescope at rest-frame 450
nm (F160W), with effective radii of Re(F560W) = 1–5 kpc and Sérsic indices mostly close to an exponential (disk-like) profile (n ≈ 1), up to n ≈ 5 (excluding active galactic nuclei). We find an average size ratio of Re(F560W)/Re(F160W)
≈ 0.7 that decreases with stellar mass. The stellar structure of the
ALMA-selected galaxies is indistinguishable from a HUDF reference sample
of all galaxies with a MIRI flux density greater than 1 μJy. We
supplement our analysis with custom-made, position-dependent, empirical
point-spread function models for the F560W observations. The results
imply that a smoother stellar structure is in place in massive gas-rich,
star-forming galaxies at "Cosmic Noon," despite a more clumpy
rest-frame optical appearance, placing additional constraints on galaxy
formation simulations. As a next step, matched-resolution, resolved ALMA
observations will be crucial to further link the mass- and
light-weighted galaxy structures to the dusty interstellar medium.
AB - We present deep James Webb Space Telescope (JWST)/Mid-Infrared
Instrument (MIRI) F560W observations of a flux-limited, Atacama Large
Millimeter/submillimeter Array (ALMA)-selected sample of 28 galaxies at z
= 0.5–3.7 in the Hubble Ultra Deep Field (HUDF). The data from the MIRI
Deep Imaging Survey (MIDIS) reveal the stellar structure of the HUDF
galaxies at rest-frame wavelengths of λ > 1 μm for the
first time. We revise the stellar mass estimates using new JWST
photometry and find good agreement with pre-JWST analyses; the few
discrepancies can be explained by blending issues in the earlier
lower-resolution Spitzer data. At z ∼ 2.5, the resolved rest-frame near-infrared (1.6 μm)
structure of the galaxies is significantly more smooth and centrally
concentrated than seen by the Hubble Space Telescope at rest-frame 450
nm (F160W), with effective radii of Re(F560W) = 1–5 kpc and Sérsic indices mostly close to an exponential (disk-like) profile (n ≈ 1), up to n ≈ 5 (excluding active galactic nuclei). We find an average size ratio of Re(F560W)/Re(F160W)
≈ 0.7 that decreases with stellar mass. The stellar structure of the
ALMA-selected galaxies is indistinguishable from a HUDF reference sample
of all galaxies with a MIRI flux density greater than 1 μJy. We
supplement our analysis with custom-made, position-dependent, empirical
point-spread function models for the F560W observations. The results
imply that a smoother stellar structure is in place in massive gas-rich,
star-forming galaxies at "Cosmic Noon," despite a more clumpy
rest-frame optical appearance, placing additional constraints on galaxy
formation simulations. As a next step, matched-resolution, resolved ALMA
observations will be crucial to further link the mass- and
light-weighted galaxy structures to the dusty interstellar medium.
KW - Galaxy structure
KW - High-redshift galaxies
KW - Galaxy evolution
KW - James Webb Space Telescope
KW - Millimeter astronomy
U2 - 10.3847/1538-4357/ad43e5
DO - 10.3847/1538-4357/ad43e5
M3 - Journal article
AN - SCOPUS:85197392150
SN - 0004-637X
VL - 969
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 27
ER -