---
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
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: 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'
...
---
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: '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: '21451'
abstract:
- lang: eng
text: The population of the little red dots (LRDs) may represent a key phase of
supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging
as a key component to explain the most striking properties of LRDs, such as strong
Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect
the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra
of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra
reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission.
We revealed a forest of optical [Fe II] lines, which we argue are emerging from
a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K.
The broad wings of Hα and Hβ have an exponential profile due to electron scattering
in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an
indicator of collisional excitation and resonant scattering dominating the Balmer
line emission. A narrow Hγ component, unseen in the other two Balmer lines due
to outshining by the broad components, could trace the ISM of a normal host galaxy
with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer
transitions, producing a characteristic P Cygni profile in the line centers suggesting
outflowing motions. This same layer is responsible for shaping the Balmer break.
The broadband spectrum can be reasonably matched by a simple photoionized slab
model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy
that could explain the narrow [O III], with only a subdominant contribution to
the UV continuum. Our findings indicate that Balmer lines are not directly tracing
the gas kinematics near the SMBH and that the BH mass scale is likely much lower
than virial indicators suggest.
acknowledgement: 'We thank the scientific referee for useful and constructive comments.
We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics
of gaseous envelopes and accretion into black holes. Funded by the European Union
(ERC, AGENTS, 101076224). Views and opinions expressed are however those of the
author(s) only and do not necessarily reflect those of the European Union or the
European Research Council. Neither the European Union nor the granting authority
can be held responsible for them. This work is based in part on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with program #5664. This work has received funding from the Swiss State Secretariat
for Education, Research and Innovation (SERI) under contract number MB22.00072,
as well as from the Swiss National Science Foundation (SNSF) through project grant
200020_207349.'
article_number: A75
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Seok Jun
full_name: Chang, Seok Jun
last_name: Chang
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Erica
full_name: Nelson, Erica
last_name: Nelson
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer
of a little red dot as the source of [Fe ii] and collisional Balmer lines with
scattering wings. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557537
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa,
Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot
as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557537
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan
P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm
Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer
Lines with Scattering Wings.” Astronomy & Astrophysics. EDP Sciences,
2026. https://doi.org/10.1051/0004-6361/202557537.
ieee: A. Torralba Torregrosa et al., “The warm outer layer of a little red
dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,”
Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer
GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene
JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete
B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little
red dot as the source of [Fe ii] and collisional Balmer lines with scattering
wings. Astronomy & Astrophysics. 707, A75.
mla: Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red
Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.”
Astronomy & Astrophysics, vol. 707, A75, EDP Sciences, 2026, doi:10.1051/0004-6361/202557537.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa,
G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare,
A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko,
Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy
& Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:59:16Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557537
external_id:
arxiv:
- '2510.00103'
file:
- access_level: open_access
checksum: fcab9cb3dcf1d68612e1fdc8191643c1
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:57:49Z
date_updated: 2026-03-16T10:57:49Z
file_id: '21460'
file_name: 2026_AstronomyAstrophysics_Torralba2.pdf
file_size: 2510157
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:57:49Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: The warm outer layer of a little red dot as the source of [Fe ii] and collisional
Balmer lines with scattering wings
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21452'
abstract:
- lang: eng
text: Galaxies exhibit a tight correlation between their star formation rate (SFR)
and stellar mass over a wide redshift range known as the star-forming main sequence
(SFMS). With JWST, the SFMS can now be investigated at high redshifts down to
masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα
emission, which allow us to probe the variability in the star formation histories.
We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5
with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell
2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little
Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α,
with α = 0.45). After we corrected this for the Hα-flux limited nature of our
survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09,
whereas current data on their own are inconclusive on the mass dependence of the
scatter. These slopes differ significantly from the slope of ∼1 that is expected
from the observed evolution of the galaxy stellar mass function and from simulations.
When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic
scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010
M⊙). This difference might be explained by a (combination of) luminosity-dependent
SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated
dust attenuation in high-mass galaxies. Future deep observations with different
facilities can quantify these processes, which will enable us to achieve better
insights into the variability of the star formation histories.
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion,
Pierluigi Rinaldi for his help with data handling and Luca Graziani and William
McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. Funded
by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are
however those of the author(s) only and do not necessarily reflect those of the
European Union or the European Research Council. Neither the European Union nor
the granting authority can be held responsible for them. This work is based on observations
made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from
the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with program # 3516. We acknowledge funding from JWST program GO-3516. Software
used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant
2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy
Collaboration 2013)."
article_number: A129
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Alberto
full_name: Torralba, Alberto
last_name: Torralba
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Jeremy
full_name: Blaizot, Jeremy
last_name: Blaizot
- first_name: Joakim
full_name: Rosdahl, Joakim
last_name: Rosdahl
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Angela
full_name: Adamo, Angela
last_name: Adamo
- first_name: Alba
full_name: Covelo-Paz, Alba
last_name: Covelo-Paz
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Michael
full_name: Romano, Michael
last_name: Romano
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
citation:
ama: 'Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming
main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557790'
apa: 'Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko,
I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence
at z ∼ 5: Reconciling observations with simulations. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557790'
chicago: 'Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba,
Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter
of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.”
Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557790.'
ieee: 'C. Di Cesare et al., “The slope and scatter of the star-forming main
sequence at z ∼ 5: Reconciling observations with simulations,” Astronomy &
Astrophysics, vol. 707. EDP Sciences, 2026.'
ista: 'Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I,
Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz
KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The
slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations
with simulations. Astronomy & Astrophysics. 707, A129.'
mla: 'Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main
Sequence at z ∼ 5: Reconciling Observations with Simulations.” Astronomy &
Astrophysics, vol. 707, A129, EDP Sciences, 2026, doi:10.1051/0004-6361/202557790.'
short: C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko,
J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak,
K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:52:44Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202557790
external_id:
arxiv:
- '2510.19044'
file:
- access_level: open_access
checksum: c056b00ce7324849754521fde10fb7ca
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:48:07Z
date_updated: 2026-03-16T10:48:07Z
file_id: '21459'
file_name: 2026_AstronomyAstrophysics_DiCesare.pdf
file_size: 1821411
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:48:07Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling
observations with simulations'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21481'
abstract:
- lang: eng
text: 'The Hα emission line in galaxies is a powerful tracer of their recent star
formation activity. With the advent of JWST, we are now able to routinely observe
Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation
rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs
leads to biased results because high-redshift galaxies are commonly characterized
by low metallicities and bursty star formation histories, affecting the conversion
factor between the Hα luminosity (LHα) and the SFR. We developed a set of new
SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3
with very little error. We used the SPHINX cosmological simulations to select
a sample of star-forming galaxies representative of the Hα-emitter population
observed with JWST. We then derived linear corrections to the classical SFR(Hα)
calibrations that took variations in the physical properties (e.g., stellar metallicities)
among individual galaxies into account. We obtained two new SFR(Hα) calibrations
that compared to the classical calibrations reduce the root mean squared error
(RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively.
Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show
that the new calibrations affect the high-redshift galaxy population statistics:
(i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed
slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.'
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene
Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala
for useful comments and productive discussions. We gratefully acknowledge support
from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de
Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS,
101076224). Views and opinions expressed are however those of the author(s) only
and do not necessarily reflect those of the European Union or the European Research
Council. Neither the European Union nor the granting authority can be held responsible
for them. This work made extensive use of several open-source software packages,
and we gratefully acknowledge the efforts of their authors: numpy (Harris et al.
2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez
& Granger 2007), and scikit-learn (Pedregosa et al. 2011)."
article_number: A184
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: J.
full_name: Rosdahl, J.
last_name: Rosdahl
- first_name: J.
full_name: Blaizot, J.
last_name: Blaizot
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: H.
full_name: Katz, H.
last_name: Katz
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
citation:
ama: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as
a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557114
apa: Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., & Di
Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological
simulations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557114
chicago: Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and
Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557114.
ieee: I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare,
“H α as a tracer of star formation in the SPHINX cosmological simulations,” Astronomy
& Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026.
H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 707, A184.
mla: Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics, vol. 707, A184, EDP Sciences,
2026, doi:10.1051/0004-6361/202557114.
short: I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-23T14:58:03Z
date_published: 2026-03-05T00:00:00Z
date_updated: 2026-03-23T15:46:31Z
day: '05'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557114
external_id:
arxiv:
- '2509.05403'
file:
- access_level: open_access
checksum: 7429076b381dd498084f40ffd199e714
content_type: application/pdf
creator: dernst
date_created: 2026-03-23T15:44:09Z
date_updated: 2026-03-23T15:44:09Z
file_id: '21492'
file_name: 2026_AstronomyAstrophysics_Kramarenko.pdf
file_size: 904565
relation: main_file
success: 1
file_date_updated: 2026-03-23T15:44:09Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
status: public
title: H α as a tracer of star formation in the SPHINX cosmological simulations
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: 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: diamond
PlanS_conform: '1'
_id: '20930'
abstract:
- lang: eng
text: "Context. Beta Pictoris is an A-type star that hosts a complex planetary system
with two massive gas giants and a prominent debris disc. Variable absorption lines
in its stellar spectrum have been interpreted as signatures of exocomets – comet-like
bodies transiting the star. Stellar flybys can gravitationally perturb objects
in the outer comet reservoir, altering their orbits and potentially injecting
them into the inner system, thereby triggering exocomet showers.\r\nAims. We assessed
the contribution of stellar flybys to the observed exocomet activity by reconstructing
the stellar encounter history of β Pictoris in the past and future.\r\nMethods.
We used Gaia DR3 data, supplemented with radial velocities from complementary
spectroscopic surveys, to compile a catalogue of stars currently within 80 pc
of β Pictoris. Their orbits were integrated backwards and forwards in time in
an axisymmetric Galactic potential (via the GALA package) to identify encounters
within 2 pc of the system.\r\nResults. We identified 99 416 stars currently within
80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including
the eight components of five binaries) encounter β Pictoris within 2 pc between
–1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories
also pass within 2 pc. We estimated the sample to be more than 60% complete within
0.5 Myr of today.\r\nConclusions. Despite β Pictoris being the eponym of its famous
moving group, none of the identified encounters involved its moving group members;
all are unrelated field stars. We found no encounter capable of shaping the observed
disc structures, although stellar flybys may contribute to the long-term evolution
of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction
of the β Pictoris encounter history to date and provides a robust foundation for
future dynamical simulations."
acknowledgement: We thank the referee for their suggestions and comments, which helped
us improve the quality and clarity of the paper. JLGM and EV acknowledge the support
from the Spanish Ministry of Science and Innovation/State Agency of Research (MCIN/AEI)
under the grant PID2021-127289-NB-I00. ST acknowledges the funding from the European
Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie
grant agreement No. 101034413. AJM acknowledges support from the Swedish National
Space Agency (Career Grant 2023-00146) and from the Swedish Research Council (Project
Grant 2022-04043). JLGM also sincerely thanks AMP for his careful final reading
of this manuscript. This work has made use of data from the European Space Agency
(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data
Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided
by national institutions, in particular the institutions participating in the Gaia
Multilateral Agreement. We acknowledge the use of the public data products from
RAVE (https://www.rave-survey.org), GALAH (https://galah-survey.org), APOGEE ((https://www.sdss.org)
and LAMOST (http://www.lamost.org) surveys. This research has also made use of the
SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg,
France, as well as the NASA Astrophysics Data System Bibliographic Services and
the arXiv pre-print server operated by Cornell University. Computational analyses
in this work relied extensively on the NumPy and SciPy libraries for numerical computing,
matplotlib and seaborn for data visualization, and the Gala package for Galactic
dynamics. This work also made use of Astropy, a community-developed core PYTHON
package and an ecosystem of tools and resources for astronomy. We thank the developers
and maintainers of these open-source resources for their invaluable contributions
to the astronomical community.
article_number: A237
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J. L.
full_name: Gragera-Más, J. L.
last_name: Gragera-Más
- first_name: Santiago
full_name: Torres Rodriguez, Santiago
id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
last_name: Torres Rodriguez
orcid: 0000-0002-3150-8988
- first_name: A. J.
full_name: Mustill, A. J.
last_name: Mustill
- first_name: E.
full_name: Villaver, E.
last_name: Villaver
citation:
ama: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. A kinematic history
of stellar encounters with Beta Pictoris. Astronomy & Astrophysics.
2025;704. doi:10.1051/0004-6361/202555940
apa: Gragera-Más, J. L., Torres Rodriguez, S., Mustill, A. J., & Villaver, E.
(2025). A kinematic history of stellar encounters with Beta Pictoris. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555940
chicago: Gragera-Más, J. L., Santiago Torres Rodriguez, A. J. Mustill, and E. Villaver.
“A Kinematic History of Stellar Encounters with Beta Pictoris.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202555940.
ieee: J. L. Gragera-Más, S. Torres Rodriguez, A. J. Mustill, and E. Villaver, “A
kinematic history of stellar encounters with Beta Pictoris,” Astronomy &
Astrophysics, vol. 704. EDP Sciences, 2025.
ista: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. 2025. A kinematic
history of stellar encounters with Beta Pictoris. Astronomy & Astrophysics.
704, A237.
mla: Gragera-Más, J. L., et al. “A Kinematic History of Stellar Encounters with
Beta Pictoris.” Astronomy & Astrophysics, vol. 704, A237, EDP Sciences,
2025, doi:10.1051/0004-6361/202555940.
short: J.L. Gragera-Más, S. Torres Rodriguez, A.J. Mustill, E. Villaver, Astronomy
& Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:34Z
date_published: 2025-12-01T00:00:00Z
date_updated: 2026-02-16T12:15:07Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202555940
ec_funded: 1
external_id:
arxiv:
- '2510.02509'
file:
- access_level: open_access
checksum: 2fb4d5a1603043aa7931a31f2c180877
content_type: application/pdf
creator: dernst
date_created: 2026-01-05T11:06:16Z
date_updated: 2026-01-05T11:06:16Z
file_id: '20942'
file_name: 2025_AstronomyAstrophysics_GrageraMas.pdf
file_size: 11021467
relation: main_file
success: 1
file_date_updated: 2026-01-05T11:06:16Z
has_accepted_license: '1'
intvolume: ' 704'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
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 kinematic history of stellar encounters with Beta Pictoris
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: 704
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20931'
abstract:
- lang: eng
text: "Context. Asymmetries in the observed rotational splittings of a multiplet
contain information about the star’s rotation profile and internal magnetic field.
Moreover, the frequency regularities of multiplets can be used for mode identification.
However, to exploit this information, highly accurate theoretical predictions
are needed.\r\n\r\nAims. We aim to quantify the difference in the predicted mode
asymmetries between a 1D perturbative method and a 2D method that includes a 2D
stellar structure model, which takes rotation into account. We then place these
differences between 1D and 2D methods in the context of asteroseismic measurements
of internal magnetic fields. We only focus on the asymmetries and not on possible
additional frequency peaks that can arise when the magnetic and rotation axis
are misaligned.\r\n\r\nMethods. We coupled the 1D pulsation codes GYRE and StORM
to the 2D stellar structure code ESTER and compared the oscillation predictions
with the results from the 2D TOP pulsation code. We focused on zero-age main-sequence
models representative of rotating β Cephei pulsators spinning at up to 20 per
cent of the critical Keplerian rotation rate. Specifically, we investigated low-radial-order
gravity and pressure modes.\r\n\r\nResults. We find a generally good agreement
between the oscillation frequencies resulting from the 1D and 2D pulsation codes.
We report differences in predicted mode multiplet asymmetries of mostly below
0.06 d−1. Since the magnetic asymmetries are small compared to the differences
in the rotational asymmetries resulting from the 1D and 2D predictions, accurate
measurements of the magnetic field are in most cases challenging.\r\n\r\nConclusions.
Differences in the predicted mode asymmetries of a rotating star between 1D perturbative
methods and 2D non-perturbative methods can greatly hinder accurate measurements
of internal magnetic fields in main-sequence pulsators with low-order modes. Nevertheless,
reasonably accurate measurements could be possible with npg ≥ 2 modes if the internal
rotation is roughly below 10 per cent of the Keplerian critical rotation frequency
for (aligned) magnetic fields of the order of a few hundred kilogauss. While the
differences between the 1D and 2D frequency predictions are mostly too large for
internal magnetic field detections, the rotational asymmetries predicted by StORM
are in general accurate enough for asteroseismic modelling of the stellar rotation
in main-sequence stars with identified low-order modes."
acknowledgement: 'We thank the anonymous referee for their comments on the manuscript,
Dario Fritzewski for providing the distribution of fractions of critical rotation
for the β Cephei sample, and Zhao Guo for the discussions. The research leading
to these results has received funding from the European Research Council (ERC) under
the Horizon Europe programme (Synergy Grant agreement N°101071505: 4D-STAR). 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. V.V. acknowledges support from the Research Foundation
Flanders (FWO) under grant agreement N°1156923N (PhD Fellowship). S.B.D. acknowledges
funding from the European Union’s Horizon 2020 research and innovation programme
under the Marie Skłodowska-Curie grant agreement N°101034413. L.B. gratefully acknowledges
support from the European Research Council (ERC) under the Horizon Europe programme
(Calcifer; Starting Grant agreement N°101165631). J.B., M.R., S.M. and J.S.G.M have
been supported by CNES, focused on the preparation of the PLATO mission. Computations
with ESTER and TOP have made use of the HPC resources from the CALMIP supercomputing
centre (Grant 2023-P0107). This research made use of the numpy (Harris et al. 2020)
and matplotlib (Hunter 2007) Python software packages.'
article_number: A336
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J. S.G.
full_name: Mombarg, J. S.G.
last_name: Mombarg
- first_name: V.
full_name: Vanlaer, V.
last_name: Vanlaer
- first_name: Srijan B
full_name: Das, Srijan B
id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
last_name: Das
orcid: 0000-0003-0896-7972
- first_name: M.
full_name: Rieutord, M.
last_name: Rieutord
- first_name: C.
full_name: Aerts, C.
last_name: Aerts
- 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: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: D. R.
full_name: Reese, D. R.
last_name: Reese
- first_name: J.
full_name: Ballot, J.
last_name: Ballot
citation:
ama: Mombarg JSG, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient
for asteroseismic modelling of β Cephei pulsators? Implications for measurements
of rotation and internal magnetic fields. Astronomy & Astrophysics.
2025;704. doi:10.1051/0004-6361/202557247
apa: Mombarg, J. S. G., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet,
L. A., … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic
modelling of β Cephei pulsators? Implications for measurements of rotation and
internal magnetic fields. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557247
chicago: Mombarg, J. S.G., V. Vanlaer, Srijan B Das, M. Rieutord, C. Aerts, Lisa
Annabelle Bugnet, S. Mathis, D. R. Reese, and J. Ballot. “Is a 1D Perturbative
Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications
for Measurements of Rotation and Internal Magnetic Fields.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202557247.
ieee: J. S. G. Mombarg et al., “Is a 1D perturbative method sufficient for
asteroseismic modelling of β Cephei pulsators? Implications for measurements of
rotation and internal magnetic fields,” Astronomy & Astrophysics, vol.
704. EDP Sciences, 2025.
ista: Mombarg JSG, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S,
Reese DR, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic
modelling of β Cephei pulsators? Implications for measurements of rotation and
internal magnetic fields. Astronomy & Astrophysics. 704, A336.
mla: Mombarg, J. S. G., et al. “Is a 1D Perturbative Method Sufficient for Asteroseismic
Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and
Internal Magnetic Fields.” Astronomy & Astrophysics, vol. 704, A336,
EDP Sciences, 2025, doi:10.1051/0004-6361/202557247.
short: J.S.G. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet,
S. Mathis, D.R. Reese, J. Ballot, Astronomy & Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:35Z
date_published: 2025-12-19T00:00:00Z
date_updated: 2026-02-16T12:14:36Z
day: '19'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202557247
ec_funded: 1
external_id:
arxiv:
- '2511.09617'
file:
- access_level: open_access
checksum: d838b4783920c43b7cc866e9cf08b383
content_type: application/pdf
creator: dernst
date_created: 2026-01-05T08:36:28Z
date_updated: 2026-01-05T08:36:28Z
file_id: '20937'
file_name: 2025_AstronomyAstrophysics_Mombarg.pdf
file_size: 2620909
relation: main_file
success: 1
file_date_updated: 2026-01-05T08:36:28Z
has_accepted_license: '1'
intvolume: ' 704'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
- _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: EDP Sciences
quality_controlled: '1'
related_material:
record:
- id: '20936'
relation: research_data
status: public
scopus_import: '1'
status: public
title: Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei
pulsators? Implications for measurements of rotation and internal magnetic fields
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: 704
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20932'
abstract:
- lang: eng
text: Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial
for understanding the properties of cosmic reionizers because the opacity of the
intergalactic medium (IGM) prevents the direct detection of LyC emission from
sources during the Epoch of Reionization (EoR). In this study, we confirm two
new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute
escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The
LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate
leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue
UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03
and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively.
These two LyC candidate leakers were detected in a catalog of 91 spectroscopically
confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed
properties that were proposed as indirect indicators of LyC emission, such as
Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according
to these properties, stacked the LyC observations of this subsample, and assessed
the limits of the escape fractions in the stacks. We aim to enhance our understanding
of LyC escape mechanisms and improve our predictions of the LyC fesc during the
EoR by analyzing the individual candidates and the stacks in the context of the
currently limited sample of known LyC leakers at z ∼ 3.
acknowledgement: 'We acknowledge support from the National Science Foundation of China
– 12225301, INAF Large grant “Spectroscopic survey with JWST” jand from PRIN 2022
MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European
Union – Next Generation EU, and Postgraduate Scholarship Program under the grant
of China Scholarship Council. P.W. and B.V. acknowledge support from the INAF Mini
Grant ‘1.05.24.07.01 RSN1: Spatially Resolved Near-IR Emission of Intermediate-Redshift
Jellyfish Galaxies’ (PI Watson). We acknowledge A. Acebron, C. Grillo, and P. Rosati
for their fundamental contribution to the strong lensing analysis and results. We
also extend our gratitude to the JWST and HST teams for their efforts in designing,
building, and operating these transformative missions.'
article_number: A328
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Y.
full_name: Liu, Y.
last_name: Liu
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: L.
full_name: Pentericci, L.
last_name: Pentericci
- first_name: P.
full_name: Watson, P.
last_name: Watson
- first_name: A.
full_name: Alavi, A.
last_name: Alavi
- first_name: P.
full_name: Bergamini, P.
last_name: Bergamini
- first_name: M.
full_name: Bradač, M.
last_name: Bradač
- first_name: A.
full_name: Calabrò, A.
last_name: Calabrò
- first_name: K.
full_name: Glazebrook, K.
last_name: Glazebrook
- first_name: A.
full_name: Henry, A.
last_name: Henry
- first_name: M.
full_name: Llerena, M.
last_name: Llerena
- first_name: E.
full_name: Merlin, E.
last_name: Merlin
- first_name: B.
full_name: Metha, B.
last_name: Metha
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: L.
full_name: Napolitano, L.
last_name: Napolitano
- first_name: N.
full_name: Roy, N.
last_name: Roy
- first_name: B.
full_name: Siana, B.
last_name: Siana
- first_name: E.
full_name: Vanzella, E.
last_name: Vanzella
- first_name: B.
full_name: Vulcani, B.
last_name: Vulcani
- first_name: X.
full_name: Wang, X.
last_name: Wang
citation:
ama: Liu Y, Mascia S, Pentericci L, et al. A Lyman continuum analysis of ∼100 galaxies
at z spec∼ 3 in the Abell 2744 cluster field. Astronomy & Astrophysics.
2025;704. doi:10.1051/0004-6361/202556410
apa: Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P.,
… Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in
the Abell 2744 cluster field. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202556410
chicago: Liu, Y., Sara Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini,
M. Bradač, et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in
the Abell 2744 Cluster Field.” Astronomy & Astrophysics. EDP Sciences,
2025. https://doi.org/10.1051/0004-6361/202556410.
ieee: Y. Liu et al., “A Lyman continuum analysis of ∼100 galaxies at z spec∼
3 in the Abell 2744 cluster field,” Astronomy & Astrophysics, vol.
704. EDP Sciences, 2025.
ista: Liu Y, Mascia S, Pentericci L, Watson P, Alavi A, Bergamini P, Bradač M, Calabrò
A, Glazebrook K, Henry A, Llerena M, Merlin E, Metha B, Nanayakkara T, Napolitano
L, Roy N, Siana B, Vanzella E, Vulcani B, Wang X. 2025. A Lyman continuum analysis
of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy &
Astrophysics. 704, A328.
mla: Liu, Y., et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in
the Abell 2744 Cluster Field.” Astronomy & Astrophysics, vol. 704,
A328, EDP Sciences, 2025, doi:10.1051/0004-6361/202556410.
short: Y. Liu, S. Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač,
A. Calabrò, K. Glazebrook, A. Henry, M. Llerena, E. Merlin, B. Metha, T. Nanayakkara,
L. Napolitano, N. Roy, B. Siana, E. Vanzella, B. Vulcani, X. Wang, Astronomy &
Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:35Z
date_published: 2025-12-01T00:00:00Z
date_updated: 2026-02-16T12:14:52Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202556410
external_id:
arxiv:
- '2507.11045'
file:
- access_level: open_access
checksum: 3e6061f3c4bfb521b3333ea4913c241a
content_type: application/pdf
creator: dernst
date_created: 2026-01-05T09:26:17Z
date_updated: 2026-01-05T09:26:17Z
file_id: '20938'
file_name: 2025_AstronomyAstrophysics_Liu.pdf
file_size: 4642530
relation: main_file
success: 1
file_date_updated: 2026-01-05T09:26:17Z
has_accepted_license: '1'
intvolume: ' 704'
language:
- iso: eng
month: '12'
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 Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744
cluster field
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: 704
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21060'
abstract:
- lang: eng
text: "Compact, star-forming galaxies with high star formation rate surface densities
(ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because
intense stellar feedback creates low-density channels that allow photons to escape.
Irregular or disturbed morphologies, such as those resulting from mergers, can
also facilitate LyC escape by creating anisotropic gas distributions. We investigated
the influence of galaxy morphology on LyC production and escape at redshifts 5
≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys.
Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15
M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent
with canonical expectations. Since direct measurements of fesc are not possible
during the Epoch of Reionization (EoR), we predicted fesc for high-redshift galaxies
by applying survival analysis to a subsample of LyC emitters from the Low-Redshift
Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era
galaxies. We find that these galaxies exhibit, on average, modest predicted escape
fractions (∼0.04). In addition, we evaluated the correlation between morphological
features and LyC emission. Our findings indicate that neither ξion nor the predicted
fesc values show a significant correlation with the presence of merger signatures.
This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances
are not the primary mechanism driving LyC emission and leakage. Instead, compactness
and star formation activity likely play a more pivotal role in regulating LyC
escape. "
acknowledgement: 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 GTO 1243, ERS 1345, DDT
2750, and GTO 1180, 1181, 3215, 1210, 1286. 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 support from the INAF Large Grant 2022 “Extragalactic Surveys
with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization
and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project
2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union
– Next Generation EU. 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
funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results
received the support of a fellowship from the “la Caixa” Foundation (ID 100010434).
The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants
PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of
Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and
by “ERDF A way of making Europe”.
article_number: A122
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: L.
full_name: Pentericci, L.
last_name: Pentericci
- first_name: M.
full_name: Llerena, M.
last_name: Llerena
- first_name: A.
full_name: Calabrò, A.
last_name: Calabrò
- 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: S.
full_name: Flury, S.
last_name: Flury
- first_name: F.
full_name: Pacucci, F.
last_name: Pacucci
- first_name: A.
full_name: Jaskot, A.
last_name: Jaskot
- first_name: R. O.
full_name: Amorín, R. O.
last_name: Amorín
- first_name: R.
full_name: Bhatawdekar, R.
last_name: Bhatawdekar
- first_name: M.
full_name: Castellano, M.
last_name: Castellano
- first_name: N.
full_name: Cleri, N.
last_name: Cleri
- first_name: L.
full_name: Costantin, L.
last_name: Costantin
- first_name: K.
full_name: Davis, K.
last_name: Davis
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: M.
full_name: Dickinson, M.
last_name: Dickinson
- first_name: A.
full_name: Fontana, A.
last_name: Fontana
- first_name: Y.
full_name: Guo, Y.
last_name: Guo
- first_name: M.
full_name: Giavalisco, M.
last_name: Giavalisco
- first_name: B. W.
full_name: Holwerda, B. W.
last_name: Holwerda
- first_name: W.
full_name: Hu, W.
last_name: Hu
- first_name: M.
full_name: Huertas-Company, M.
last_name: Huertas-Company
- first_name: Intae
full_name: Jung, Intae
last_name: Jung
- first_name: J.
full_name: Kartaltepe, J.
last_name: Kartaltepe
- first_name: D.
full_name: Kashino, D.
last_name: Kashino
- 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: J.
full_name: Lotz, J.
last_name: Lotz
- first_name: L.
full_name: Napolitano, L.
last_name: Napolitano
- first_name: S.
full_name: Jogee, S.
last_name: Jogee
- first_name: S.
full_name: Wilkins, S.
last_name: Wilkins
citation:
ama: Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy
morphology on the production and escape of ionizing photons in the early Universe.
Astronomy & Astrophysics. 2025;701. doi:10.1051/0004-6361/202553760
apa: Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury,
S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the
production and escape of ionizing photons in the early Universe. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202553760
chicago: Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee,
S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on
the Production and Escape of Ionizing Photons in the Early Universe.” Astronomy
& Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202553760.
ieee: S. Mascia et al., “Little impact of mergers and galaxy morphology on
the production and escape of ionizing photons in the early Universe,” Astronomy
& Astrophysics, vol. 701. EDP Sciences, 2025.
ista: Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci
F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis
K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W,
Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz
J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy
morphology on the production and escape of ionizing photons in the early Universe.
Astronomy & Astrophysics. 701, A122.
mla: Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the
Production and Escape of Ionizing Photons in the Early Universe.” Astronomy
& Astrophysics, vol. 701, A122, EDP Sciences, 2025, doi:10.1051/0004-6361/202553760.
short: S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury,
F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L.
Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco,
B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino,
A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy
& Astrophysics 701 (2025).
corr_author: '1'
date_created: 2026-01-28T15:24:24Z
date_published: 2025-09-01T00:00:00Z
date_updated: 2026-02-09T07:33:46Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202553760
external_id:
arxiv:
- '2501.08268'
file:
- access_level: open_access
checksum: 990e384ca19e14b35296712d3b9e2919
content_type: application/pdf
creator: dernst
date_created: 2026-02-09T07:28:08Z
date_updated: 2026-02-09T07:28:08Z
file_id: '21166'
file_name: 2025_AstronomyAstrophysics_Mascia.pdf
file_size: 9994234
relation: main_file
success: 1
file_date_updated: 2026-02-09T07:28:08Z
has_accepted_license: '1'
intvolume: ' 701'
language:
- iso: eng
month: '09'
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: Little impact of mergers and galaxy morphology on the production and escape
of ionizing photons in the early Universe
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: 701
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21252'
abstract:
- lang: eng
text: "Context. Recent observational results from asteroseismic studies show that
an important fraction of solar-like stars do not present detectable stochastically
excited acoustic oscillations. This non-detectability seems to correlate with
a high rotation rate in the convective envelope and a high surface magnetic activity.
At the same time, the properties of stellar convection are affected by rotation
and magnetism.\r\nAims. We investigate the role of rotation in the excitation
of acoustic modes in the convective envelope of solar-like stars, to evaluate
its impact on the energy injected in the oscillations.\r\nMethods. We derived
theoretical prescriptions for the excitation of acoustic waves in the convective
envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory
to model the influence of rotation on convection. We used the MESA stellar evolution
code and the GYRE stellar oscillation code to estimate the power injected in the
oscillations from our theoretical prescriptions.\r\nResults. We demonstrate that
the power injected in the acoustic modes is insensitive to rotation if a Gaussian
time-correlation function is assumed, while it can decrease by up to 60% for a
Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that
the modification of the excitation rate by rotation depends not only on the rotation
rate but also on the radial and angular orders of the considered oscillation mode.
This result can allow for better constraints on the properties of stellar convection
by studying observationally acoustic mode excitation.\r\nConclusions. These results
demonstrate how important it is to take into account the modification of stellar
convection by rotation when evaluating the amplitude of the stellar oscillations
it stochastically excites. They open the path for understanding the large variety
of observed acoustic-mode amplitudes at the surface of solar-like stars as a function
of surface rotation rates."
acknowledgement: 'The authors thank the referee for detailed comments that allow them
to improve their work. The authors thank Jordan Philidet and Kevin Belkacem for
fruitful discussions. L.B. and Stéphane M. acknowledge support from the European
Research Council (ERC) under the Horizon Europe program (Synergy Grant agreement
101071505: 4D-STAR), from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from
PNPS (CNRS/INSU). While partially funded by the European Union, views and opinions
expressed are however those of the author 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. Savita M. acknowledges
support from the Spanish Ministry of Science and Innovation with the grant no. PID2019-107061GB-C66
and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023
(CEX2019-000920-S).'
article_number: A25
article_processing_charge: Yes
article_type: original
author:
- first_name: L.
full_name: Bessila, L.
last_name: Bessila
- first_name: A.
full_name: Deckx van Ruys, A.
last_name: Deckx van Ruys
- first_name: V.
full_name: Buriasco, V.
last_name: Buriasco
- 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: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
citation:
ama: Bessila L, Deckx van Ruys A, Buriasco V, et al. The impact of rotation on the
stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy
& Astrophysics. 2025;700. doi:10.1051/0004-6361/202452093
apa: Bessila, L., Deckx van Ruys, A., Buriasco, V., Mathis, S., Bugnet, L. A., García,
R. A., & Mathur, S. (2025). The impact of rotation on the stochastic excitation
of stellar acoustic modes in solar-like pulsators. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202452093
chicago: Bessila, L., A. Deckx van Ruys, V. Buriasco, S. Mathis, Lisa Annabelle
Bugnet, R. A. García, and S. Mathur. “The Impact of Rotation on the Stochastic
Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452093.
ieee: L. Bessila et al., “The impact of rotation on the stochastic excitation
of stellar acoustic modes in solar-like pulsators,” Astronomy & Astrophysics,
vol. 700. EDP Sciences, 2025.
ista: Bessila L, Deckx van Ruys A, Buriasco V, Mathis S, Bugnet LA, García RA, Mathur
S. 2025. The impact of rotation on the stochastic excitation of stellar acoustic
modes in solar-like pulsators. Astronomy & Astrophysics. 700, A25.
mla: Bessila, L., et al. “The Impact of Rotation on the Stochastic Excitation of
Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy & Astrophysics,
vol. 700, A25, EDP Sciences, 2025, doi:10.1051/0004-6361/202452093.
short: L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A.
García, S. Mathur, Astronomy & Astrophysics 700 (2025).
date_created: 2026-02-16T15:46:59Z
date_published: 2025-08-01T00:00:00Z
date_updated: 2026-02-17T13:10:18Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202452093
file:
- access_level: open_access
checksum: b8a0927307c1d82025bcb5af47b20b26
content_type: application/pdf
creator: dernst
date_created: 2026-02-17T13:07:45Z
date_updated: 2026-02-17T13:07:45Z
file_id: '21306'
file_name: 2025_AstronomyAstrophysics_Bessila.pdf
file_size: 7161755
relation: main_file
success: 1
file_date_updated: 2026-02-17T13:07:45Z
has_accepted_license: '1'
intvolume: ' 700'
language:
- iso: eng
month: '08'
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'
status: public
title: The impact of rotation on the stochastic excitation of stellar acoustic modes
in solar-like pulsators
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: 700
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '18852'
abstract:
- lang: eng
text: 'Recent observations have found a growing number of hypervelocity stars with
speeds of ≈1500 − 2500 km s−1 that could have only been produced through thermonuclear
supernovae in white dwarf binaries. Most of the observed hypervelocity runaways
in this class display a surprising inflated structure: their current radii are
roughly an order of magnitude greater than they would have been as white dwarfs
filling their Roche lobe. While many simulations exist studying the dynamical
phase leading to supernova detonation in these systems, no detailed calculations
of the long-term structure of the runaways have yet been performed. We used an
existing AREPO hydrodynamical simulation of a supernova in a white dwarf binary
as a starting point for the evolution of these stars with the one-dimensional
stellar evolution code MESA. We show that the supernova shock is not energetic
enough to inflate the white dwarf over timescales longer than a few thousand years,
significantly shorter than the 105 − 6 year lifetimes inferred for observed hypervelocity
runaways. Although they experience a shock from a supernova less than ≈0.02 R⊙
away, our models do not experience significant interior heating, and all contract
back to radii of around 0.01 R⊙ within about 104 years. Explaining the observed
inflated states requires either an additional source of significant heating or
some other physics that is not yet accounted for in the subsequent evolution.'
acknowledgement: 'This project was originally started as part of the Kavli Summer
Program which took place in the Max Planck Institute for Astrophysics in Garching
in July 2023, supported by the Kavli Foundation. We are grateful to Stephen Justham,
Selma de Mink, and Jim Fuller for enriching discussions. We would like to thank
the anonymous referee for their helpful report. A.B. was supported by the Deutsche
Forschungsgemeinschaft (DFG) through grant GE2506/18-1. K.J.S. was supported by
NASA through the Astrophysics Theory Program (80NSSC20K0544) and by NASA/ESA Hubble
Space Telescope programs #15871 and #15918. W.E.K. was supported by NSF Grants OAC-2311323,
AST-2206523, and NASA/ESA HST-AR-Theory HSTAR-16613.002-A. K.E. was supported in
part by HST-GO-17441.001-A. AB and ASR would like to thank Rob Farmer for his support
with PyMESA.'
article_number: A114
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Aakash
full_name: Bhat, Aakash
last_name: Bhat
- first_name: Evan B.
full_name: Bauer, Evan B.
last_name: Bauer
- first_name: Rüdiger
full_name: Pakmor, Rüdiger
last_name: Pakmor
- first_name: Ken J.
full_name: Shen, Ken J.
last_name: Shen
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Abinaya Swaruba
full_name: Rajamuthukumar, Abinaya Swaruba
last_name: Rajamuthukumar
- first_name: Kareem
full_name: El-Badry, Kareem
last_name: El-Badry
- first_name: Wolfgang E.
full_name: Kerzendorf, Wolfgang E.
last_name: Kerzendorf
citation:
ama: Bhat A, Bauer EB, Pakmor R, et al. Supernova shocks cannot explain the inflated
state of hypervelocity runaways from white dwarf binaries. Astronomy &
Astrophysics. 2025;693(1). doi:10.1051/0004-6361/202451371
apa: Bhat, A., Bauer, E. B., Pakmor, R., Shen, K. J., Caiazzo, I., Rajamuthukumar,
A. S., … Kerzendorf, W. E. (2025). Supernova shocks cannot explain the inflated
state of hypervelocity runaways from white dwarf binaries. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451371
chicago: Bhat, Aakash, Evan B. Bauer, Rüdiger Pakmor, Ken J. Shen, Ilaria Caiazzo,
Abinaya Swaruba Rajamuthukumar, Kareem El-Badry, and Wolfgang E. Kerzendorf. “Supernova
Shocks Cannot Explain the Inflated State of Hypervelocity Runaways from White
Dwarf Binaries.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202451371.
ieee: A. Bhat et al., “Supernova shocks cannot explain the inflated state
of hypervelocity runaways from white dwarf binaries,” Astronomy & Astrophysics,
vol. 693, no. 1. EDP Sciences, 2025.
ista: Bhat A, Bauer EB, Pakmor R, Shen KJ, Caiazzo I, Rajamuthukumar AS, El-Badry
K, Kerzendorf WE. 2025. Supernova shocks cannot explain the inflated state of
hypervelocity runaways from white dwarf binaries. Astronomy & Astrophysics.
693(1), A114.
mla: Bhat, Aakash, et al. “Supernova Shocks Cannot Explain the Inflated State of
Hypervelocity Runaways from White Dwarf Binaries.” Astronomy & Astrophysics,
vol. 693, no. 1, A114, EDP Sciences, 2025, doi:10.1051/0004-6361/202451371.
short: A. Bhat, E.B. Bauer, R. Pakmor, K.J. Shen, I. Caiazzo, A.S. Rajamuthukumar,
K. El-Badry, W.E. Kerzendorf, Astronomy & Astrophysics 693 (2025).
date_created: 2025-01-19T23:01:51Z
date_published: 2025-01-07T00:00:00Z
date_updated: 2026-02-16T12:08:05Z
day: '07'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.1051/0004-6361/202451371
external_id:
arxiv:
- '2407.03424'
isi:
- '001406577300001'
file:
- access_level: open_access
checksum: e532b9c8123c29cfb0ee758e6d00453c
content_type: application/pdf
creator: dernst
date_created: 2025-01-20T09:57:00Z
date_updated: 2025-01-20T09:57:00Z
file_id: '18861'
file_name: 2025_AstronomyAstrophysics_Bhat.pdf
file_size: 1692527
relation: main_file
success: 1
file_date_updated: 2025-01-20T09:57:00Z
has_accepted_license: '1'
intvolume: ' 693'
isi: 1
issue: '1'
language:
- iso: eng
month: '01'
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: Supernova shocks cannot explain the inflated state of hypervelocity runaways
from white dwarf binaries
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: 693
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '18854'
abstract:
- lang: eng
text: "Context. One of the surprising early findings with JWST has been the discovery
of a strong “roll-over” or a softening of the absorption edge of Lyα in a large
number of galaxies at z ≳ 6, in addition to systematic offsets from photometric
redshift estimates and fundamental galaxy scaling relations. This has been interpreted
as strong cumulative damped Lyα absorption (DLA) wings from high column densities
of neutral atomic hydrogen (H I), signifying major gas accretion events in the
formation of these galaxies.\r\nAims. To explore this new phenomenon systematically,
we assembled the JWST/NIRSpec PRImordial gas Mass AssembLy (PRIMAL) legacy survey
of 584 galaxies at z = 5.0 − 13.4, designed to study the physical properties and
gas in and around galaxies during the reionization epoch.\r\nMethods. We characterized
this benchmark sample in full and spectroscopically derived the galaxy redshifts,
metallicities, star formation rates, and ultraviolet (UV) slopes. We defined a
new diagnostic, the Lyα damping parameter DLyα, to measure and quantify the net
effect of Lyα emission strength, the H I fraction in the intergalactic medium,
or the local H I column density for each source. The JWST-PRIMAL survey is based
on the spectroscopic DAWN JWST Archive (DJA-Spec). We describe DJA-Spec in this
paper, detailing the reduction methods, the post-processing steps, and basic analysis
tools. All the software, reduced spectra, and spectroscopically derived quantities
and catalogs are made publicly available in dedicated repositories.\r\nResults.
We find that the fraction of galaxies showing strong integrated DLAs with NHI > 1021 cm−2
only increases slightly from ≈60% at z ≈ 6 up to ≈65 − 90% at z > 8. Similarly,
the prevalence and prominence of Lyα emission is found to increase with decreasing
redshift, in qualitative agreement with previous observational results. Strong
Lyα emitters (LAEs) are predominantly found to be associated with low-metallicity
and UV faint galaxies. By contrast, strong DLAs are observed in galaxies with
a variety of intrinsic physical properties, but predominantly at high redshifts
and low metallicities.\r\nConclusions. Our results indicate that strong DLAs likely
reflect a particular early assembly phase of reionization-era galaxies, at which
point they are largely dominated by pristine H I gas accretion. At z = 8 − 10,
this gas gradually cools and forms into stars that ionize their local surroundings,
forming large ionized bubbles and producing strong observed Lyα emission at z < 8."
acknowledgement: 'We would like to thank the referee for a detailed and constructive
report, greatly improving the presentation of the results in this work. We would
like to thank Peter Jakobsen for his vision and heroic endeavor in optimally designing
the JWST/NIRSpec instrument and some of its first on-sky observations and for enlightening
discussions about the intricacies of the NIRSpec data. Further, we would like to
thank John Chisholm for helpful clarifications and discussions related to the escape
fraction of ionizing photons and Aayush Saxena for enlightening conversations on
the escape and absorption of Lyman-α photons. This work has received funding from
the Swiss State Secretariat for Education, Research and Innovation (SERI) under
contract number MB22.00072. The Cosmic Dawn Center (DAWN) is funded by the Danish
National Research Foundation under grant DNRF140. The data products presented herein
were retrieved from the DAWN JWST Archive (DJA). DJA is an initiative of the Cosmic
Dawn Center, which is funded by the Danish National Research Foundation under grant
DNRF140. P.D. acknowledge support from the NWO grant 016.VIDI.189.162 (“ODIN") and
warmly thanks the European Commission’s and University of Groningen’s CO-FUND Rosalind
Franklin program. Support from the ERC Advanced Grant INTERSTELLAR H2020/740120
is kindly acknowledged (A.F.). S.G. acknowledges financial support from the Villum
Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. M.K. was supported
by the ANID BASAL project FB210003. G.E.M. acknowledges financial support from the
Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. J.W.
acknowledges support from the Science and Technology Facilities Council (STFC),
by the ERC through Advanced Grant 695671 “QUENCH”, by the UKRI Frontier Research
grant RISEandFALL. Support for this work was provided by NASA through the NASA Hubble
Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Incorporated, under NASA contract NAS5-26555. F.C. acknowledges support from a UKRI
Frontier Research Guarantee Grant (PI Cullen; grant reference EP/X021025/1). J.H.W.
acknowledges support by NSF grant AST-2108020 and NASA grants 80NSSC20K0520 and
80NSSC21K1053. NRT acknowledges support through STFC consolidated grant ST/W000857/1.
M.J.H. is supported by the Swedish Research Council, VetenskapsrÅdet, and is fellow
of the Knut & Alice Wallenberg foundation. 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 (MAST) at the Space Telescope Science
Institute, which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. Software: This work made
use of and acknowledge the following software: NumPy (Harris et al. 2020), Matplotlib
(Hunter 2007), LMfit (Newville et al. 2014), SciPy (Virtanen et al. 2020), grizli
(Brammer 2023a), Astrodrizzle (Gonzaga et al. 2012), and MsaExp (v0.3; Brammer 2023b).'
article_number: A60
article_processing_charge: No
article_type: original
author:
- first_name: K. E.
full_name: Heintz, K. E.
last_name: Heintz
- first_name: G. B.
full_name: Brammer, G. B.
last_name: Brammer
- first_name: D.
full_name: Watson, D.
last_name: Watson
- first_name: P. A.
full_name: Oesch, P. A.
last_name: Oesch
- first_name: L. C.
full_name: Keating, L. C.
last_name: Keating
- first_name: M. J.
full_name: Hayes, M. J.
last_name: Hayes
- first_name: Unknown
full_name: Abdurro'Uf, Unknown
last_name: Abdurro'Uf
- first_name: K. Z.
full_name: Arellano-Córdova, K. Z.
last_name: Arellano-Córdova
- first_name: A. C.
full_name: Carnall, A. C.
last_name: Carnall
- first_name: C. R.
full_name: Christiansen, C. R.
last_name: Christiansen
- first_name: F.
full_name: Cullen, F.
last_name: Cullen
- first_name: R.
full_name: Davé, R.
last_name: Davé
- first_name: P.
full_name: Dayal, P.
last_name: Dayal
- first_name: A.
full_name: Ferrara, A.
last_name: Ferrara
- first_name: K.
full_name: Finlator, K.
last_name: Finlator
- first_name: J. P.U.
full_name: Fynbo, J. P.U.
last_name: Fynbo
- first_name: S. R.
full_name: Flury, S. R.
last_name: Flury
- first_name: V.
full_name: Gelli, V.
last_name: Gelli
- first_name: S.
full_name: Gillman, S.
last_name: Gillman
- first_name: R.
full_name: Gottumukkala, R.
last_name: Gottumukkala
- first_name: K.
full_name: Gould, K.
last_name: Gould
- first_name: T. R.
full_name: Greve, T. R.
last_name: Greve
- first_name: S. E.
full_name: Hardin, S. E.
last_name: Hardin
- first_name: T. Y.Y.
full_name: Hsiao, T. Y.Y.
last_name: Hsiao
- first_name: A.
full_name: Hutter, A.
last_name: Hutter
- first_name: P.
full_name: Jakobsson, P.
last_name: Jakobsson
- first_name: M.
full_name: Killi, M.
last_name: Killi
- first_name: N.
full_name: Khosravaninezhad, N.
last_name: Khosravaninezhad
- first_name: P.
full_name: Laursen, P.
last_name: Laursen
- first_name: M. M.
full_name: Lee, M. M.
last_name: Lee
- first_name: G. E.
full_name: Magdis, G. E.
last_name: Magdis
- 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: R. P.
full_name: Naidu, R. P.
last_name: Naidu
- first_name: D.
full_name: Narayanan, D.
last_name: Narayanan
- first_name: C.
full_name: Pollock, C.
last_name: Pollock
- first_name: M. K.M.
full_name: Prescott, M. K.M.
last_name: Prescott
- first_name: V.
full_name: Rusakov, V.
last_name: Rusakov
- first_name: M.
full_name: Shuntov, M.
last_name: Shuntov
- first_name: A.
full_name: Sneppen, A.
last_name: Sneppen
- first_name: R.
full_name: Smit, R.
last_name: Smit
- first_name: N. R.
full_name: Tanvir, N. R.
last_name: Tanvir
- first_name: C.
full_name: Terp, C.
last_name: Terp
- first_name: S.
full_name: Toft, S.
last_name: Toft
- first_name: F.
full_name: Valentino, F.
last_name: Valentino
- first_name: A. P.
full_name: Vijayan, A. P.
last_name: Vijayan
- first_name: J. R.
full_name: Weaver, J. R.
last_name: Weaver
- first_name: J. H.
full_name: Wise, J. H.
last_name: Wise
- first_name: J.
full_name: Witstok, J.
last_name: Witstok
citation:
ama: 'Heintz KE, Brammer GB, Watson D, et al. The JWST-PRIMAL archival survey: A
JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption
and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy & Astrophysics.
2025;693. doi:10.1051/0004-6361/202450243'
apa: 'Heintz, K. E., Brammer, G. B., Watson, D., Oesch, P. A., Keating, L. C., Hayes,
M. J., … Witstok, J. (2025). The JWST-PRIMAL archival survey: A JWST/NIRSpec reference
sample for the physical properties and Lyman-α absorption and emission of ∼600
galaxies at z = 5.0-13.4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202450243'
chicago: 'Heintz, K. E., G. B. Brammer, D. Watson, P. A. Oesch, L. C. Keating, M.
J. Hayes, Unknown Abdurro’Uf, et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec
Reference Sample for the Physical Properties and Lyman-α Absorption and Emission
of ∼600 Galaxies at z = 5.0-13.4.” Astronomy & Astrophysics. EDP Sciences,
2025. https://doi.org/10.1051/0004-6361/202450243.'
ieee: 'K. E. Heintz et al., “The JWST-PRIMAL archival survey: A JWST/NIRSpec
reference sample for the physical properties and Lyman-α absorption and emission
of ∼600 galaxies at z = 5.0-13.4,” Astronomy & Astrophysics, vol. 693.
EDP Sciences, 2025.'
ista: 'Heintz KE, Brammer GB, Watson D, Oesch PA, Keating LC, Hayes MJ, Abdurro’Uf
U, Arellano-Córdova KZ, Carnall AC, Christiansen CR, Cullen F, Davé R, Dayal P,
Ferrara A, Finlator K, Fynbo JPU, Flury SR, Gelli V, Gillman S, Gottumukkala R,
Gould K, Greve TR, Hardin SE, Hsiao TYY, Hutter A, Jakobsson P, Killi M, Khosravaninezhad
N, Laursen P, Lee MM, Magdis GE, Matthee JJ, Naidu RP, Narayanan D, Pollock C,
Prescott MKM, Rusakov V, Shuntov M, Sneppen A, Smit R, Tanvir NR, Terp C, Toft
S, Valentino F, Vijayan AP, Weaver JR, Wise JH, Witstok J. 2025. The JWST-PRIMAL
archival survey: A JWST/NIRSpec reference sample for the physical properties and
Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy &
Astrophysics. 693, A60.'
mla: 'Heintz, K. E., et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference
Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600
Galaxies at z = 5.0-13.4.” Astronomy & Astrophysics, vol. 693, A60,
EDP Sciences, 2025, doi:10.1051/0004-6361/202450243.'
short: K.E. Heintz, G.B. Brammer, D. Watson, P.A. Oesch, L.C. Keating, M.J. Hayes,
U. Abdurro’Uf, K.Z. Arellano-Córdova, A.C. Carnall, C.R. Christiansen, F. Cullen,
R. Davé, P. Dayal, A. Ferrara, K. Finlator, J.P.U. Fynbo, S.R. Flury, V. Gelli,
S. Gillman, R. Gottumukkala, K. Gould, T.R. Greve, S.E. Hardin, T.Y.Y. Hsiao,
A. Hutter, P. Jakobsson, M. Killi, N. Khosravaninezhad, P. Laursen, M.M. Lee,
G.E. Magdis, J.J. Matthee, R.P. Naidu, D. Narayanan, C. Pollock, M.K.M. Prescott,
V. Rusakov, M. Shuntov, A. Sneppen, R. Smit, N.R. Tanvir, C. Terp, S. Toft, F.
Valentino, A.P. Vijayan, J.R. Weaver, J.H. Wise, J. Witstok, Astronomy & Astrophysics
693 (2025).
date_created: 2025-01-19T23:01:52Z
date_published: 2025-01-06T00:00:00Z
date_updated: 2026-02-16T12:07:37Z
day: '06'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450243
external_id:
isi:
- '001390856800001'
file:
- access_level: open_access
checksum: 67a791080ade9bfb449d249de2af7456
content_type: application/pdf
creator: dernst
date_created: 2025-01-20T09:17:33Z
date_updated: 2025-01-20T09:17:33Z
file_id: '18858'
file_name: 2025_AstronomyAstrophysics_Heintz.pdf
file_size: 4513466
relation: main_file
success: 1
file_date_updated: 2025-01-20T09:17:33Z
has_accepted_license: '1'
intvolume: ' 693'
isi: 1
language:
- iso: eng
month: '01'
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 JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical
properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4'
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: 693
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '18866'
abstract:
- lang: eng
text: Using JWST Near Infrared Camera (NIRCam) images of the globular cluster 47,Tucanæ,
(or NGC,104), taken at two epochs just 7 months apart, we derived proper-motion
membership down to F322W2 ∼ 27. We identified an intriguing feature at the very
low-mass end of the main sequence, around ∼ 0.08,M_⋅, at magnitudes F322W2 ∼ 24
and m_ F150W2 ∼ 25. This feature, dubbed 'kink', is characterized by a prominent
discontinuity in the slope of the main sequence. A similar discontinuity is seen
in theoretical isochrones with oxygen-poor chemistries, related to the rapid onset
of absorption. We therefore hypothesize that the cluster hosts disproportionately
more oxygen-poor stars near the bottom of the main sequence compared to the upper
main sequence and the red giant branch. Our results show no strong or conclusive
evidence of a rise in the brown dwarf luminosity function at faint magnitudes,
in contrast to previous findings likely affected by faint red background galaxies.
In our analysis, we accounted for this contamination by using proper motion membership.
acknowledgement: We dedicate this paper to the memory of our colleague Prof. Harvey
Richer (⋆ April 1944 —† 13 November 2023), a highly accomplished astronomer and
expert in stellar populations and in particular within globular clusters, who passed
away during this project. Harvey grew up in Montreal and was at least the second
star man to graduate from his high school, having been preceded by William Shatner
by more than a decade. He worked at the University of British Columbia for most
of his career, and his focus was the late stages of stellar evolution, in particular
carbon stars and white dwarfs. We thank the referee for his valuable suggestions
and comments, which helped improve the paper, as well as for his prompt revision.
article_number: A68
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: M.
full_name: Scalco, M.
last_name: Scalco
- first_name: R.
full_name: Gerasimov, R.
last_name: Gerasimov
- first_name: L. R.
full_name: Bedin, L. R.
last_name: Bedin
- first_name: E.
full_name: Vesperini, E.
last_name: Vesperini
- first_name: M.
full_name: Correnti, M.
last_name: Correnti
- first_name: D.
full_name: Nardiello, D.
last_name: Nardiello
- first_name: A.
full_name: Burgasser, A.
last_name: Burgasser
- first_name: H.
full_name: Richer, H.
last_name: Richer
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: J.
full_name: Heyl, J.
last_name: Heyl
- first_name: M.
full_name: Libralato, M.
last_name: Libralato
- first_name: J.
full_name: Anderson, J.
last_name: Anderson
- first_name: M.
full_name: Griggio, M.
last_name: Griggio
citation:
ama: Scalco M, Gerasimov R, Bedin LR, et al. JWST photometry and astrometry of 47
Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition.
Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202452907
apa: Scalco, M., Gerasimov, R., Bedin, L. R., Vesperini, E., Correnti, M., Nardiello,
D., … Griggio, M. (2025). JWST photometry and astrometry of 47 Tucanae. Discontinuity
in the stellar sequence at the star--brown dwarf transition. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452907
chicago: Scalco, M., R. Gerasimov, L. R. Bedin, E. Vesperini, M. Correnti, D. Nardiello,
A. Burgasser, et al. “JWST Photometry and Astrometry of 47 Tucanae. Discontinuity
in the Stellar Sequence at the Star--Brown Dwarf Transition.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452907.
ieee: M. Scalco et al., “JWST photometry and astrometry of 47 Tucanae. Discontinuity
in the stellar sequence at the star--brown dwarf transition,” Astronomy &
Astrophysics, vol. 694. EDP Sciences, 2025.
ista: Scalco M, Gerasimov R, Bedin LR, Vesperini E, Correnti M, Nardiello D, Burgasser
A, Richer H, Caiazzo I, Heyl J, Libralato M, Anderson J, Griggio M. 2025. JWST
photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence
at the star--brown dwarf transition. Astronomy & Astrophysics. 694, A68.
mla: Scalco, M., et al. “JWST Photometry and Astrometry of 47 Tucanae. Discontinuity
in the Stellar Sequence at the Star--Brown Dwarf Transition.” Astronomy &
Astrophysics, vol. 694, A68, EDP Sciences, 2025, doi:10.1051/0004-6361/202452907.
short: M. Scalco, R. Gerasimov, L.R. Bedin, E. Vesperini, M. Correnti, D. Nardiello,
A. Burgasser, H. Richer, I. Caiazzo, J. Heyl, M. Libralato, J. Anderson, M. Griggio,
Astronomy & Astrophysics 694 (2025).
date_created: 2025-01-21T15:29:36Z
date_published: 2025-02-04T00:00:00Z
date_updated: 2025-07-10T11:51:28Z
day: '04'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.1051/0004-6361/202452907
external_id:
arxiv:
- '2501.04446'
isi:
- '001414753300007'
file:
- access_level: open_access
checksum: db765ce222df60a1e7c19da1968906a8
content_type: application/pdf
creator: dernst
date_created: 2025-04-16T07:13:31Z
date_updated: 2025-04-16T07:13:31Z
file_id: '19569'
file_name: 2025_AstronomyAstrophysics_Scalco.pdf
file_size: 18080704
relation: main_file
success: 1
file_date_updated: 2025-04-16T07:13:31Z
has_accepted_license: '1'
intvolume: ' 694'
isi: 1
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: JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar
sequence at the star--brown dwarf transition
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: 694
year: '2025'
...
---
OA_place: publisher
OA_type: hybrid
_id: '19069'
abstract:
- lang: eng
text: "Context. The hydrogen Lyman-alpha (Lyα) line, the brightest rest-frame ultraviolet
line of high-redshift galaxies, exhibits a large variety of shapes, which is due
to factors at different scales, from the interstellar medium to the intergalactic
medium (IGM).\r\nAims. The aim of this work is to provide a systematic inventory
and classification of the spectral shapes of Lyα emission lines to better understand
the general population of high-redshift Lyα emitting galaxies (LAEs).\r\nMethods.
Using the unprecedentedly deep data from the MUSE eXtremely Deep Field (MXDF;
up to 140 hour exposure time), we selected 477 galaxies observed in the ∼2.8−6.6
redshift range, 15 of which have a systemic redshift from nebular lines. We developed
a method to classify Lyα emission lines in four spectral and three spatial categories
by combining a pure spectral analysis with a narrow-band image analysis. We measured
spectral properties, such as the peak separation and the blue-to-total flux ratio
for the double-peaked galaxies.\r\nResults. To ensure a robust sample for statistical
analysis, we define two unbiased subsets, inclusive and restrictive, by applying
thresholds for signal-to-noise ratio, peak separation, and Lyα luminosity, yielding
a final unbiased sample of 206 galaxies. Our analysis reveals that between 32%
and 51% of the galaxies exhibit double-peaked profiles, with peak separations
ranging from 150 km s−1 to nearly 1600 km s−1. The fraction of double-peaked galaxies
seems to evolve dependently with the Lyα luminosity, while we do not see a severe
decrease in this fraction with redshift, which is expected given the IGM attenuation
at high redshift. An artificial increase in the number of double-peaked galaxies
at the highest redshifts may cause the observation of a plateau instead of a decrease.
A notable number of these double-peaked profiles show blue-dominated spectra,
suggesting unique gas dynamics and inflow characteristics in some high-redshift
galaxies. The consequent fraction of blue-dominated spectra needs to be confirmed
by obtaining new systemic redshift measurements. Among the double-peaked galaxies,
4% are spurious detections, that is, the blue and red peaks do not come from the
same spatial location. Around 20% out of the 477 sources of the parent sample
lie in a complex environment, meaning there are other clumps or galaxies at the
same redshift within a distance of 30 kpc.\r\nConclusions. Our results suggest
that the double-peaked LAE fraction may trace the evolution of IGM attenuation,
but the faintest galaxies must be observed at high redshift. We also need more
data to confirm the trend seen at low redshift. In addition, it is crucial to
obtain secure systemic redshifts for LAEs to better constrain the nature of the
Lyα double-peaked lines. Statistical samples of double-peaked and triple-peaked
galaxies are a promising probe of the evolution of the physical properties of
galaxies across cosmic time."
acknowledgement: 'EV and AV acknowledges the support from the SNF grants PP00P2 176808
and 211023. HK acknowledges support from Japan Society for the Promotion of Science
(JSPS) Overseas Research Fellowship as well as JSPS Research Fellowships for Young
Scientists. JP acknowledges funding by the Deutsche Forschungsgemeinschaft, Grant
Wi 1369/31-1. This work is based on observations taken by VLT, which is operated
by European Southern Observatory. This research made use of ASTROPY, which is a
community-developed core Python package for Astronomy (Astropy Collaboration 2013,
2018, 2022), and other software and packages: MPDAF (Piqueras et al. 2019), PHOTUTILS
(Bradley 2023), NUMPY (van der Walt et al. 2011), SCIPY (Virtanen et al. 2020).
The plots in this paper were created using MATPLOTLIB (Hunter 2007).'
article_number: A100
article_processing_charge: No
article_type: original
author:
- first_name: Eloïse
full_name: Vitte, Eloïse
last_name: Vitte
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Pascale
full_name: Hibon, Pascale
last_name: Hibon
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Belén
full_name: Alcalde Pampliega, Belén
last_name: Alcalde Pampliega
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- 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: Yucheng
full_name: Guo, Yucheng
last_name: Guo
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: John
full_name: Pharo, John
last_name: Pharo
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
citation:
ama: 'Vitte E, Verhamme A, Hibon P, et al. The MUSE eXtremely Deep Field: Classifying
the spectral shapes of Ly α -emitting galaxies. Astronomy & Astrophysics.
2025;694. doi:10.1051/0004-6361/202450426'
apa: 'Vitte, E., Verhamme, A., Hibon, P., Leclercq, F., Alcalde Pampliega, B., Kerutt,
J., … Contini, T. (2025). The MUSE eXtremely Deep Field: Classifying the spectral
shapes of Ly α -emitting galaxies. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202450426'
chicago: 'Vitte, Eloïse, Anne Verhamme, Pascale Hibon, Floriane Leclercq, Belén
Alcalde Pampliega, Josephine Kerutt, Haruka Kusakabe, et al. “The MUSE EXtremely
Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” Astronomy
& Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202450426.'
ieee: 'E. Vitte et al., “The MUSE eXtremely Deep Field: Classifying the spectral
shapes of Ly α -emitting galaxies,” Astronomy & Astrophysics, vol.
694. EDP Sciences, 2025.'
ista: 'Vitte E, Verhamme A, Hibon P, Leclercq F, Alcalde Pampliega B, Kerutt J,
Kusakabe H, Matthee JJ, Guo Y, Bacon R, Maseda M, Richard J, Pharo J, Schaye J,
Boogaard L, Nanayakkara T, Contini T. 2025. The MUSE eXtremely Deep Field: Classifying
the spectral shapes of Ly α -emitting galaxies. Astronomy & Astrophysics.
694, A100.'
mla: 'Vitte, Eloïse, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral
Shapes of Ly α -Emitting Galaxies.” Astronomy & Astrophysics, vol.
694, A100, EDP Sciences, 2025, doi:10.1051/0004-6361/202450426.'
short: E. Vitte, A. Verhamme, P. Hibon, F. Leclercq, B. Alcalde Pampliega, J. Kerutt,
H. Kusakabe, J.J. Matthee, Y. Guo, R. Bacon, M. Maseda, J. Richard, J. Pharo,
J. Schaye, L. Boogaard, T. Nanayakkara, T. Contini, Astronomy & Astrophysics
694 (2025).
date_created: 2025-02-23T23:01:56Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2026-02-16T12:08:40Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450426
external_id:
isi:
- '001417357000009'
file:
- access_level: open_access
checksum: ed2a5bba313e54ed250be348bd8c1d95
content_type: application/pdf
creator: dernst
date_created: 2025-02-25T07:19:34Z
date_updated: 2025-02-25T07:19:34Z
file_id: '19087'
file_name: 2025_AstronomyAstrophysics_Vitte.pdf
file_size: 3444203
relation: main_file
success: 1
file_date_updated: 2025-02-25T07:19:34Z
has_accepted_license: '1'
intvolume: ' 694'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
issnl:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting
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: 694
year: '2025'
...