---
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
relation: main_file
success: 1
file_date_updated: 2026-02-16T07:35:03Z
has_accepted_license: '1'
intvolume: ' 705'
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
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'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21160'
abstract:
- lang: eng
text: "Context. AM Canum Venaticorum (AM CVn) stars are ultra-compact binary systems
composed of a white dwarf primary accreting from a hydrogen-deficient donor. They
play a crucial role in astrophysics as potential progenitors of Type Ia supernovae
and as laboratories for gravitational wave studies. However, their formation and
evolutionary history remain incomplete. Three formation channels have been discussed
in the literature: the white dwarf, He-star, and cataclysmic variable channels.\r\n\r\nAims.
The chemical composition of the accretor atmosphere reflects the material transferred
from the donor. In this work we took the first accurate measurements of the fundamental
parameters of the accreting white dwarf in ZTF J225237.05−051917.4, including
the abundances of key elements such as carbon, nitrogen, and silicon, by analysing
ultraviolet spectra obtained with the Hubble Space Telescope (HST). These measurements
provide new insight into the evolutionary history of the system and, together
with existing optical observations, establish it as a benchmark to develop our
pipeline, paving the way for its application to a larger sample of AM CVn systems.\r\n\r\nMethods.
We determined the binary parameters through photometric analysis and constrained
the atmospheric parameters of the white dwarf accretor, including its effective
temperature, surface gravity, and chemical abundances, by fitting the HST ultraviolet
spectrum with synthetic spectral models. We then inferred the system’s formation
channel by comparing the results with theoretical evolutionary models.\r\n\r\nResults.
According to our measurements, the accretor’s effective temperature (Teff) is
23 300 ± 600 K and the surface gravity (log g) is 8.4 ± 0.3, which imply an accretor
mass (MWD) of 0.86 ± 0.16 M⊙. We find a high nitrogen-to-carbon abundance ratio
by mass of > 153.\r\n\r\nConclusions. The accretor is significantly hotter than
previous estimates based on simplified blackbody fits to the spectral energy distribution,
underscoring the importance of detailed spectral modelling for accurately determining
system parameters. Our results show that ultraviolet spectroscopy is well suited
to constraining the formation channels of AM CVn systems. Of the three proposed
formation channels, the He-star channel can be excluded given the high nitrogen-to-carbon
ratio. Our results are consistent with both the white dwarf and cataclysmic variable
channels."
acknowledgement: "We thank Lars Bildsten for valuable insights and discussions. We
acknowledge with thanks the variable star observations from the\r\nAAVSO International
Database contributed by observers worldwide and used in this research. We thank
the members of the Spanish Observers of Supernovae\r\n(ObSN) group for their valuable
photometric contributions. This research was\r\nsupported by Deutsche Forschungsgemeinschaft
(DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC 2121
“Quantum Universe”\r\n– 390833306. Co-funded by the European Union (ERC, CompactBINARIES,\r\n101078773).
Views and opinions expressed are however those of the author(s)\r\nonly and do not
necessarily reflect those of the European Union or the European Research Council.
Neither the European Union nor the granting authority\r\ncan be held responsible
for them. DB acknowledges support from the São Paulo\r\nResearch Foundation (FAPESP),
Brazil, Process Numbers #2024/03736-2 and\r\n#2025/00817-4. MRS is supported by
Fondecyt (grant 1221059). MJG acknowledges support from the European Research Council
through ERC Advanced\r\nGrant No. 101054731, from the National Aeronautics and Space
Administration under grants 80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380,\r\nand
from the National Science Foundation under grant AST-2205736. PJG\r\nis supported
by NRF SARChI grant 111692. PR-G acknowledges support by\r\nthe Agencia Estatal
de Investigación del Ministerio de Ciencia e Innovación\r\n(MCIN/AEI) and the European
Regional Development Fund (ERDF) under grant\r\nPID2021–124879NB–I00. DS is supported
by the UK Science and Technology Facilities Council (STFC, grant numbers ST/T007184/1,
ST/T003103/1,\r\nand ST/T000406/1). OT acknowledges Proyectos Internos USM 2025,
PI-LII2025-03. GT was supported by grants IN109723 from the Programa de Apoyo a\r\nProyectos
de Investigación e Innovación Tecnológica (PAPIIT). This project has\r\nreceived
funding from the European Research Council (ERC) under the European Union’s Horizon
2020 research and innovation programme (Grant agreement No. 101020057)."
article_number: A14
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: W.
full_name: Yu, W.
last_name: Yu
- first_name: A. F.
full_name: Pala, A. F.
last_name: Pala
- first_name: T.
full_name: Kupfer, T.
last_name: Kupfer
- first_name: B. T.
full_name: Gänsicke, B. T.
last_name: Gänsicke
- first_name: D.
full_name: Koester, D.
last_name: Koester
- first_name: D.
full_name: Belloni, D.
last_name: Belloni
- first_name: T. L.S.
full_name: Wong, T. L.S.
last_name: Wong
- first_name: M. R.
full_name: Schreiber, M. R.
last_name: Schreiber
- first_name: Joannes C
full_name: van Roestel, Joannes C
id: 4d122fc8-6083-11f0-87a5-97d68b860333
last_name: van Roestel
- first_name: A. J.
full_name: Brown, A. J.
last_name: Brown
- first_name: E. O.
full_name: Waagen, E. O.
last_name: Waagen
- first_name: J. L.
full_name: González-Carballo, J. L.
last_name: González-Carballo
- first_name: S.
full_name: Bednarz, S.
last_name: Bednarz
- first_name: K.
full_name: Bernacki, K.
last_name: Bernacki
- first_name: D.
full_name: De Martino, D.
last_name: De Martino
- first_name: E.
full_name: Fernández Mañanes, E.
last_name: Fernández Mañanes
- first_name: R.
full_name: González Farfán, R.
last_name: González Farfán
- first_name: M. J.
full_name: Green, M. J.
last_name: Green
- first_name: P. J.
full_name: Groot, P. J.
last_name: Groot
- first_name: F. J.
full_name: Hambsch, F. J.
last_name: Hambsch
- first_name: C.
full_name: Knigge, C.
last_name: Knigge
- first_name: J. L.
full_name: Martin-Velasco, J. L.
last_name: Martin-Velasco
- first_name: M.
full_name: Morales-Aimar, M.
last_name: Morales-Aimar
- first_name: G.
full_name: Myers, G.
last_name: Myers
- first_name: R.
full_name: Naves Nogues, R.
last_name: Naves Nogues
- first_name: R.
full_name: Poggiani, R.
last_name: Poggiani
- first_name: A.
full_name: Popowicz, A.
last_name: Popowicz
- first_name: G.
full_name: Ramsay, G.
last_name: Ramsay
- first_name: E.
full_name: Reina-Lorenz, E.
last_name: Reina-Lorenz
- first_name: P.
full_name: Rodríguez-Gil, P.
last_name: Rodríguez-Gil
- first_name: J. L.
full_name: Salto-González, J. L.
last_name: Salto-González
- first_name: E. M.
full_name: Sion, E. M.
last_name: Sion
- first_name: D.
full_name: Steeghs, D.
last_name: Steeghs
- first_name: P.
full_name: Szkody, P.
last_name: Szkody
- first_name: O.
full_name: Toloza, O.
last_name: Toloza
- first_name: G.
full_name: Tovmassian, G.
last_name: Tovmassian
citation:
ama: 'Yu W, Pala AF, Kupfer T, et al. The evolutionary history of ultra-compact
accreting binaries: I. Chemical abundances and the formation channel of the eclipsing
AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy and
Astrophysics. 2026;706. doi:10.1051/0004-6361/202557568'
apa: 'Yu, W., Pala, A. F., Kupfer, T., Gänsicke, B. T., Koester, D., Belloni, D.,
… Tovmassian, G. (2026). The evolutionary history of ultra-compact accreting binaries:
I. Chemical abundances and the formation channel of the eclipsing AM CVn system
ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy and Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557568'
chicago: 'Yu, W., A. F. Pala, T. Kupfer, B. T. Gänsicke, D. Koester, D. Belloni,
T. L.S. Wong, et al. “The Evolutionary History of Ultra-Compact Accreting Binaries:
I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System
ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy and Astrophysics.
EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557568.'
ieee: 'W. Yu et al., “The evolutionary history of ultra-compact accreting
binaries: I. Chemical abundances and the formation channel of the eclipsing AM
CVn system ZTF J225237.05-051917.4 from HST spectroscopy,” Astronomy and Astrophysics,
vol. 706. EDP Sciences, 2026.'
ista: 'Yu W, Pala AF, Kupfer T, Gänsicke BT, Koester D, Belloni D, Wong TLS, Schreiber
MR, van Roestel JC, Brown AJ, Waagen EO, González-Carballo JL, Bednarz S, Bernacki
K, De Martino D, Fernández Mañanes E, González Farfán R, Green MJ, Groot PJ, Hambsch
FJ, Knigge C, Martin-Velasco JL, Morales-Aimar M, Myers G, Naves Nogues R, Poggiani
R, Popowicz A, Ramsay G, Reina-Lorenz E, Rodríguez-Gil P, Salto-González JL, Sion
EM, Steeghs D, Szkody P, Toloza O, Tovmassian G. 2026. The evolutionary history
of ultra-compact accreting binaries: I. Chemical abundances and the formation
channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy.
Astronomy and Astrophysics. 706, A14.'
mla: 'Yu, W., et al. “The Evolutionary History of Ultra-Compact Accreting Binaries:
I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System
ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy and Astrophysics,
vol. 706, A14, EDP Sciences, 2026, doi:10.1051/0004-6361/202557568.'
short: W. Yu, A.F. Pala, T. Kupfer, B.T. Gänsicke, D. Koester, D. Belloni, T.L.S.
Wong, M.R. Schreiber, J.C. van Roestel, A.J. Brown, E.O. Waagen, J.L. González-Carballo,
S. Bednarz, K. Bernacki, D. De Martino, E. Fernández Mañanes, R. González Farfán,
M.J. Green, P.J. Groot, F.J. Hambsch, C. Knigge, J.L. Martin-Velasco, M. Morales-Aimar,
G. Myers, R. Naves Nogues, R. Poggiani, A. Popowicz, G. Ramsay, E. Reina-Lorenz,
P. Rodríguez-Gil, J.L. Salto-González, E.M. Sion, D. Steeghs, P. Szkody, O. Toloza,
G. Tovmassian, Astronomy and Astrophysics 706 (2026).
date_created: 2026-02-08T23:02:49Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-02-16T09:36:24Z
day: '01'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.1051/0004-6361/202557568
external_id:
arxiv:
- '2512.04147'
file:
- access_level: open_access
checksum: 2faec710fd04f927aa43deb57e35c9b2
content_type: application/pdf
creator: dernst
date_created: 2026-02-16T09:33:56Z
date_updated: 2026-02-16T09:33:56Z
file_id: '21227'
file_name: 2026_AstronomyAstrophysics_Yu.pdf
file_size: 4020466
relation: main_file
success: 1
file_date_updated: 2026-02-16T09:33:56Z
has_accepted_license: '1'
intvolume: ' 706'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
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: 'The evolutionary history of ultra-compact accreting binaries: I. Chemical
abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4
from HST 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'
...
---
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
success: 1
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'
...
---
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: '21450'
abstract:
- lang: eng
text: Stellar wind mass loss of massive stars is often assumed to depend on their
metallicity Z. Therefore, evolutionary models predict that massive stars in lower-Z
environments are able to retain more of their hydrogen-rich layers and evolve
into brighter cool supergiants (cool SGs; Teff < 7 kK). Surprisingly, in galaxies
in the metallicity range 0.2 ≲ Z/Z⊙ ≲ 1.5, previous studies have not found a metallicity
dependence on the upper luminosity limit Lmax of cool SGs. Here, we add four galaxies
to the sample studied for this purpose with data from the Hubble Space Telescope
and the James Webb Space Telescope (JWST). Observations of the extremely metal-poor
dwarf galaxy I Zw 18 from JWST allow us to extend the studied metallicity range
down to Z/Z⊙ ≈ 1/40. For cool SGs in all studied galaxies, including I Zw 18,
we find a constant value of Lmax ≈ 105.6 L⊙, similar to literature results for
0.2 ≲ Z/Z⊙ ≲ 1.5. In I Zw 18 and the other studied galaxies, the presence of Wolf-Rayet
stars has been previously inferred. Although we cannot rule out that some of them
become intermediate-temperature objects, this paints a picture in which evolved
stars with L > 105.6 L⊙ burn helium as hot, helium-rich stars down to extremely
low metallicity. We argue that metallicity-independent late-phase mass loss would
be the most likely mechanism responsible for this. Regardless of the exact stripping
mechanism (winds or, for example, binary interaction), for the Early Universe
our results imply a limitation on black hole masses and a contribution of stars
born with M ≳ 30 M⊙ to its surprisingly strong nitrogen enrichment. We propose
a scenario in which single stars at low metallicity emit sufficiently hard ionizing
radiation to produce He II and C IV lines. In this scenario, late-phase metallicity-independent
mass loss produces hot, helium-rich stars. Due to the well-understood metallicity
dependence on the radiation-driven winds of hot stars, a window of opportunity
would open below 0.2 Z⊙, where self-stripped helium-rich stars can exist without
dense Wolf-Rayet winds that absorb hard ionizing radiation.
acknowledgement: "We thank our anonymous referee for carefully reading the manuscript
and providing a constructive report with helpful feedback. 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 #1233. The specific observations analyzed can be accessed
via DOI: 10.17909/3c1d-6182. Moreover, this research is based in part on observations
made with the NASA/ESA Hubble Space Telescope obtained from the\r\nSpace Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated
with programs #13664, GO-10915, and DD-11307. This research was supported in part
by grant NSF PHY-2309135 to the Kavli Institute for Theoretical Physics (KITP).
LRP acknowledges support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41
funded\r\nby MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. LRP
acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033."
article_number: A116
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Abel
full_name: Schootemeijer, Abel
last_name: Schootemeijer
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Norbert
full_name: Langer, Norbert
last_name: Langer
- first_name: Giacomo
full_name: Bortolini, Giacomo
last_name: Bortolini
- first_name: Alec S.
full_name: Hirschauer, Alec S.
last_name: Hirschauer
- first_name: Lee
full_name: Patrick, Lee
last_name: Patrick
citation:
ama: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick
L. A constant upper luminosity limit of cool supergiant stars down to the extremely
low metallicity of I Zw 18. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557675
apa: Schootemeijer, A., Götberg, Y. L. L., Langer, N., Bortolini, G., Hirschauer,
A. S., & Patrick, L. (2026). A constant upper luminosity limit of cool supergiant
stars down to the extremely low metallicity of I Zw 18. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557675
chicago: Schootemeijer, Abel, Ylva Louise Linsdotter Götberg, Norbert Langer, Giacomo
Bortolini, Alec S. Hirschauer, and Lee Patrick. “A Constant Upper Luminosity Limit
of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy
& Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557675.
ieee: A. Schootemeijer, Y. L. L. Götberg, N. Langer, G. Bortolini, A. S. Hirschauer,
and L. Patrick, “A constant upper luminosity limit of cool supergiant stars down
to the extremely low metallicity of I Zw 18,” Astronomy & Astrophysics,
vol. 707. EDP Sciences, 2026.
ista: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick
L. 2026. A constant upper luminosity limit of cool supergiant stars down to the
extremely low metallicity of I Zw 18. Astronomy & Astrophysics. 707, A116.
mla: Schootemeijer, Abel, et al. “A Constant Upper Luminosity Limit of Cool Supergiant
Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy & Astrophysics,
vol. 707, A116, EDP Sciences, 2026, doi:10.1051/0004-6361/202557675.
short: A. Schootemeijer, Y.L.L. Götberg, N. Langer, G. Bortolini, A.S. Hirschauer,
L. Patrick, Astronomy & Astrophysics 707 (2026).
date_created: 2026-03-15T23:01:35Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T09:07:55Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202557675
external_id:
arxiv:
- '2510.12594'
file:
- access_level: open_access
checksum: 02a0cd932340207c96fdd3059490ad29
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T09:05:06Z
date_updated: 2026-03-16T09:05:06Z
file_id: '21455'
file_name: 2026_AstronomyAstrophysics_Schootemeijer.pdf
file_size: 2102107
relation: main_file
success: 1
file_date_updated: 2026-03-16T09:05:06Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
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: A constant upper luminosity limit of cool supergiant stars down to the extremely
low metallicity of I Zw 18
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: diamond
PlanS_conform: '1'
_id: '21658'
abstract:
- lang: eng
text: Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential
rotation between the core and the envelope of evolved solar-like stars. Quadrupolar
(ℓ = 2) mixed modes also contain information regarding internal dynamics but are
very rarely characterised due to their low amplitude and the challenging identification
of adjacent or overlapping rotationally split multiplets affected by near-degeneracy
effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond
ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed
modes while explicitly accounting for near-degeneracy effects that distort their
rotational multiplets. We have derived a new asymptotic formulation of near-degenerate
mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction
between modes of adjacent radial orders. This formalism, expressed directly in
the mixed-mode basis, provides analytical expressions for the near-degeneracy
effects. We implemented the formalism within a global Bayesian mode-fitting framework
for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were
able to asymptotically model the asymmetric rotational splitting present in various
radial orders of ℓ = 2 modes observed in young red giant stars without the need
for any numerical stellar modelling. We applied our formalism to the Kepler target
KIC 7341231, and it yielded core and envelope rotation rates consistent with previous
numerical modelling while providing improved constraints from the global and model-independent
approach. We also characterised the new target, KIC 8179973, measuring its rotation
rate and mixed-mode parameters for the first time. As our framework relies on
a direct global fit, it allows for much better precision on the asteroseismic
parameters and rotation rate estimates than standard methods, yielding better
constraints for rotation inversions. We have placed the first observational constraints
on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving
the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.
acknowledgement: 'We thank the referee for their careful and constructive report,
which has substantially enhanced both the quality and clarity of the manuscript.
L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research
Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement
N°101165631). While partially funded by the European Union, 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. Neither the European Union
nor the granting authority can be held responsible for them. The authors acknowledge
the great support and feedback provided during the redaction of this article by
Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt
for her insights on uncertainty estimates. The authors also thank the members of
the Asteroseismology and Stellar Dynamics group of the Institute of Science and
Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K.
Smith. This paper includes data collected by the Kepler mission and obtained from
the MAST data archive at the Space Telescope Science Institute (STScI). Funding
for the Kepler mission is provided by the NASA Science Mission Directorate. STScI
is operated by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013,
2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et
al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017),
slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011),
sloscillations (Kuszlewicz et al. 2019, 2023).'
article_number: A321
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Bastien Raymond Bernard
full_name: Liagre, Bastien Raymond Bernard
id: 662f1873-cab4-11f0-a719-8087d302868d
last_name: Liagre
- first_name: Aayush A
full_name: Desai, Aayush A
id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
last_name: Desai
- first_name: Lukas
full_name: Einramhof, Lukas
id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c
last_name: Einramhof
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar
mixed modes: From an asymptotic description to data fitting. Astronomy and
Astrophysics. 2026;707. doi:10.1051/0004-6361/202558023'
apa: 'Liagre, B. R. B., Desai, A. A., Einramhof, L., & Bugnet, L. A. (2026).
Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
to data fitting. Astronomy and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558023'
chicago: 'Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and
Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From
an Asymptotic Description to Data Fitting.” Astronomy and Astrophysics.
EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558023.'
ieee: 'B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy
effects in quadrupolar mixed modes: From an asymptotic description to data fitting,”
Astronomy and Astrophysics, vol. 707. EDP Sciences, 2026.'
ista: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects
in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy
and Astrophysics. 707, A321.'
mla: 'Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar
Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy and
Astrophysics, vol. 707, A321, EDP Sciences, 2026, doi:10.1051/0004-6361/202558023.'
short: B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics
707 (2026).
corr_author: '1'
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-04-07T09:01:44Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
- _id: IlCa
- _id: GradSch
doi: 10.1051/0004-6361/202558023
external_id:
arxiv:
- '2511.05314 '
file:
- access_level: open_access
checksum: 560cac19dc70184626b85e71a26ee22e
content_type: application/pdf
creator: dernst
date_created: 2026-04-07T09:00:50Z
date_updated: 2026-04-07T09:00:50Z
file_id: '21664'
file_name: 2026_AstronomyAstrophysics_Liagre.pdf
file_size: 12287607
relation: main_file
success: 1
file_date_updated: 2026-04-07T09:00:50Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
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: 'Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
to data fitting'
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: '21659'
abstract:
- lang: eng
text: The recent detection of solar equatorial Rossby waves has renewed interest
in the study of gravito-inertial waves propagating in the convective envelope
of solar-type stars. In particular, the ability of these envelope gravito-inertial
modes to couple with those trapped in the radiative interior could open up new
opportunities for probing the deep-layer dynamics of solar-type stars. The possibility
for such a coupling to occur is particularly favoured among pre-main-sequence
(PMS) solar-type stars. Indeed, due to the contraction of the protostellar object,
they are able to reach high rotation frequencies before nuclear reactions are
ignited and magnetic braking becomes the driving mechanism for their rotational
evolution. In this work, we studied the coupling between the envelope inertial
waves and the radiative interior g modes in PMS stars, focussing on the case of
prograde dipolar modes. We considered the cases of 0.5 M⊙ and 1 M⊙ PMS models,
each with three different scenarios of rotational evolution. We show that for
stars that have formed with a sufficient amount of angular momentum, this coupling
can occur in frequency ranges that are accessible to space-borne photometry, creating
inertial dips in the period spacing pattern. Using an asymptotic analysis, we
characterised the shape of these inertial dips to show that they depend on rotation
and on the stiffness of the convective-radiative interface.
acknowledgement: 'The authors want to thank the anonymous referee for useful comments.
SNB acknowledges support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase
D”. SNB and AFL acknowledge support from the INAF grant MASTODINT. CP thanks the
Belgian Federal Science Policy Office (BELSPO) for the financial support in the
framework of the PRODEX Program of the European Space Agency (ESA) under contract
number 4000141194. S.M acknowledges support from the CNES GOLF-SOHO and PLATO grants
at CEA/DAp. LB and SM gratefully acknowledge support from the European Research
Council (ERC) under the Horizon Europe programme (LB: Calcifer; Starting Grant agreement
N°101165631; SM: 4D-STAR; Synergy Grant agreement N°101071505). While partially
funded by the European Union, 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. Neither the European Union nor the granting authority
can be held responsible for them. The authors acknowledge G. Buldgen, H. Dhouib,
and M.A. Dupret for fruitful discussions.'
article_number: L16
article_processing_charge: No
article_type: letter_editor
arxiv: 1
author:
- first_name: S. N.
full_name: Breton, S. N.
last_name: Breton
- first_name: C.
full_name: Pezzotti, C.
last_name: Pezzotti
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: M. P.
full_name: Di Mauro, M. P.
last_name: Di Mauro
- first_name: J.
full_name: Joergensen, J.
last_name: Joergensen
- first_name: K.
full_name: Zwintz, K.
last_name: Zwintz
- first_name: A. F.
full_name: Lanza, A. F.
last_name: Lanza
citation:
ama: Breton SN, Pezzotti C, Mathis S, et al. Core-envelope coupling of gravito-inertial
waves in pre-main-sequence solar-type stars. Astronomy & Astrophysics.
2026;707. doi:10.1051/0004-6361/202659309
apa: Breton, S. N., Pezzotti, C., Mathis, S., Bugnet, L. A., Di Mauro, M. P., Joergensen,
J., … Lanza, A. F. (2026). Core-envelope coupling of gravito-inertial waves in
pre-main-sequence solar-type stars. Astronomy & Astrophysics. Wiley.
https://doi.org/10.1051/0004-6361/202659309
chicago: Breton, S. N., C. Pezzotti, S. Mathis, Lisa Annabelle Bugnet, M. P. Di
Mauro, J. Joergensen, K. Zwintz, and A. F. Lanza. “Core-Envelope Coupling of Gravito-Inertial
Waves in Pre-Main-Sequence Solar-Type Stars.” Astronomy & Astrophysics.
Wiley, 2026. https://doi.org/10.1051/0004-6361/202659309.
ieee: S. N. Breton et al., “Core-envelope coupling of gravito-inertial waves
in pre-main-sequence solar-type stars,” Astronomy & Astrophysics, vol.
707. Wiley, 2026.
ista: Breton SN, Pezzotti C, Mathis S, Bugnet LA, Di Mauro MP, Joergensen J, Zwintz
K, Lanza AF. 2026. Core-envelope coupling of gravito-inertial waves in pre-main-sequence
solar-type stars. Astronomy & Astrophysics. 707, L16.
mla: Breton, S. N., et al. “Core-Envelope Coupling of Gravito-Inertial Waves in
Pre-Main-Sequence Solar-Type Stars.” Astronomy & Astrophysics, vol.
707, L16, Wiley, 2026, doi:10.1051/0004-6361/202659309.
short: S.N. Breton, C. Pezzotti, S. Mathis, L.A. Bugnet, M.P. Di Mauro, J. Joergensen,
K. Zwintz, A.F. Lanza, Astronomy & Astrophysics 707 (2026).
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-04-07T09:23:27Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202659309
external_id:
arxiv:
- '2603.01979'
file:
- access_level: open_access
checksum: a7fd798bf450d67d4166fdf54ff2c70c
content_type: application/pdf
creator: dernst
date_created: 2026-04-07T09:20:02Z
date_updated: 2026-04-07T09:20:02Z
file_id: '21666'
file_name: 2026_AstronomyAstrophysics_Breton.pdf
file_size: 1535506
relation: main_file
success: 1
file_date_updated: 2026-04-07T09:20:02Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
grant_number: '101165631'
name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
title: Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type
stars
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
PlanS_conform: '1'
_id: '21274'
abstract:
- lang: eng
text: "Many white dwarfs are observed in compact double white dwarf binaries, and
through the emission of gravitational waves, a large fraction are destined to
merge. The merger remnants that do not explode in a Type Ia supernova are expected
to initially be rapidly rotating and highly magnetized. In this work, we present
our discovery of the variable white dwarf ZTF J200832.79+444939.67, hereafter
ZTF J2008+4449, as a likely merger remnant showing signs of circumstellar material
without a stellar or substellar companion. The nature of ZTF J2008+4449 as a merger
remnant is supported by its physical properties: it is hot (35 500 ± 300 K) and
massive (1.12 ± 0.03 M\r\n ⊙\r\n ),
rapidly rotating with a period of ≈6.6 minutes, and likely possesses exceptionally
strong magnetic fields (∼400−600 MG) at its surface. Remarkably, we detect a significant
period derivative of (1.80 ± 0.09)×10\r\n −12\r\n
\ s/s, indicating that the white dwarf is spinning down, and
a soft X-ray emission that is inconsistent with photospheric emission. As the
presence of a mass-transferring stellar or brown dwarf companion is excluded by
infrared photometry, the detected spin-down and X-ray emission could be tell-tale
signs of a magnetically driven wind or of interaction with circumstellar material,
possibly originating from the fallback of gravitationally bound merger ejecta
or from the tidal disruption of a planetary object. We also detect Balmer emission,
which requires the presence of ionized hydrogen in the vicinity of the white dwarf,
showing Doppler shifts as high as ≈2000 km s\r\n −1\r\n
\ . The unusual variability of the Balmer emission on the spin
period of the white dwarf is consistent with the trapping of a half ring of ionized
gas in the magnetosphere of the white dwarf.\r\n "
acknowledgement: "We thank Lynne Hillenbrand and Soumyadeep Bhattacharjee for helpful
discussions, and Kishalay De for his help with the WIRC\r\nreduction pipeline. IC
was supported by NASA through grants from the Space\r\nTelescope Science Institute,
under NASA contracts NASA.22K1813, NAS5-\r\n26555 and NAS5-03127. TC was supported
by NASA through the NASA Hubble\r\nFellowship grant HST-HF2-51527.001-A awarded
by the Space Telescope Science Institute, which is operated by the Association of
Universities for Research\r\nin Astronomy, Inc., for NASA, under contract NAS5-26555.
This project has\r\nreceived funding from the European Research Council (ERC) under
the European Union’s Horizon 2020 research and innovation programme (Grant agreement
No. 101020057). This work was based on observations obtained with the\r\nSamuel
Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar\r\nObservatory
as part of the Zwicky Transient Facility project. ZTF is supported\r\nby the National
Science Foundation under Grants No. AST-1440341, AST2034437, and currently Award
#2407588. ZTF receives additional funding from\r\nthe ZTF partnership. Current members
include Caltech, USA; Caltech/IPAC,\r\nUSA; University of Maryland, USA; University
of California, Berkeley, USA;\r\nUniversity of Wisconsin at Milwaukee, USA; Cornell
University, USA; Drexel\r\nUniversity, USA; University of North Carolina at Chapel
Hill, USA; Institute\r\nof Science and Technology, Austria; National Central University,
Taiwan, and\r\nOKC, University of Stockholm, Sweden. Operations are conducted by
Caltech’s\r\nOptical Observatory (COO), Caltech/IPAC, and the University of Washington
at\r\nSeattle, USA. This work has made use of data from the European Space Agency\r\n(ESA)
mission Gaia (https://www.cosmos.esa.int/gaia), processed by\r\nthe Gaia Data Processing
and Analysis Consortium (DPAC, https://www.\r\ncosmos.esa.int/web/gaia/dpac/consortium).
Funding for the DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys
(PS1)\r\nand the PS1 public science archive have been made possible through contributions
by the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project
Office, the Max-Planck Society and its participating institutes, the Max Planck
Institute for Astronomy, Heidelberg and the Max Planck\r\nInstitute for Extraterrestrial
Physics, Garching, The Johns Hopkins University,\r\nDurham University, the University
of Edinburgh, the Queen’s University Belfast,\r\nthe Harvard-Smithsonian Center
for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated,
the National Central University of Taiwan, the Space Telescope Science Institute,
the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued
through\r\nthe Planetary Science Division of the NASA Science Mission Directorate,
the\r\nNational Science Foundation Grant No. AST–1238877, the University of Maryland,
Eotvos Lorand University (ELTE), the Los Alamos National Laboratory,\r\nand the
Gordon and Betty Moore Foundation. This work made use of Astropy\r\n(http://www.astropy.org):
a community-developed core Python package\r\nand an ecosystem of tools and resources
for astronomy (Astropy Collaboration\r\n2013, 2018, 2022)."
article_number: A188
article_processing_charge: Yes
article_type: original
author:
- first_name: Andrei-Alexandru
full_name: Cristea, Andrei-Alexandru
id: 4d500bea-31f8-11ee-a48d-d4904fb363c7
last_name: Cristea
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Tim
full_name: Cunningham, Tim
last_name: Cunningham
- first_name: John C.
full_name: Raymond, John C.
last_name: Raymond
- first_name: Stephane
full_name: Vennes, Stephane
last_name: Vennes
- first_name: Adela
full_name: Kawka, Adela
last_name: Kawka
- first_name: Aayush A
full_name: Desai, Aayush A
id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
last_name: Desai
- first_name: David R.
full_name: Miller, David R.
last_name: Miller
- first_name: J. J.
full_name: Hermes, J. J.
last_name: Hermes
- first_name: Jim
full_name: Fuller, Jim
last_name: Fuller
- first_name: Jeremy
full_name: Heyl, Jeremy
last_name: Heyl
- first_name: Jan
full_name: van Roestel, Jan
last_name: van Roestel
- first_name: Kevin B.
full_name: Burdge, Kevin B.
last_name: Burdge
- first_name: Antonio C.
full_name: Rodriguez, Antonio C.
last_name: Rodriguez
- first_name: Ingrid
full_name: Pelisoli, Ingrid
last_name: Pelisoli
- first_name: Boris T.
full_name: Gänsicke, Boris T.
last_name: Gänsicke
- first_name: Paula
full_name: Szkody, Paula
last_name: Szkody
- first_name: Scott J.
full_name: Kenyon, Scott J.
last_name: Kenyon
- first_name: Zach
full_name: Vanderbosch, Zach
last_name: Vanderbosch
- first_name: Andrew
full_name: Drake, Andrew
last_name: Drake
- first_name: Lilia
full_name: Ferrario, Lilia
last_name: Ferrario
- first_name: Dayal
full_name: Wickramasinghe, Dayal
last_name: Wickramasinghe
- first_name: Viraj R.
full_name: Karambelkar, Viraj R.
last_name: Karambelkar
- first_name: Stephen
full_name: Justham, Stephen
last_name: Justham
- first_name: Ruediger
full_name: Pakmor, Ruediger
last_name: Pakmor
- first_name: Kareem
full_name: El-Badry, Kareem
last_name: El-Badry
- first_name: Thomas
full_name: Prince, Thomas
last_name: Prince
- first_name: S. R.
full_name: Kulkarni, S. R.
last_name: Kulkarni
- first_name: Matthew J.
full_name: Graham, Matthew J.
last_name: Graham
- first_name: Frank J.
full_name: Masci, Frank J.
last_name: Masci
- first_name: Steven L.
full_name: Groom, Steven L.
last_name: Groom
- first_name: Josiah
full_name: Purdum, Josiah
last_name: Purdum
- first_name: Richard
full_name: Dekany, Richard
last_name: Dekany
- first_name: Eric C.
full_name: Bellm, Eric C.
last_name: Bellm
citation:
ama: Cristea A-A, Caiazzo I, Cunningham T, et al. A half ring of ionized circumstellar
material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy
& Astrophysics. 2026;706. doi:10.1051/0004-6361/202556432
apa: Cristea, A.-A., Caiazzo, I., Cunningham, T., Raymond, J. C., Vennes, S., Kawka,
A., … Bellm, E. C. (2026). A half ring of ionized circumstellar material trapped
in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202556432
chicago: Cristea, Andrei-Alexandru, Ilaria Caiazzo, Tim Cunningham, John C. Raymond,
Stephane Vennes, Adela Kawka, Aayush A Desai, et al. “A Half Ring of Ionized Circumstellar
Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy
& Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202556432.
ieee: A.-A. Cristea et al., “A half ring of ionized circumstellar material
trapped in the magnetosphere of a white dwarf merger remnant,” Astronomy &
Astrophysics, vol. 706. EDP Sciences, 2026.
ista: Cristea A-A, Caiazzo I, Cunningham T, Raymond JC, Vennes S, Kawka A, Desai
AA, Miller DR, Hermes JJ, Fuller J, Heyl J, van Roestel J, Burdge KB, Rodriguez
AC, Pelisoli I, Gänsicke BT, Szkody P, Kenyon SJ, Vanderbosch Z, Drake A, Ferrario
L, Wickramasinghe D, Karambelkar VR, Justham S, Pakmor R, El-Badry K, Prince T,
Kulkarni SR, Graham MJ, Masci FJ, Groom SL, Purdum J, Dekany R, Bellm EC. 2026.
A half ring of ionized circumstellar material trapped in the magnetosphere of
a white dwarf merger remnant. Astronomy & Astrophysics. 706, A188.
mla: Cristea, Andrei-Alexandru, et al. “A Half Ring of Ionized Circumstellar Material
Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy &
Astrophysics, vol. 706, A188, EDP Sciences, 2026, doi:10.1051/0004-6361/202556432.
short: A.-A. Cristea, I. Caiazzo, T. Cunningham, J.C. Raymond, S. Vennes, A. Kawka,
A.A. Desai, D.R. Miller, J.J. Hermes, J. Fuller, J. Heyl, J. van Roestel, K.B.
Burdge, A.C. Rodriguez, I. Pelisoli, B.T. Gänsicke, P. Szkody, S.J. Kenyon, Z.
Vanderbosch, A. Drake, L. Ferrario, D. Wickramasinghe, V.R. Karambelkar, S. Justham,
R. Pakmor, K. El-Badry, T. Prince, S.R. Kulkarni, M.J. Graham, F.J. Masci, S.L.
Groom, J. Purdum, R. Dekany, E.C. Bellm, Astronomy & Astrophysics 706 (2026).
corr_author: '1'
date_created: 2026-02-17T08:12:05Z
date_published: 2026-02-10T00:00:00Z
date_updated: 2026-04-28T12:01:21Z
day: '10'
ddc:
- '520'
department:
- _id: IlCa
- _id: GradSch
doi: 10.1051/0004-6361/202556432
file:
- access_level: open_access
checksum: 229b688e6e78cab5bb8e2bac366d1575
content_type: application/pdf
creator: dernst
date_created: 2026-02-23T12:04:37Z
date_updated: 2026-02-23T12:04:37Z
file_id: '21350'
file_name: 2026_AstronomyAstrophysics_Cristea.pdf
file_size: 5352853
relation: main_file
success: 1
file_date_updated: 2026-02-23T12:04:37Z
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'
related_material:
link:
- description: News on ISTA website
relation: press_release
url: https://ista.ac.at/en/news/twos-company-new-class-of-star-remnants/
status: public
title: A half ring of ionized circumstellar material trapped in the magnetosphere
of a white dwarf merger remnant
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: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 706
year: '2026'
...
---
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: '19797'
abstract:
- lang: eng
text: Stars stripped of their hydrogen-rich envelopes through binary interaction
are thought to be responsible for both hydrogen-poor supernovae and the hard ionizing
radiation observed in low-Z galaxies. A population of these stars was recently
observed for the first time, but their prevalence remains unknown. In preparation
for such measurements, we estimate the mass distribution of hot, stripped stars
using a population synthesis code that interpolates over detailed single and binary
stellar evolution tracks. We predict that for a constant star formation rate of
1 M⊙/yr and regardless of metallicity, a scalable model population contains ∼30
000 stripped stars with mass Mstrip > 1 M⊙ and ∼4000 stripped stars that are sufficiently
massive to explode (Mstrip > 2.6 M⊙). Below Mstrip = 5 M⊙, the distribution is
metallicity-independent and can be described by a power law with the exponent
α ∼ −2. At higher masses and lower metallicity (Z ≲ 0.002), the mass distribution
exhibits a drop. This originates from the prediction, frequently seen in evolutionary
models, that massive low-metallicity stars do not expand substantially until central
helium burning or later and therefore cannot form long-lived stripped stars. With
weaker line-driven winds at low metallicity, this suggests that neither binary
interaction nor wind mass loss can efficiently strip massive stars at low metallicity.
As a result, a “helium-star desert” emerges around Mstrip = 15 M⊙ at Z = 0.002,
covering an increasingly large mass range with decreasing metallicity. We note
that these high-mass stars are those that potentially boost a galaxy’s He+-ionizing
radiation and that participate in the formation of merging black holes. This “helium-star
desert” therefore merits further study.
acknowledgement: We thank the anonymous referee for providing a constructive report.
We thank Tomer Shenar and Selma de Mink for the interesting discussions that helped
us improve the content of Sect. 4. Thank you to Jorick Vink and Andreas Sander for
helpful discussions about wind driving. BHA thanks the Caltech Summer Undergraduate
Research Fellowship (SURF) program and Peter Adams for supporting this project in
memory of Alain Porter and Arthur R. Adams. BHA thanks Gwen Rudie for organizing
the Carnegie Astrophysics Summer Student Internship (CASSI) program and all the
staff at Carnegie Observatories who help to support this program. BHA also thanks
Laura Jaliff, Sal Wanying Fu, Ivanna Escala, Johanna Teske, Tony Piro, Brian Lorenz,
and Peter Senchyna for their mentorship during this project. Computing resources
used for this work were made possible by a grant from the Ahmanson Foundation. We
thank the Observatories of the Carnegie Institution for Science for support, including
Chris Burns for help with computations. This work used computing resources provided
by Northwestern University and the Center for Interdisciplinary Exploration and
Research in Astrophysics (CIERA). This research was supported in part through the
computational resources and staff contributions provided for the Quest high performance
computing facility at Northwestern University which is jointly supported by the
Office of the Provost, the Office for Research, and Northwestern University Information
Technology. MRD acknowledges support from the NSERC through grant RGPIN-2019-06186,
the Canada Research Chairs Program, and the Dunlap Institute at the University of
Toronto. BHA is supported by the National Science Foundation Graduate Research Fellowship
under Grant No. DGE-2234667.
article_number: A239
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: B.
full_name: Hovis-Afflerbach, B.
last_name: Hovis-Afflerbach
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: A. L.
full_name: Strom, A. L.
last_name: Strom
- first_name: B. A.
full_name: Ludwig, B. A.
last_name: Ludwig
- first_name: M. R.
full_name: Drout, M. R.
last_name: Drout
citation:
ama: 'Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, et al. The mass distribution
of stars stripped in binaries: The effect of metallicity. Astronomy & Astrophysics.
2025;697. doi:10.1051/0004-6361/202453185'
apa: 'Hovis-Afflerbach, B., Götberg, Y. L. L., Schootemeijer, A., Klencki, J., Strom,
A. L., Ludwig, B. A., & Drout, M. R. (2025). The mass distribution of stars
stripped in binaries: The effect of metallicity. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202453185'
chicago: 'Hovis-Afflerbach, B., Ylva Louise Linsdotter Götberg, A. Schootemeijer,
J. Klencki, A. L. Strom, B. A. Ludwig, and M. R. Drout. “The Mass Distribution
of Stars Stripped in Binaries: The Effect of Metallicity.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202453185.'
ieee: 'B. Hovis-Afflerbach et al., “The mass distribution of stars stripped
in binaries: The effect of metallicity,” Astronomy & Astrophysics,
vol. 697. EDP Sciences, 2025.'
ista: 'Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, Klencki J, Strom AL, Ludwig
BA, Drout MR. 2025. The mass distribution of stars stripped in binaries: The effect
of metallicity. Astronomy & Astrophysics. 697, A239.'
mla: 'Hovis-Afflerbach, B., et al. “The Mass Distribution of Stars Stripped in Binaries:
The Effect of Metallicity.” Astronomy & Astrophysics, vol. 697, A239,
EDP Sciences, 2025, doi:10.1051/0004-6361/202453185.'
short: B. Hovis-Afflerbach, Y.L.L. Götberg, A. Schootemeijer, J. Klencki, A.L. Strom,
B.A. Ludwig, M.R. Drout, Astronomy & Astrophysics 697 (2025).
corr_author: '1'
date_created: 2025-06-08T22:01:22Z
date_published: 2025-05-01T00:00:00Z
date_updated: 2026-02-16T12:10:11Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202453185
external_id:
arxiv:
- '2412.05356'
isi:
- '001494033100007'
file:
- access_level: open_access
checksum: caa92beb22ab3146a75c5b03e926de1f
content_type: application/pdf
creator: dernst
date_created: 2025-06-10T07:00:38Z
date_updated: 2025-06-10T07:00:38Z
file_id: '19799'
file_name: 2025_AstronomyAstrophysics_HovisAfflerbach.pdf
file_size: 6378030
relation: main_file
success: 1
file_date_updated: 2025-06-10T07:00:38Z
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: 'The mass distribution of stars stripped in binaries: The effect of metallicity'
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: 697
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19841'
abstract:
- lang: eng
text: "Context. The blue supergiant (BSG) domain contains a large variety of stars
whose past and future evolutionary paths are still highly uncertain. Since binary
interaction plays a crucial role in the fate of massive stars, investigating the
multiplicity among BSGs helps shed light on the fate of such objects.\r\nAims.
We aim to estimate the binary fraction of a large sample of BSGs in the Small
Magellanic Cloud (SMC) within the Binarity at LOw Metallicity (BLOeM) survey.
In total, we selected 262 targets with spectral types B0-B3 and luminosity classes
I-II.\r\n\r\nMethods. This work is based on spectroscopic data collected by the
FLAMES instrument, mounted on the Very Large Telescope, which gathered nine epochs
over three months. Our spectroscopic analysis for each target includes the individual
and peak-to-peak radial velocity measurements, an investigation of the line profile
variability, and a periodogram analysis to search for possible short- and long-period
binaries.\r\n\r\nResults. By applying a 20 km s−1 threshold on the peak-to-peak
radial velocities above which we would consider the star to be binary, the resulting
observed spectroscopic binary fraction for our BSG sample is 23 ± 3%. An independent
analysis of line profile variability reveals 11 (plus 5 candidates) double-lined
spectroscopic binaries and 32 (plus 41 candidates) single-lined spectroscopic
binaries. Based on these results, we estimated the overall observed binary fraction
in this sample to be 34 ± 3%, which is close to the computed intrinsic binary
fraction of 40 ± 4%. In addition, we derived reliable orbital periods for 41 spectroscopic
binaries and potential binary candidates, among which there are 17 eclipsing binaries,
including 20 SB1 and SB2 systems with periods of less than 10 days. We reported
a significant drop in the binary fraction of BSGs with spectral types later than
B2 and effective temperatures less than 18 kK, which could indicate the end of
the main sequence phase in this temperature regime. We found no metallicity dependence
in the binary fraction of BSGs, compared to existing spectroscopic surveys of
the Galaxy and Large Magellanic Cloud."
acknowledgement: 'We thank the anonymous referee for helpful comments that have improved
the manuscript. This project has received funding from the European Research Council
(ERC) under the European Union’s Horizon 2020 research and innovation programme
(grant agreement 101164755/METAL) and was supported by the Israel Science Foundation
(ISF) under grant number 2434/24. NB acknowledges support from the Belgian federal
government grant for Ukrainian postdoctoral researchers (contract UF/2022/10). TS
acknowledges support by the Israel Science Foundation (ISF) under grant number 0603225041.
DP acknowledges financial support from the Deutsches Zentrum für Luft und Raumfahrt
(DLR) grant FKZ 50OR2005 and the FWO junior postdoctoral fellowship No. 1256225N.
DMB gratefully acknowledges UK Research and Innovation (UKRI) in the form of a Frontier
Research grant under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY;
PI Bowman; grant number: EP/Y031059/1), and a Royal Society University Research
Fellowship (PI Bowman; grant number: URF\R1\231631). KS is funded by the National
Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. IM acknowledges
support from the Australian Research Council (ARC) Centre of Excellence for Gravitational
Wave Discovery (OzGav), through project number CE230100016. JIV acknowledges support
from the European Research Council through ERC Advanced Grant No. 101054731. SS-D,
and GH acknowledge support from the Spanish Ministry of Science and Innovation and
Universities (MICIU) through the Spanish State Research Agency (AEI) through grants
PID2021-122397NB-C21, and the Severo Ochoa Program 2020-2023 (CEX2019-000920-S).'
article_number: A40
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: C.
full_name: Johnston, C.
last_name: Johnston
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: M.
full_name: Moe, M.
last_name: Moe
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Pawlak, M.
last_name: Pawlak
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: S.
full_name: Simón-Díaz, S.
last_name: Simón-Díaz
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
citation:
ama: 'Britavskiy N, Mahy L, Lennon DJ, et al. Binarity at LOw Metallicity (BLOeM):
Multiplicity of early B-type supergiants in the Small Magellanic Cloud. Astronomy
& Astrophysics. 2025;698. doi:10.1051/0004-6361/202452963'
apa: 'Britavskiy, N., Mahy, L., Lennon, D. J., Patrick, L. R., Sana, H., Villaseñor,
J. I., … Vink, J. S. (2025). Binarity at LOw Metallicity (BLOeM): Multiplicity
of early B-type supergiants in the Small Magellanic Cloud. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452963'
chicago: 'Britavskiy, N., L. Mahy, D. J. Lennon, L. R. Patrick, H. Sana, J. I. Villaseñor,
T. Shenar, et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity of Early
B-Type Supergiants in the Small Magellanic Cloud.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452963.'
ieee: 'N. Britavskiy et al., “Binarity at LOw Metallicity (BLOeM): Multiplicity
of early B-type supergiants in the Small Magellanic Cloud,” Astronomy &
Astrophysics, vol. 698. EDP Sciences, 2025.'
ista: 'Britavskiy N, Mahy L, Lennon DJ, Patrick LR, Sana H, Villaseñor JI, Shenar
T, Bodensteiner J, Bernini-Peron M, Berlanas SR, Bowman DM, Crowther PA, De Mink
SE, Evans CJ, Götberg YLL, Holgado G, Johnston C, Keszthelyi Z, Klencki J, Langer
N, Mandel I, Menon A, Moe M, Oskinova LM, Pauli D, Pawlak M, Ramachandran V, Renzo
M, Sander AAC, Schneider FRN, Schootemeijer A, Sen K, Simón-Díaz S, Van Loon JT,
Vink JS. 2025. Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type
supergiants in the Small Magellanic Cloud. Astronomy & Astrophysics. 698,
A40.'
mla: 'Britavskiy, N., et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
of Early B-Type Supergiants in the Small Magellanic Cloud.” Astronomy &
Astrophysics, vol. 698, A40, EDP Sciences, 2025, doi:10.1051/0004-6361/202452963.'
short: N. Britavskiy, L. Mahy, D.J. Lennon, L.R. Patrick, H. Sana, J.I. Villaseñor,
T. Shenar, J. Bodensteiner, M. Bernini-Peron, S.R. Berlanas, D.M. Bowman, P.A.
Crowther, S.E. De Mink, C.J. Evans, Y.L.L. Götberg, G. Holgado, C. Johnston, Z.
Keszthelyi, J. Klencki, N. Langer, I. Mandel, A. Menon, M. Moe, L.M. Oskinova,
D. Pauli, M. Pawlak, V. Ramachandran, M. Renzo, A.A.C. Sander, F.R.N. Schneider,
A. Schootemeijer, K. Sen, S. Simón-Díaz, J.T. Van Loon, J.S. Vink, Astronomy &
Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:29Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:09:34Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452963
external_id:
arxiv:
- '2502.12239'
isi:
- '001497903100019'
file:
- access_level: open_access
checksum: 53a9f290cb1f468895e0d4446e0020f0
content_type: application/pdf
creator: dernst
date_created: 2025-06-25T08:38:02Z
date_updated: 2025-06-25T08:38:02Z
file_id: '19901'
file_name: 2025_AstronomyAstrophysics_Britavskiy.pdf
file_size: 7106568
relation: main_file
success: 1
file_date_updated: 2025-06-25T08:38:02Z
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: 'Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants
in the Small Magellanic Cloud'
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: '19842'
abstract:
- lang: eng
text: Given the uncertain evolutionary status of blue supergiant stars, their multiplicity
properties hold vital clues to better understand their origin and evolution. As
part of The Binarity at LOw Metallicity (BLOeM) campaign in the Small Magellanic
Cloud, we present a multi-epoch spectroscopic survey of 128 supergiant stars of
spectral type B5–F5, which roughly correspond to initial masses in the 6–30 M⊙
range. The observed binary fraction for the B5–9 supergiants is 25 ± 6% (10 ±
4%) and 5 ± 2% (0%) for the A–F stars, which were found using a radial-velocity
(RV) variability threshold of 5 km s−1 (10 km s−1) as a criterion for binarity.
Accounting for observational biases, we find an intrinsic multiplicity fraction
of less than 18% for the B5–9 stars and 8−7+9% for the AF stars, for the orbital
periods up to 103.5 days and mass ratios (q) in the 0.1 < q < 1 range. The large
stellar radii of these supergiant stars prevent short orbital periods, but we
demonstrate that this effect alone cannot explain our results. We assessed the
spectra and RV time series of the detected binary systems and find that only a
small fraction display convincing solutions. We conclude that the multiplicity
fractions are compromised by intrinsic stellar variability, such that the true
multiplicity fraction may be significantly smaller. Our main conclusions from
comparing the multiplicity properties of the B5–9- and AF-type supergiants to
that of their less evolved counterparts is that such stars cannot be explained
by a direct evolution from the main sequence. Furthermore, by comparing their
multiplicity properties to red supergiant stars, we conclude that the AF supergiant
stars are neither progenitors nor descendants of red supergiants.
acknowledgement: 'We thank Sipra Hota for kindly sharing the SMC UVIT catalogue prior
to publication. LRP, FN. and FT acknowledge support by grants PID2019-105552RB-C41
and PID2022-137779OB-C41 funded by MCIN/AEI/10.13039/501100011033 by “ERDF A way
of making Europe”. LRP acknowledges support from grant PID2022-140483NB-C22 funded
by MCIN/AEI/10.13039/501100011033. TS acknowledges support by the Israel Science
Foundation (ISF) under grant number 0603225041. The research leading to these results
has received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation programme (grant agreement numbers
772225: MULTIPLES). DMB gratefully acknowledges support from UK Research and Innovation
(UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon
Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1), and a Royal Society
University Research Fellowship (grant number: URF\R1\231631). GGT is supported by
the German Deutsche Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1,
PI Sander). AACS is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research
Foundation) in the form of an Emmy Noether Research Group – Project-ID 445674056
(SA4064/1-1, PI Sander). GGT and AACS further acknowledges support from the Federal
Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of
Science as part of the Excellence Strategy of the German Federal and State Governments.
This paper benefited from discussions at the International Space Science Institute
(ISSI) in Bern through ISSI International Team project 512 (Multiwavelength View
on Massive Stars in the Era of Multimessenger Astronomy). DP acknowledges financial
support by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005.
JIV acknowledges support from the European Research Council for the ERC Advanced
Grant 101054731. PAC is supported by the Science and Technology Facilities Council
research grant ST/V000853/1 (PI. V. Dhillon). JSV is supported by Science and Technology
Facilities Council funding under grant number ST/V000233/1. DFR is thankful for
the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). This work
has received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation programme (Grant agreement No. 945806)
and is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)
under Germany’s Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES
Excellence Cluster).'
article_number: A39
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: F.
full_name: Najarro, F.
last_name: Najarro
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A. J.G.
full_name: O’Grady, A. J.G.
last_name: O’Grady
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: G.
full_name: González-Torà, G.
last_name: González-Torà
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z.
full_name: K̃Eszthelyi, Z.
last_name: K̃Eszthelyi
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: M.
full_name: Moe, M.
last_name: Moe
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
citation:
ama: 'Patrick LR, Lennon DJ, Najarro F, et al. Binarity at LOw Metallicity (BLOeM):
The multiplicity properties and evolution of BAF-type supergiants. Astronomy
& Astrophysics. 2025;698. doi:10.1051/0004-6361/202452949'
apa: 'Patrick, L. R., Lennon, D. J., Najarro, F., Shenar, T., Bodensteiner, J.,
Sana, H., … Wang, C. (2025). Binarity at LOw Metallicity (BLOeM): The multiplicity
properties and evolution of BAF-type supergiants. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202452949'
chicago: 'Patrick, L. R., D. J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner,
H. Sana, P. A. Crowther, et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity
Properties and Evolution of BAF-Type Supergiants.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452949.'
ieee: 'L. R. Patrick et al., “Binarity at LOw Metallicity (BLOeM): The multiplicity
properties and evolution of BAF-type supergiants,” Astronomy & Astrophysics,
vol. 698. EDP Sciences, 2025.'
ista: 'Patrick LR, Lennon DJ, Najarro F, Shenar T, Bodensteiner J, Sana H, Crowther
PA, Britavskiy N, Langer N, Schootemeijer A, Evans CJ, Mahy L, Götberg YLL, De
Mink SE, Schneider FRN, O’Grady AJG, Villaseñor JI, Bernini-Peron M, Bowman DM,
De Koter A, Deshmukh K, Gilkis A, González-Torà G, Kalari VM, K̃Eszthelyi Z, Mandel
I, Menon A, Moe M, Oskinova LM, Pauli D, Renzo M, Sander AAC, Sen K, Stoop M,
Van Loon JT, Toonen S, Tramper F, Vink JS, Wang C. 2025. Binarity at LOw Metallicity
(BLOeM): The multiplicity properties and evolution of BAF-type supergiants. Astronomy
& Astrophysics. 698, A39.'
mla: 'Patrick, L. R., et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity
Properties and Evolution of BAF-Type Supergiants.” Astronomy & Astrophysics,
vol. 698, A39, EDP Sciences, 2025, doi:10.1051/0004-6361/202452949.'
short: L.R. Patrick, D.J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner, H. Sana,
P.A. Crowther, N. Britavskiy, N. Langer, A. Schootemeijer, C.J. Evans, L. Mahy,
Y.L.L. Götberg, S.E. De Mink, F.R.N. Schneider, A.J.G. O’Grady, J.I. Villaseñor,
M. Bernini-Peron, D.M. Bowman, A. De Koter, K. Deshmukh, A. Gilkis, G. González-Torà,
V.M. Kalari, Z. K̃Eszthelyi, I. Mandel, A. Menon, M. Moe, L.M. Oskinova, D. Pauli,
M. Renzo, A.A.C. Sander, K. Sen, M. Stoop, J.T. Van Loon, S. Toonen, F. Tramper,
J.S. Vink, C. Wang, Astronomy & Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:29Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:09:50Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452949
external_id:
arxiv:
- '2502.02644'
isi:
- '001497903100028'
file:
- access_level: open_access
checksum: 93a907bf48da7e2ba7d75b53ea6011f5
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T07:09:38Z
date_updated: 2025-06-23T07:09:38Z
file_id: '19863'
file_name: 2025_AstronomyAstrophysics_Patrick.pdf
file_size: 2130448
relation: main_file
success: 1
file_date_updated: 2025-06-23T07:09:38Z
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: 'Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution
of BAF-type supergiants'
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: '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: 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'
...
---
OA_place: publisher
OA_type: diamond
_id: '19967'
abstract:
- lang: eng
text: "Context. Investigating the ionizing emission of star-forming galaxies and
the escape fraction of ionizing photons is critical to understanding their contribution
to reionization and their impact on the surrounding environment. The number of
ionizing photons available to reionize the intergalactic medium (IGM) depends
on not only the abundance of galaxies but also their efficiency in producing ionizing
photons (ξion). This quantity is thus fundamental to quantify the role of faint
versus bright sources in driving this process, as we must assess their relative
contribution to the total ionizing emissivity.\r\n\r\nAims. Our goal is to estimate
the ξion using Balmer lines (Hα or Hβ) in a sample of 761 galaxies at 4 ≤ z ≤ 10
selected from different JWST spectroscopic surveys. We aim to determine the redshift
evolution of ξion and the relation of ξion with the physical properties of the
galaxies.\r\n\r\nMethods. We used the available HST and JWST photometry to perform
a spectral energy distribution (SED) fitting in the sample to determine their
physical properties and relate them with ξion. We used the BAGPIPES code for the
SED fitting and assumed a delayed exponential model for the star formation history.
We used the NIRSpec spectra from prism or grating configurations to estimate Balmer
luminosities, and then constrained ξion values after dust correction.\r\n\r\nResults.
We find a mean value of 1025.22 Hz erg−1 for ξion in the sample with an observed
scatter of 0.42 dex. We find an increase in the median values of ξion with redshift
from 1025.09 Hz erg−1 at z ∼ 4.18 to 1025.28 Hz erg−1 at z ∼ 7.14, confirming
the redshift evolution of ξion found in other studies. Regarding the relation
between ξion and physical properties, we find a decrease in ξion with increasing
stellar mass, indicating that low-mass galaxies are efficient producers of ionizing
photons. We also find an increase in ξion with increasing specific star formation
rate (sSFR) and increasing UV absolute magnitude. This indicates that faint galaxies
and galaxies with high sSFR are also efficient producers. We also investigated
the relation of ξion with the rest-frame equivalent width (EW) of [OIII]λ5007
and find that galaxies with the higher EW([OIII]λ5007) are more efficient producers
of ionizing photons, with the best fit leading to the relation log(ξion) = 0.43 × log(EW[OIII])+23.99.
Similarly, we find that galaxies with higher O32 = [OIII]λ5007/[OII]λλ3727,3729
and lower gas-phase metallicities (based on the R23 = ([OIII]λλ4959,5007+[OII]λλ3727,3729)/Hβ
calibration) show higher ξion values."
acknowledgement: We thank the anonymous referee for the detailed review and useful
suggestions that helped to improve this paper. We wish to thank all our colleagues
in the CEERS collaboration for their hard work and valuable contributions to this
project. We thank Pietro Bergamini for providing us with the magnification factors
for the lensed sources. MLl acknowledges support from the INAF Large Grant 2022
“Extragalactic Surveys with JWST” (PI L. Pentericci), the PRIN 2022 MUR project
2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union
– Next Generation EU, and INAF Mini-grant “Galaxies in the epoch of Reionization
and their analogs at lower redshift” (PI M. Llerena). RA 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 This work is based on observations made
with the NASA/ESA/CSA James Webb Space Telescope (JWST). The JWST data presented
in this article were obtained from the Mikulski Archive for Space Telescopes (MAST)
at the Space Telescope Science Institute. The specific observations analyzed are
associated with program JWST-GO-3073 and can be accessed via DOI. We acknowledge
support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift
Galaxies”. This work has made extensive use of Python packages astropy (Astropy
Collaboration 2018), numpy (Harris et al. 2020), Matplotlib (Hunter 2007) and LiMe
(Fernández et al. 2024).
article_number: A302
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: M.
full_name: Llerena, M.
last_name: Llerena
- first_name: L.
full_name: Pentericci, L.
last_name: Pentericci
- first_name: L.
full_name: Napolitano, L.
last_name: Napolitano
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: R.
full_name: Amorín, R.
last_name: Amorín
- first_name: A.
full_name: Calabrò, A.
last_name: Calabrò
- first_name: M.
full_name: Castellano, M.
last_name: Castellano
- first_name: N. J.
full_name: Cleri, N. J.
last_name: Cleri
- first_name: M.
full_name: Giavalisco, M.
last_name: Giavalisco
- first_name: N. A.
full_name: Grogin, N. A.
last_name: Grogin
- first_name: N. P.
full_name: Hathi, N. P.
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: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: F.
full_name: Pacucci, F.
last_name: Pacucci
- first_name: L.
full_name: Shen, L.
last_name: Shen
- first_name: S. M.
full_name: Wilkins, S. M.
last_name: Wilkins
- first_name: I.
full_name: Yoon, I.
last_name: Yoon
- first_name: L. Y.A.
full_name: Yung, L. Y.A.
last_name: Yung
- first_name: R.
full_name: Bhatawdekar, R.
last_name: Bhatawdekar
- first_name: R. A.
full_name: Lucas, R. A.
last_name: Lucas
- first_name: X.
full_name: Wang, X.
last_name: Wang
- first_name: P.
full_name: Arrabal Haro, P.
last_name: Arrabal Haro
- first_name: M. B.
full_name: Bagley, M. B.
last_name: Bagley
- first_name: S. L.
full_name: Finkelstein, S. L.
last_name: Finkelstein
- first_name: J. S.
full_name: Kartaltepe, J. S.
last_name: Kartaltepe
- first_name: E.
full_name: Merlin, E.
last_name: Merlin
- first_name: C.
full_name: Papovich, C.
last_name: Papovich
- first_name: N.
full_name: Pirzkal, N.
last_name: Pirzkal
- first_name: P.
full_name: Santini, P.
last_name: Santini
citation:
ama: Llerena M, Pentericci L, Napolitano L, et al. The ionizing photon production
efficiency of star-forming galaxies at z ∼ 4–10. Astronomy & Astrophysics.
2025;698. doi:10.1051/0004-6361/202453251
apa: Llerena, M., Pentericci, L., Napolitano, L., Mascia, S., Amorín, R., Calabrò,
A., … Santini, P. (2025). The ionizing photon production efficiency of star-forming
galaxies at z ∼ 4–10. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202453251
chicago: Llerena, M., L. Pentericci, L. Napolitano, Sara Mascia, R. Amorín, A. Calabrò,
M. Castellano, et al. “The Ionizing Photon Production Efficiency of Star-Forming
Galaxies at z ∼ 4–10.” Astronomy & Astrophysics. EDP Sciences, 2025.
https://doi.org/10.1051/0004-6361/202453251.
ieee: M. Llerena et al., “The ionizing photon production efficiency of star-forming
galaxies at z ∼ 4–10,” Astronomy & Astrophysics, vol. 698. EDP Sciences,
2025.
ista: Llerena M, Pentericci L, Napolitano L, Mascia S, Amorín R, Calabrò A, Castellano
M, Cleri NJ, Giavalisco M, Grogin NA, Hathi NP, Hirschmann M, Koekemoer AM, Nanayakkara
T, Pacucci F, Shen L, Wilkins SM, Yoon I, Yung LYA, Bhatawdekar R, Lucas RA, Wang
X, Arrabal Haro P, Bagley MB, Finkelstein SL, Kartaltepe JS, Merlin E, Papovich
C, Pirzkal N, Santini P. 2025. The ionizing photon production efficiency of star-forming
galaxies at z ∼ 4–10. Astronomy & Astrophysics. 698, A302.
mla: Llerena, M., et al. “The Ionizing Photon Production Efficiency of Star-Forming
Galaxies at z ∼ 4–10.” Astronomy & Astrophysics, vol. 698, A302, EDP
Sciences, 2025, doi:10.1051/0004-6361/202453251.
short: M. Llerena, L. Pentericci, L. Napolitano, S. Mascia, R. Amorín, A. Calabrò,
M. Castellano, N.J. Cleri, M. Giavalisco, N.A. Grogin, N.P. Hathi, M. Hirschmann,
A.M. Koekemoer, T. Nanayakkara, F. Pacucci, L. Shen, S.M. Wilkins, I. Yoon, L.Y.A.
Yung, R. Bhatawdekar, R.A. Lucas, X. Wang, P. Arrabal Haro, M.B. Bagley, S.L.
Finkelstein, J.S. Kartaltepe, E. Merlin, C. Papovich, N. Pirzkal, P. Santini,
Astronomy & Astrophysics 698 (2025).
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