---
OA_type: closed access
_id: '20975'
abstract:
- lang: eng
text: Galaxy clusters are the most massive, gravitationally bound structures in
the Universe. They emerged through hierarchical structure formation of large-scale
dark matter and baryon overdensities. Early galaxy ‘proto-clusters’ are believed
to have substantially contributed to the cosmic star-formation rate density and
served as ‘hotspots’ for the reionization of the intergalactic medium. Our understanding
of the formation of these structures at the earliest cosmic epochs is, however,
limited to sparse observations of their galaxy members or is based on phenomenological
models and cosmological simulations. Here we report the detection of a large and
coherent structure of neutral atomic hydrogen gas (H i) extending from a galaxy
proto-cluster at redshift z = 5.4, one billion years after the Big Bang. The presence
of this H i gas is revealed by strong damped Lyman-α absorption features observed
in several background-galaxy spectra. Although the sight lines overall probe a
large range in H i column densities, NHI = 1020 cm−2 to 1023.5 cm−2, they are
similar across nearby sight lines, demonstrating that they probe the same dense
neutral gas. This observation of a dense large-scale overdensity of cold neutral
gas challenges current cosmological simulations and has strong implications for
the reionization topology of the Universe.
acknowledgement: This work has received funding from the Swiss State Secretariat for
Education, Research and Innovation (Contract No. MB22.00072). The Cosmic Dawn Center
(DAWN) is funded by the Danish National Research Foundation (Grant No. DNRF140).
The data products presented herein were retrieved from the DJA, which is an initiative
of the Cosmic Dawn Center. This work is based on observations made with the NASA/ESA/CSA
JWST. The data were obtained from MAST at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. J.S.B. acknowledges support from
the Simons Collaboration on Learning the Universe. J.S.B.’s simulations used resources
from the Cambridge Service for Data Driven Discovery operated by the University
of Cambridge Research Computing Service (www.csd3.cam.ac.uk), provided by Dell EMC
and Intel using tier 2 funding from the Engineering and Physical Sciences Research
Council (Capital Grant No. EP/P020259/1). K.F. gratefully acknowledges support from
the National Science Foundation (Award No. 2006550). M.J.H. is fellow of the Knut
& Alice Wallenberg Foundation. D.S. acknowledges support from the Science and Technology
Facilities Council. U.S.K. was partially funded by the Summer Undergraduate Research
Fellowships programme at Caltech.
article_processing_charge: No
article_type: original
author:
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: Jake S.
full_name: Bennett, Jake S.
last_name: Bennett
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Albert
full_name: Sneppen, Albert
last_name: Sneppen
- first_name: Douglas
full_name: Rennehan, Douglas
last_name: Rennehan
- first_name: Clara L.
full_name: Pollock, Clara L.
last_name: Pollock
- first_name: Joris
full_name: Witstok, Joris
last_name: Witstok
- first_name: Renske
full_name: Smit, Renske
last_name: Smit
- first_name: Simone
full_name: Vejlgaard, Simone
last_name: Vejlgaard
- first_name: Chamilla
full_name: Terp, Chamilla
last_name: Terp
- first_name: Umran S.
full_name: Koca, Umran S.
last_name: Koca
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Kristian
full_name: Finlator, Kristian
last_name: Finlator
- first_name: Matthew J.
full_name: Hayes, Matthew J.
last_name: Hayes
- first_name: Debora
full_name: Sijacki, Debora
last_name: Sijacki
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Francesco
full_name: Valentino, Francesco
last_name: Valentino
- first_name: Nial R.
full_name: Tanvir, Nial R.
last_name: Tanvir
- first_name: Páll
full_name: Jakobsson, Páll
last_name: Jakobsson
- first_name: Peter
full_name: Laursen, Peter
last_name: Laursen
- first_name: Darach J.
full_name: Watson, Darach J.
last_name: Watson
- first_name: Romeel
full_name: Davé, Romeel
last_name: Davé
- first_name: Laura C.
full_name: Keating, Laura C.
last_name: Keating
- first_name: Alba
full_name: Covelo-Paz, Alba
last_name: Covelo-Paz
citation:
ama: Heintz KE, Bennett JS, Oesch PA, et al. A dense web of neutral gas in a galaxy
proto-cluster post-reionization. Nature Astronomy. 2026. doi:10.1038/s41550-025-02745-x
apa: Heintz, K. E., Bennett, J. S., Oesch, P. A., Sneppen, A., Rennehan, D., Pollock,
C. L., … Covelo-Paz, A. (2026). A dense web of neutral gas in a galaxy proto-cluster
post-reionization. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-025-02745-x
chicago: Heintz, Kasper E., Jake S. Bennett, Pascal A. Oesch, Albert Sneppen, Douglas
Rennehan, Clara L. Pollock, Joris Witstok, et al. “A Dense Web of Neutral Gas
in a Galaxy Proto-Cluster Post-Reionization.” Nature Astronomy. Springer
Nature, 2026. https://doi.org/10.1038/s41550-025-02745-x.
ieee: K. E. Heintz et al., “A dense web of neutral gas in a galaxy proto-cluster
post-reionization,” Nature Astronomy. Springer Nature, 2026.
ista: Heintz KE, Bennett JS, Oesch PA, Sneppen A, Rennehan D, Pollock CL, Witstok
J, Smit R, Vejlgaard S, Terp C, Koca US, Brammer GB, Finlator K, Hayes MJ, Sijacki
D, Naidu RP, Matthee JJ, Valentino F, Tanvir NR, Jakobsson P, Laursen P, Watson
DJ, Davé R, Keating LC, Covelo-Paz A. 2026. A dense web of neutral gas in a galaxy
proto-cluster post-reionization. Nature Astronomy.
mla: Heintz, Kasper E., et al. “A Dense Web of Neutral Gas in a Galaxy Proto-Cluster
Post-Reionization.” Nature Astronomy, Springer Nature, 2026, doi:10.1038/s41550-025-02745-x.
short: K.E. Heintz, J.S. Bennett, P.A. Oesch, A. Sneppen, D. Rennehan, C.L. Pollock,
J. Witstok, R. Smit, S. Vejlgaard, C. Terp, U.S. Koca, G.B. Brammer, K. Finlator,
M.J. Hayes, D. Sijacki, R.P. Naidu, J.J. Matthee, F. Valentino, N.R. Tanvir, P.
Jakobsson, P. Laursen, D.J. Watson, R. Davé, L.C. Keating, A. Covelo-Paz, Nature
Astronomy (2026).
date_created: 2026-01-11T23:01:34Z
date_published: 2026-01-02T00:00:00Z
date_updated: 2026-01-12T09:53:21Z
day: '02'
department:
- _id: JoMa
doi: 10.1038/s41550-025-02745-x
language:
- iso: eng
month: '01'
oa_version: None
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: A dense web of neutral gas in a galaxy proto-cluster post-reionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21038'
abstract:
- lang: eng
text: "Little Red Dots (LRDs) are compact sources at z > 5 discovered through James
Webb Space Telescope spectroscopy. Their spectra exhibit broad Balmer emission
lines (>~1000 km s^−1), alongside absorption features and a pronounced Balmer
break – evidence for a dense, neutral hydrogen medium, in which the n = 2 state
is significantly populated. When interpreted as arising\r\nfrom active galactic
nucleus broad-line regions, inferred black hole masses from local scaling relations
exceed expectations given their stellar masses, challenging models of early black
hole–galaxy co-evolution. However, radiative transfer effects in dense media may
also impact the formation of hydrogen emission lines. We model three scattering
processes shaping hydrogen\r\nline profiles: resonance scattering by hydrogen
in the n = 2 state, Raman scattering of ultraviolet (UV) radiation by ground-state
hydrogen, and Thomson scattering by free electrons. Using 3D Monte Carlo radiative
transfer simulations, we examine their imprint on line shapes and ratios. Resonance
scattering produces strong deviations from Case B flux ratios, clear differences\r\nbetween
Hα and Hβ, and encodes gas kinematics in line profiles but cannot broaden Hβ due
to conversion to Paα. While Raman scattering can yield broad wings, scattering
of the UV continuum is disfavoured given the absence of strong full width at half-maximum
variations across transitions. Raman scattering of higher Lyman-series emission
can produce Hα/Hβ wing\r\nwidth ratios of >~1.28, agreeing with observations.
Thomson scattering can reproduce the observed >~ 1000 km s^−1 wings under plausible
conditions – e.g. Te ∼ 10^4 K and Ne ∼ 10^24 cm^−2 – and lead to black hole mass
overestimates by factors 10. Our results provide a framework for interpreting
hydrogen lines in LRDs and similar systems."
acknowledgement: "The authorsthank the anonymousreferee for constructive comments,
which improved the clarity of this paper. SJC acknowledges support from the ERC
synergy grant 101166930 – RECAP. MG thanks the Max Planck Society for support through
the Max Planck Research Group, and the European Union forsupport through ERC-2024-STG
101165038 (ReMMU). JM acknowledges funding by the European Union (ERC, AGENTS, 101076224).
CAM acknowledges support\r\nby the European Union ERC grant RISES (101163035), Carlsberg
Foundation (CF22-1322), and VILLUM FONDEN (37459). Computations were performed on
HPC systems Freya and Orion at the Max Planck Computing and Data Facility."
article_number: staf2131
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Seok Jun
full_name: Chang, Seok Jun
last_name: Chang
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Charlotte
full_name: Mason, Charlotte
last_name: Mason
citation:
ama: Chang SJ, Gronke M, Matthee JJ, Mason C. Impact of resonance, Raman, and Thomson
scattering on hydrogen line formation in Little Red Dots. Monthly Notices of
the Royal Astronomical Society. 2026;545(4). doi:10.1093/mnras/staf2131
apa: Chang, S. J., Gronke, M., Matthee, J. J., & Mason, C. (2026). Impact of
resonance, Raman, and Thomson scattering on hydrogen line formation in Little
Red Dots. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/staf2131
chicago: Chang, Seok Jun, Max Gronke, Jorryt J Matthee, and Charlotte Mason. “Impact
of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little
Red Dots.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2026. https://doi.org/10.1093/mnras/staf2131.
ieee: S. J. Chang, M. Gronke, J. J. Matthee, and C. Mason, “Impact of resonance,
Raman, and Thomson scattering on hydrogen line formation in Little Red Dots,”
Monthly Notices of the Royal Astronomical Society, vol. 545, no. 4. Oxford
University Press, 2026.
ista: Chang SJ, Gronke M, Matthee JJ, Mason C. 2026. Impact of resonance, Raman,
and Thomson scattering on hydrogen line formation in Little Red Dots. Monthly
Notices of the Royal Astronomical Society. 545(4), staf2131.
mla: Chang, Seok Jun, et al. “Impact of Resonance, Raman, and Thomson Scattering
on Hydrogen Line Formation in Little Red Dots.” Monthly Notices of the Royal
Astronomical Society, vol. 545, no. 4, staf2131, Oxford University Press,
2026, doi:10.1093/mnras/staf2131.
short: S.J. Chang, M. Gronke, J.J. Matthee, C. Mason, Monthly Notices of the Royal
Astronomical Society 545 (2026).
date_created: 2026-01-25T23:01:39Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-02-12T12:56:33Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1093/mnras/staf2131
external_id:
arxiv:
- '2508.08768'
file:
- access_level: open_access
checksum: 52ba7d7b5b80af0c50f57e4c2acc3930
content_type: application/pdf
creator: dernst
date_created: 2026-02-12T12:44:33Z
date_updated: 2026-02-12T12:44:33Z
file_id: '21220'
file_name: 2026_MonthNoticesRAS_Chang.pdf
file_size: 5600366
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intvolume: ' 545'
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language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Impact of resonance, Raman, and Thomson scattering on hydrogen line formation
in Little Red Dots
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 545
year: '2026'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21045'
abstract:
- lang: eng
text: 'The abundant population of little red dots (LRDs), compact objects with red
UV to optical colors and broad Balmer lines at high redshift, is revealing new
insights into the properties of early active galactic nuclei (AGN). Perhaps the
most surprising features of this population are the presence of Balmer absorption
and ubiquitous strong Balmer breaks. Recent models link these features to an active
supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We
present a stringent test of such models using VLT/MUSE observations of A2744-45924,
the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744
lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula
(h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc.
The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα)
compared to Lyα nebulae typically observed around quasars of similar luminosity.
We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial
shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and
Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered
by star formation. In the environment of A2744-45924, we identified four extended
Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations
based on Hα emission, and show no evidence for radiation from A2744-45924 affecting
its surroundings. The lack of strong, compact, and broad Lyα and the absence of
a luminous extended halo, suggest that the UV AGN light is obscured by dense gas
cloaking the SMBH with a covering factor close to unity.'
acknowledgement: 'We thank the anonymous referee for constructive and useful comments.
We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected
at the European Organisation for Astronomical Research in the Southern Hemisphere
under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224).
Views and opinions expressed are however those of the author(s) only and do not
necessarily reflect those of the European Union or the European Research Council.
Neither the European Union nor the granting authority can be held responsible for
them. We acknowledge funding from JWST program GO-3516. This work is based in part
on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data
were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations
are associated with program #3516. MG thanks the Max Planck Society for support
through the MPRG. FDE acknowledges support by the Science and Technology Facilities
Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI
Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant
SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.'
article_number: A147
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for
an extremely bright little red dot. Indications of enshrouded supermassive black
hole growth. Astronomy and Astrophysics. 2026;705. doi:10.1051/0004-6361/202555596
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke,
M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth. Astronomy
and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555596
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya
Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo
for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive
Black Hole Growth.” Astronomy and Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202555596.
ieee: A. Torralba Torregrosa et al., “A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth,” Astronomy
and Astrophysics, vol. 705. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia
S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie
R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely
bright little red dot. Indications of enshrouded supermassive black hole growth.
Astronomy and Astrophysics. 705, A147.
mla: Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright
Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” Astronomy
and Astrophysics, vol. 705, A147, EDP Sciences, 2026, doi:10.1051/0004-6361/202555596.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke,
S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa,
R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy and Astrophysics
705 (2026).
corr_author: '1'
date_created: 2026-01-25T23:01:41Z
date_published: 2026-01-14T00:00:00Z
date_updated: 2026-02-16T07:46:53Z
day: '14'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202555596
external_id:
arxiv:
- '2505.09542'
file:
- access_level: open_access
checksum: 3782e03bc0843438aae8487f6af779c5
content_type: application/pdf
creator: dernst
date_created: 2026-02-16T07:35:03Z
date_updated: 2026-02-16T07:35:03Z
file_id: '21224'
file_name: 2026_AstronomyAstrophysics_Torralba.pdf
file_size: 2259914
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success: 1
file_date_updated: 2026-02-16T07:35:03Z
has_accepted_license: '1'
intvolume: ' 705'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy and Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded
supermassive black hole growth
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 705
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21341'
abstract:
- lang: eng
text: We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation
between the stellar mass, metallicity, and star formation rate (SFR) known as
the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800
[O III] selected galaxies from deep NIRCam grism surveys, we present our stacked
measurements of direct-Te metallicities, which we used to test recent strong-line
metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for
M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However,
there are significant inconsistencies between observations and hydrodynamical
simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations,
which cannot be attributed to selection effects. With simple models, we show that
the effect of an [O III] flux-limited sample on the observed shape of the MZR
is strongly dependent on the FMR. If the FMR is similar to the one in the local
Universe, the intrinsic high-redshift MZR should be even flatter than is observed.
In turn, a 3D relation where SFR correlates positively with metallicity at fixed
mass would imply an intrinsically steeper MZR. Our measurements indicate that
metallicity variations at fixed mass show little dependence on the SFR, suggesting
a flat intrinsic MZR. This could indicate that the low-mass galaxies at these
redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass
galaxies. However, being limited by our stacking analysis, we are yet to probe
the scatter in the MZR and its dependence on SFR. Large carefully selected samples
of galaxies with robust metallicity measurements can put tight constraints on
the high-redshift FMR and help us to understand the interplay between gas flows,
star formation, and feedback in early galaxies.
acknowledgement: 'We thank the anonymous referee for the insightful comments that
helped improving this paper. This work is based on observations made with the NASA/ESA/CSA
James Webb Space Telescope. The data were obtained from the Mikulski Archive for
Space Telescopes at the Space Telescope Science Institute, which is operated by
the Associations of Universities for Research in Astronomy, Inc., under NASA contract
NAS 5-03127 for JWST. These observations were taken under programmes # 1243, # 1933
and # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions
expressed are however those of the author(s) only and do not necessarily reflect
those of the European Union or the European Research Council. Neither the European
Union nor the granting authority can be held responsible for them. GK acknowledges
support from the Foundation MERAC. APV acknowledge support from the Sussex Astronomy
Centre STFC Consolidated Grant (ST/X001040/1).'
article_number: A165
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Aswin P.
full_name: Vijayan, Aswin P.
last_name: Vijayan
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: A. Lola
full_name: Danhaive, A. Lola
last_name: Danhaive
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: David
full_name: Sobral, David
last_name: Sobral
citation:
ama: Kotiwale G, Matthee JJ, Kashino D, et al. Rapid, out-of-equilibrium metal enrichment
indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy.
Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202556597
apa: Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa,
A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment
indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556597
chicago: Kotiwale, Gauri, Jorryt J Matthee, Daichi Kashino, Aswin P. Vijayan, Alberto
Torralba Torregrosa, Claudia Di Cesare, Edoardo Iani, et al. “Rapid, out-of-Equilibrium
Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam
Grism Spectroscopy.” Astronomy & Astrophysics. EDP Sciences, 2026.
https://doi.org/10.1051/0004-6361/202556597.
ieee: G. Kotiwale et al., “Rapid, out-of-equilibrium metal enrichment indicated
by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,”
Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.
ista: Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare
C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive
AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026.
Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity
relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy & Astrophysics.
706, A165.
mla: Kotiwale, Gauri, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated
by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.”
Astronomy & Astrophysics, vol. 706, A165, EDP Sciences, 2026, doi:10.1051/0004-6361/202556597.
short: G. Kotiwale, J.J. Matthee, D. Kashino, A.P. Vijayan, A. Torralba Torregrosa,
C. Di Cesare, E. Iani, R. Bordoloi, J. Leja, M.V. Maseda, S. Tacchella, I. Shivaei,
K.E. Heintz, A.L. Danhaive, S. Mascia, I. Kramarenko, B. Navarrete, R. Mackenzie,
R.P. Naidu, D. Sobral, Astronomy & Astrophysics 706 (2026).
corr_author: '1'
date_created: 2026-02-22T23:01:35Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-02-24T07:49:42Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202556597
external_id:
arxiv:
- '2510.19959'
file:
- access_level: open_access
checksum: 6f5849d29ad43bee32f90152f6fc0294
content_type: application/pdf
creator: dernst
date_created: 2026-02-24T07:46:47Z
date_updated: 2026-02-24T07:46:47Z
file_id: '21355'
file_name: 2026_AstronomyAstrophysics_Kotiwale.pdf
file_size: 6531719
relation: main_file
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file_date_updated: 2026-02-24T07:46:47Z
has_accepted_license: '1'
intvolume: ' 706'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
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: Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity
relation at z ∼ 6 from NIRCam grism spectroscopy
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 706
year: '2026'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21342'
abstract:
- lang: eng
text: "JWST has revealed a stunning population of bright galaxies at surprisingly
early epochs, z > 10,\r\nwhere few such sources were expected. Here we present
the most distant example of this class yet – MoM-z14, a luminous (MUV = −20.2)
source in the COSMOS legacy field at zspec = 14.44+0.02−0.02 that expands the
observational frontier to a mere 280 million years after the Big Bang. The redshift
is confirmed with NIRSpec/prism spectroscopy through a sharp Lyman-α break and
≈ 3σ detections of five rest-UV emission lines. The number density of bright zspec
≈ 14 − 15 sources implied by our “Mirage or Miracle” survey spanning ≈ 350 arcmin2
is > 100× larger (182+329 −105×) than pre-JWST consensus models. The high EWs
of UV lines (≈15−35˚A) signal a rising star-formation history, with a ≈10× increase
in the last 5 Myr (SFR5Myr/SFR50Myr = 9.9 +3.0 −5.8). The source is extremely
compact (circularized re = 74+15\r\n−12 pc), and yet elongated (b/a = 0.25+0.11−0.06),
suggesting an AGN is not the dominant source of UV light. The steep UV slope (β
= −2.5 +0.2 −0.2) implies negligible dust attenuation\r\nand a young stellar population.
The absence of a strong damping wing provides tentative evidence that the immediate
surroundings of MoM-z14 may be partially ionized at a redshift where virtually
every reionization model predicts a ≈ 100% neutral fraction. The nitrogen emission
and highly supersolar [N/C]> 1 hint at an abundance pattern similar to local globular
clusters that may have once hosted luminous supermassive stars. Since this abundance
pattern is also common among the most ancient stars born in the Milky Way, we
may be directly witnessing the formation of such stars in dense clusters, connecting
galaxy evolution across the entire sweep of cosmic time. "
acknowledgement: "We thank the two anonymous referees for their insightful comments
that have strengthened this work. “Mirage or Miracle” is but the latest link in
a long chain of surveys that have built COSMOS into a premier extragalactic legacy
field. We are thankful to all the teams who have contributed to this legacy, particularly
those mentioned in §3 for leading recent JWST programs whose imaging\r\nwe have
incorporated in our analysis. We are grateful to Vasily Belokurov for help in compiling
the Milky Way reference sample featured in Fig 8. We thank Danielle Berg for sharing
a highly complete, highly decimalized NUV vacuum line list. We are grateful to our
program’s NIRSpec reviewer, Dan Coe, and program coordinator, Allison Vick, for
valuable input on our MSA design. We acknowledge illuminating conversations with
Risa Wechsler and Chao-Lin Kuo about early reionization. RPN thanks Neil Pappalardo
and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships
in Physics, and for their enthusiasm and encouragement for seeking galaxies at the
highest redshifts. RPN acknowledges funding from JWST program GO5224. Support for
this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A
awarded by the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
This work has received funding from the Swiss State Secretariat for Education, Research
and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss
National Science Foundation (SNSF) through project grant 200020 207349. Funded by
the European Union (ERC, AGENTS, 101076224 and HEAVYMETAL, 101071865). Views and
opinions expressed are however those of the author(s) only and do not necessarily
reflect those of\r\nthe European Union or the European Research Council. Neither
the European Union nor the granting authority can be held responsible for them.
The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation
under grant DNRF140. This work has also been supported by JSPS KAKENHI Grant Number
23H00131. HA acknowledges support from CNES, focused on the JWST mission, and the
Programme National Cosmology and Galaxies (PNCG)\r\nof CNRS/INSU with INP and IN2P3,
co-funded by CEA and CNES. HA is supported by the French National Research Agency
(ANR) under the project FIRSTGAL, grant number ANR-24-CE31-0838. SB is supported
by the UK Research and Innovation (UKRI) Future Leaders Fellowship [grant number
MR/V023381/1]. R.D. acknowledges support from the INAF GO 2022\r\ngrant “The birth
of the giants: JWST sheds light on the build-up of quasars at cosmic dawn” and by
the PRIN MUR “2022935STW”, RFF M4.C2.1.1, CUP J53D23001570006 and C53D23000950006.
Computations supporting this paper were run on MIT’s Engaging cluster. This publication
made use of the NASA Astrophysical Data System for bibliographic information. Some
of the data products presented herein were retrieved from the Dawn JWST Archive
(DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by
the Danish National Research Foundation under grant DNRF140. Software used in developing
this work includes: matplotlib (Hunter 2007), jupyter (Kluyver et al. 2016), IPython
(P´erez & Granger 2007), numpy (Oliphant 2015), scipy (Virtanen et al. 2020), TOPCAT
(Taylor 2005), and Astropy (Astropy Collaboration et al. 2013).This work is based
on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data
were obtained from the Mikulski Archive for Space\r\nTelescopes at the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations
are associated with program # 5224."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Yijia
full_name: Li, Yijia
last_name: Li
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Clara L.
full_name: Pollock, Clara L.
last_name: Pollock
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: Benjamin D.
full_name: Johnson, Benjamin D.
last_name: Johnson
- first_name: Xuejian
full_name: Shen, Xuejian
last_name: Shen
- first_name: Raphael E.
full_name: Hviding, Raphael E.
last_name: Hviding
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Arpita
full_name: Ganguly, Arpita
last_name: Ganguly
- first_name: Callum
full_name: Witten, Callum
last_name: Witten
- first_name: Hakim
full_name: Atek, Hakim
last_name: Atek
- first_name: Sirio
full_name: Belli, Sirio
last_name: Belli
- first_name: Sownak
full_name: Bose, Sownak
last_name: Bose
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Pratika
full_name: Dayal, Pratika
last_name: Dayal
- first_name: Roberto
full_name: Decarli, Roberto
last_name: Decarli
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Yoshinobu
full_name: Fudamoto, Yoshinobu
last_name: Fudamoto
- first_name: Emma
full_name: Giovinazzo, Emma
last_name: Giovinazzo
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Garth
full_name: Illingworth, Garth
last_name: Illingworth
- first_name: Akio K.
full_name: Inoue, Akio K.
last_name: Inoue
- first_name: Sarah G.
full_name: Kane, Sarah G.
last_name: Kane
- first_name: Ivo
full_name: Labbe, Ivo
last_name: Labbe
- first_name: Ecaterina
full_name: Leonova, Ecaterina
last_name: Leonova
- first_name: Rui
full_name: Marques-Chaves, Rui
last_name: Marques-Chaves
- first_name: Romain A.
full_name: Meyer, Romain A.
last_name: Meyer
- first_name: Erica J.
full_name: Nelson, Erica J.
last_name: Nelson
- first_name: Guido
full_name: Roberts-Borsani, Guido
last_name: Roberts-Borsani
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Mauro
full_name: Stefanon, Mauro
last_name: Stefanon
- first_name: Yuma
full_name: Sugahara, Yuma
last_name: Sugahara
- first_name: Sune
full_name: Toft, Sune
last_name: Toft
- first_name: Arjen
full_name: Van Der Wel, Arjen
last_name: Van Der Wel
- first_name: Pieter
full_name: Van Dokkum, Pieter
last_name: Van Dokkum
- first_name: Fabian
full_name: Walter, Fabian
last_name: Walter
- first_name: Darach
full_name: Watson, Darach
last_name: Watson
- first_name: John R.
full_name: Weaver, John R.
last_name: Weaver
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
citation:
ama: 'Naidu RP, Oesch PA, Brammer G, et al. A cosmic miracle: A remarkably luminous
galaxy at zspec = 14.44 confirmed with JWST. The Open Journal of Astrophysics.
2026;9. doi:10.33232/001c.156033'
apa: 'Naidu, R. P., Oesch, P. A., Brammer, G., Weibel, A., Li, Y., Matthee, J. J.,
… Whitaker, K. E. (2026). A cosmic miracle: A remarkably luminous galaxy at zspec
= 14.44 confirmed with JWST. The Open Journal of Astrophysics. Maynooth
Academic Publishing. https://doi.org/10.33232/001c.156033'
chicago: 'Naidu, Rohan P., Pascal A. Oesch, Gabriel Brammer, Andrea Weibel, Yijia
Li, Jorryt J Matthee, John Chisholm, et al. “A Cosmic Miracle: A Remarkably Luminous
Galaxy at Zspec = 14.44 Confirmed with JWST.” The Open Journal of Astrophysics.
Maynooth Academic Publishing, 2026. https://doi.org/10.33232/001c.156033.'
ieee: 'R. P. Naidu et al., “A cosmic miracle: A remarkably luminous galaxy
at zspec = 14.44 confirmed with JWST,” The Open Journal of Astrophysics,
vol. 9. Maynooth Academic Publishing, 2026.'
ista: 'Naidu RP, Oesch PA, Brammer G, Weibel A, Li Y, Matthee JJ, Chisholm J, Pollock
CL, Heintz KE, Johnson BD, Shen X, Hviding RE, Leja J, Tacchella S, Ganguly A,
Witten C, Atek H, Belli S, Bose S, Bouwens R, Dayal P, Decarli R, De Graaff A,
Fudamoto Y, Giovinazzo E, Greene JE, Illingworth G, Inoue AK, Kane SG, Labbe I,
Leonova E, Marques-Chaves R, Meyer RA, Nelson EJ, Roberts-Borsani G, Schaerer
D, Simcoe RA, Stefanon M, Sugahara Y, Toft S, Van Der Wel A, Van Dokkum P, Walter
F, Watson D, Weaver JR, Whitaker KE. 2026. A cosmic miracle: A remarkably luminous
galaxy at zspec = 14.44 confirmed with JWST. The Open Journal of Astrophysics.
9.'
mla: 'Naidu, Rohan P., et al. “A Cosmic Miracle: A Remarkably Luminous Galaxy at
Zspec = 14.44 Confirmed with JWST.” The Open Journal of Astrophysics, vol.
9, Maynooth Academic Publishing, 2026, doi:10.33232/001c.156033.'
short: R.P. Naidu, P.A. Oesch, G. Brammer, A. Weibel, Y. Li, J.J. Matthee, J. Chisholm,
C.L. Pollock, K.E. Heintz, B.D. Johnson, X. Shen, R.E. Hviding, J. Leja, S. Tacchella,
A. Ganguly, C. Witten, H. Atek, S. Belli, S. Bose, R. Bouwens, P. Dayal, R. Decarli,
A. De Graaff, Y. Fudamoto, E. Giovinazzo, J.E. Greene, G. Illingworth, A.K. Inoue,
S.G. Kane, I. Labbe, E. Leonova, R. Marques-Chaves, R.A. Meyer, E.J. Nelson, G.
Roberts-Borsani, D. Schaerer, R.A. Simcoe, M. Stefanon, Y. Sugahara, S. Toft,
A. Van Der Wel, P. Van Dokkum, F. Walter, D. Watson, J.R. Weaver, K.E. Whitaker,
The Open Journal of Astrophysics 9 (2026).
date_created: 2026-02-22T23:01:35Z
date_published: 2026-01-30T00:00:00Z
date_updated: 2026-02-24T07:37:17Z
day: '30'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.33232/001c.156033
external_id:
arxiv:
- '2505.11263'
has_accepted_license: '1'
intvolume: ' 9'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.33232/001c.156033
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Open Journal of Astrophysics
publication_identifier:
eissn:
- 2565-6120
publication_status: published
publisher: Maynooth Academic Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed
with JWST'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 9
year: '2026'
...
---
OA_type: closed access
_id: '21371'
abstract:
- lang: eng
text: There may be a newly identified early phase of supermassive black hole growth
acknowledgement: The author acknowledges the support from the European Union (European
Research Council, AGENTS, 101076224).
article_processing_charge: No
article_type: comment
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Matthee JJ. Black holes disguised as little red dots. Science. 2026;391(6787):767-768.
doi:10.1126/science.adz8603
apa: Matthee, J. J. (2026). Black holes disguised as little red dots. Science.
AAAS. https://doi.org/10.1126/science.adz8603
chicago: Matthee, Jorryt J. “Black Holes Disguised as Little Red Dots.” Science.
AAAS, 2026. https://doi.org/10.1126/science.adz8603.
ieee: J. J. Matthee, “Black holes disguised as little red dots,” Science,
vol. 391, no. 6787. AAAS, pp. 767–768, 2026.
ista: Matthee JJ. 2026. Black holes disguised as little red dots. Science. 391(6787),
767–768.
mla: Matthee, Jorryt J. “Black Holes Disguised as Little Red Dots.” Science,
vol. 391, no. 6787, AAAS, 2026, pp. 767–68, doi:10.1126/science.adz8603.
short: J.J. Matthee, Science 391 (2026) 767–768.
corr_author: '1'
date_created: 2026-03-01T23:01:39Z
date_published: 2026-02-19T00:00:00Z
date_updated: 2026-03-02T09:15:45Z
day: '19'
department:
- _id: JoMa
doi: 10.1126/science.adz8603
external_id:
pmid:
- '41712710'
intvolume: ' 391'
issue: '6787'
language:
- iso: eng
month: '02'
oa_version: None
page: 767-768
pmid: 1
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Science
publication_identifier:
eissn:
- 1095-9203
publication_status: published
publisher: AAAS
quality_controlled: '1'
scopus_import: '1'
status: public
title: Black holes disguised as little red dots
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 391
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
_id: '21380'
abstract:
- lang: eng
text: "Context. Extreme emission line galaxies (EELGs) are believed to significantly
contribute to the star formation activity and mass assembly in galaxies. EELGs
likely also play a leading role in the cosmic re-ionization as their interstellar
medium may allow a significant fraction of their ionizing photons to escape (>
5%). Finding low-redshift analogues of these high-z galaxies is therefore essential
to characterizing the physical conditions in the interstellar medium of these
galaxies and understanding the processes that re-ionized the Universe.\r\n\r\nAims.
We aimed to develop a robust and efficient method for the photometric identification
of EELGs using the J-PAS survey. J-PAS will cover approximately 8500 deg2 of the
sky with 54 narrow-band filters in the optical range plus i-SDSS, enabling detailed
studies of the physical properties of these galaxies. In this work we focused
on an initial subset of the survey: a 30 square degree area with complete observations
in all bands.\r\n\r\nMethods. We combine equivalent width (EW) measurements from
J-PAS narrow-band photometry with artificial intelligence techniques to identify
galaxies with emission lines exceeding 300 Å. We validated our selection using
spectroscopic data from DESI DR1 and characterized the selected sample through
spectral energy distribution fitting with CIGALE.\r\n\r\nResults. We identify
917 EELGs up to z = 0.8 over 30 deg2, achieving a purity of 95% and a completeness
of 96% for i-SDSS < 22.5 mag. Importantly, active galactic nucleus contamination
was carefully considered and is estimated to be around 5%. Furthermore, a cross-match
with DESI yielded 79 counterparts; their redshifts are in excellent agreement
with our photometric estimates, thereby confirming the reliability of our redshift
determination. In addition, the derived emission line fluxes are in good agreement
with spectroscopic measurements. Moreover, the selected sample reveals strong
correlations between the ionizing photon production efficiency (ξion) and EW(Hβ),
which are consistent with previous observational studies at low and high redshifts
and theoretical expectations. Finally, most of the sources surpass the ionizing
efficiency threshold required for re-ionization, highlighting their relevance
as local analogues of early-Universe galaxies."
acknowledgement: "We thank the referee for several helpful suggestions. AGA, MGO and
IM acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S, funded
by MICIU/AEI/10.13039/501100011033. AGA also acknowledges FPI support under grant
code CEX2021-001131-S20-7. Both AGA and MGO acknowledge support from the research
grant\r\nPID2022-136598NB-C32 (“Estallidos8”). MGO also acknowledges the support
by the project ref. AST22_00001_Subp_11 funded from the EU – NextGenerationEU. RA
acknowledges support from PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033
and ERDF/EU. IM acknowledges support from PID2022-140871NB-C21 funded by MICIU/AEI/10.13039/501100011033
and FEDER/UE. RGD acknowledge financial support from the project PID2022-141755NB-I00,
and the Severo Ochoa grant CEX2021-001131-S funded\r\nby MICIU/AEI/ 10.13039/501100011033.
JAFO and AE acknowledge support from the Spanish Ministry of Science and Innovation
and the EU–NextGenerationEU through the RRF project ICTS-MRR-2021-03-CEFCA. AHC
and ALC acknowledge support from MCIN/AEI/10.13039/501100011033, “ERDF A way of
making Europe”, and “EU NextGenerationEU/PRTR” through PID2021-124918NB-C44 and
CNS2023-145339, as well as from the RRF project ICTS-MRR-2021-03-CEFCA ALC and RPT
acknowledge the financial\r\nsupport from the European Union – NextGenerationEU
through the RRF program Planes Complementarios con las CCAA de Astrofísica y Física
de Altas Energías – LA4. I.B. acknowledges support from the EU Horizon 2020 programme
(Marie Sklodowska-Curie Grant 101059532) and the Franziska Seidl Funding Program,
University of Vienna. This paper has gone through internal‘ review by the J-PAS
collaboration. Based on observations made with the\r\nJST/T250 telescope and JPCam
at the Observatorio Astrofísico de Javalambre (OAJ), in Teruel, owned, managed,
and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). We
acknowledge the OAJ Data Processing and Archiving Unit (UPAD) for reducing and calibrating
the OAJ data used in this work. Funding for the J-PAS Project has been provided
by the Governments of Spain and Aragón through the Fondo de Inversiones de Teruel;
the Aragonese Government through the Research Groups E96, E103, E16_17R, E16_20R,
and E16_23R; the Spanish Ministry of Science and Innovation (MCIN/AEI/10.13039/501100011033
y FEDER, Una manera de hacer Europa) with grants PID2021-124918NB-C41, PID2021-124918NB-C42,
PID2021-124918NA-C43, and PID2021-124918NB-C44; the Spanish Ministry\r\nof Science,
Innovation and Universities (MCIU/AEI/FEDER, UE) with grants\r\nPGC2018-097585-B-C21
and PGC2018-097585-B-C22; the Spanish Ministry of Economy and Competitiveness (MINECO)
under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, and AYA2012-30789; and European
FEDER funding (FCDD10-4E-867, FCDD13-4E-2685)."
article_number: A261
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A.
full_name: Giménez-Alcázar, A.
last_name: Giménez-Alcázar
- first_name: R.
full_name: Amorín, R.
last_name: Amorín
- first_name: J. M.
full_name: Vílchez, J. M.
last_name: Vílchez
- first_name: A.
full_name: Hernán-Caballero, A.
last_name: Hernán-Caballero
- first_name: M.
full_name: González-Otero, M.
last_name: González-Otero
- first_name: A.
full_name: Arroyo-Polonio, A.
last_name: Arroyo-Polonio
- first_name: J.
full_name: Iglesias-Páramo, J.
last_name: Iglesias-Páramo
- first_name: A.
full_name: Lumbreras-Calle, A.
last_name: Lumbreras-Calle
- first_name: J. A.
full_name: Fernández-Ontiveros, J. A.
last_name: Fernández-Ontiveros
- first_name: C.
full_name: López-Sanjuan, C.
last_name: López-Sanjuan
- first_name: L.
full_name: Bonatto, L.
last_name: Bonatto
- first_name: R. M.
full_name: González Delgado, R. M.
last_name: González Delgado
- first_name: C.
full_name: Kehrig, C.
last_name: Kehrig
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: P. T.
full_name: Rahna, P. T.
last_name: Rahna
- first_name: Y.
full_name: Jiménez-Teja, Y.
last_name: Jiménez-Teja
- first_name: I.
full_name: Márquez, I.
last_name: Márquez
- first_name: I.
full_name: Breda, I.
last_name: Breda
- first_name: A.
full_name: Álvarez-Candal, A.
last_name: Álvarez-Candal
- first_name: R.
full_name: Abramo, R.
last_name: Abramo
- first_name: J.
full_name: Alcaniz, J.
last_name: Alcaniz
- first_name: N.
full_name: Benitez, N.
last_name: Benitez
- first_name: S.
full_name: Bonoli, S.
last_name: Bonoli
- first_name: S.
full_name: Carneiro, S.
last_name: Carneiro
- first_name: J.
full_name: Cenarro, J.
last_name: Cenarro
- first_name: D.
full_name: Cristóbal-Hornillos, D.
last_name: Cristóbal-Hornillos
- first_name: R.
full_name: Dupke, R.
last_name: Dupke
- first_name: A.
full_name: Ederoclite, A.
last_name: Ederoclite
- first_name: C.
full_name: Hernández-Monteagudo, C.
last_name: Hernández-Monteagudo
- first_name: A.
full_name: Marín-Franch, A.
last_name: Marín-Franch
- first_name: C.
full_name: Mendes de Oliveira, C.
last_name: Mendes de Oliveira
- first_name: M.
full_name: Moles, M.
last_name: Moles
- first_name: L.
full_name: Sodré, L.
last_name: Sodré
- first_name: K.
full_name: Taylor, K.
last_name: Taylor
- first_name: J.
full_name: Varela, J.
last_name: Varela
- first_name: H.
full_name: Vázquez Ramió, H.
last_name: Vázquez Ramió
citation:
ama: 'Giménez-Alcázar A, Amorín R, Vílchez JM, et al. J-PAS: First identification,
physical properties, and ionization efficiency of extreme emission line galaxies.
Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202557358'
apa: 'Giménez-Alcázar, A., Amorín, R., Vílchez, J. M., Hernán-Caballero, A., González-Otero,
M., Arroyo-Polonio, A., … Vázquez Ramió, H. (2026). J-PAS: First identification,
physical properties, and ionization efficiency of extreme emission line galaxies.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557358'
chicago: 'Giménez-Alcázar, A., R. Amorín, J. M. Vílchez, A. Hernán-Caballero, M.
González-Otero, A. Arroyo-Polonio, J. Iglesias-Páramo, et al. “J-PAS: First Identification,
Physical Properties, and Ionization Efficiency of Extreme Emission Line Galaxies.”
Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557358.'
ieee: 'A. Giménez-Alcázar et al., “J-PAS: First identification, physical
properties, and ionization efficiency of extreme emission line galaxies,” Astronomy
& Astrophysics, vol. 706. EDP Sciences, 2026.'
ista: 'Giménez-Alcázar A, Amorín R, Vílchez JM, Hernán-Caballero A, González-Otero
M, Arroyo-Polonio A, Iglesias-Páramo J, Lumbreras-Calle A, Fernández-Ontiveros
JA, López-Sanjuan C, Bonatto L, González Delgado RM, Kehrig C, Torralba Torregrosa
A, Rahna PT, Jiménez-Teja Y, Márquez I, Breda I, Álvarez-Candal A, Abramo R, Alcaniz
J, Benitez N, Bonoli S, Carneiro S, Cenarro J, Cristóbal-Hornillos D, Dupke R,
Ederoclite A, Hernández-Monteagudo C, Marín-Franch A, Mendes de Oliveira C, Moles
M, Sodré L, Taylor K, Varela J, Vázquez Ramió H. 2026. J-PAS: First identification,
physical properties, and ionization efficiency of extreme emission line galaxies.
Astronomy & Astrophysics. 706, A261.'
mla: 'Giménez-Alcázar, A., et al. “J-PAS: First Identification, Physical Properties,
and Ionization Efficiency of Extreme Emission Line Galaxies.” Astronomy &
Astrophysics, vol. 706, A261, EDP Sciences, 2026, doi:10.1051/0004-6361/202557358.'
short: A. Giménez-Alcázar, R. Amorín, J.M. Vílchez, A. Hernán-Caballero, M. González-Otero,
A. Arroyo-Polonio, J. Iglesias-Páramo, A. Lumbreras-Calle, J.A. Fernández-Ontiveros,
C. López-Sanjuan, L. Bonatto, R.M. González Delgado, C. Kehrig, A. Torralba Torregrosa,
P.T. Rahna, Y. Jiménez-Teja, I. Márquez, I. Breda, A. Álvarez-Candal, R. Abramo,
J. Alcaniz, N. Benitez, S. Bonoli, S. Carneiro, J. Cenarro, D. Cristóbal-Hornillos,
R. Dupke, A. Ederoclite, C. Hernández-Monteagudo, A. Marín-Franch, C. Mendes de
Oliveira, M. Moles, L. Sodré, K. Taylor, J. Varela, H. Vázquez Ramió, Astronomy
& Astrophysics 706 (2026).
date_created: 2026-03-02T10:06:10Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-03-02T15:10:27Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557358
external_id:
arxiv:
- '2512.08484'
file:
- access_level: open_access
checksum: cd25a05386ab5638ae5baf8add0ecbee
content_type: application/pdf
creator: dernst
date_created: 2026-03-02T14:51:57Z
date_updated: 2026-03-02T14:51:57Z
file_id: '21391'
file_name: 2026_AstronomyAstrophysics_GimenezAlcazar.pdf
file_size: 1813456
relation: main_file
success: 1
file_date_updated: 2026-03-02T14:51:57Z
has_accepted_license: '1'
intvolume: ' 706'
language:
- iso: eng
month: '02'
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: 'J-PAS: First identification, physical properties, and ionization efficiency
of extreme emission line galaxies'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 706
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21451'
abstract:
- lang: eng
text: The population of the little red dots (LRDs) may represent a key phase of
supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging
as a key component to explain the most striking properties of LRDs, such as strong
Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect
the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra
of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra
reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission.
We revealed a forest of optical [Fe II] lines, which we argue are emerging from
a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K.
The broad wings of Hα and Hβ have an exponential profile due to electron scattering
in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an
indicator of collisional excitation and resonant scattering dominating the Balmer
line emission. A narrow Hγ component, unseen in the other two Balmer lines due
to outshining by the broad components, could trace the ISM of a normal host galaxy
with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer
transitions, producing a characteristic P Cygni profile in the line centers suggesting
outflowing motions. This same layer is responsible for shaping the Balmer break.
The broadband spectrum can be reasonably matched by a simple photoionized slab
model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy
that could explain the narrow [O III], with only a subdominant contribution to
the UV continuum. Our findings indicate that Balmer lines are not directly tracing
the gas kinematics near the SMBH and that the BH mass scale is likely much lower
than virial indicators suggest.
acknowledgement: 'We thank the scientific referee for useful and constructive comments.
We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics
of gaseous envelopes and accretion into black holes. Funded by the European Union
(ERC, AGENTS, 101076224). Views and opinions expressed are however those of the
author(s) only and do not necessarily reflect those of the European Union or the
European Research Council. Neither the European Union nor the granting authority
can be held responsible for them. This work is based in part on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with program #5664. This work has received funding from the Swiss State Secretariat
for Education, Research and Innovation (SERI) under contract number MB22.00072,
as well as from the Swiss National Science Foundation (SNSF) through project grant
200020_207349.'
article_number: A75
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Seok Jun
full_name: Chang, Seok Jun
last_name: Chang
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Erica
full_name: Nelson, Erica
last_name: Nelson
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer
of a little red dot as the source of [Fe ii] and collisional Balmer lines with
scattering wings. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557537
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa,
Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot
as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557537
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan
P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm
Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer
Lines with Scattering Wings.” Astronomy & Astrophysics. EDP Sciences,
2026. https://doi.org/10.1051/0004-6361/202557537.
ieee: A. Torralba Torregrosa et al., “The warm outer layer of a little red
dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,”
Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer
GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene
JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete
B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little
red dot as the source of [Fe ii] and collisional Balmer lines with scattering
wings. Astronomy & Astrophysics. 707, A75.
mla: Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red
Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.”
Astronomy & Astrophysics, vol. 707, A75, EDP Sciences, 2026, doi:10.1051/0004-6361/202557537.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa,
G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare,
A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko,
Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy
& Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:59:16Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557537
external_id:
arxiv:
- '2510.00103'
file:
- access_level: open_access
checksum: fcab9cb3dcf1d68612e1fdc8191643c1
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:57:49Z
date_updated: 2026-03-16T10:57:49Z
file_id: '21460'
file_name: 2026_AstronomyAstrophysics_Torralba2.pdf
file_size: 2510157
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:57:49Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
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: The warm outer layer of a little red dot as the source of [Fe ii] and collisional
Balmer lines with scattering wings
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21452'
abstract:
- lang: eng
text: Galaxies exhibit a tight correlation between their star formation rate (SFR)
and stellar mass over a wide redshift range known as the star-forming main sequence
(SFMS). With JWST, the SFMS can now be investigated at high redshifts down to
masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα
emission, which allow us to probe the variability in the star formation histories.
We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5
with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell
2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little
Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α,
with α = 0.45). After we corrected this for the Hα-flux limited nature of our
survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09,
whereas current data on their own are inconclusive on the mass dependence of the
scatter. These slopes differ significantly from the slope of ∼1 that is expected
from the observed evolution of the galaxy stellar mass function and from simulations.
When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic
scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010
M⊙). This difference might be explained by a (combination of) luminosity-dependent
SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated
dust attenuation in high-mass galaxies. Future deep observations with different
facilities can quantify these processes, which will enable us to achieve better
insights into the variability of the star formation histories.
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion,
Pierluigi Rinaldi for his help with data handling and Luca Graziani and William
McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. Funded
by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are
however those of the author(s) only and do not necessarily reflect those of the
European Union or the European Research Council. Neither the European Union nor
the granting authority can be held responsible for them. This work is based on observations
made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from
the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with program # 3516. We acknowledge funding from JWST program GO-3516. Software
used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant
2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy
Collaboration 2013)."
article_number: A129
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Alberto
full_name: Torralba, Alberto
last_name: Torralba
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Jeremy
full_name: Blaizot, Jeremy
last_name: Blaizot
- first_name: Joakim
full_name: Rosdahl, Joakim
last_name: Rosdahl
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Angela
full_name: Adamo, Angela
last_name: Adamo
- first_name: Alba
full_name: Covelo-Paz, Alba
last_name: Covelo-Paz
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Michael
full_name: Romano, Michael
last_name: Romano
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
citation:
ama: 'Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming
main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557790'
apa: 'Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko,
I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence
at z ∼ 5: Reconciling observations with simulations. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557790'
chicago: 'Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba,
Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter
of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.”
Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557790.'
ieee: 'C. Di Cesare et al., “The slope and scatter of the star-forming main
sequence at z ∼ 5: Reconciling observations with simulations,” Astronomy &
Astrophysics, vol. 707. EDP Sciences, 2026.'
ista: 'Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I,
Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz
KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The
slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations
with simulations. Astronomy & Astrophysics. 707, A129.'
mla: 'Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main
Sequence at z ∼ 5: Reconciling Observations with Simulations.” Astronomy &
Astrophysics, vol. 707, A129, EDP Sciences, 2026, doi:10.1051/0004-6361/202557790.'
short: C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko,
J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak,
K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:52:44Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202557790
external_id:
arxiv:
- '2510.19044'
file:
- access_level: open_access
checksum: c056b00ce7324849754521fde10fb7ca
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:48:07Z
date_updated: 2026-03-16T10:48:07Z
file_id: '21459'
file_name: 2026_AstronomyAstrophysics_DiCesare.pdf
file_size: 1821411
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:48:07Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
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: 'The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling
observations with simulations'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21481'
abstract:
- lang: eng
text: 'The Hα emission line in galaxies is a powerful tracer of their recent star
formation activity. With the advent of JWST, we are now able to routinely observe
Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation
rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs
leads to biased results because high-redshift galaxies are commonly characterized
by low metallicities and bursty star formation histories, affecting the conversion
factor between the Hα luminosity (LHα) and the SFR. We developed a set of new
SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3
with very little error. We used the SPHINX cosmological simulations to select
a sample of star-forming galaxies representative of the Hα-emitter population
observed with JWST. We then derived linear corrections to the classical SFR(Hα)
calibrations that took variations in the physical properties (e.g., stellar metallicities)
among individual galaxies into account. We obtained two new SFR(Hα) calibrations
that compared to the classical calibrations reduce the root mean squared error
(RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively.
Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show
that the new calibrations affect the high-redshift galaxy population statistics:
(i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed
slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.'
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene
Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala
for useful comments and productive discussions. We gratefully acknowledge support
from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de
Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS,
101076224). Views and opinions expressed are however those of the author(s) only
and do not necessarily reflect those of the European Union or the European Research
Council. Neither the European Union nor the granting authority can be held responsible
for them. This work made extensive use of several open-source software packages,
and we gratefully acknowledge the efforts of their authors: numpy (Harris et al.
2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez
& Granger 2007), and scikit-learn (Pedregosa et al. 2011)."
article_number: A184
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: J.
full_name: Rosdahl, J.
last_name: Rosdahl
- first_name: J.
full_name: Blaizot, J.
last_name: Blaizot
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: H.
full_name: Katz, H.
last_name: Katz
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
citation:
ama: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as
a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557114
apa: Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., & Di
Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological
simulations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557114
chicago: Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and
Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557114.
ieee: I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare,
“H α as a tracer of star formation in the SPHINX cosmological simulations,” Astronomy
& Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026.
H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 707, A184.
mla: Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics, vol. 707, A184, EDP Sciences,
2026, doi:10.1051/0004-6361/202557114.
short: I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-23T14:58:03Z
date_published: 2026-03-05T00:00:00Z
date_updated: 2026-03-23T15:46:31Z
day: '05'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557114
external_id:
arxiv:
- '2509.05403'
file:
- access_level: open_access
checksum: 7429076b381dd498084f40ffd199e714
content_type: application/pdf
creator: dernst
date_created: 2026-03-23T15:44:09Z
date_updated: 2026-03-23T15:44:09Z
file_id: '21492'
file_name: 2026_AstronomyAstrophysics_Kramarenko.pdf
file_size: 904565
relation: main_file
success: 1
file_date_updated: 2026-03-23T15:44:09Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
status: public
title: H α as a tracer of star formation in the SPHINX cosmological simulations
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '21709'
abstract:
- lang: eng
text: 'JWST’s “little red dots” (LRDs) are increasingly interpreted as active galactic
nuclei (AGN) obscured by dense thermalized gas rather than dust as evidenced by
their X-ray weakness, blackbody-like continua, and Balmer line profiles. Key questions
are how LRDs connect to standard UV-luminous AGN, whether transitional phases
exist, and whether they are observable. We present the “X-ray dot” (XRD), a compact
source at z = 3.28 observed by the NIRSpec Wide Guaranteed Time Observation survey.
The XRD exhibits LRD hallmarks: a blackbody-like (Teff ≃ 6400 K) red continuum,
a faint but blue rest-UV excess, falling mid-IR emission, and broad Balmer lines
(FWHM ∼ 2700–3200 km s−1). Unlike LRDs, however, it is remarkably X-ray luminous
(L2−10 keV = 1044.18 erg s−1) and has a continuum inflection that is blueward
of the Balmer limit. We find that the red rest-optical and blue mid-IR continuum
cannot be reproduced by standard dust-attenuated AGN models without invoking extremely
steep extinction curves, nor can the weak mid-IR emission be reconciled with well-established
X-ray–torus scaling relations. We therefore consider an alternative scenario:
the XRD may be an LRD in transition, where the gas envelope dominates the optical
continuum but optically thin sight lines allow X-rays to escape. The XRD may thus
provide a physical link between LRDs and standard AGN, offering direct evidence
that LRDs are powered by supermassive black holes and providing insight into their
accretion properties.'
acknowledgement: "We would like to thank the anonymous reviewer for their constructive
comments, which improved the final manuscript.\r\n\r\nWe thank Bernd Husemann for
his critical contributions to the NIRSpec Wide GTO survey, and in particular his
help in selecting high-priority X-ray-luminous targets.\r\n\r\nR.E.H. acknowledges
support by the German Aerospace Center (DLR) and the Federal Ministry for Economic
Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.” A.d.G. acknowledges
support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.
A.J.B. acknowledges funding from the “FirstGalaxies” Advanced grant from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
program (grant agreement No. 789056). R.P.N. thanks Neil Pappalardo and Jane Pappalardo
for their generous support of the MIT Pappalardo Fellowships in Physics. Support
for this work was provided by the Brinson Foundation through a Brinson Prize Fellowship
grant. H.Ü. acknowledges funding by the European Union (ERC APEX, 101164796). Views
and opinions expressed are, however, those of the authors only and do not necessarily
reflect those of the European Union or the European Research Council Executive Agency.
Neither the European Union nor the granting authority can be held responsible for
them. G.V. acknowledges support from European Union’s HE ERC Starting grant No.
101040227—WINGS. B.W. acknowledges support provided by NASA through Hubble Fellowship
grant HST-HF2-51592.001 awarded by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in Astronomy, In., for
NASA, under the contract NAS 5-26555.\r\n\r\nThe data products presented herein
were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic
Dawn Center (DAWN).\r\n\r\nThis work is based in part on observations made with
the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski
Archive for Space Telescopes at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-03127 for JWST. These observations are associated with programs
Nos. GTO-1213. The data described here may be obtained from the MAST archive at
DOI: 10.17909/qffz-b324.\r\n\r\nThis Letter employs a list of Chandra datasets,
obtained by the Chandra X-ray Observatory, contained in DOI: 10.25574/cdc.540.\r\n\r\nThis
work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and
12328) with the NASA/ESA HST, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555.\r\n\r\nThis work
makes use of color palettes created by Martin Krzywinski designed for colorblindness.
The color palettes and more information can be found at http://mkweb.bcgsc.ca/colorblind/.\r\n\r\nFacilities:
CXO - Chandra X-ray Observatory satellite (ACIS), HST - Hubble Space Telescope satellite
(ACS, WFC3) - , CFHT - Canada-France-Hawaii Telescope (WIRCam), JWST - James Webb
Space Telescope (NIRSpec), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS)
- , JCMT - James Clerk Maxwell Telescope (SCUBA).\r\n\r\nSoftware: Astropy (Astropy
Collaboration et al. 2013, 2018, 2022), dust_attenuation, dust_extinction (K. Gordon
2024), jax (J. Bradbury et al. 2018), LaTeX (L. Lamport 1994), Matplotlib (J. D.
Hunter 2007), NumPy (T. E. Oliphant 2006; S. van der Walt et al. 2011; C. R. Harris
et al. 2020), NumPyro (D. Phan et al. 2019), scipy (P. Virtanen et al. 2020), sedpy
(B. Johnson & J. Leja 2017), specutils (Astropy-Specutils Development Team 2019),
unite (R. E. Hviding 2025)."
article_number: L18
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Raphael E.
full_name: Hviding, Raphael E.
last_name: Hviding
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Hanpu
full_name: Liu, Hanpu
last_name: Liu
- first_name: Andy D.
full_name: Goulding, Andy D.
last_name: Goulding
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Andrew J.
full_name: Bunker, Andrew J.
last_name: Bunker
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Marijn
full_name: Franx, Marijn
last_name: Franx
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Hannah
full_name: Übler, Hannah
last_name: Übler
- first_name: Giacomo
full_name: Venturi, Giacomo
last_name: Venturi
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
citation:
ama: 'Hviding RE, De Graaff A, Liu H, et al. The X-ray dot: Exotic dust or a late-stage
Little Red Dot? The Astrophysical Journal Letters. 2026;1000(1). doi:10.3847/2041-8213/ae4c88'
apa: 'Hviding, R. E., De Graaff, A., Liu, H., Goulding, A. D., Ma, Y., Greene, J.
E., … Wang, B. (2026). The X-ray dot: Exotic dust or a late-stage Little Red Dot?
The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae4c88'
chicago: 'Hviding, Raphael E., Anna De Graaff, Hanpu Liu, Andy D. Goulding, Yilun
Ma, Jenny E. Greene, Leindert A. Boogaard, et al. “The X-Ray Dot: Exotic Dust
or a Late-Stage Little Red Dot?” The Astrophysical Journal Letters. IOP
Publishing, 2026. https://doi.org/10.3847/2041-8213/ae4c88.'
ieee: 'R. E. Hviding et al., “The X-ray dot: Exotic dust or a late-stage
Little Red Dot?,” The Astrophysical Journal Letters, vol. 1000, no. 1.
IOP Publishing, 2026.'
ista: 'Hviding RE, De Graaff A, Liu H, Goulding AD, Ma Y, Greene JE, Boogaard LA,
Bunker AJ, Cleri NJ, Franx M, Hirschmann M, Leja J, Matthee JJ, Naidu RP, Setton
DJ, Übler H, Venturi G, Wang B. 2026. The X-ray dot: Exotic dust or a late-stage
Little Red Dot? The Astrophysical Journal Letters. 1000(1), L18.'
mla: 'Hviding, Raphael E., et al. “The X-Ray Dot: Exotic Dust or a Late-Stage Little
Red Dot?” The Astrophysical Journal Letters, vol. 1000, no. 1, L18, IOP
Publishing, 2026, doi:10.3847/2041-8213/ae4c88.'
short: R.E. Hviding, A. De Graaff, H. Liu, A.D. Goulding, Y. Ma, J.E. Greene, L.A.
Boogaard, A.J. Bunker, N.J. Cleri, M. Franx, M. Hirschmann, J. Leja, J.J. Matthee,
R.P. Naidu, D.J. Setton, H. Übler, G. Venturi, B. Wang, The Astrophysical Journal
Letters 1000 (2026).
date_created: 2026-04-12T22:01:48Z
date_published: 2026-03-20T00:00:00Z
date_updated: 2026-05-04T07:13:07Z
day: '20'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ae4c88
external_id:
arxiv:
- '2601.09778'
file:
- access_level: open_access
checksum: 1be4f361bf59aa08b8c98ed4f475a463
content_type: application/pdf
creator: dernst
date_created: 2026-05-04T07:11:37Z
date_updated: 2026-05-04T07:11:37Z
file_id: '21784'
file_name: 2026_AstrophysicalJourLetters_Hviding.pdf
file_size: 2821786
relation: main_file
success: 1
file_date_updated: 2026-05-04T07:11:37Z
has_accepted_license: '1'
intvolume: ' 1000'
issue: '1'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The X-ray dot: Exotic dust or a late-stage Little Red Dot?'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 1000
year: '2026'
...
---
OA_place: publisher
OA_type: gold
_id: '21710'
abstract:
- lang: eng
text: "Early results from JWST suggest that Epoch of Reionization (EoR) galaxies
produce copious ionizing photons, which, if they escape efficiently, could cause
reionization to occur too early. We study this problem using JWST imaging and
prism spectroscopy for 412 galaxies at 4.5 < z < 9.0. We fit these data simultaneously
with stellar population and nebular emission models that include a parameter for
the fraction of ionizing photons that escape the galaxy, fesc. We find that the
ionization production efficiency, ξion = Q(H0)/LUV, increases with redshift and
decreasing UV luminosity, but shows significant scatter, (log ion z, MUV) 0.3
dex. The inferred escape fractions averaged over the population are low, ranging
from〈fesc〉 ≃ 2.6% ± 1.4% at 6 < z < 9 to 6.5% ± 2.2% at 4.5 < z < 6, with weak
or no indication of evolution with redshift. This implies that in our models most
of the ionizing photons need to be absorbed to account for the nebular emission.
We compute the impact of our results on reionization, including the distributions
for ξion and fesc, and the evolution and uncertainty of the UV luminosity function.
Considering galaxies brighter than MUV < −16 mag would produce an intergalactic
medium hydrogen-ionized fraction of xe = 0.5 at 5.3 < z < 5.8, possibly too late
compared to constraints from from quasistellar\r\nobject (QSO) sight lines. Including
fainter galaxies, MUV < −14 mag, we obtain xe = 0.5 at 6.0 < z < 8.1, fully consistent
with QSO and cosmic microwave background data. This implies that EoR galaxies
produce plenty of ionizing photons, but that these do not efficiently escape.
This may be a result of high gas column densities combined with burstier star
formation histories, which limit the time massive stars are able to clear channels
through the gas for ionizing photons to escape."
acknowledgement: "We wish to thank our colleagues in the CEERS collaboration for their
hard work and valuable contributions on this project. We extend our sincerest thanks
to the anonymous referee whose critical and constructive report improved the quality
of this manuscript. We also thank the JADES team for providing an excellent dataset
for science. We with to thank colleagues for valuable discussions, feedback, and
suggestions, including John Chisholm, Kevin Huffenberger, Jessica\r\nMeh, Julian
Muñoz, Irene Shivaei, Justin Spilker, Aaron Smith, and Romain Teyssier.\r\nPortions
of this research were conducted with the advanced computing resources provided by
Texas A&M High Performance Research Computing (HPRC, http://hprc.tamu.edu). This
work benefited from support from the George P. and Cynthia Woods Mitchell Institute
for Fundamental Physics and Astronomy at Texas A&M University. CP thanks Marsha
and Ralph Schilling for generous support of this research. This work was partially
support by the Future Investigators in NASA Earth and Space Science and Technology
(FINESST) program grant No. 80NSSC23K1487. R.A. acknowledges support of grant PID2023-147386NB-I00
funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant
CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. A.C.C. acknowledges support
from a UKRI Frontier Research Guarantee Grant (PI Carnall; grant reference EP/Y037065/1)
This work acknowledges support from the NASA/ESA/CSA James Webb Space Telescope
through the\r\nSpace Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-03127.
Support for program JWST-ERS-01345.009-A, JWST-GO-02079.013-A, JWST-GO-06368.011-A,
and JWST-GO-01837.030-A, was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127. This work made use of v2.2
of the Binary Population\r\nand Spectral Synthesis (BPASS) models as described in
E. R. Stanway & J. J. Eldridge (2018)."
article_number: '111'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Casey
full_name: Papovich, Casey
last_name: Papovich
- first_name: Justin W.
full_name: Cole, Justin W.
last_name: Cole
- first_name: Weida
full_name: Hu, Weida
last_name: Hu
- first_name: Steven L.
full_name: Finkelstein, Steven L.
last_name: Finkelstein
- first_name: Lu
full_name: Shen, Lu
last_name: Shen
- first_name: Pablo
full_name: Arrabal Haro, Pablo
last_name: Arrabal Haro
- first_name: Ricardo O.
full_name: Amorín, Ricardo O.
last_name: Amorín
- first_name: Bren E.
full_name: Backhaus, Bren E.
last_name: Backhaus
- first_name: Micaela B.
full_name: Bagley, Micaela B.
last_name: Bagley
- first_name: Rachana
full_name: Bhatawdekar, Rachana
last_name: Bhatawdekar
- first_name: Antonello
full_name: Calabrò, Antonello
last_name: Calabrò
- first_name: Adam C.
full_name: Carnall, Adam C.
last_name: Carnall
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Emanuele
full_name: Daddi, Emanuele
last_name: Daddi
- first_name: Mark
full_name: Dickinson, Mark
last_name: Dickinson
- first_name: Norman A.
full_name: Grogin, Norman A.
last_name: Grogin
- first_name: Benne W.
full_name: Holwerda, Benne W.
last_name: Holwerda
- first_name: Anne E.
full_name: Jaskot, Anne E.
last_name: Jaskot
- first_name: Anton M.
full_name: Koekemoer, Anton M.
last_name: Koekemoer
- first_name: Mario
full_name: Llerena, Mario
last_name: Llerena
- first_name: Ray A.
full_name: Lucas, Ray A.
last_name: Lucas
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Fabio
full_name: Pacucci, Fabio
last_name: Pacucci
- first_name: Laura
full_name: Pentericci, Laura
last_name: Pentericci
- first_name: Pablo G.
full_name: Pérez-González, Pablo G.
last_name: Pérez-González
- first_name: Nor
full_name: Pirzkal, Nor
last_name: Pirzkal
- first_name: Srinivasan
full_name: Raghunathan, Srinivasan
last_name: Raghunathan
- first_name: Lise Marie
full_name: Seillé, Lise Marie
last_name: Seillé
- first_name: Rachel S.
full_name: Somerville, Rachel S.
last_name: Somerville
- first_name: L. Y.Aaron
full_name: Yung, L. Y.Aaron
last_name: Yung
citation:
ama: Papovich C, Cole JW, Hu W, et al. Galaxies in the epoch of reionization are
all bark and no bite-plenty of ionizing photons, low escape fractions. The
Astrophysical Journal. 2026;1000(1). doi:10.3847/1538-4357/ae3b25
apa: Papovich, C., Cole, J. W., Hu, W., Finkelstein, S. L., Shen, L., Arrabal Haro,
P., … Yung, L. Y. A. (2026). Galaxies in the epoch of reionization are all bark
and no bite-plenty of ionizing photons, low escape fractions. The Astrophysical
Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae3b25
chicago: Papovich, Casey, Justin W. Cole, Weida Hu, Steven L. Finkelstein, Lu Shen,
Pablo Arrabal Haro, Ricardo O. Amorín, et al. “Galaxies in the Epoch of Reionization
Are All Bark and No Bite-Plenty of Ionizing Photons, Low Escape Fractions.” The
Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae3b25.
ieee: C. Papovich et al., “Galaxies in the epoch of reionization are all
bark and no bite-plenty of ionizing photons, low escape fractions,” The Astrophysical
Journal, vol. 1000, no. 1. IOP Publishing, 2026.
ista: Papovich C, Cole JW, Hu W, Finkelstein SL, Shen L, Arrabal Haro P, Amorín
RO, Backhaus BE, Bagley MB, Bhatawdekar R, Calabrò A, Carnall AC, Cleri NJ, Daddi
E, Dickinson M, Grogin NA, Holwerda BW, Jaskot AE, Koekemoer AM, Llerena M, Lucas
RA, Mascia S, Pacucci F, Pentericci L, Pérez-González PG, Pirzkal N, Raghunathan
S, Seillé LM, Somerville RS, Yung LYA. 2026. Galaxies in the epoch of reionization
are all bark and no bite-plenty of ionizing photons, low escape fractions. The
Astrophysical Journal. 1000(1), 111.
mla: Papovich, Casey, et al. “Galaxies in the Epoch of Reionization Are All Bark
and No Bite-Plenty of Ionizing Photons, Low Escape Fractions.” The Astrophysical
Journal, vol. 1000, no. 1, 111, IOP Publishing, 2026, doi:10.3847/1538-4357/ae3b25.
short: C. Papovich, J.W. Cole, W. Hu, S.L. Finkelstein, L. Shen, P. Arrabal Haro,
R.O. Amorín, B.E. Backhaus, M.B. Bagley, R. Bhatawdekar, A. Calabrò, A.C. Carnall,
N.J. Cleri, E. Daddi, M. Dickinson, N.A. Grogin, B.W. Holwerda, A.E. Jaskot, A.M.
Koekemoer, M. Llerena, R.A. Lucas, S. Mascia, F. Pacucci, L. Pentericci, P.G.
Pérez-González, N. Pirzkal, S. Raghunathan, L.M. Seillé, R.S. Somerville, L.Y.A.
Yung, The Astrophysical Journal 1000 (2026).
date_created: 2026-04-12T22:01:49Z
date_published: 2026-03-20T00:00:00Z
date_updated: 2026-05-04T10:44:57Z
day: '20'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae3b25
external_id:
arxiv:
- '2505.08870'
file:
- access_level: open_access
checksum: 0031a6f197a3fa8c2845de10b6bdc696
content_type: application/pdf
creator: dernst
date_created: 2026-05-04T10:40:07Z
date_updated: 2026-05-04T10:40:07Z
file_id: '21791'
file_name: 2026_AstrophysicalJour_Papovich.pdf
file_size: 6670398
relation: main_file
success: 1
file_date_updated: 2026-05-04T10:40:07Z
has_accepted_license: '1'
intvolume: ' 1000'
issue: '1'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing
photons, low escape fractions
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 1000
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21715'
abstract:
- lang: eng
text: New populations of red active galactic nuclei (known as “little red dots”)
discovered by JWST exhibit remarkable spectral energy distributions. Leveraging
X-ray through far-infrared observations of two of the most luminous known little
red dots, we directly measure their bolometric luminosities. We find evidence
that more than half of the bolometric luminosity likely emerges in the rest-frame
optical, with Lbol/L5100 = 5, roughly half the value for “standard” active galactic
nuclei. Meanwhile, the X-ray emitting corona, UV-emitting blackbody, and reprocessed
mid to far-infrared emission are all considerably subdominant, assuming that the
far-infrared luminosity is well below current measured limits. We present new
bolometric corrections that dramatically lower inferred bolometric luminosities
by a factor of 10 compared to published values in the literature. These bolometric
corrections are in accord with expectations from models in which gas absorption
and reprocessing are responsible for the red rest-frame optical colors of little
red dots. We discuss how this lowered luminosity scale suggests a lower mass scale
for the population by at least an order of magnitude (e.g., ∼105–107 M⊙ black
holes, and ∼108 M⊙ galaxies), alleviating tensions with clustering, overmassive
black holes, and the integrated black hole mass density in the Universe.
acknowledgement: "We benefit from the following JWST programs: UNCOVER (JWST/GO #2561;
Labbé & Bezanson); ALT (JWST-GO #3516; Naidu & Matthee); MegaScience (JWST-GO #4111;
Suess); RUBIES (JWST-GO #4233; de Graaff & Brammer); PRIMER (JWST/GO #1837; Dunlop).\r\n\r\nWe
acknowledge funding from NSF/AAG #2306950, JWST-GO-02561, JWST-GO-03516, and JWST-GO-04111,
provided through a grant from the STScI under NASA contract NAS5-03127. I.L. acknowledges
support from Australian Research Council Future Fellowship FT220100798. K.G. and
T.N. acknowledge support from Australian Research Council Laureate Fellowship FL180100060.
A.Z. acknowledges support by grant No. 2020750 from the United States-Israel Binational
Science Foundation (BSF) and grant No. 2109066 from the United States National Science
Foundation (NSF); by the Ministry of Science & Technology, Israel; and by the Israel
Science Foundation grant No. 864/23. J.M. and I.K. are funded by the European Union
(ERC, AGENTS, 101076224). Views and opinions expressed are, however, those of the
author(s) only and do not necessarily reflect those of the European Union or the
European Research Council. Neither the European Union nor the granting authority
can be held responsible for them. Y.F. acknowledges support from JSPS KAKENHI grant
No. JSPS KAKENHI grant Nos. JP22K21349 and JP23K13149. This work has received funding
from the Swiss State Secretariat for Education, Research and Innovation (SERI) under
contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF)
through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by
the Danish National Research Foundation under grant DNRF140. Support for this work
for RPN was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A
awarded by the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
The work of CCW is supported by NOIRLab, which is managed by the Association of
Universities for Research in Astronomy (AURA) under a cooperative agreement with
the National Science Foundation. J.M. acknowledges funding by the European Union
(ERC, AGENTS, 101076224). R.E.H. acknowledges support by the German Aerospace Center
(DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program
50OR2403 “RUBIES.”"
article_number: '129'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Marta
full_name: Volonteri, Marta
last_name: Volonteri
- first_name: Pratika
full_name: Dayal, Pratika
last_name: Dayal
- first_name: Ivo
full_name: Labbe, Ivo
last_name: Labbe
- first_name: Pieter
full_name: Van Dokkum, Pieter
last_name: Van Dokkum
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Sam E.
full_name: Cutler, Sam E.
last_name: Cutler
- first_name: Karl
full_name: Glazebrook, Karl
last_name: Glazebrook
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Raphael E.
full_name: Hviding, Raphael E.
last_name: Hviding
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Hanpu
full_name: Liu, Hanpu
last_name: Liu
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Richard
full_name: Pan, Richard
last_name: Pan
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Justin S.
full_name: Spilker, Justin S.
last_name: Spilker
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: John R.
full_name: Weaver, John R.
last_name: Weaver
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
- first_name: Adi
full_name: Zitrin, Adi
last_name: Zitrin
citation:
ama: 'Greene JE, Setton DJ, Furtak LJ, et al. What you see is what you get: Empirically
measured bolometric luminosities of Little Red Dots. The Astrophysical Journal.
2026;996(2). doi:10.3847/1538-4357/ae1836'
apa: 'Greene, J. E., Setton, D. J., Furtak, L. J., Naidu, R. P., Volonteri, M.,
Dayal, P., … Zitrin, A. (2026). What you see is what you get: Empirically measured
bolometric luminosities of Little Red Dots. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ae1836'
chicago: 'Greene, Jenny E., David J. Setton, Lukas J. Furtak, Rohan P. Naidu, Marta
Volonteri, Pratika Dayal, Ivo Labbe, et al. “What You See Is What You Get: Empirically
Measured Bolometric Luminosities of Little Red Dots.” The Astrophysical Journal.
IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae1836.'
ieee: 'J. E. Greene et al., “What you see is what you get: Empirically measured
bolometric luminosities of Little Red Dots,” The Astrophysical Journal,
vol. 996, no. 2. IOP Publishing, 2026.'
ista: 'Greene JE, Setton DJ, Furtak LJ, Naidu RP, Volonteri M, Dayal P, Labbe I,
Van Dokkum P, Bezanson R, Brammer G, Cutler SE, Glazebrook K, De Graaff A, Hirschmann
M, Hviding RE, Kokorev V, Leja J, Liu H, Ma Y, Matthee JJ, Nanayakkara T, Oesch
PA, Pan R, Price SH, Spilker JS, Wang B, Weaver JR, Whitaker KE, Williams CC,
Zitrin A. 2026. What you see is what you get: Empirically measured bolometric
luminosities of Little Red Dots. The Astrophysical Journal. 996(2), 129.'
mla: 'Greene, Jenny E., et al. “What You See Is What You Get: Empirically Measured
Bolometric Luminosities of Little Red Dots.” The Astrophysical Journal,
vol. 996, no. 2, 129, IOP Publishing, 2026, doi:10.3847/1538-4357/ae1836.'
short: J.E. Greene, D.J. Setton, L.J. Furtak, R.P. Naidu, M. Volonteri, P. Dayal,
I. Labbe, P. Van Dokkum, R. Bezanson, G. Brammer, S.E. Cutler, K. Glazebrook,
A. De Graaff, M. Hirschmann, R.E. Hviding, V. Kokorev, J. Leja, H. Liu, Y. Ma,
J.J. Matthee, T. Nanayakkara, P.A. Oesch, R. Pan, S.H. Price, J.S. Spilker, B.
Wang, J.R. Weaver, K.E. Whitaker, C.C. Williams, A. Zitrin, The Astrophysical
Journal 996 (2026).
date_created: 2026-04-12T22:01:50Z
date_published: 2026-01-10T00:00:00Z
date_updated: 2026-05-04T11:20:42Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae1836
external_id:
arxiv:
- '2509.05434'
file:
- access_level: open_access
checksum: 7b3cb025d4bcaa35c6e52bd0c8fb6cf4
content_type: application/pdf
creator: dernst
date_created: 2026-05-04T11:19:48Z
date_updated: 2026-05-04T11:19:48Z
file_id: '21792'
file_name: 2026_AstrophysicalJour_Greene.pdf
file_size: 684400
relation: main_file
success: 1
file_date_updated: 2026-05-04T11:19:48Z
has_accepted_license: '1'
intvolume: ' 996'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'What you see is what you get: Empirically measured bolometric luminosities
of Little Red Dots'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 996
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18631'
abstract:
- lang: eng
text: Within the established framework of structure formation, galaxies start as
systems of low stellar mass and gradually grow into far more massive galaxies.
The existence of massive galaxies in the first billion years of the Universe,
as suggested by recent observations, seems to challenge this model, as such galaxies
would require highly efficient conversion of baryons into stars. An even greater
challenge in this epoch is the existence of massive galaxies that have already
ceased forming stars. However, robust detections of early massive quiescent galaxies
have been challenging due to the coarse wavelength sampling of photometric surveys.
Here we report the spectroscopic confirmation with the James Webb Space Telescope
of the quiescent galaxy RUBIES-EGS-QG-1 at redshift z = 4.90, 1.2 billion years
after the Big Bang. Deep stellar absorption features in the spectrum reveal that
the stellar mass of the galaxy of 1011 M⊙ formed in a short 200 Myr burst of star
formation, after which star formation activity dropped rapidly and persistently.
According to current galaxy formation models, systems with such rapid stellar
mass growth and early quenching are too rare to plausibly occur in the small area
probed spectroscopically with JWST. Instead, the discovery of RUBIES-EGS-QG-1
implies that early massive quiescent galaxies can be quenched earlier or exhaust
gas available for star formation more efficiently than assumed at present.
acknowledgement: We thank V. Buat, D. Burgarella and J. Zavala for sharing their NOEMA
data and constraints on the dust-obscured star formation of RUBIES-EGS-QG-1. This
work is partially based on observations carried out under project number W20CK with
the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany)
and IGN (Spain). We thank C. Lagos for providing measurements from the SHARK simulation.
This research was supported by the International Space Science Institute (ISSI)
in Bern, through ISSI International Team Project No. 562. M.V.M., J.L. and B.W.
acknowledge funding support from NASA through JWST-GO-4233. The Cosmic Dawn Center
is funded by the Danish National Research Foundation (Grant No. DNRF140 to G.B.,
P.A.O. and K.E.W.). This work has received funding from the Swiss State Secretariat
for Education, Research and Innovation (Contract No. MB22.00072) and the Swiss National
Science Foundation (Project Grant No. 200020_207349 to P.A.O.). Support for this
work was provided by the Brinson Foundation through a Brinson Prize Fellowship grant
(D.J.S.). K.A.S. is a NHFP Hubble Fellow. Support for this work was provided by
NASA through the NASA Hubble Fellowship Grant No. HST-HF2-51515.001-A awarded by
the Space Telescope Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Incorporated, under NASA contract NAS 5-26555 (R.P.N.).
This work is based on observations made with the NASA/ESA/CSA JWST. The data were
obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science
Institute, which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. The observations in this
work are associated with programmes ERS-1345, GO-2234, DDT-2750 and GO-4233. We
gratefully acknowledge the CEERS and DDT-2750 teams for developing their observing
programme with a zero-exclusive-access period. Open access funding provided by Max
Planck Society.
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Sam
full_name: Cutler, Sam
last_name: Cutler
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Gabriella
full_name: De Lucia, Gabriella
last_name: De Lucia
- first_name: Marijn
full_name: Franx, Marijn
last_name: Franx
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Ian
full_name: Mcconachie, Ian
last_name: Mcconachie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Hans Walter
full_name: Rix, Hans Walter
last_name: Rix
- first_name: Francesco
full_name: Valentino, Francesco
last_name: Valentino
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: De Graaff A, Setton DJ, Brammer G, et al. Efficient formation of a massive
quiescent galaxy at redshift 4.9. Nature Astronomy. 2025;9:280-292. doi:10.1038/s41550-024-02424-3
apa: De Graaff, A., Setton, D. J., Brammer, G., Cutler, S., Suess, K. A., Labbé,
I., … Williams, C. C. (2025). Efficient formation of a massive quiescent galaxy
at redshift 4.9. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-024-02424-3
chicago: De Graaff, Anna, David J. Setton, Gabriel Brammer, Sam Cutler, Katherine
A. Suess, Ivo Labbé, Joel Leja, et al. “Efficient Formation of a Massive Quiescent
Galaxy at Redshift 4.9.” Nature Astronomy. Springer Nature, 2025. https://doi.org/10.1038/s41550-024-02424-3.
ieee: A. De Graaff et al., “Efficient formation of a massive quiescent galaxy
at redshift 4.9,” Nature Astronomy, vol. 9. Springer Nature, pp. 280–292,
2025.
ista: De Graaff A, Setton DJ, Brammer G, Cutler S, Suess KA, Labbé I, Leja J, Weibel
A, Maseda MV, Whitaker KE, Bezanson R, Boogaard LA, Cleri NJ, De Lucia G, Franx
M, Greene JE, Hirschmann M, Matthee JJ, Mcconachie I, Naidu RP, Oesch PA, Price
SH, Rix HW, Valentino F, Wang B, Williams CC. 2025. Efficient formation of a massive
quiescent galaxy at redshift 4.9. Nature Astronomy. 9, 280–292.
mla: De Graaff, Anna, et al. “Efficient Formation of a Massive Quiescent Galaxy
at Redshift 4.9.” Nature Astronomy, vol. 9, Springer Nature, 2025, pp.
280–92, doi:10.1038/s41550-024-02424-3.
short: A. De Graaff, D.J. Setton, G. Brammer, S. Cutler, K.A. Suess, I. Labbé, J.
Leja, A. Weibel, M.V. Maseda, K.E. Whitaker, R. Bezanson, L.A. Boogaard, N.J.
Cleri, G. De Lucia, M. Franx, J.E. Greene, M. Hirschmann, J.J. Matthee, I. Mcconachie,
R.P. Naidu, P.A. Oesch, S.H. Price, H.W. Rix, F. Valentino, B. Wang, C.C. Williams,
Nature Astronomy 9 (2025) 280–292.
date_created: 2024-12-08T23:01:56Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2025-05-19T14:01:21Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1038/s41550-024-02424-3
external_id:
isi:
- '001420347200001'
pmid:
- '39990236'
file:
- access_level: open_access
checksum: fb9109951dfe72f08c04c72cd7cfba69
content_type: application/pdf
creator: dernst
date_created: 2025-04-16T08:53:59Z
date_updated: 2025-04-16T08:53:59Z
file_id: '19574'
file_name: 2025_NatureAstronomy_deGraaff.pdf
file_size: 2034513
relation: main_file
success: 1
file_date_updated: 2025-04-16T08:53:59Z
has_accepted_license: '1'
intvolume: ' 9'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
page: 280-292
pmid: 1
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Efficient formation of a massive quiescent galaxy at redshift 4.9
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 9
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19784'
abstract:
- lang: eng
text: 'We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES)
providing JWST/NIRSpec spectroscopy of red sources selected across ∼150 arcmin2
from public JWST/NIRCam imaging in the UDS and EGS fields. The novel observing
strategy of RUBIES offers a well-quantified selection function. The survey has
been optimised to reach high (>70%) spectroscopic completeness for bright and
red (F150W−F444W>2) sources that are very rare. To place these rare sources in
context, we simultaneously observed a reference sample of the 23 using only the G395M
disperser. The RUBIES data reveal a highly diverse population of red sources that
span a broad redshift range (zspec∼1−9), with photometric redshift scatter and
an outlier fraction that are three times higher than for similarly bright sources
that are less red. This diversity is not apparent from the photometric spectral
energy distributions (SEDs). Only spectroscopy reveals that the SEDs encompass
a mixture of galaxies with dust-obscured star formation, extreme line emission,
a lack of star formation indicating early quenching, and luminous active galactic
nuclei. As a first demonstration of our broader selection function we compared
the stellar masses and rest-frame U−V colours of the red sources and our reference
sample. We find that the red sources are typically more massive (M*∼1010−11.5 M⊙)
across all redshifts. However, we also find that the most massive systems span
a wide range in U−V colour. We describe our data reduction procedure and data
quality, and we publicly release the reduced RUBIES data and vetted spectroscopic
redshifts of the first half of the survey through the DAWN JWST Archive.'
acknowledgement: 'We thank the CEERS and PRIMER teams for making their imaging data
publicly available immediately. This work is based on observations made with the
NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski
Archive for Space Telescopes at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-03127 for JWST. These observations are associated with programs
#1345, #1837 #2234, #2279, #2514, #2750, #3990 and #4233. Support for program #4233
was provided by NASA through a grant from the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127. REH acknowledges support by the German Aerospace
Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through
program 50OR2403 ‘RUBIES’. This research was supported by the International Space
Science Institute (ISSI) in Bern, through ISSI International Team project #562.
The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF)
under grant #140. This work has received funding from the Swiss State Secretariat
for Education, Research and Innovation (SERI) under contract number MB22.00072,
as well as from the Swiss National Science Foundation (SNSF) through project grant
200020_207349. Support for this work for RPN was provided by NASA through the NASA
Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555. Open Access funding provided
by Max Planck Society.'
article_number: A189
article_processing_charge: Yes
article_type: original
author:
- first_name: Anna
full_name: de Graaff, Anna
last_name: de Graaff
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Zach
full_name: Lewis, Zach
last_name: Lewis
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Olivia R.
full_name: Cooper, Olivia R.
last_name: Cooper
- first_name: Rashmi
full_name: Gottumukkala, Rashmi
last_name: Gottumukkala
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Raphael E.
full_name: Hviding, Raphael E.
last_name: Hviding
- first_name: Harley
full_name: Katz, Harley
last_name: Katz
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Ian
full_name: McConachie, Ian
last_name: McConachie
- first_name: Tim B.
full_name: Miller, Tim B.
last_name: Miller
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Hans-Walter
full_name: Rix, Hans-Walter
last_name: Rix
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: 'de Graaff A, Brammer G, Weibel A, et al. RUBIES: A complete census of the
bright and red distant universe with JWST/NIRSpec. Astronomy & Astrophysics.
2025;697. doi:10.1051/0004-6361/202452186'
apa: 'de Graaff, A., Brammer, G., Weibel, A., Lewis, Z., Maseda, M. V., Oesch, P.
A., … Williams, C. C. (2025). RUBIES: A complete census of the bright and red
distant universe with JWST/NIRSpec. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202452186'
chicago: 'Graaff, Anna de, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V.
Maseda, Pascal A. Oesch, Rachel Bezanson, et al. “RUBIES: A Complete Census of
the Bright and Red Distant Universe with JWST/NIRSpec.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452186.'
ieee: 'A. de Graaff et al., “RUBIES: A complete census of the bright and
red distant universe with JWST/NIRSpec,” Astronomy & Astrophysics,
vol. 697. EDP Sciences, 2025.'
ista: 'de Graaff A, Brammer G, Weibel A, Lewis Z, Maseda MV, Oesch PA, Bezanson
R, Boogaard LA, Cleri NJ, Cooper OR, Gottumukkala R, Greene JE, Hirschmann M,
Hviding RE, Katz H, Labbé I, Leja J, Matthee JJ, McConachie I, Miller TB, Naidu
RP, Price SH, Rix H-W, Setton DJ, Suess KA, Wang B, Whitaker KE, Williams CC.
2025. RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec.
Astronomy & Astrophysics. 697, A189.'
mla: 'de Graaff, Anna, et al. “RUBIES: A Complete Census of the Bright and Red Distant
Universe with JWST/NIRSpec.” Astronomy & Astrophysics, vol. 697, A189,
EDP Sciences, 2025, doi:10.1051/0004-6361/202452186.'
short: A. de Graaff, G. Brammer, A. Weibel, Z. Lewis, M.V. Maseda, P.A. Oesch, R.
Bezanson, L.A. Boogaard, N.J. Cleri, O.R. Cooper, R. Gottumukkala, J.E. Greene,
M. Hirschmann, R.E. Hviding, H. Katz, I. Labbé, J. Leja, J.J. Matthee, I. McConachie,
T.B. Miller, R.P. Naidu, S.H. Price, H.-W. Rix, D.J. Setton, K.A. Suess, B. Wang,
K.E. Whitaker, C.C. Williams, Astronomy & Astrophysics 697 (2025).
date_created: 2025-06-03T08:59:52Z
date_published: 2025-05-19T00:00:00Z
date_updated: 2025-09-30T12:45:25Z
day: '19'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202452186
external_id:
isi:
- '001490583400004'
file:
- access_level: open_access
checksum: cccf44629f28535dde91f2ebdf38c054
content_type: application/pdf
creator: dernst
date_created: 2025-06-03T09:25:49Z
date_updated: 2025-06-03T09:25:49Z
file_id: '19788'
file_name: 2025_AstronomyAstrophysics_deGraaff.pdf
file_size: 6874721
relation: main_file
success: 1
file_date_updated: 2025-06-03T09:25:49Z
has_accepted_license: '1'
intvolume: ' 697'
isi: 1
language:
- iso: eng
month: '05'
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: 'RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 697
year: '2025'
...
---
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. Astronomy & Astrophysics. 2025;696.
doi:10.1051/0004-6361/202451723'
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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451723'
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.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202451723.'
ieee: 'G. Östlin 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,” Astronomy & Astrophysics, 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 & 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.” Astronomy & Astrophysics, vol. 696, A57, EDP Sciences,
2025, doi:10.1051/0004-6361/202451723.'
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 & 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'
file:
- access_level: open_access
checksum: 67600eba8bda24987a130ac334f10456
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T07:46:01Z
date_updated: 2025-06-23T07:46:01Z
file_id: '19865'
file_name: 2025_AstronomyAstrophysics_Oestlin.pdf
file_size: 15858045
relation: main_file
success: 1
file_date_updated: 2025-06-23T07:46:01Z
has_accepted_license: '1'
intvolume: ' 696'
isi: 1
language:
- iso: eng
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:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 696
year: '2025'
...
---
OA_place: publisher
OA_type: gold
_id: '19855'
abstract:
- lang: eng
text: We present indirect constraints on the absolute escape fraction of ionizing
photons (f_{\rm esc}^{\rm LyC}) of the system GN 42912 which comprises two luminous
galaxies (M_{\rm UV} magnitudes of -20.89 and -20.37) at z\sim7.5, GN 42912-NE
and GN 42912-SW, to determine their contribution to the ionizing photon budget
of the Epoch of Reionization (EoR). The high-resolution James Webb Space Telescope
NIRSpec and NIRCam observations reveal the two galaxies are separated by only
~0.1" (0.5 kpc) on the sky and have a 358 km s^{-1} velocity separation. GN 42912-NE
and GN 42912-SW are relatively massive for this redshift (log(M_\ast/M_\odot)
\sim 8.4 and 8.9, respectively), with gas-phase metallicities of 18 per cent and
23 per cent solar, O_{32} ratios of 5.3 and >5.8, and \beta slopes of -1.92 and
-1.51, respectively. We use the Mg II\lambda\lambda2796,2803 doublet to constrain
f_{\rm esc}^{\rm LyC}. Mg II has an ionization potential close to that of neutral
hydrogen and, in the optically thin regime, can be used as an indirect tracer
of the LyC leakage. We establish realistic conservative upper limits on f_{\rm
esc}^{\rm LyC} of 8.5 per cent for GN 42912-NE and 14 per cent for GN 42912-SW.
These estimates align with f_{\rm esc}^{\rm LyC} trends observed with \beta, O_{32},
and the H\beta equivalent width at z<4. The small inferred ionized region sizes
(<0.3 pMpc) around both galaxies indicate they have not ionized a significant
fraction of the surrounding neutral gas. While these z>7 f_{\rm esc}^{\rm LyC}
constraints do not decisively determine a specific reionization model, they support
a minor contribution from these two relatively luminous galaxies to the EoR.
acknowledgement: 'This work is based on observations made with the NASA/ESA/CSA JWST.
The data were obtained from the Mikulski Archive for Space Telescopes at the Space
Telescope Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5–03127 for JWST. These
observations are associated with program #01871. Support for program #01871 was
provided by NASA through a grant from the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS 5–03127. SG is grateful for the support enabled by the Harlan
J. Smith McDonald fellowship. YI and NG acknowledge support from the Simons Foundation
and the National Academy of Sciences of Ukraine (Project 0121U109612). ASL acknowledges
support from Knut and Alice Wallenberg Foundation.'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: S.
full_name: Gazagnes, S.
last_name: Gazagnes
- first_name: J.
full_name: Chisholm, J.
last_name: Chisholm
- first_name: R.
full_name: Endsley, R.
last_name: Endsley
- first_name: D. A.
full_name: Berg, D. A.
last_name: Berg
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: N.
full_name: Jurlin, N.
last_name: Jurlin
- first_name: A.
full_name: Saldana-Lopez, A.
last_name: Saldana-Lopez
- first_name: S. L.
full_name: Finkelstein, S. L.
last_name: Finkelstein
- first_name: S. R.
full_name: Flury, S. R.
last_name: Flury
- first_name: N. G.
full_name: Guseva, N. G.
last_name: Guseva
- first_name: A.
full_name: Henry, A.
last_name: Henry
- first_name: Y. I.
full_name: Izotov, Y. I.
last_name: Izotov
- first_name: I.
full_name: Jung, I.
last_name: Jung
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: D.
full_name: Schaerer, D.
last_name: Schaerer
citation:
ama: Gazagnes S, Chisholm J, Endsley R, et al. A negligible contribution of two
luminous z ∼7.5 galaxies to the ionizing photon budget of reionization. Monthly
Notices of the Royal Astronomical Society. 2025;540(3):2331-2348. doi:10.1093/mnras/staf768
apa: Gazagnes, S., Chisholm, J., Endsley, R., Berg, D. A., Leclercq, F., Jurlin,
N., … Schaerer, D. (2025). A negligible contribution of two luminous z ∼7.5 galaxies
to the ionizing photon budget of reionization. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf768
chicago: Gazagnes, S., J. Chisholm, R. Endsley, D. A. Berg, F. Leclercq, N. Jurlin,
A. Saldana-Lopez, et al. “A Negligible Contribution of Two Luminous z ∼7.5 Galaxies
to the Ionizing Photon Budget of Reionization.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf768.
ieee: S. Gazagnes et al., “A negligible contribution of two luminous z ∼7.5
galaxies to the ionizing photon budget of reionization,” Monthly Notices of
the Royal Astronomical Society, vol. 540, no. 3. Oxford University Press,
pp. 2331–2348, 2025.
ista: Gazagnes S, Chisholm J, Endsley R, Berg DA, Leclercq F, Jurlin N, Saldana-Lopez
A, Finkelstein SL, Flury SR, Guseva NG, Henry A, Izotov YI, Jung I, Matthee JJ,
Schaerer D. 2025. A negligible contribution of two luminous z ∼7.5 galaxies to
the ionizing photon budget of reionization. Monthly Notices of the Royal Astronomical
Society. 540(3), 2331–2348.
mla: Gazagnes, S., et al. “A Negligible Contribution of Two Luminous z ∼7.5 Galaxies
to the Ionizing Photon Budget of Reionization.” Monthly Notices of the Royal
Astronomical Society, vol. 540, no. 3, Oxford University Press, 2025, pp.
2331–48, doi:10.1093/mnras/staf768.
short: S. Gazagnes, J. Chisholm, R. Endsley, D.A. Berg, F. Leclercq, N. Jurlin,
A. Saldana-Lopez, S.L. Finkelstein, S.R. Flury, N.G. Guseva, A. Henry, Y.I. Izotov,
I. Jung, J.J. Matthee, D. Schaerer, Monthly Notices of the Royal Astronomical
Society 540 (2025) 2331–2348.
date_created: 2025-06-22T22:02:05Z
date_published: 2025-07-01T00:00:00Z
date_updated: 2025-09-30T13:34:20Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1093/mnras/staf768
external_id:
arxiv:
- '2410.03337'
isi:
- '001506103600001'
file:
- access_level: open_access
checksum: f912c990a0474f1ddf9be6b8a89c7759
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T11:02:59Z
date_updated: 2025-06-23T11:02:59Z
file_id: '19870'
file_name: 2025_MonthlyNoticesRAS_Gazagnes.pdf
file_size: 3111567
relation: main_file
success: 1
file_date_updated: 2025-06-23T11:02:59Z
has_accepted_license: '1'
intvolume: ' 540'
isi: 1
issue: '3'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
page: 2331-2348
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon
budget of reionization
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 540
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19929'
abstract:
- lang: eng
text: "Context. The observed Lyman-alpha (Lyα) line profile is a convolution of
the complex Lyα radiative transfer taking place in the interstellar, circumgalactic,
and intergalactic media (ISM, CGM, and IGM, respectively). Discerning the different
components of the Lyα line is crucial in order to use it as a probe of galaxy
formation or the evolution of the IGM.\r\n\r\nAims. We aim to present the second
version of zELDA (redshift Estimator for Line profiles of Distant Lyman-Alpha
emitters), an open-source Python module focused on modelling and fitting observed
Lyα line profiles. This new version of zELDA focuses on disentangling the galactic
from the IGM effects.\r\n\r\nMethods. We built realistic Lyα line profiles that
include the ISM and IGM contributions by combining the Monte Carlo radiative-transfer
simulations for the so-called shell model (ISM) and IGM transmission curves generated
from TNG100. We used these mock line profiles to train different artificial neural
networks. These use the observed spectrum as input and the outflow parameters
of the best fitting ‘shell model’ as output along with the redshift and Lyα emission
IGM escape fraction of the source.\r\n\r\nResults. We measured the accuracy of
zELDA on mock Lyα line profiles. We find that zELDA is capable of reconstructing
the ISM emerging Lyα line profile with high levels of accuracy (Kolmogórov-Smirnov<0.1)
for 95% of the cases for HST/COS-like observations and 80% for MUSE-WIDE-like
observations. zELDA is able to measure the IGM transmission with typical uncertainties
below 10% for HST/COS and MUSE-WIDE data.\r\n\r\nConclusions. This work represents
a step forward in the high-precision reconstruction of IGM-attenuated Lyα line
profiles. zELDA allows the disentanglement of the galactic and IGM contribution
shaping the Lyα line shape and thus allows us to use Lyα as a tool to study galaxy
and ISM evolution."
acknowledgement: The authors acknowledge the financial support from the MICIU with
funding from the European Union NextGenerationEU and Generalitat Valenciana in the
call Programa de Planes Complementarios de I+D+i (PRTR 2022) Project (VAL-JPAS),
reference ASFAE/2022/025. This work is part of the research Project PID2023-149420NB-I00
funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU. This work is also supported
by the project of excellence PROMETEO CIPROM/2023/21 of the Conselleria de Educación,
Universidades y Empleo (Generalitat Valenciana). MG thanks the Max Planck Society
for support through the Max Planck Research Group. DS acknowledges the support by
the Tsinghua Shui Mu Scholarship, funding of the National Key R&D Program of China
(grant no. 2023YFA1605600), the science research grants from the China Manned Space
Project with no. CMS-CSST2021-A05, and the Tsinghua University Initiative Scientific
Research Program (no. 20223080023). This research made use of matplotlib, a Python
library for publication quality graphics (Hunter 2007), NumPy (Harris et al. 2020)
and SciPy (Virtanen et al. 2020).
article_number: A139
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Siddhartha
full_name: Gurung-López, Siddhartha
last_name: Gurung-López
- first_name: Chris
full_name: Byrohl, Chris
last_name: Byrohl
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Daniele
full_name: Spinoso, Daniele
last_name: Spinoso
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Alberto
full_name: Fernández-Soto, Alberto
last_name: Fernández-Soto
- first_name: Pablo
full_name: Arnalte-Mur, Pablo
last_name: Arnalte-Mur
- first_name: Vicent J.
full_name: Martínez, Vicent J.
last_name: Martínez
citation:
ama: 'Gurung-López S, Byrohl C, Gronke M, et al. zELDA II: Reconstruction of galactic
Lyman-alpha spectra attenuated by the intergalactic medium using neural networks.
Astronomy & Astrophysics. 2025;698. doi:10.1051/0004-6361/202453547'
apa: 'Gurung-López, S., Byrohl, C., Gronke, M., Spinoso, D., Torralba Torregrosa,
A., Fernández-Soto, A., … Martínez, V. J. (2025). zELDA II: Reconstruction of
galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural
networks. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202453547'
chicago: 'Gurung-López, Siddhartha, Chris Byrohl, Max Gronke, Daniele Spinoso, Alberto
Torralba Torregrosa, Alberto Fernández-Soto, Pablo Arnalte-Mur, and Vicent J.
Martínez. “ZELDA II: Reconstruction of Galactic Lyman-Alpha Spectra Attenuated
by the Intergalactic Medium Using Neural Networks.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202453547.'
ieee: 'S. Gurung-López et al., “zELDA II: Reconstruction of galactic Lyman-alpha
spectra attenuated by the intergalactic medium using neural networks,” Astronomy
& Astrophysics, vol. 698. EDP Sciences, 2025.'
ista: 'Gurung-López S, Byrohl C, Gronke M, Spinoso D, Torralba Torregrosa A, Fernández-Soto
A, Arnalte-Mur P, Martínez VJ. 2025. zELDA II: Reconstruction of galactic Lyman-alpha
spectra attenuated by the intergalactic medium using neural networks. Astronomy
& Astrophysics. 698, A139.'
mla: 'Gurung-López, Siddhartha, et al. “ZELDA II: Reconstruction of Galactic Lyman-Alpha
Spectra Attenuated by the Intergalactic Medium Using Neural Networks.” Astronomy
& Astrophysics, vol. 698, A139, EDP Sciences, 2025, doi:10.1051/0004-6361/202453547.'
short: S. Gurung-López, C. Byrohl, M. Gronke, D. Spinoso, A. Torralba Torregrosa,
A. Fernández-Soto, P. Arnalte-Mur, V.J. Martínez, Astronomy & Astrophysics
698 (2025).
date_created: 2025-06-29T22:01:15Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:11:56Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202453547
external_id:
arxiv:
- '2501.04077'
isi:
- '001507317300003'
file:
- access_level: open_access
checksum: a50a817b72f03534c6a867035b51e433
content_type: application/pdf
creator: dernst
date_created: 2025-06-30T08:28:40Z
date_updated: 2025-06-30T08:28:40Z
file_id: '19933'
file_name: 2025_AstronomyAstrophysics_GurungLopez.pdf
file_size: 5758102
relation: main_file
success: 1
file_date_updated: 2025-06-30T08:28:40Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
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: 'zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the
intergalactic medium using neural networks'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 698
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19930'
abstract:
- lang: eng
text: We present an analysis of the UV continuum slope, β, using a sample of 726
galaxies with z > 4, selected from a mixture of JWST ERS, GTO, and GO observational
programs. We considered only spectroscopic data obtained with the low-resolution
(R ∼ 30 − 300) PRISM/CLEAR NIRSpec configuration. Studying the correlation between
β and MUV, we find an overall decreasing trend, described by β = ( − 0.055 ± 0.017)MUV + ( − 2.98 ± 0.34).
This is consistent with previous studies, where brighter galaxies show redder
β values. However, when analyzing the trend in separate redshift bins, we find
that at high redshift the relation becomes much flatter and is consistent with
a flat slope within 1σ. Furthermore, we find that β tends to decrease with redshift,
following β = ( − 0.075 ± 0.010)z + ( − 1.496 ± 0.056). This is consistent with
most recent results showing a steepening of the spectra at higher z. We selected
a sample of galaxies with extremely blue slopes (i.e., β < −2.6). Such slopes
are steeper than predicted by stellar evolution models – even for dust-free, young,
metal-poor populations – when the contribution of nebular emission is included.
We selected 44 extremely blue galaxies (XBGs) and investigated the possible physical
origin of their steep slopes by comparing them to a subsample of redder galaxies
(matched in Δz = ±0.5 and ΔMUV = ±0.2). We find that XBGs have younger stellar
populations, stronger ionization fields, lower dust attenuation, and lower but
not pristine metallicity (∼10% Z⊙) compared to red galaxies. However, these properties
alone cannot explain the extreme β values. Using indirect inference of Lyman continuum
escape with the most recent models, we estimated the escape fraction fesc > 10%
in at least 25% of the XBGs, whereas all the red sources exhibit much lower fesc
values. A reduced nebular continuum contribution – resulting from either a high
escape fraction or a bursty star formation history – is likely the origin of the
extremely blue slopes.
acknowledgement: We acknowledges support from the INAF Large Grant for Extragalactic
Surveys with JWST and from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And
Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. PS acknowledges
INAF Mini Grant 2022 “The evolution of passive galaxies through cosmic time”. Part
of the research activities described in this paper were carried out with the contribution
of the Next Generation EU funds within the National Recovery and Resilience Plan
(PNRR), Mission 4 – Education and Research, Component 2 – From Research to Business
(M4C2), Investment Line 3.1 – Strengthening and creation of Research Infrastructures,
Project IR0000034 – “STILES – Strengthening the Italian Leadership in ELT and SKA”.
RA acknowledges support of Grant project PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033
and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103.
article_number: A234
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: D.
full_name: Dottorini, D.
last_name: Dottorini
- first_name: A.
full_name: Calabrò, A.
last_name: Calabrò
- first_name: L.
full_name: Pentericci, L.
last_name: Pentericci
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: M.
full_name: Llerena, M.
last_name: Llerena
- first_name: L.
full_name: Napolitano, L.
last_name: Napolitano
- first_name: P.
full_name: Santini, P.
last_name: Santini
- first_name: G.
full_name: Roberts-Borsani, G.
last_name: Roberts-Borsani
- first_name: M.
full_name: Castellano, M.
last_name: Castellano
- first_name: R.
full_name: Amorin, R.
last_name: Amorin
- first_name: M.
full_name: Dickinson, M.
last_name: Dickinson
- first_name: A.
full_name: Fontana, A.
last_name: Fontana
- first_name: N.
full_name: Hathi, N.
last_name: Hathi
- first_name: M.
full_name: Hirschmann, M.
last_name: Hirschmann
- first_name: A. M.
full_name: Koekemoer, A. M.
last_name: Koekemoer
- first_name: R. A.
full_name: Lucas, R. A.
last_name: Lucas
- first_name: E.
full_name: Merlin, E.
last_name: Merlin
- first_name: A.
full_name: Morales, A.
last_name: Morales
- first_name: F.
full_name: Pacucci, F.
last_name: Pacucci
- first_name: S.
full_name: Wilkins, S.
last_name: Wilkins
- first_name: P.
full_name: Arrabal Haro, P.
last_name: Arrabal Haro
- first_name: M.
full_name: Bagley, M.
last_name: Bagley
- first_name: S. L.
full_name: Finkelstein, S. L.
last_name: Finkelstein
- first_name: J.
full_name: Kartaltepe, J.
last_name: Kartaltepe
- first_name: C.
full_name: Papovich, C.
last_name: Papovich
- first_name: N.
full_name: Pirzkal, N.
last_name: Pirzkal
citation:
ama: 'Dottorini D, Calabrò A, Pentericci L, et al. Evolution of the UV slope of
galaxies at cosmic morning (z > 4): The properties of extremely blue galaxies.
Astronomy & Astrophysics. 2025;698. doi:10.1051/0004-6361/202453267'
apa: 'Dottorini, D., Calabrò, A., Pentericci, L., Mascia, S., Llerena, M., Napolitano,
L., … Pirzkal, N. (2025). Evolution of the UV slope of galaxies at cosmic morning
(z > 4): The properties of extremely blue galaxies. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202453267'
chicago: 'Dottorini, D., A. Calabrò, L. Pentericci, Sara Mascia, M. Llerena, L.
Napolitano, P. Santini, et al. “Evolution of the UV Slope of Galaxies at Cosmic
Morning (z > 4): The Properties of Extremely Blue Galaxies.” Astronomy
& Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202453267.'
ieee: 'D. Dottorini et al., “Evolution of the UV slope of galaxies at cosmic
morning (z > 4): The properties of extremely blue galaxies,” Astronomy
& Astrophysics, vol. 698. EDP Sciences, 2025.'
ista: 'Dottorini D, Calabrò A, Pentericci L, Mascia S, Llerena M, Napolitano L,
Santini P, Roberts-Borsani G, Castellano M, Amorin R, Dickinson M, Fontana A,
Hathi N, Hirschmann M, Koekemoer AM, Lucas RA, Merlin E, Morales A, Pacucci F,
Wilkins S, Arrabal Haro P, Bagley M, Finkelstein SL, Kartaltepe J, Papovich C,
Pirzkal N. 2025. Evolution of the UV slope of galaxies at cosmic morning (z >
4): The properties of extremely blue galaxies. Astronomy & Astrophysics. 698,
A234.'
mla: 'Dottorini, D., et al. “Evolution of the UV Slope of Galaxies at Cosmic Morning
(z > 4): The Properties of Extremely Blue Galaxies.” Astronomy & Astrophysics,
vol. 698, A234, EDP Sciences, 2025, doi:10.1051/0004-6361/202453267.'
short: D. Dottorini, A. Calabrò, L. Pentericci, S. Mascia, M. Llerena, L. Napolitano,
P. Santini, G. Roberts-Borsani, M. Castellano, R. Amorin, M. Dickinson, A. Fontana,
N. Hathi, M. Hirschmann, A.M. Koekemoer, R.A. Lucas, E. Merlin, A. Morales, F.
Pacucci, S. Wilkins, P. Arrabal Haro, M. Bagley, S.L. Finkelstein, J. Kartaltepe,
C. Papovich, N. Pirzkal, Astronomy & Astrophysics 698 (2025).
date_created: 2025-06-29T22:01:15Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:11:39Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202453267
external_id:
arxiv:
- '2412.01623'
isi:
- '001510826300019'
file:
- access_level: open_access
checksum: 100f897d468de9d0113277c870035b62
content_type: application/pdf
creator: dernst
date_created: 2025-06-30T08:22:08Z
date_updated: 2025-06-30T08:22:08Z
file_id: '19932'
file_name: 2025_AstronomyAstrophysics_Dottorini.pdf
file_size: 2442076
relation: main_file
success: 1
file_date_updated: 2025-06-30T08:22:08Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
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: 'Evolution of the UV slope of galaxies at cosmic morning (z > 4): The properties
of extremely blue galaxies'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 698
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19931'
abstract:
- lang: eng
text: JWST observations have uncovered a new population of red, compact objects
at high redshifts dubbed “little red dots” (LRDs), which typically show broad
emission lines and are thought to be dusty active galactic nuclei (AGNs). Some
of their other features, however, challenge the AGN explanation, such as prominent
Balmer breaks and extremely faint or even missing metal high-ionization lines,
X-ray, or radio emission, including in deep stacks. Time variability is another
robust test of AGN activity. Here, we exploit the z = 7.045 multiply imaged LRD
A2744-QSO1, which offers a particularly unique test of variability due to lensing-induced
time delays between the three images spanning 22 yr (2.7 yr in the rest-frame),
to investigate its photometric and spectroscopic variability. We find the equivalent
widths (EWs) of the broad Hα and Hβ lines, which are independent of magnification
and other systematics, to exhibit significant variations, of up to 18 ± 3% for
Hα and up to 22 ± 8% in Hβ, on a timescale of 875 d (2.4 yr) in the rest-frame.
This suggests that A2744-QSO1 is indeed an AGN. We find no significant photometric
variability beyond the limiting systematic uncertainties, so it currently cannot
be determined whether the EW variations are due to line-flux or continuum variability.
These results are consistent with a typical damped random walk variability model
for an AGN such as A2744-QSO1 (MBH = 4 × 107 M⊙) given the sparse sampling of
the light curve with the available data. Our results therefore support the AGN
interpretation of this LRD, and highlight the need for further photometric and
spectroscopic monitoring in order to build a detailed and reliable light curve.
acknowledgement: 'We would like to thank Xihan Ji, Hannah Übler, and Roberto Maiolino,
for cordial and useful discussions. The BGU lensing group acknowledges support by
grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF)
and grant No. 2109066 from the United States National Science Foundation (NSF),
and by the Israel Science Foundation Grant No. 864/23. P.D. warmly thanks the European
Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. This
work is based on observations obtained with the NASA/ESA/CSA JWST, namely programs
GO-2756, -2561, -2883, -3538, -4111, and -3516, retrieved from the Mikulski Archive
for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI
is operated by the Association of Universities for Research in Astronomy, Inc. under
NASA contract NAS 5-26555. The spectroscopy products presented herein, from JWST
program GO-2561, were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative
of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research
Foundation under grant DNRF140. The data used in this work may be retrieved from
the MAST archive at: http://dx.doi.org/10.17909/p7t7-te67. This work also makes
use of the Center for Computational Astrophysics at the Flatiron Institute which
is supported by the Simons Foundation. Support for JWST programs GO-2561, -4111,
and -3516 was provided by NASA through grants from STScI. This research made use
of Astropy, (http://www.astropy.org) a community-developed core Python package for
Astronomy (Astropy Collaboration 2013, 2018) and Photutils, an Astropy package for
detection and photometry of astronomical sources (Bradley et al. 2024), as well
as the packages NumPy (van der Walt et al. 2011), SciPy (Virtanen et al. 2020),
Matplotlib (Hunter 2007), and the MAAT Astronomy and Astrophysics tools for MATLAB
(Ofek 2014).'
article_number: A227
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Amy R.
full_name: Secunda, Amy R.
last_name: Secunda
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Adi
full_name: Zitrin, Adi
last_name: Zitrin
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- first_name: Miriam
full_name: Golubchik, Miriam
last_name: Golubchik
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Hakim
full_name: Atek, Hakim
last_name: Atek
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Iryna
full_name: Chemerynska, Iryna
last_name: Chemerynska
- first_name: Sam E.
full_name: Cutler, Sam E.
last_name: Cutler
- first_name: Pratika
full_name: Dayal, Pratika
last_name: Dayal
- first_name: Robert
full_name: Feldmann, Robert
last_name: Feldmann
- first_name: Seiji
full_name: Fujimoto, Seiji
last_name: Fujimoto
- first_name: Karl
full_name: Glazebrook, Karl
last_name: Glazebrook
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Erica J.
full_name: Nelson, Erica J.
last_name: Nelson
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Richard
full_name: Pan, Richard
last_name: Pan
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: John R.
full_name: Weaver, John R.
last_name: Weaver
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
citation:
ama: Furtak LJ, Secunda AR, Greene JE, et al. Investigating photometric and spectroscopic
variability in the multiply imaged little red dot A2744-QSO1. Astronomy &
Astrophysics. 2025;698. doi:10.1051/0004-6361/202554110
apa: Furtak, L. J., Secunda, A. R., Greene, J. E., Zitrin, A., Labbé, I., Golubchik,
M., … Whitaker, K. E. (2025). Investigating photometric and spectroscopic variability
in the multiply imaged little red dot A2744-QSO1. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202554110
chicago: Furtak, Lukas J., Amy R. Secunda, Jenny E. Greene, Adi Zitrin, Ivo Labbé,
Miriam Golubchik, Rachel Bezanson, et al. “Investigating Photometric and Spectroscopic
Variability in the Multiply Imaged Little Red Dot A2744-QSO1.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202554110.
ieee: L. J. Furtak et al., “Investigating photometric and spectroscopic variability
in the multiply imaged little red dot A2744-QSO1,” Astronomy & Astrophysics,
vol. 698. EDP Sciences, 2025.
ista: Furtak LJ, Secunda AR, Greene JE, Zitrin A, Labbé I, Golubchik M, Bezanson
R, Kokorev V, Atek H, Brammer GB, Chemerynska I, Cutler SE, Dayal P, Feldmann
R, Fujimoto S, Glazebrook K, Leja J, Ma Y, Matthee JJ, Naidu RP, Nelson EJ, Oesch
PA, Pan R, Price SH, Suess KA, Wang B, Weaver JR, Whitaker KE. 2025. Investigating
photometric and spectroscopic variability in the multiply imaged little red dot
A2744-QSO1. Astronomy & Astrophysics. 698, A227.
mla: Furtak, Lukas J., et al. “Investigating Photometric and Spectroscopic Variability
in the Multiply Imaged Little Red Dot A2744-QSO1.” Astronomy & Astrophysics,
vol. 698, A227, EDP Sciences, 2025, doi:10.1051/0004-6361/202554110.
short: L.J. Furtak, A.R. Secunda, J.E. Greene, A. Zitrin, I. Labbé, M. Golubchik,
R. Bezanson, V. Kokorev, H. Atek, G.B. Brammer, I. Chemerynska, S.E. Cutler, P.
Dayal, R. Feldmann, S. Fujimoto, K. Glazebrook, J. Leja, Y. Ma, J.J. Matthee,
R.P. Naidu, E.J. Nelson, P.A. Oesch, R. Pan, S.H. Price, K.A. Suess, B. Wang,
J.R. Weaver, K.E. Whitaker, Astronomy & Astrophysics 698 (2025).
date_created: 2025-06-29T22:01:16Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:11:22Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202554110
external_id:
arxiv:
- '2502.07875'
isi:
- '001510826300017'
file:
- access_level: open_access
checksum: 567fa02a9791d489355ec75d02bb1cb9
content_type: application/pdf
creator: dernst
date_created: 2025-06-30T08:44:24Z
date_updated: 2025-06-30T08:44:24Z
file_id: '19934'
file_name: 2025_AstronomyAstrophysics_Furtak.pdf
file_size: 1835865
relation: main_file
success: 1
file_date_updated: 2025-06-30T08:44:24Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
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: Investigating photometric and spectroscopic variability in the multiply imaged
little red dot A2744-QSO1
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 698
year: '2025'
...