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 - 2024/7/1
Y1 - 2024/7/1
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 R e (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 R e (F560W)/R e (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 R e (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 R e (F560W)/R e (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.
UR - http://www.scopus.com/inward/record.url?scp=85197392150&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ad43e5
DO - 10.3847/1538-4357/ad43e5
M3 - Article
AN - SCOPUS:85197392150
SN - 0004-637X
VL - 969
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 27
ER -