---
OA_place: publisher
OA_type: diamond
_id: '19845'
abstract:
- lang: eng
  text: "Context. The recently launched James Webb Space Telescope (JWST) is opening
    new observing windows on the distant Universe. Among JWST’s instruments, the Mid
    Infrared Instrument (MIRI) offers the unique capability of imaging observations
    at wavelengths of λ > 5 μm. This enables unique access to the rest frame near-infrared
    (NIR, λ ≥ 1 μm) emission from galaxies at redshifts of z > 4 and the visual (λ ≳ 5000
    Å) rest frame for z > 9. We report here on the guaranteed time observations (GTO),
    from the MIRI European Consortium, of the Hubble Ultra Deep Field (HUDF), forming
    the MIRI Deep Imaging Survey (MIDIS), consisting of an on source integration time
    of ∼41 hours in the MIRI/F560W (5.6 μm) filter. The F560W filter was selected
    since it would produce the deepest data in terms of AB magnitudes in a given time.
    To our knowledge, this constitutes the longest single filter exposure obtained
    with JWST of an extragalactic field as of yet.\r\nAims. The HUDF is one of the
    most observed extragalactic fields, with extensive multi-wavelength coverage,
    where (before JWST) galaxies up to z ∼ 7 have been confirmed, and at z > 10 suggested,
    from HST photometry. We aim to characterise the galaxy population in HUDF at 5.6
    μm, enabling studies such as: the rest frame NIR morphologies for galaxies at
    z ≲ 4.6, probing mature stellar populations and emission lines in z > 6 sources,
    intrinsically red and dusty galaxies, and active galactic nuclei (AGNs) and their
    host galaxies at intermediate redshifts.\r\n\r\nMethods. We reduced the MIRI data
    using the official JWST pipeline, augmented by in-house custom scripts. We measured
    the noise characteristics of the resulting image. Galaxy photometry was obtained,
    and photometric redshifts were estimated for sources with available multi-wavelength
    photometry (and compared to spectroscopic redshifts when available).\r\n\r\nResults.
    Over the deepest part of our image, the 5σ point source limit is 28.65 mag AB
    (12.6 nJy), ∼0.35 mag better than predicted by the JWST exposure time calculator.
    We find ∼2500 sources, the overwhelming majority of which are distant galaxies,
    but we note that spurious sources likely remain at faint magnitudes due to imperfect
    cosmic ray rejection in the JWST pipeline. More than 500 galaxies with available
    spectroscopic redshifts, up to z ≈ 11, have been identified, the majority of which
    are at z < 6. More than 1000 galaxies have reliable photometric redshift estimates,
    of which ∼25 are at 6 < z < 12. The point spread function in the F560W filter
    has a full width at half maximum (FWHM) of ≈0.2″ (corresponding to 1.4 kpc at
    z = 4), allowing the NIR rest frame morphologies and stellar mass distributions
    to be resolved for z < 4.5. Moreover, > 100 objects with very red NIRCam vs MIRI
    (3.6–5.6 μm > 1 mag) colours have been found, suggestive of dusty or old stellar
    populations at high redshifts.\r\n\r\nConclusions. We conclude that MIDIS surpasses
    preflight expectations and that deep MIRI imaging has great potential to characterise
    the galaxy population from cosmic noon to dawn."
acknowledgement: 'We dedicate this paper to the memory of our deceased and much valued
  MIRI-EC team members Hans Ulrik Nørgaard-Nielsen and Olivier Le Fèvre, both of whom
  played a central role in defining the MIDIS project. This work is based on observations
  made with the NASA/ESA/CSA James Webb Space Telescope. The work presented is the
  effort of the entire MIRI team and the enthusiasm within the MIRI partnership is
  a significant factor in its success. The following National and International Funding
  Agencies funded and supported the MIRI development: NASA; ESA; Belgian Science Policy
  Office (BELSPO); Centre Nationale d’Etudes Spatiales (CNES); Danish National Space
  Centre; Deutsches Zentrum fur Luftund Raumfahrt (DLR); Enterprise Ireland; Ministerio
  De Economia y Competividad; Netherlands Research School for Astronomy (NOVA); Netherlands
  Organisation for Scientific Research (NWO); Science and Technology Facilities Council;
  Swiss Space Office; Swedish National Space Agency (SNSA); and UK Space Agency. MIRI
  drew on the scientific and technical expertise of the following organizations: Ames
  Research Center, USA; Airbus Defence and Space, UK; CEAIrfu, Saclay, France; Centre
  Spatial de Liège, Belgium; Consejo Superior de Investigaciones Cientficas, Spain;
  Carl Zeiss Optronics, Germany; Chalmers University of Technology, Sweden; Danish
  Space Research Institute, Denmark; Dublin Institute for Advanced Studies, Ireland;
  European Space Agency, Netherlands; ETCA, Belgium; ETH Zurich, Switzerland; Goddard
  Space Flight Center, USA; Institute d’Astrophysique Spatiale, France; Instituto
  Nacional de Técnica Aeroespacial,Spain; Institute for Astronomy, Edinburgh, UK;
  Jet Propulsion Laboratory, USA; Laboratoire d’Astrophysique de Marseille (LAM),
  France; Leiden University, Netherlands; Lockheed Advanced Technology Center (USA);
  NOVA Opt-IR group at Dwingeloo, Netherlands; Northrop Grumman, USA; Max Planck Institut
  f ür Astronomie (MPIA), Heidelberg, Germany; Laboratoire d’Etudes Spatiales et d’Instrumentation
  en Astrophysique (LESIA), France; Paul Scherrer Institut, Switzerland; Raytheon
  Vision Systems, USA; RUAG Aerospace, Switzerland; Rutherford Appleton Laboratory
  (RAL Space), UK; Space Telescope Science Institute, USA; Stockholm University, Sweden;
  Toegepast- Natuurwetenschappelijk Onderzoek (TNOTPD), Netherlands; UK Astronomy
  Technology Centre, UK; University College London, UK; University of Amsterdam, Netherlands;
  University of Arizona, USA; University of Cardiff, UK; University of Cologne, Germany;
  University of Ghent; University of Groningen, Netherlands; University of Leicester,
  UK; University of Leuven, Belgium; Utah State University, USA. Additional acknowledgements
  related to specific grants: G.Ö., J.M. and A.B. acknowledges funding from the Swedish
  National Space Administration (SNSA). P.G.P.-G. acknowledges support from grant
  PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033,
  FEDER Una manera de hacer Europa. This work was supported by research grants (VIL16599,VIL54489)
  from VILLUM FONDEN. L.C. and J.A.-M. acknowledge support by grant PIB2021-127718NB-100
  from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033
  and by “ERDF A way of making Europe”. M.A. acknowledges financial support from Comunidad
  de Madrid under Atracción de Talento grant 2020-T2/TIC-19971. J.P.P. and T.V.T.
  acknowledge financial support from the UK Science and Technology Facilities Council,
  and the UK Space Agency. A.A.-H. acknowledges financial support from grant PID2021-124665NB-I00
  funded by MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. E.I.
  and K.I.C. acknowledge funding from the Netherlands Research School for Astronomy
  (NOVA). K.I.C. acknowledges funding from the Dutch Research Council (NWO) through
  the award of the Vici Grant VI.C.212.036. RAM acknowledges support from the Swiss
  National Science Foundation (SNSF) through project grant 200020_207349. The paper
  uses JWST data from programme #1283, obtained from the Barbara Mikulski Archive
  for Space Telescopes at the Space Telescope Science Institute (STScI). For the purpose
  of open access, the authors have applied a Creative Commons Attribution (CC BY)
  licence to the Author Accepted Manuscript version arising from this submission.'
article_number: A57
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Göran
  full_name: Östlin, Göran
  last_name: Östlin
- first_name: Pablo G.
  full_name: Pérez-González, Pablo G.
  last_name: Pérez-González
- first_name: Jens
  full_name: Melinder, Jens
  last_name: Melinder
- first_name: Steven
  full_name: Gillman, Steven
  last_name: Gillman
- first_name: Edoardo
  full_name: Iani, Edoardo
  id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
  last_name: Iani
  orcid: 0000-0001-8386-3546
- first_name: Luca
  full_name: Costantin, Luca
  last_name: Costantin
- first_name: Leindert A.
  full_name: Boogaard, Leindert A.
  last_name: Boogaard
- first_name: Pierluigi
  full_name: Rinaldi, Pierluigi
  last_name: Rinaldi
- first_name: Luis
  full_name: Colina, Luis
  last_name: Colina
- first_name: Hans Ulrik
  full_name: Nørgaard-Nielsen, Hans Ulrik
  last_name: Nørgaard-Nielsen
- first_name: Daniel
  full_name: Dicken, Daniel
  last_name: Dicken
- first_name: Thomas R.
  full_name: Greve, Thomas R.
  last_name: Greve
- first_name: Gillian
  full_name: Wright, Gillian
  last_name: Wright
- first_name: Almudena
  full_name: Alonso-Herrero, Almudena
  last_name: Alonso-Herrero
- first_name: Javier
  full_name: Álvarez-Márquez, Javier
  last_name: Álvarez-Márquez
- first_name: Marianna
  full_name: Annunziatella, Marianna
  last_name: Annunziatella
- first_name: Arjan
  full_name: Bik, Arjan
  last_name: Bik
- first_name: Sarah E.I.
  full_name: Bosman, Sarah E.I.
  last_name: Bosman
- first_name: Karina I.
  full_name: Caputi, Karina I.
  last_name: Caputi
- first_name: Alejandro Crespo
  full_name: Gomez, Alejandro Crespo
  last_name: Gomez
- first_name: Andreas
  full_name: Eckart, Andreas
  last_name: Eckart
- first_name: Macarena
  full_name: Garcia-Marin, Macarena
  last_name: Garcia-Marin
- first_name: Jens
  full_name: Hjorth, Jens
  last_name: Hjorth
- first_name: Olivier
  full_name: Ilbert, Olivier
  last_name: Ilbert
- first_name: Iris
  full_name: Jermann, Iris
  last_name: Jermann
- first_name: Sarah
  full_name: Kendrew, Sarah
  last_name: Kendrew
- first_name: Alvaro
  full_name: Labiano, Alvaro
  last_name: Labiano
- first_name: Danial
  full_name: Langeroodi, Danial
  last_name: Langeroodi
- first_name: Olivier
  full_name: Le Fevre, Olivier
  last_name: Le Fevre
- first_name: Mattia
  full_name: Libralato, Mattia
  last_name: Libralato
- first_name: Romain A.
  full_name: Meyer, Romain A.
  last_name: Meyer
- first_name: Thibaud
  full_name: Moutard, Thibaud
  last_name: Moutard
- first_name: Florian
  full_name: Peissker, Florian
  last_name: Peissker
- first_name: John P.
  full_name: Pye, John P.
  last_name: Pye
- first_name: Tuomo V.
  full_name: Tikkanen, Tuomo V.
  last_name: Tikkanen
- first_name: Martin
  full_name: Topinka, Martin
  last_name: Topinka
- first_name: Fabian
  full_name: Walter, Fabian
  last_name: Walter
- first_name: Martin
  full_name: Ward, Martin
  last_name: Ward
- first_name: Paul
  full_name: Van Der Werf, Paul
  last_name: Van Der Werf
- first_name: Ewine F.
  full_name: Van Dishoeck, Ewine F.
  last_name: Van Dishoeck
- first_name: Manuel
  full_name: Güdel, Manuel
  last_name: Güdel
- first_name: Thomas
  full_name: Henning, Thomas
  last_name: Henning
- first_name: Pierre Olivier
  full_name: Lagage, Pierre Olivier
  last_name: Lagage
- first_name: Tom P.
  full_name: Ray, Tom P.
  last_name: Ray
- first_name: Bart
  full_name: Vandenbussche, Bart
  last_name: Vandenbussche
citation:
  ama: 'Östlin G, Pérez-González PG, Melinder J, et al. MIRI Deep Imaging Survey (MIDIS)
    of the Hubble Ultra Deep Field: Survey description and early results for the galaxy
    population detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. 2025;696.
    doi:<a href="https://doi.org/10.1051/0004-6361/202451723">10.1051/0004-6361/202451723</a>'
  apa: 'Östlin, G., Pérez-González, P. G., Melinder, J., Gillman, S., Iani, E., Costantin,
    L., … Vandenbussche, B. (2025). MIRI Deep Imaging Survey (MIDIS) of the Hubble
    Ultra Deep Field: Survey description and early results for the galaxy population
    detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202451723">https://doi.org/10.1051/0004-6361/202451723</a>'
  chicago: 'Östlin, Göran, Pablo G. Pérez-González, Jens Melinder, Steven Gillman,
    Edoardo Iani, Luca Costantin, Leindert A. Boogaard, et al. “MIRI Deep Imaging
    Survey (MIDIS) of the Hubble Ultra Deep Field: Survey Description and Early Results
    for the Galaxy Population Detected at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202451723">https://doi.org/10.1051/0004-6361/202451723</a>.'
  ieee: 'G. Östlin <i>et al.</i>, “MIRI Deep Imaging Survey (MIDIS) of the Hubble
    Ultra Deep Field: Survey description and early results for the galaxy population
    detected at 5.6 µm,” <i>Astronomy &#38; Astrophysics</i>, vol. 696. EDP Sciences,
    2025.'
  ista: 'Östlin G, Pérez-González PG, Melinder J, Gillman S, Iani E, Costantin L,
    Boogaard LA, Rinaldi P, Colina L, Nørgaard-Nielsen HU, Dicken D, Greve TR, Wright
    G, Alonso-Herrero A, Álvarez-Márquez J, Annunziatella M, Bik A, Bosman SEI, Caputi
    KI, Gomez AC, Eckart A, Garcia-Marin M, Hjorth J, Ilbert O, Jermann I, Kendrew
    S, Labiano A, Langeroodi D, Le Fevre O, Libralato M, Meyer RA, Moutard T, Peissker
    F, Pye JP, Tikkanen TV, Topinka M, Walter F, Ward M, Van Der Werf P, Van Dishoeck
    EF, Güdel M, Henning T, Lagage PO, Ray TP, Vandenbussche B. 2025. MIRI Deep Imaging
    Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results
    for the galaxy population detected at 5.6 µm. Astronomy &#38; Astrophysics. 696,
    A57.'
  mla: 'Östlin, Göran, et al. “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra
    Deep Field: Survey Description and Early Results for the Galaxy Population Detected
    at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>, vol. 696, A57, EDP Sciences,
    2025, doi:<a href="https://doi.org/10.1051/0004-6361/202451723">10.1051/0004-6361/202451723</a>.'
  short: G. Östlin, P.G. Pérez-González, J. Melinder, S. Gillman, E. Iani, L. Costantin,
    L.A. Boogaard, P. Rinaldi, L. Colina, H.U. Nørgaard-Nielsen, D. Dicken, T.R. Greve,
    G. Wright, A. Alonso-Herrero, J. Álvarez-Márquez, M. Annunziatella, A. Bik, S.E.I.
    Bosman, K.I. Caputi, A.C. Gomez, A. Eckart, M. Garcia-Marin, J. Hjorth, O. Ilbert,
    I. Jermann, S. Kendrew, A. Labiano, D. Langeroodi, O. Le Fevre, M. Libralato,
    R.A. Meyer, T. Moutard, F. Peissker, J.P. Pye, T.V. Tikkanen, M. Topinka, F. Walter,
    M. Ward, P. Van Der Werf, E.F. Van Dishoeck, M. Güdel, T. Henning, P.O. Lagage,
    T.P. Ray, B. Vandenbussche, Astronomy &#38; Astrophysics 696 (2025).
date_created: 2025-06-15T22:01:30Z
date_published: 2025-04-01T00:00:00Z
date_updated: 2026-02-16T12:10:36Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202451723
external_id:
  arxiv:
  - '2411.19686 '
  isi:
  - '001459780300005'
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language:
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license: https://creativecommons.org/licenses/by/4.0/
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description
  and early results for the galaxy population detected at 5.6 µm'
tmp:
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type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 696
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...