MIRI spectrophotometry of GN-z11: Detection and nature of an optical red continuum component

¹ Space Telescope Science Institute (STScI) 3700 San martin Drive Baltimore MD 21218, USA
² Centro de Astrobiología (CAB), CSIC-INTA Ctra. de Ajalvir km 4 Torrejón de Ardoz E-28850 Madrid, Spain
³ European Space Agency, Space Telescope Science Institute Baltimore MD, USA
⁴ Centro de Astrobiología (CAB), CSIC-INTA Camino Viejo del Castillo s/n 28692 Villanueva de la Cañada Madrid, Spain
⁵ Department of Astronomy, Stockholm University, Oscar Klein Centre, AlbaNova University Centre 106 91 Stockholm, Sweden
⁶ Institute for Theoretical Physics, Heidelberg University Philosophenweg 12 69120 Heidelberg, Germany
⁷ Max-Planck-Institut für Astronomie Königstuhl 17 69117 Heidelberg, Germany
⁸ Department of Physics, University of Oxford, Denys Wilkinson Building Keble Road Oxford OX13RH, UK
⁹ Telespazio UK for the European Space Agency, ESAC Camino Bajo del Castillo s/n 28692 Villanueva de la Cañada, Spain
¹⁰ DARK, Niels Bohr Institute, University of Copenhagen Jagtvej 128 2200 Copenhagen, Denmark
¹¹ Steward Observatory, University of Arizona 933 North Cherry Avenue Tucson AZ 85721, USA
¹² Cosmic Dawn Center, DTU Space, Technical University of Denmark Elektrovej 327 2800 Kgs. Lyngby, Denmark
¹³ Cosmic Dawn Centre Copenhagen, Denmark
¹⁴ University of the Pacific Stockton CA 90340, USA
¹⁵ Leiden Observatory, Leiden University PO Box 9513 NL-2300 RA Leiden, The Netherlands
¹⁶ Department of Astronomy, The University of Texas at Austin Austin TX, USA
¹⁷ MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. Cambridge MA 02139, USA

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Received: 11 August 2025
Accepted: 22 November 2025

Abstract

We present new MIRI F560W, F770W, and F1000W imaging of the galaxy GN-z11 at a redshift of 10.603. We report a significant detection (14σ) in the F560W and F770W images, and a marginal detection (3.2σ) in the F1000W filter. The new MIRI observations cover the optical-red spectral range and significantly extend previous NIRCam wavelength coverage from rest-frame 0.38 μm up to 0.86 μm. In this work, we analyse the spectral energy distribution (SED) combining this new MIRI imaging data with archival NIRSpec/Prism and MRS spectroscopy, and NIRCam imaging, i.e. covering the rest-frame 0.12–0.86 μm. New constraints such as the equivalent widths of the strong optical lines ([O III]λ5008, Hβ and Hα) and the continuum emission at rest-frame 0.48 μm, 0.66 μm, and 0.86 μm, free of emission line contributions, are presented. The continuum emission shows a flat energy distribution, in f_ν, up to 0.5 μm, compatible with the presence of a mixed stellar population of young (4 ± 1 Myr) and mature (63 ± 23 Myr) stars that also account for the [O III], Hβ, and Hα emission lines. The continuum at rest-frame 0.66 μm shows a 36 ± 3% flux excess above the predicted flux for a mixed stellar population, pointing to the presence of an additional source contributing at these wavelengths. This excess increases to 91 ± 28% at rest-frame 0.86 μm, although with a large uncertainty due to the marginal detection in the F1000W filter. We consider that hot dust emission in the dusty torus around a type 2 active galactic nucleus (AGN) could be responsible for the observed excess. Alternatively, this excess could be due to hot dust emission or a photoluminiscence dust process (Extended Red Emission, ERE) under the extreme UV radiation field, as is observed in local metal-poor galaxies and in young compact starbursts. The presence of a type 1 AGN is not supported by the observed SED as the hot dust emission in luminous high-z quasi-stellar objects (QSOs) contributes at wavelengths above rest-frame 1 μm, and an additional ad hoc red source would be required to explain the observed flux excess at 0.66 and 0.86 μm. Additional deep MIRI imaging covering the rest-frame near-IR is needed to confirm the flux detection at 10 μm, and to discriminate between the different hot dust emission in the extreme starburst and AGN scenarios.