---
OA_place: repository
OA_type: free access
_id: '21439'
abstract:
- lang: eng
  text: These files contain supplementary movies accompanying the PhD thesis “Geometry-driven
    self-organization of migrating cells and chiral filaments” by Zuzana Dunajova
    (2026). The videos provide additional visual material supporting the experiments
    and results described in the thesis.
acknowledged_ssus:
- _id: Bio
- _id: ScienComp
article_processing_charge: No
author:
- first_name: Zuzana
  full_name: Dunajova, Zuzana
  id: 4B39F286-F248-11E8-B48F-1D18A9856A87
  last_name: Dunajova
citation:
  ama: Dunajova Z. Supplementary movies to PhD thesis “Geometry-driven self-organization
    of migrating cells and chiral filaments.” 2026. doi:<a href="https://doi.org/10.15479/AT-ISTA-21439">10.15479/AT-ISTA-21439</a>
  apa: Dunajova, Z. (2026). Supplementary movies to PhD thesis “Geometry-driven self-organization
    of migrating cells and chiral filaments.” Institute of Science and Technology
    Austria. <a href="https://doi.org/10.15479/AT-ISTA-21439">https://doi.org/10.15479/AT-ISTA-21439</a>
  chicago: Dunajova, Zuzana. “Supplementary Movies to PhD Thesis ‘Geometry-Driven
    Self-Organization of Migrating Cells and Chiral Filaments.’” Institute of Science
    and Technology Austria, 2026. <a href="https://doi.org/10.15479/AT-ISTA-21439">https://doi.org/10.15479/AT-ISTA-21439</a>.
  ieee: Z. Dunajova, “Supplementary movies to PhD thesis ‘Geometry-driven self-organization
    of migrating cells and chiral filaments.’” Institute of Science and Technology
    Austria, 2026.
  ista: Dunajova Z. 2026. Supplementary movies to PhD thesis “Geometry-driven self-organization
    of migrating cells and chiral filaments”, Institute of Science and Technology
    Austria, <a href="https://doi.org/10.15479/AT-ISTA-21439">10.15479/AT-ISTA-21439</a>.
  mla: Dunajova, Zuzana. <i>Supplementary Movies to PhD Thesis “Geometry-Driven Self-Organization
    of Migrating Cells and Chiral Filaments.”</i> Institute of Science and Technology
    Austria, 2026, doi:<a href="https://doi.org/10.15479/AT-ISTA-21439">10.15479/AT-ISTA-21439</a>.
  short: Z. Dunajova, (2026).
contributor:
- contributor_type: researcher
  first_name: Saren
  id: 4323B49C-F248-11E8-B48F-1D18A9856A87
  last_name: Tasciyan
  orcid: 0000-0003-1671-393X
- contributor_type: researcher
  first_name: Philipp
  id: 40136C2A-F248-11E8-B48F-1D18A9856A87
  last_name: Radler
  orcid: '0000-0001-9198-2182 '
corr_author: '1'
date_created: 2026-03-11T21:05:20Z
date_published: 2026-03-12T00:00:00Z
date_updated: 2026-07-06T12:38:16Z
day: '12'
ddc:
- '570'
department:
- _id: GradSch
- _id: EdHa
doi: 10.15479/AT-ISTA-21439
file:
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  content_type: application/zip
  creator: zdunajov
  date_created: 2026-03-11T20:41:28Z
  date_updated: 2026-03-11T20:41:28Z
  file_id: '21440'
  file_name: Supplementary_movies_Thesis_Dunajova.zip
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  relation: main_file
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  checksum: a64a174bc6abf0a5e77631e4fd121f1f
  content_type: text/plain
  creator: zdunajov
  date_created: 2026-03-11T20:52:39Z
  date_updated: 2026-03-11T20:52:39Z
  file_id: '21441'
  file_name: readme.txt
  file_size: 2289
  relation: main_file
  success: 1
file_date_updated: 2026-03-11T20:52:39Z
has_accepted_license: '1'
license: https://creativecommons.org/licenses/by-nc-sa/4.0/
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: 34d75525-11ca-11ed-8bc3-89b6307fee9d
  grant_number: '26360'
  name: Motile active matter models of migrating cells and chiral filaments
publisher: Institute of Science and Technology Austria
related_material:
  record:
  - id: '13314'
    relation: used_in_publication
    status: public
  - id: '21423'
    relation: used_in_publication
    status: public
  - id: '21427'
    relation: used_in_publication
    status: public
status: public
title: Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating
  cells and chiral filaments”
tmp:
  image: /images/cc_by_nc_sa.png
  legal_code_url: https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode
  name: Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC
    BY-NC-SA 4.0)
  short: CC BY-NC-SA (4.0)
type: research_data
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year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21233'
abstract:
- lang: eng
  text: Potential self-perpetuating dieback of the Amazon rain forest has been a topic
    of concern. The concern is that initial deforestation could critically impair
    the forest’s water recycling capacities, further harming the remaining forest
    through reduced annual precipitation. Many studies have focused on annual mean
    precipitation changes, due to its widespread perception as a central control on
    the Amazon rain forest’s stability. However, the impact of deforestation goes
    beyond changes in the annual mean precipitation. Yet, global coarse-resolution
    climate models are not well suited to investigate changes in short-duration and
    localized events due to their coarse resolution. Here, we circumvent these issues
    by analyzing a full-deforestation scenario simulated by a global storm-resolving
    model. We focus on changes in the tail of the hourly distribution of precipitation,
    temperature, and wind. Hourly precipitation becomes more extreme in the absence
    of the forest than in an intact forest, with an increased occurrence of both no
    rain and intense rainfall. These changes are driven by enhanced moisture convergence
    that strengthens vertical velocity. On average, the near-surface temperature rises
    significantly by about 3.84 °C, and the daily minimum temperature after deforestation
    becomes similar to the daily maximum temperature before deforestation. Except
    for wet-bulb temperature, human heat stress indicators shift to more severe levels,
    with implications for health and a significant reduction in work productivity.
    Finally, the mean 10 m wind speed intensifies by a factor of four, with the 99th
    percentile wind speed doubling. To summarize, our findings, while based on an
    idealized case, provide a stark warning of the effects of continuing deforestation
    of the Amazon.
acknowledgement: AY acknowledges funding by the CLICCS centre of excellence subproject
  A3 funded by DFG. We thank the German Climate Computing Center DKRZ for providing
  computing resources and the Integrated Climate Data Center (ICDC), the Center for
  Earth System Research and Sustainability (CEN), University of Hamburg, for supporting
  the IMERG data. In addition, we would like to thank Jana Sillmann for suggesting
  the analysis of heat stress indices and Keno Riechers for providing a thorough internal
  review of the initial manuscript at the Max Planck Institute for Meteorology. Open
  Access funding is enabled and organized by Projekt DEAL. This research has been
  supported by the Deutsche Forschungsgemeinschaft (grant no. CLICCS 390683824 (A3)).
  The article processing charges for this open-access publication were covered by
  the Max Planck Society.
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Arim
  full_name: Yoon, Arim
  last_name: Yoon
- first_name: Cathy
  full_name: Hohenegger, Cathy
  last_name: Hohenegger
- first_name: Jiawei
  full_name: Bao, Jiawei
  id: bb9a7399-fefd-11ed-be3c-ae648fd1d160
  last_name: Bao
- first_name: Lukas
  full_name: Brunner, Lukas
  last_name: Brunner
citation:
  ama: Yoon A, Hohenegger C, Bao J, Brunner L. Extreme events in the Amazon after
    deforestation. <i>Earth System Dynamics</i>. 2026;17(1):167-179. doi:<a href="https://doi.org/10.5194/esd-17-167-2026">10.5194/esd-17-167-2026</a>
  apa: Yoon, A., Hohenegger, C., Bao, J., &#38; Brunner, L. (2026). Extreme events
    in the Amazon after deforestation. <i>Earth System Dynamics</i>. Copernicus Publications.
    <a href="https://doi.org/10.5194/esd-17-167-2026">https://doi.org/10.5194/esd-17-167-2026</a>
  chicago: Yoon, Arim, Cathy Hohenegger, Jiawei Bao, and Lukas Brunner. “Extreme Events
    in the Amazon after Deforestation.” <i>Earth System Dynamics</i>. Copernicus Publications,
    2026. <a href="https://doi.org/10.5194/esd-17-167-2026">https://doi.org/10.5194/esd-17-167-2026</a>.
  ieee: A. Yoon, C. Hohenegger, J. Bao, and L. Brunner, “Extreme events in the Amazon
    after deforestation,” <i>Earth System Dynamics</i>, vol. 17, no. 1. Copernicus
    Publications, pp. 167–179, 2026.
  ista: Yoon A, Hohenegger C, Bao J, Brunner L. 2026. Extreme events in the Amazon
    after deforestation. Earth System Dynamics. 17(1), 167–179.
  mla: Yoon, Arim, et al. “Extreme Events in the Amazon after Deforestation.” <i>Earth
    System Dynamics</i>, vol. 17, no. 1, Copernicus Publications, 2026, pp. 167–79,
    doi:<a href="https://doi.org/10.5194/esd-17-167-2026">10.5194/esd-17-167-2026</a>.
  short: A. Yoon, C. Hohenegger, J. Bao, L. Brunner, Earth System Dynamics 17 (2026)
    167–179.
das_tickbox: '1'
date_created: 2026-02-16T10:44:58Z
date_published: 2026-02-04T00:00:00Z
date_updated: 2026-07-06T12:55:02Z
day: '04'
ddc:
- '550'
department:
- _id: CaMu
doi: 10.5194/esd-17-167-2026
file:
- access_level: open_access
  checksum: 6c3669c463731ad7c484b2990eb8ee0d
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-23T10:26:29Z
  date_updated: 2026-02-23T10:26:29Z
  file_id: '21348'
  file_name: 2026_EarthSystDynam_Yoon.pdf
  file_size: 2068229
  relation: main_file
  success: 1
file_date_updated: 2026-02-23T10:26:29Z
has_accepted_license: '1'
intvolume: '        17'
issue: '1'
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '02'
oa: 1
oa_version: Published Version
page: 167-179
publication: Earth System Dynamics
publication_identifier:
  eissn:
  - 2190-4987
publication_status: published
publisher: Copernicus Publications
quality_controlled: '1'
scopus_import: '1'
status: public
title: Extreme events in the Amazon after deforestation
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: 17
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '20971'
abstract:
- lang: eng
  text: Mountain glaciers are among the natural systems most vulnerable to climate
    change. However, their interactions with the atmosphere are complex and not fully
    understood. These interactions can trigger rapid adjustments and climate feedbacks
    that either amplify or attenuate atmospheric signals, influencing both glacier
    response and large-scale atmospheric circulation. Observing this functional coupling
    in nature is challenging because the key processes occur over a wide range of
    spatial and temporal scales. However, recent advances in observational techniques
    and modeling have provided new insights into these interactions. In this review,
    we summarize the current state of knowledge on glacier-atmosphere interactions
    in high-mountain regions at different scales, and highlight recent advances in
    observational and numerical modeling. We also highlight important knowledge gaps
    and outline future research directions to improve the prediction of glacier change
    in a warming world.
acknowledgement: This work is the result of collaboration and discussions within HEFEX
  II, and we are grateful to all colleagues who have contributed to and enriched these
  discussions in various ways. T. Sauter acknowledges funding from the German Research
  Foundation (DFG) (Grant 543257843). This research was funded in part by the Austrian
  Science Fund (FWF) (Grant https://doi.org/10.55776/P36624 and https://doi.org/10.55776/P36306)
  for which E. Collier and R. Prinz are grateful. A. R. Groos, T. E. Shaw, R. Mott
  and M. Haugeneder acknowledge Transnational Access from the European Union's H2020
  project INTERACT III (Grant 871120) for participation in the HEFEX II campaign and
  working group. I. Stiperski (Grant Agreement No. 101001691) and A. R. Groos (Grant
  Agreement No. 948290) acknowledge funding from the European Research Council (ERC)
  under the European Union's Horizon 2020 research and innovation program. R. Mott
  acknowledges funding from the Swiss National Science Foundation (SNSF) (Grant 200021_219918).
  B. Goger is supported by EXCLAIM, a project funded by ETH Zurich. J.E. Sicart acknowledges
  LabEx OSUG@2020 (Investissements d'avenir - ANR10 LABX56) for participation in the
  HEFEX II campaign and working group. T. E. Shaw acknowledges funding from the EU
  Horizon 2020 Marie Skłodowska-Curie Grant 101026058 and 101034413. K. F. Haualand
  and T. Sauter are supported by the JOSTICE project funded by the Research Council
  of Norway (RCN Grant 302458).
article_number: e2024RG000869
article_processing_charge: Yes (in subscription journal)
article_type: original
author:
- first_name: T.
  full_name: Sauter, T.
  last_name: Sauter
- first_name: B. W.
  full_name: Brock, B. W.
  last_name: Brock
- first_name: E.
  full_name: Collier, E.
  last_name: Collier
- first_name: B.
  full_name: Goger, B.
  last_name: Goger
- first_name: A. R.
  full_name: Groos, A. R.
  last_name: Groos
- first_name: K. F.
  full_name: Haualand, K. F.
  last_name: Haualand
- first_name: R.
  full_name: Mott, R.
  last_name: Mott
- first_name: L.
  full_name: Nicholson, L.
  last_name: Nicholson
- first_name: R.
  full_name: Prinz, R.
  last_name: Prinz
- first_name: Thomas
  full_name: Shaw, Thomas
  id: 3caa3f91-1f03-11ee-96ce-e0e553054d6e
  last_name: Shaw
  orcid: 0000-0001-7640-6152
- first_name: I.
  full_name: Stiperski, I.
  last_name: Stiperski
- first_name: A.
  full_name: Georgi, A.
  last_name: Georgi
- first_name: M.
  full_name: Haugeneder, M.
  last_name: Haugeneder
- first_name: A.
  full_name: Mandal, A.
  last_name: Mandal
- first_name: D.
  full_name: Reynolds, D.
  last_name: Reynolds
- first_name: M.
  full_name: Saigger, M.
  last_name: Saigger
- first_name: J. E.
  full_name: Sicart, J. E.
  last_name: Sicart
- first_name: A.
  full_name: Voordendag, A.
  last_name: Voordendag
citation:
  ama: Sauter T, Brock BW, Collier E, et al. Glacier-atmosphere interactions and feedbacks
    in high-mountain regions - A review. <i>Reviews of Geophysics</i>. 2026;64(1).
    doi:<a href="https://doi.org/10.1029/2024RG000869">10.1029/2024RG000869</a>
  apa: Sauter, T., Brock, B. W., Collier, E., Goger, B., Groos, A. R., Haualand, K.
    F., … Voordendag, A. (2026). Glacier-atmosphere interactions and feedbacks in
    high-mountain regions - A review. <i>Reviews of Geophysics</i>. Wiley. <a href="https://doi.org/10.1029/2024RG000869">https://doi.org/10.1029/2024RG000869</a>
  chicago: Sauter, T., B. W. Brock, E. Collier, B. Goger, A. R. Groos, K. F. Haualand,
    R. Mott, et al. “Glacier-Atmosphere Interactions and Feedbacks in High-Mountain
    Regions - A Review.” <i>Reviews of Geophysics</i>. Wiley, 2026. <a href="https://doi.org/10.1029/2024RG000869">https://doi.org/10.1029/2024RG000869</a>.
  ieee: T. Sauter <i>et al.</i>, “Glacier-atmosphere interactions and feedbacks in
    high-mountain regions - A review,” <i>Reviews of Geophysics</i>, vol. 64, no.
    1. Wiley, 2026.
  ista: Sauter T, Brock BW, Collier E, Goger B, Groos AR, Haualand KF, Mott R, Nicholson
    L, Prinz R, Shaw T, Stiperski I, Georgi A, Haugeneder M, Mandal A, Reynolds D,
    Saigger M, Sicart JE, Voordendag A. 2026. Glacier-atmosphere interactions and
    feedbacks in high-mountain regions - A review. Reviews of Geophysics. 64(1), e2024RG000869.
  mla: Sauter, T., et al. “Glacier-Atmosphere Interactions and Feedbacks in High-Mountain
    Regions - A Review.” <i>Reviews of Geophysics</i>, vol. 64, no. 1, e2024RG000869,
    Wiley, 2026, doi:<a href="https://doi.org/10.1029/2024RG000869">10.1029/2024RG000869</a>.
  short: T. Sauter, B.W. Brock, E. Collier, B. Goger, A.R. Groos, K.F. Haualand, R.
    Mott, L. Nicholson, R. Prinz, T. Shaw, I. Stiperski, A. Georgi, M. Haugeneder,
    A. Mandal, D. Reynolds, M. Saigger, J.E. Sicart, A. Voordendag, Reviews of Geophysics
    64 (2026).
das_tickbox: '1'
date_created: 2026-01-11T23:01:33Z
date_published: 2026-01-05T00:00:00Z
date_updated: 2026-07-07T06:16:15Z
day: '05'
ddc:
- '550'
department:
- _id: FrPe
doi: 10.1029/2024RG000869
ec_funded: 1
has_accepted_license: '1'
intvolume: '        64'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1029/2024RG000869
month: '01'
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: Reviews of Geophysics
publication_identifier:
  eissn:
  - 1944-9208
  issn:
  - 8755-1209
publication_status: epub_ahead
publisher: Wiley
scopus_import: '1'
status: public
title: Glacier-atmosphere interactions and feedbacks in high-mountain regions - A
  review
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: 64
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. <i>Astronomy &#38;
    Astrophysics</i>. 2026;706. doi:<a href="https://doi.org/10.1051/0004-6361/202557568">10.1051/0004-6361/202557568</a>'
  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. <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202557568">https://doi.org/10.1051/0004-6361/202557568</a>'
  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.” <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences, 2026. <a href="https://doi.org/10.1051/0004-6361/202557568">https://doi.org/10.1051/0004-6361/202557568</a>.'
  ieee: 'W. Yu <i>et al.</i>, “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,” <i>Astronomy &#38;
    Astrophysics</i>, 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 &#38; 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.” <i>Astronomy &#38; Astrophysics</i>,
    vol. 706, A14, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202557568">10.1051/0004-6361/202557568</a>.'
  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 &#38; Astrophysics 706 (2026).
das_tickbox: '1'
date_created: 2026-02-08T23:02:49Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-07-08T06:38:46Z
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 & 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'
...
---
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. <i>Astronomy &#38; Astrophysics</i>. 2026;705. doi:<a href="https://doi.org/10.1051/0004-6361/202555596">10.1051/0004-6361/202555596</a>
  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. <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202555596">https://doi.org/10.1051/0004-6361/202555596</a>
  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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a
    href="https://doi.org/10.1051/0004-6361/202555596">https://doi.org/10.1051/0004-6361/202555596</a>.
  ieee: A. Torralba Torregrosa <i>et al.</i>, “A weak Ly α halo for an extremely bright
    little red dot. Indications of enshrouded supermassive black hole growth,” <i>Astronomy
    &#38; Astrophysics</i>, 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 &#38; 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.” <i>Astronomy
    &#38; Astrophysics</i>, vol. 705, A147, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202555596">10.1051/0004-6361/202555596</a>.
  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 &#38; Astrophysics
    705 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-01-25T23:01:41Z
date_published: 2026-01-14T00:00:00Z
date_updated: 2026-07-08T06:38:23Z
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 & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded
  supermassive black hole growth
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 705
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '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. <i>Astronomy &#38;
    Astrophysics</i>. 2026;707. doi:<a href="https://doi.org/10.1051/0004-6361/202558023">10.1051/0004-6361/202558023</a>'
  apa: 'Liagre, B. R. B., Desai, A. A., Einramhof, L., &#38; Bugnet, L. A. (2026).
    Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
    to data fitting. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202558023">https://doi.org/10.1051/0004-6361/202558023</a>'
  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.” <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences, 2026. <a href="https://doi.org/10.1051/0004-6361/202558023">https://doi.org/10.1051/0004-6361/202558023</a>.'
  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,”
    <i>Astronomy &#38; Astrophysics</i>, 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
    &#38; Astrophysics. 707, A321.'
  mla: 'Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar
    Mixed Modes: From an Asymptotic Description to Data Fitting.” <i>Astronomy &#38;
    Astrophysics</i>, vol. 707, A321, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202558023">10.1051/0004-6361/202558023</a>.'
  short: B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy &#38; Astrophysics
    707 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-07-08T06:39:05Z
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 & 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'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21896'
abstract:
- lang: eng
  text: Redox-mediated flow batteries boost energy density by utilizing dissolved
    redox species as charge carriers for solid charge-storage materials. This strategy
    strongly depends on the thermodynamics and kinetics between the solid booster
    and dissolved redox species. Conventional electrochemical methods often convolute
    intrinsic reactivity with mass transport effects, introducing complexity in determining
    limiting steps. We propose a strategy that confines solid boosters within recessed
    microelectrodes and employs scanning electrochemical microscopy (SECM) to estimate
    reaction kinetics between booster and dissolved active redox species. Confining
    the solid booster in the recessed microelectrode overcomes mass transport limitations
    of dissolved redox species and enables controlled polarization of the booster
    material, allowing deconvolution of key rate-determining factors. As an initial
    model system, Prussian blue-ferricyanide/ferrocyanide [Fe(CN)6]3−/4− was used
    as solid booster and dissolved redox active species, respectively. The methodology
    was further explored for copper hexacyanoferrate with N,N,N-2,2,6,6-heptamethylpiperidinyl
    oxy-4-ammonium chloride and nickel hydroxide with [Fe(CN)6]3−/4− and extended
    to Mn-based Prussian blue analogues in combination with organic redox species.
    Our results demonstrate that SECM coupled with the proposed recessed microelectrode
    strategy provides a powerful platform to disentangle interfacial kinetics and
    guide the rational design of solid booster-dissolved redox species and electrolytes
    for high-performance redox-mediated flow batteries.
acknowledgement: "The authors acknowledge funding from the European Union's Horizon
  Europe research and innovation programme— European Innovation Council (EIC) under
  the grant agreement No 101046742 (MeBattery). P.P. acknowledges the funding from
  the European Research Council through a Starting Grant (agreement no. 950038). Dr.
  Mahdi Moghaddam, University of Turku, is acknowledged for providing the CuHCF, and
  Prof. Hubert Girault, EPFL, is acknowledged for providing the TEMPTMA.\r\nOpen Access
  funding enabled and organized by Projekt DEAL."
article_number: e70303
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Carla
  full_name: Santana Santos, Carla
  last_name: Santana Santos
- first_name: Nomnotho
  full_name: Jiyane, Nomnotho
  last_name: Jiyane
- first_name: Thomas
  full_name: Quast, Thomas
  last_name: Quast
- first_name: Maria
  full_name: Ibáñez, Maria
  id: 43C61214-F248-11E8-B48F-1D18A9856A87
  last_name: Ibáñez
  orcid: 0000-0001-5013-2843
- first_name: Rubén
  full_name: Rubio‐Presa, Rubén
  last_name: Rubio‐Presa
- first_name: Pekka
  full_name: Peljo, Pekka
  last_name: Peljo
- first_name: Wolfgang
  full_name: Schuhmann, Wolfgang
  last_name: Schuhmann
citation:
  ama: Santana Santos C, Jiyane N, Quast T, et al. Evaluating reaction kinetics between
    solid booster and dissolved active species in redox‐mediated flow batteries using
    scanning electrochemical microscopy. <i>Batteries &#38; Supercaps</i>. 2026;9(5).
    doi:<a href="https://doi.org/10.1002/batt.70303">10.1002/batt.70303</a>
  apa: Santana Santos, C., Jiyane, N., Quast, T., Ibáñez, M., Rubio‐Presa, R., Peljo,
    P., &#38; Schuhmann, W. (2026). Evaluating reaction kinetics between solid booster
    and dissolved active species in redox‐mediated flow batteries using scanning electrochemical
    microscopy. <i>Batteries &#38; Supercaps</i>. Wiley. <a href="https://doi.org/10.1002/batt.70303">https://doi.org/10.1002/batt.70303</a>
  chicago: Santana Santos, Carla, Nomnotho Jiyane, Thomas Quast, Maria Ibáñez, Rubén
    Rubio‐Presa, Pekka Peljo, and Wolfgang Schuhmann. “Evaluating Reaction Kinetics
    between Solid Booster and Dissolved Active Species in Redox‐mediated Flow Batteries
    Using Scanning Electrochemical Microscopy.” <i>Batteries &#38; Supercaps</i>.
    Wiley, 2026. <a href="https://doi.org/10.1002/batt.70303">https://doi.org/10.1002/batt.70303</a>.
  ieee: C. Santana Santos <i>et al.</i>, “Evaluating reaction kinetics between solid
    booster and dissolved active species in redox‐mediated flow batteries using scanning
    electrochemical microscopy,” <i>Batteries &#38; Supercaps</i>, vol. 9, no. 5.
    Wiley, 2026.
  ista: Santana Santos C, Jiyane N, Quast T, Ibáñez M, Rubio‐Presa R, Peljo P, Schuhmann
    W. 2026. Evaluating reaction kinetics between solid booster and dissolved active
    species in redox‐mediated flow batteries using scanning electrochemical microscopy.
    Batteries &#38; Supercaps. 9(5), e70303.
  mla: Santana Santos, Carla, et al. “Evaluating Reaction Kinetics between Solid Booster
    and Dissolved Active Species in Redox‐mediated Flow Batteries Using Scanning Electrochemical
    Microscopy.” <i>Batteries &#38; Supercaps</i>, vol. 9, no. 5, e70303, Wiley, 2026,
    doi:<a href="https://doi.org/10.1002/batt.70303">10.1002/batt.70303</a>.
  short: C. Santana Santos, N. Jiyane, T. Quast, M. Ibáñez, R. Rubio‐Presa, P. Peljo,
    W. Schuhmann, Batteries &#38; Supercaps 9 (2026).
das_tickbox: '1'
date_created: 2026-05-20T14:32:37Z
date_published: 2026-05-01T00:00:00Z
date_updated: 2026-07-08T06:48:01Z
day: '01'
ddc:
- '530'
department:
- _id: MaIb
doi: 10.1002/batt.70303
file:
- access_level: open_access
  checksum: 292d65503a63cc7df92b960627634dad
  content_type: application/pdf
  creator: dernst
  date_created: 2026-05-21T06:54:57Z
  date_updated: 2026-05-21T06:54:57Z
  file_id: '21904'
  file_name: 2026_BatteriesSupercaps_SantanaSantos.pdf
  file_size: 756344
  relation: main_file
  success: 1
file_date_updated: 2026-05-21T06:54:57Z
has_accepted_license: '1'
intvolume: '         9'
issue: '5'
language:
- iso: eng
month: '05'
oa: 1
oa_version: Published Version
publication: Batteries & Supercaps
publication_identifier:
  eissn:
  - 2566-6223
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
title: Evaluating reaction kinetics between solid booster and dissolved active species
  in redox‐mediated flow batteries using scanning electrochemical microscopy
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 9
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21161'
abstract:
- lang: eng
  text: In many species, sex-biased expression is widespread and thought to contribute
    to sexual dimorphism. While bulk RNA-sequencing has been instrumental in identifying
    strongly sex-biased genes, it lacks resolution to assess variation across cell-types
    and tissue compartments. Using single-nucleus expression data from the Fly Cell
    Atlas, we investigate sex differences in adult Drosophila melanogaster. We find
    that differences in cell-type composition between the sexes are not a major source
    of sex-bias, as for the vast majority of genes, the degree of sex-bias is similar
    regardless of whether sex differences in cell-type composition are controlled
    for or not. Our analysis confirms a deficit of X-linked male-biased genes in the
    body’s somatic tissues that is widespread across cell-types. We also find the
    excess of X-linked female-biased genes to be associated with nervous system cells
    in the head but with epithelial cells in the body’s somatic tissues, showing that
    single-nucleus data crucially resolves sex-bias at the cell-type level. We investigate
    dosage compensation (DC) across 15 tissues and 17 cell-types. We observe that
    it varies throughout the body. Surprisingly, we observe a lack of DC in a cluster
    of main cells within the male accessory glands. This result highlights the importance
    of understanding context-dependent DC.
acknowledged_ssus:
- _id: ScienComp
- _id: Bio
acknowledgement: This work was partly funded by an Austrian Science Foundation FWF
  ESPRIT fellowship (10.55776/ESP6331524) to C.B. We would like to thank the Vicoso
  group for their invaluable input and discussions throughout this work. We thank
  Filip Ruzicka for his insightful comments on the manuscript. All computational resources
  were provided by the Scientific Computing Unit at ISTA. This research was also supported
  through resources provided by the Imaging & Optics Facility (IOF) at ISTA.
article_number: '20252471'
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Carolina
  full_name: De Castro Barbosa Rodrigues Barata, Carolina
  id: 20565186-803f-11ed-ab7e-96a4ff7694ef
  last_name: De Castro Barbosa Rodrigues Barata
  orcid: 0000-0003-1945-2245
- first_name: Beatriz
  full_name: Vicoso, Beatriz
  id: 49E1C5C6-F248-11E8-B48F-1D18A9856A87
  last_name: Vicoso
  orcid: 0000-0002-4579-8306
citation:
  ama: de Castro Barbosa Rodrigues Barata C, Vicoso B. Single-nucleus resolution of
    sex-biased expression and dosage compensation in Drosophila melanogaster. <i>Proceedings
    of the Royal Society B Biological Sciences</i>. 2026;293(2063). doi:<a href="https://doi.org/10.1098/rspb.2025.2471">10.1098/rspb.2025.2471</a>
  apa: de Castro Barbosa Rodrigues Barata, C., &#38; Vicoso, B. (2026). Single-nucleus
    resolution of sex-biased expression and dosage compensation in Drosophila melanogaster.
    <i>Proceedings of the Royal Society B Biological Sciences</i>. Royal Society of
    London. <a href="https://doi.org/10.1098/rspb.2025.2471">https://doi.org/10.1098/rspb.2025.2471</a>
  chicago: Castro Barbosa Rodrigues Barata, Carolina de, and Beatriz Vicoso. “Single-Nucleus
    Resolution of Sex-Biased Expression and Dosage Compensation in Drosophila Melanogaster.”
    <i>Proceedings of the Royal Society B Biological Sciences</i>. Royal Society of
    London, 2026. <a href="https://doi.org/10.1098/rspb.2025.2471">https://doi.org/10.1098/rspb.2025.2471</a>.
  ieee: C. de Castro Barbosa Rodrigues Barata and B. Vicoso, “Single-nucleus resolution
    of sex-biased expression and dosage compensation in Drosophila melanogaster,”
    <i>Proceedings of the Royal Society B Biological Sciences</i>, vol. 293, no. 2063.
    Royal Society of London, 2026.
  ista: de Castro Barbosa Rodrigues Barata C, Vicoso B. 2026. Single-nucleus resolution
    of sex-biased expression and dosage compensation in Drosophila melanogaster. Proceedings
    of the Royal Society B Biological Sciences. 293(2063), 20252471.
  mla: de Castro Barbosa Rodrigues Barata, Carolina, and Beatriz Vicoso. “Single-Nucleus
    Resolution of Sex-Biased Expression and Dosage Compensation in Drosophila Melanogaster.”
    <i>Proceedings of the Royal Society B Biological Sciences</i>, vol. 293, no. 2063,
    20252471, Royal Society of London, 2026, doi:<a href="https://doi.org/10.1098/rspb.2025.2471">10.1098/rspb.2025.2471</a>.
  short: C. de Castro Barbosa Rodrigues Barata, B. Vicoso, Proceedings of the Royal
    Society B Biological Sciences 293 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-02-08T23:02:49Z
date_published: 2026-01-28T00:00:00Z
date_updated: 2026-07-08T09:17:41Z
day: '28'
ddc:
- '570'
department:
- _id: BeVi
doi: 10.1098/rspb.2025.2471
external_id:
  pmid:
  - '41592777'
file:
- access_level: open_access
  checksum: d76afebca0a6f112df0146ae2d929f36
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-16T09:26:02Z
  date_updated: 2026-02-16T09:26:02Z
  file_id: '21226'
  file_name: 2026_RoyalSocPubProceedingsB_Barata.pdf
  file_size: 2230841
  relation: main_file
  success: 1
file_date_updated: 2026-02-16T09:26:02Z
has_accepted_license: '1'
intvolume: '       293'
issue: '2063'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
pmid: 1
project:
- _id: 90ef7108-16d5-11f0-9cad-e6e116913473
  grant_number: ESP 6331524
  name: Does genetic drift set a limit on the adaptive evolution of sex-biased expression?
publication: Proceedings of the Royal Society B Biological Sciences
publication_identifier:
  eissn:
  - 1471-2954
publication_status: published
publisher: Royal Society of London
quality_controlled: '1'
scopus_import: '1'
status: public
title: Single-nucleus resolution of sex-biased expression and dosage compensation
  in Drosophila melanogaster
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: 293
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '22254'
abstract:
- lang: eng
  text: The global rise of antimicrobial resistance has intensified the search for
    new microbial metabolites from underexplored environments and taxonomic groups.
    Extreme and geographically isolated habitats such as Antarctic terrestrial ecosystems
    represent promising reservoirs of biosynthetic diversity, particularly among rare
    and difficult-to-cultivate actinomycetes that may produce chemically diverse metabolites
    with potential biotechnological applications. Here, we report the characterization
    of kineochelins, a previously undescribed group of siderophores produced by the
    Antarctic isolate Actinokineospora sp. UV203, representing a difficult-to-cultivate
    actinomycete lineage. Structural elucidation revealed a set of closely related
    congeners with a mixed-ligand architecture consistent with metal-chelating activity.
    Genome mining combined with transcriptomic analysis identified a dedicated nonribosomal
    peptide synthetase-encoding biosynthetic gene cluster responsible for kineochelin
    production. Comparative genomic analyses indicated that, although kineochelin
    biosynthetic genes share limited similarity with known mixed-ligand siderophores,
    their gene content and organization differ substantially, suggesting a distinct
    biosynthetic lineage. Functional characterization of the culture supernatant and
    an enriched pre-purified kineochelin fraction demonstrated strong and selective
    iron chelation, with high affinity for ferric and ferrous iron. Crude culture
    extracts inhibited the growth of bacterial strains isolated from the same Antarctic
    environment, indicating that kineochelins may contribute to iron-mediated microbial
    competition. In addition, kineochelin-enriched pre-purified fractions showed moderate
    selective inhibitory activity against the opportunistic yeast pathogen Nakaseomyces
    glabratus and a clinical isolate of Saccharomyces cerevisiae associated with invasive
    infection. These findings expand the chemical and biosynthetic diversity known
    within the genus Actinokineospora and demonstrate that Antarctic rare actinomycetes
    represent valuable sources of previously unexplored natural products. The discovery
    of kineochelins highlights the potential of genome-guided exploration of polar
    microorganisms for identifying bioactive metabolites with relevance for antimicrobial
    discovery and biotechnology.
acknowledgement: This work was supported by the Czech Antarctic Research Programme
  2025–2027 (VAN 2025) and the University of Vienna via the Research Platform Secondary
  Metabolomes of Bacterial Communities (MetaBac). S.K. has received funding from the
  European Union's Horizon 2020 research and innovation programme under the Marie
  Skłodowska-Curie grant agreement No. 101020356 (DEFCOMANT, https://doi.org/10.3030/101020356)
  and MASH StG/CoG (MUNI/SC/1946/2024) by Masaryk University. T.R. and A.L. were funded
  in part by the Austrian Science Fund FWF [grant DOI https://doi.org/10.55776/COE7].
  M.B. was funded by the Ministry of Health, Czech Republic—conceptual development
  of research organization (FNBr, 65269705). The Life Science Compute Cluster LiSC
  at the University of Vienna provided the high-performance computing infrastructure
  for this study. We thank Julia Ramesmayer and Sara Malinowski (Joint Microbiome
  Facility of the Medical University of Vienna and the University of Vienna) for assistance
  during high molecular weight extraction and RNA extraction. The authors thank Anna
  Fabisikova and Michael Klemm-Abraham from the Mass Spectrometry Centre and the team
  of the NMR Centre (both core facilities of the Faculty of Chemistry, University
  of Vienna, and members of the Vienna Life Science Instruments) for assistance with
  data acquisition. We are thankful to Dr. Jaime Felipe Guerrero Garzón for helpful
  discussions on the use of a rrn operon promoter strategy. For open access purposes,
  the authors have applied for a CC BY public copyright licence to any author-accepted
  manuscript version arising from this submission. Dr. Martin Kello (Department of
  Pharmacology, Faculty of Medicine, Pavol Jozef Šafárik University, Košice, Slovakia)
  and Dr. Michal Goga (Department of Plant Biology, Faculty of Science and Center
  for Interdisciplinary Biosciences, Technology and Innovation Park, Pavol Jozef Šafárik
  University in Košice, Košice, Slovakia), funded by VEGA 1/0498/23, are acknowledged
  for their assistance with the antiproliferative assays. This work was supported
  by Horizon 2020 Framework Programme, 101020356; Universität Wien, MetaBac; Ministry
  of Education, Youth and Sports, VAN 2025; Masarykova Univerzita, MUNI/SC/1946/2024;
  Austrian Science Fund, 10.55776/COE7; Ministerstvo Zdravotnictví České Republiky,
  FNBr, 65269705; Vedecká grantová agentúra Ministerstva školstva, výskumu, vývoja
  a mládeže Slovenskej republiky a Slovenskej akadémie vied, VEGA 1/0498/23.
article_number: e70386
article_processing_charge: Yes
article_type: original
author:
- first_name: Stanislava
  full_name: Kralova, Stanislava
  last_name: Kralova
- first_name: Peter
  full_name: Spacek, Peter
  last_name: Spacek
- first_name: Johannes
  full_name: Gafriller, Johannes
  last_name: Gafriller
- first_name: Matej
  full_name: Bezdicek, Matej
  last_name: Bezdicek
- first_name: Viktoria
  full_name: Medvedcova, Viktoria
  last_name: Medvedcova
- first_name: Joana
  full_name: Séneca, Joana
  last_name: Séneca
- first_name: Jay
  full_name: Osvatic, Jay
  last_name: Osvatic
- first_name: Ulrike
  full_name: Grienke, Ulrike
  last_name: Grienke
- first_name: Thomas
  full_name: Rattei, Thomas
  last_name: Rattei
- first_name: Olga N.
  full_name: Sekurova, Olga N.
  last_name: Sekurova
- first_name: Sergey B.
  full_name: Zotchev, Sergey B.
  last_name: Zotchev
- first_name: Martin
  full_name: Zehl, Martin
  id: 8e016d5b-5d77-11f0-86d2-96cdb3922a55
  last_name: Zehl
  orcid: 0000-0001-9685-0373
- first_name: Alexander
  full_name: Loy, Alexander
  last_name: Loy
biorxivid: 1
citation:
  ama: Kralova S, Spacek P, Gafriller J, et al. Kineochelins - A new group of siderophores
    from an antarctic bacterium. <i>Microbial Biotechnology</i>. 2026;19(6). doi:<a
    href="https://doi.org/10.1111/1751-7915.70386">10.1111/1751-7915.70386</a>
  apa: Kralova, S., Spacek, P., Gafriller, J., Bezdicek, M., Medvedcova, V., Séneca,
    J., … Loy, A. (2026). Kineochelins - A new group of siderophores from an antarctic
    bacterium. <i>Microbial Biotechnology</i>. Wiley. <a href="https://doi.org/10.1111/1751-7915.70386">https://doi.org/10.1111/1751-7915.70386</a>
  chicago: Kralova, Stanislava, Peter Spacek, Johannes Gafriller, Matej Bezdicek,
    Viktoria Medvedcova, Joana Séneca, Jay Osvatic, et al. “Kineochelins - A New Group
    of Siderophores from an Antarctic Bacterium.” <i>Microbial Biotechnology</i>.
    Wiley, 2026. <a href="https://doi.org/10.1111/1751-7915.70386">https://doi.org/10.1111/1751-7915.70386</a>.
  ieee: S. Kralova <i>et al.</i>, “Kineochelins - A new group of siderophores from
    an antarctic bacterium,” <i>Microbial Biotechnology</i>, vol. 19, no. 6. Wiley,
    2026.
  ista: Kralova S, Spacek P, Gafriller J, Bezdicek M, Medvedcova V, Séneca J, Osvatic
    J, Grienke U, Rattei T, Sekurova ON, Zotchev SB, Zehl M, Loy A. 2026. Kineochelins
    - A new group of siderophores from an antarctic bacterium. Microbial Biotechnology.
    19(6), e70386.
  mla: Kralova, Stanislava, et al. “Kineochelins - A New Group of Siderophores from
    an Antarctic Bacterium.” <i>Microbial Biotechnology</i>, vol. 19, no. 6, e70386,
    Wiley, 2026, doi:<a href="https://doi.org/10.1111/1751-7915.70386">10.1111/1751-7915.70386</a>.
  short: S. Kralova, P. Spacek, J. Gafriller, M. Bezdicek, V. Medvedcova, J. Séneca,
    J. Osvatic, U. Grienke, T. Rattei, O.N. Sekurova, S.B. Zotchev, M. Zehl, A. Loy,
    Microbial Biotechnology 19 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: The genome sequence and transcriptomic data of strain Actinokineospora
  sp. UV203 are available on NCBI (BioProject accession number PRJNA1331526). The
  nearly full-length 16S rRNA gene (1395 bp) of strain Actinokineospora sp. UV203
  is available on NCBI (accession number PX090945). The NMR data of kineochelin E1
  and A1 are deposited in the Natural Products Magnetic Resonance Database (NP-MRD)
  under accession numbers NP0352113 and NP0352114, respectively.
date_created: 2026-07-08T09:19:43Z
date_published: 2026-06-01T00:00:00Z
date_updated: 2026-07-13T06:59:08Z
day: '01'
ddc:
- '570'
department:
- _id: MassSpec
doi: 10.1111/1751-7915.70386
external_id:
  biorxivid:
  - 10.64898/2026.02.23.707395
  pmid:
  - '42210522'
file:
- access_level: open_access
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  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T06:57:19Z
  date_updated: 2026-07-13T06:57:19Z
  file_id: '22271'
  file_name: 2026_MicrobialBiotechnology_Kralova.pdf
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  success: 1
file_date_updated: 2026-07-13T06:57:19Z
has_accepted_license: '1'
intvolume: '        19'
issue: '6'
keyword:
- Actinokineospora
- Antarctica
- antimicrobial discovery
- biosynthetic gene cluster
- genome mining
- microbial competition
- nonribosomalpeptide synthetase
- siderophores
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
pmid: 1
publication: Microbial Biotechnology
publication_identifier:
  eissn:
  - 1751-7915
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Kineochelins - A new group of siderophores from an antarctic bacterium
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: 19
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22265'
abstract:
- lang: eng
  text: 'The well-known bimodality between star-forming discs and quiescent spheroids
    requires the existence of two main processes: galaxy quenching, causing the strong
    reduction of star formation, and morphological transformation, causing the transition
    from disc-dominated structures to bulge-dominated ones. In this paper, we aim
    to understand the link between these two processes and their relation with the
    stellar mass of galaxies and their local environment. Taking advantage of the
    first data released by the Euclid Collaboration, covering more than 60 deg2 with
    space-based imaging and photometry, we analyse a mass-complete sample of nearly
    one million galaxies in the range 0.25 < z < 1 with M* > 109.5 M⊙, using a combination
    of photometric and spectroscopic redshifts. We divide the sample into four sub-populations
    of galaxies, based on their star-formation activity (star-forming and quiescent)
    and morphology (disc-dominated and bulge-dominated). We then analyse the physical
    properties of these populations and their relative abundances in the stellar mass
    versus local density plane. Together with confirming the passivity-density relation
    and the morphology-density relation, we find that quiescent discy galaxies are
    more abundant in the low-mass regime of high-density environment where log10(1 + δ)
    > 1.3. At the same time, star-forming bulge-dominated galaxies are more common
    in field regions with log10(1 + δ) < 0.8, preferentially at high masses. Building
    on these results and interpreting them through comparison with simulations, we
    propose a scenario where the evolution of galaxies in the field significantly
    differs from that in higher-density environments. The morphological transformation
    in the majority of field galaxies takes place before the onset of quenching and
    is mainly driven by secular processes taking place within the main sequence, leading
    to the formation of star-forming bulge-dominated galaxies as intermediate-stage
    galaxies. Conversely, quenching of star formation precedes morphological transformation
    for most galaxies in higher-density environments. This causes the formation of
    quiescent disc-dominated galaxies before their transition into bulge-dominated
    ones.'
acknowledgement: 'FaGe, AnEn, EmDa, LoGa, SaQu, GaDe, MaTa, ChDe, LuPo acknowledge
  support from the ELSA project. “ELSA: Euclid Legacy Science Advanced analysis tools”
  (Grant Agreement no. 101135203) is funded by the European Union. Views and opinions
  expressed are however those of the author(s) only and do not necessarily reflect
  those of the European Union or Innovate UK. Neither the European Union nor the granting
  authority can be held responsible for them. UK participation is funded through the
  UK HORIZON guarantee scheme under Innovate UK grant 10093177. AnEn acknowledge support
  from the INAF MiniGrant 2023 “ADIEU: Anomaly Detections In EUclid”. CaLo acknowledges
  support by FCT-Fundação para a Ciência e a Tecnologia through grants UIDB/04434/2020
  DOI: 10.54499/UIDB/04434/2020, UIDP/04434/2020 DOI: 10.54499/UIDP/04434/2020. The
  Euclid Consortium acknowledges the European Space Agency and a number of agencies
  and institutes that have supported the development of Euclid, in particular the
  Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded
  through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches
  Zentrum für Luft-und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark,
  the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia,
  the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades,
  the National Aeronautics and Space Administration, the National Astronomical Observatory
  of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space
  Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat
  for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO),
  and the United Kingdom Space Agency. A complete and detailed list is available on
  the Euclid website (www.euclid-ec.org). This work has made use of the Euclid Quick
  Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025,
  https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed
  by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub
  received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the
  EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on
  data from UNIONS, a scientific collaboration using three Hawaii-based telescopes:
  CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy
  Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org'
article_number: A12
article_processing_charge: Yes
article_type: original
arxiv: 1
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citation:
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  apa: 'Gentile, F., Daddi, E., Elbaz, D., Enia, A., Magnelli, B., Billand, J. B.,
    … Walton, N. A. (2026). Euclid Quick Data Release (Q1): XII. Quenching precedes
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    and Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202557633">https://doi.org/10.1051/0004-6361/202557633</a>'
  chicago: 'Gentile, F., E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J. B. Billand,
    P. Corcho-Caballero, et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes
    Bulge Formation in Dense Environments but Follows It in the Field.” <i>Astronomy
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  ieee: 'F. Gentile <i>et al.</i>, “Euclid Quick Data Release (Q1): XII. Quenching
    precedes bulge formation in dense environments but follows it in the field,” <i>Astronomy
    and Astrophysics</i>, vol. 711. EDP Sciences, 2026.'
  ista: 'Gentile F et al. 2026. Euclid Quick Data Release (Q1): XII. Quenching precedes
    bulge formation in dense environments but follows it in the field. Astronomy and
    Astrophysics. 711, A12.'
  mla: 'Gentile, F., et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes
    Bulge Formation in Dense Environments but Follows It in the Field.” <i>Astronomy
    and Astrophysics</i>, vol. 711, A12, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202557633">10.1051/0004-6361/202557633</a>.'
  short: F. Gentile, E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J.B. Billand, P. Corcho-Caballero,
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    A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, A.M.C. Le Brun, S.
    Ligori, P.B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano,
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    M. Viel, M. Wiesmann, Y. Akrami, I.T. Andika, S. Anselmi, M. Archidiacono, F.
    Atrio-Barandela, D. Bertacca, M. Bethermin, L. Bisigello, A. Blanchard, L. Blot,
    H. Böhringer, M. Bonici, S. Borgani, M.L. Brown, S. Bruton, A. Calabro, B. Camacho
    Quevedo, F. Caro, C.S. Carvalho, T. Castro, F. Cogato, S. Conseil, T. Contini,
    A.R. Cooray, O. Cucciati, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J.M. Diego,
    P. Dimauro, P.A. Duc, M.Y. Elkhashab, Y. Fang, A. Finoguenov, A. Fontana, F. Fontanot,
    A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, R. Gavazzi,
    E. Gaztanaga, F. Giacomini, F. Gianotti, A.H. Gonzalez, G. Gozaliasl, M. Guidi,
    C.M. Gutierrez, A. Hall, S. Hemmati, H. Hildebrandt, J. Hjorth, J.J.E. Kajava,
    Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, J. Kim, C.C. Kirkpatrick, S. Kruk,
    L. Legrand, M. Lembo, F. Lepori, G. Leroy, G.F. Lesci, J. Lesgourgues, L. Leuzzi,
    T.I. Liaudat, A. Loureiro, J. Macias-Perez, E.A. Magnier, F. Mannucci, R. Maoli,
    C.J.A.P. Martins, L. Maurin, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, K.
    Naidoo, A. Navarro-Alsina, S. Nesseris, D. Paoletti, F. Passalacqua, K. Paterson,
    L. Patrizii, A. Pisani, D. Potter, M. Radovich, G. Rodighiero, S. Sacquegna, M.
    Sahlén, D.B. Sanders, E. Sarpa, C. Scarlata, A. Schneider, M. Schultheis, D. Sciotti,
    E. Sellentin, L.C. Smith, S.A. Stanford, K. Tanidis, G. Testera, R. Teyssier,
    S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P.
    Vielzeuf, N.A. Walton, Astronomy and Astrophysics 711 (2026).
das_tickbox: '1'
dataavailabilitystatement: 'This work has made use of the Euclid Quick Release Q1
  data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b.
  This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT)
  in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government
  (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and
  the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration
  using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc.
  Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at
  CTIO in Chile https://www.darkenergysurvey.org'
date_created: 2026-07-12T22:02:18Z
date_published: 2026-07-01T00:00:00Z
date_updated: 2026-07-13T08:43:41Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557633
external_id:
  arxiv:
  - '2511.02964'
file:
- access_level: open_access
  checksum: 29c087abb97eed26d4aa2a19bbb46666
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T08:42:10Z
  date_updated: 2026-07-13T08:42:10Z
  file_id: '22277'
  file_name: 2026_AstronomyAstrophysics_Euclid.pdf
  file_size: 3482066
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T08:42:10Z
has_accepted_license: '1'
intvolume: '       711'
keyword:
- 'galaxies: evolution'
- 'galaxies: interactions'
- 'galaxies: statistics'
language:
- iso: eng
month: '07'
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'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: no
title: 'Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in
  dense environments but follows it in the 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: 711
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '22263'
abstract:
- lang: eng
  text: Recent studies at high redshift have revealed an enigmatic class of little
    red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere.
    However, it is unclear whether such objects exist at lower redshift, especially
    given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
    of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from
    JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed
    by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral
    energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with
    effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably
    deep absorption, stronger than previously measured in any LRD. The absorption
    trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The
    presence of blue- and red-shifted absorption suggests complex dynamics of the
    obscuring gas along the line of sight. We speculate that the absorption trough
    can be produced by a thick wind launched from a thick, rotating photospheric disk,
    the latter being the source of the red optical continuum. While the source is
    unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble
    Space Telescope imaging shows an extended morphology with (formular displayed)
    kpc, which we interpret as a host galaxy with a stellar mass of ∼10^8 M⊙, in line
    with the narrow Hα emission. The discovery of this object at cosmic noon highlights
    the feasibility of systematic searches for extreme LRDs with wide-area facilities
    such as Euclid and Roman.
acknowledgement: "IOP Science home\r\nThe Astrophysical Journal Letters\r\nThe American
  Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA
  Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and
  Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7\r\nAlberto Torralba,
  Jorryt Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush
  Desai, Anna de Graaff, Jenny E. Greene, Christian Kragh JespersenShow full author
  list\r\n\r\nPublished 2026 June 30 • © 2026. The Author(s). Published by the American
  Astronomical Society.\r\nThe Astrophysical Journal Letters, Volume 1005, Number
  2\r\nCitation Alberto Torralba et al 2026 ApJL 1005 L37\r\nDOI 10.3847/2041-8213/ae7bfd\r\n\r\nPDFOpens
  in a new tab.ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens
  in a new tab.ePub\r\nArticle metrics\r\n122 Total downloads\r\n\r\nShare this article\r\nArticle
  information\r\nAbstract\r\nRecent studies at high redshift have revealed an enigmatic
  class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any
  stellar atmosphere. However, it is unclear whether such objects exist at lower redshift,
  especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
  of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam
  pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter
  spectroscopy. The rest-optical to near-infrared spectral energy distribution of
  PAN-BH*-1 is consistent with a photospheric continuum with effective temperature
  Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger
  than previously measured in any LRD. The absorption trough spans from −520 to +267
  km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted
  absorption suggests complex dynamics of the obscuring gas along the line of sight.
  We speculate that the absorption trough can be produced by a thick wind launched
  from a thick, rotating photospheric disk, the latter being the source of the red
  optical continuum. While the source is unresolved in the rest-optical JWST data
  (reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended
  morphology with \r\n kpc, which we interpret as a host galaxy with a stellar mass
  of ∼108 M⊙, in line with the narrow Hα emission. The discovery of this object at
  cosmic noon highlights the feasibility of systematic searches for extreme LRDs with
  wide-area facilities such as Euclid and Roman.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious
  article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work
  may be used under the terms of the Creative Commons Attribution 4.0 licence. Any
  further distribution of this work must maintain attribution to the author(s) and
  the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe unprecedented
  sensitivity of JWST has enabled the discovery of a new, abundant population of objects
  at redshifts z ≈ 3–9 nicknamed the “little red dots” (LRDs). These are characterized
  by their compact rest-frame optical morphology, broad emission lines, and a characteristic
  rest-UV to optical “V-shape” in their spectral energy distributions (SED; e.g.,
  D. D. Kocevski et al. 2023; V. Kokorev et al. 2024; J. Matthee et al. 2024; I. Labbe
  et al. 2025).\r\n\r\nThe nature of LRDs is highly debated (see K. Inayoshi & L.
  C. Ho 2025, for a recent overview) as the LRDs show systematic differences with
  respect to other types of active galactic nuclei (AGN), such as faintness in X-rays
  (e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024), mid-to-far-infrared dust emission
  (e.g., G. C. K. Leung et al. 2025; C. C. Williams et al. 2024; I. Delvecchio et
  al. 2025; D. J. Setton et al. 2025; M. Xiao et al. 2025), and radio (e.g., G. Mazzolari
  et al. 2026; M. A. Latif et al. 2025; K. Perger et al. 2025, see A. J. Gloudemans
  et al. 2025).\r\n\r\nA recurring spectral feature of LRDs is the presence of a strong
  Balmer break (e.g., D. J. Setton et al. 2025; B. Wang et al. 2024; R. E. Hviding
  et al. 2025; W. Q. Sun et al. 2026), in some cases stronger than any star or stellar
  population can produce. The two most prominent examples known to date are The Cliff
  at z ≈ 3.5 (A. de Graaff et al. 2025a) and MoM-BH* at z ≈ 7.8 (R. P. Naidu et al.
  2025). The joint appearance of strong Balmer lines as well as strong Balmer breaks
  has been modeled as being due to absorption by a dense, neutral gas with a high
  column density in the line of sight to a highly ionizing source (K. Inayoshi & R.
  Maiolino 2025; X. Ji et al. 2025; A. Sneppen et al. 2026; A. Torralba et al. 2026).
  These observations have sparked the development of new theoretical models, ranging
  from a spherical envelope analogous to stellar atmospheres (e.g., M. C. Begelman
  & J. Dexter 2026; D. Kido et al. 2025; H. Liu et al. 2025; D. Nandal & A. Loeb 2026)
  or a thick accretion disk (e.g., H. Liu et al. 2025, 2026; K. Inayoshi et al. 2025;
  Y.-X. Chen et al. 2026).\r\n\r\nBesides their spectral features, the evolution of
  the LRD number densities is also in stark contrast to other types of AGNs (e.g.,
  K. Inayoshi 2025). At 4 ≲ z ≲ 7, LRDs represent a few percent of the galaxy population
  (e.g., D. D. Kocevski et al. 2023, 2025; J. E. Greene et al. 2024; V. Kokorev et
  al. 2024; X. Lin et al. 2024; R. Maiolino et al. 2024; J. Matthee et al. 2024),
  with number densities of ≳10−5 Mpc−3. The number density does not appear to drop
  quickly beyond z > 5 (e.g., J. Zhang et al. 2026), with various LRDs having been
  confirmed at z  >  8 (V. Kokorev et al. 2023; A. J. Taylor et al. 2025; R. Tripodi
  et al. 2025), well beyond the quasar redshift record (F. Wang et al. 2021). Photometric
  LRD candidates exist beyond z  >  10 (T. S. Tanaka et al. 2025). In turn, the number
  density of LRDs seems to decline steeply at z  <  4 (e.g., Y. Ma et al. 2026), with
  estimates of a number density of ∼10−6 cMpc−3 at z ∼ 2 and even ∼10−10 cMpc−3 at
  z ≈ 0.3 (X. Lin et al. 2026). While it is challenging to ensure a uniform selection
  function across such a large redshift baseline and dedicated spectroscopic follow-up
  of such lower redshift candidates has only just started, it is challenging to attribute
  five orders of magnitude to such effects.\r\n\r\nMotivated by the discovery of rare
  objects with extreme Balmer breaks at z  >  3 and the very small number of known
  LRDs at lower redshift, we performed a dedicated search for extreme Balmer break
  objects using a template-match approach on a large compilation of JWST NIRCam data
  over ≈0.3 deg2 and z ≈ 1.5–7.0. This survey is presented in A. Weibel et al. (2026a).
  As part of an ongoing ground-based spectroscopic campaign of LRD candidates at z
  ∼ 2 (Y. Ma et al. 2026), we followed up the most luminous candidate with a photometric
  redshift of z ≈ 2 with the X-Shooter spectrograph on the Very Large Telescope (VLT).
  In this Letter, we present the discovery and spectroscopic confirmation of PAN-BH*-1,
  a luminous LRD at z = 1.73 with an extreme Balmer break comparable to the strongest
  observed in any LRD (and, in general, any astrophysical source). The low redshift
  of this source enables high-resolution spectroscopy from ground-based observatories
  that is otherwise impossible to obtain at high redshift.\r\n\r\nThroughout this
  Letter, we use a ΛCDM cosmology with Ωm = 0.31, ΩΛ = 0.69, and h = 0.677 as described
  by Planck Collaboration et al. (2020). All the magnitudes are given in the AB system
  (J. B. Oke & J. E. Gunn 1983).\r\n\r\n2. Observations\r\n2.1. Photometry and Source
  Selection\r\nWe identified PAN-BH*-1 (ID: PAN-1115, RA, DEC: 40.015835, −1.659363
  J2000) as part of a systematic search across ≈0.3 deg2 of JWST NIRCam legacy imaging
  comprising at least six filters of coverage (A. Weibel et al. 2026b). Notably, this
  dataset includes the Cycle 1 pure parallel survey PANORAMIC (PID: 2514, PIs: Williams
  & Oesch; C. C. Williams et al. 2025) that contributes 28 of the 35 independent lines
  of sight, thereby enabling the discovery of rare objects such as PAN-BH*-1 across
  diverse large-scale structure environments. Specifically, this source was identified
  in the footprint j024000m0142 of the PANORAMIC DR1,15 which is adjacent to the A370
  field (G. O. Abell et al. 1989), where archival images by the Hubble Space Telescope
  (HST) are available from the BUFFALO survey (C. L. Steinhardt et al. 2020). The
  HST/ACS images were processed with grizli and also released as part of the PANORAMIC
  dataset.\r\n\r\nPAN-BH*-1 is in the outskirts of the A370 lensing cluster, but the
  magnification is only μ ≈ 1.05 according to the models from A. Niemiec et al. (2023).
  Throughout the rest of the paper, we report the uncorrected flux measurements, since
  the effect of magnification (∼5%) is negligible given the uncertainties in the observations
  and the lensing model.\r\n\r\nThe search strategy and full photometric selection
  are described in a companion paper (A. Weibel et al. 2026a). Briefly, that work
  presents a new selection of LRDs as a combination of a “black hole star” template
  (BH*; R. P. Naidu et al. 2025) embedded in a host galaxy, instead of the typically
  used “V-shaped” selections (e.g., D. D. Kocevski et al. 2025; V. Kokorev et al.
  2024). The host galaxies are modeled using eazy’s blue_sfhz templates. The BH*s
  are modeled using a novel template set comprising empirical luminosity-based stacks
  constructed in W. Q. Sun et al. (2026), the cloudy template from R. P. Naidu et
  al. (2025), and by using spectra of prominent LRDs spanning the observed effective
  temperature range (I. Labbe et al. 2024; A. de Graaff et al. 2025a; B. Wang et al.
  2026).\r\n\r\nPAN-BH*-1 stood out as one of the few sources where the BH* template
  effectively dominated all the light over the full wavelength range covered by NIRCam
  (hence the name). The redshift of PAN-BH*-1 was estimated to be zphot = 1.85. Follow-up
  VLT/X-Shooter spectroscopy confirmed the redshift as zspec = 1.731 (see Section
  3.2).\r\n\r\nPAN-BH*-1 is also covered by archival data from the VLT with the HAWK-I
  camera in the Ks band (G. B. Brammer et al. 2016) and in data from the Spitzer Space
  Telescope in IRAC bands 1 and 3 (3.6 and 5.7 μm), and MIPS 24 μm (P. Capak 2019).
  PAN-BH*-1 is detected in the Ks band and in the two IRAC filters. Performing Spitzer
  photometry of this source is challenging due to the large point spread function
  (PSF) and a neighboring source, especially in the MIPS band. However, the NIRCam
  photometry of the neighboring source suggests it has a limited contribution to the
  IRAC fluxes. The details of the photometry extraction are described in Appendix
  A, and the measured magnitudes in Table 2.\r\n\r\n2.2. VLT/X-Shooter Spectroscopy\r\nPAN-BH*-1
  was observed for 5.8 ks with the X-Shooter spectrograph (J. Vernet et al. 2011)
  on the VLT as a bright backup target for program 116.294D (PI: Matthee) in visitor
  mode on 2025 December 17. The main aim of this program was to confirm candidate
  LRDs at cosmic noon (Y. Ma et al. 2026). These observations confirmed the redshift
  through the detection of Hα at z = 1.731. A DDT program (ID 116.2AQ0; PI: Matthee)
  obtained additional follow-up data of PAN-BH*-1 in service mode for 26.2 ks during
  2026 January 10–26, yielding a total exposure time of 8.9 hr. X-Shooter observes
  with three arms simultaneously, UVB, VIS, and near-infrared (NIR), covering rest-frame
  wavelengths of ≈0.14–0.9 μm, albeit hampered by skyline emission and telluric absorption,
  primarily in the rest-frame optical.\r\n\r\nThe observing conditions were clear,
  with a seeing ranging from 05 to 07 (median 06). The service mode observations were
  primarily conducted during dark nights, with some gray (FLI = 0.03–0.6, median 0.1),
  and a typical airmass of 1.35. We used UVB, VIS, and NIR slits with widths 10, 09,
  and 09, yielding a nominal resolution of R = 5400, 8900, and 5600, respectively
  (FWHM ∼53 km s−1 for NIR). The target acquisition was done using blind offsets from
  a reference star, due to the target being too faint for direct acquisition. We used
  a standard nodding on the slit pattern, with 4″ nod throws in an ABBA pattern, and
  1″ jitters in the NIR arm to improve the sky subtraction. In each observing block
  of ≈1 hr, the exposure times were 700, 655, and (2×)365 s for the three arms at
  each nod position.\r\n\r\nThe reduction of the X-Shooter data uses a combination
  of EsoRex libraries16 and Python code based on the reduction pipeline employed in
  J. Matthee et al. (2021). Each observing block was reduced separately. We used standard
  stars taken during the observing night for a first-pass flux calibration. Telluric
  corrections were applied using the molecfit tool (A. Smette et al. 2015) implemented
  in the X-Shooter EsoRex pipeline. Telluric stars were observed during the visitor
  nights, but they were not always observed during the service mode observations in
  January. For those observations, we took the telluric star that was observed at
  the closest observing date. Based on the variation in telluric absorption among
  the reference stars taken during this period, we estimate the variation in the transmission
  and propagate the uncertainty in the telluric correction. For each observing block,
  we then extracted an optimally extracted 1D spectrum using the spatial profile of
  the Hα line, thus accounting for seeing variations and (more importantly) minor
  errors in the accuracy of the slit pointing. Before median combining these spectra,
  we normalize them by the median Hα flux of all observations to account for variations
  in slit losses and flux calibrations.\r\n\r\nBesides Hα (integrated S/N = 75) and
  Hβ (integrated S/N = 6; Section 3.2), we also detect continuum emission in the best
  regions in the H and K bands at 1.6 μm and 2.1 μm, respectively, with a low signal-to-noise
  ratio (S/N) of ∼1 per resolution element. Unfortunately, the [O iii] λλ4960, 5008
  doublet is undetectable because the observed wavelengths are impacted by very strong
  telluric absorption. No other lines or continuum are detected in the X-Shooter spectrum.\r\n\r\n3.
  Properties of PAN-BH*-1\r\n3.1. Spectral Shape: A Photospheric Continuum with Strong
  Hα Emission\r\nThe photometric SED of PAN-BH*-1 has remarkable similarities with
  The Cliff (Figure 1): luminous in the rest optical, with a sudden drop toward the
  rest-UV around the Balmer limit, and very weak near-to-mid infrared continuum emission.
  With a rough extrapolation of the two HST photometric points using a power-law fit
  (fλ ∝ λβ), we obtain a UV slope of β = −0.1 ± 1.2, and MUV = −16.7 ± 0.7. For the
  rest-frame optical to NIR data, we fit a Planck blackbody law to the JWST data points,
  after subtracting the measured Hα flux (see Section 3.2) from the F200W photometry.
  The rest-optical and NIR photometry of PAN-BH*-1 is remarkably well described by
  a single temperature blackbody with T = 4204 K (with a best-fit ). We measure the
  strength of the Balmer break from the fν ratio F115W/F814W = 7 ± 1, in line with
  the Balmer break strengths of The Cliff (; A. de Graaff et al. 2025a)17 and MoM-BH*
  (7.8 ± 1.8; R. P. Naidu et al. 2025), measured from JWST/NIRSpec PRISM spectra as
  fν,4000–4100/fν,3620−3720. In Figure 2, we compare the Balmer break strength with
  the spectroscopic sample of A. de Graaff et al. (2025b), showing that out of 134
  sources, only two have breaks significantly above 5. This suggests that PAN-BH*-1
  has among the most extreme Balmer breaks known, although we caution that our value
  is derived from wide-band photometry with pivot wavelengths corresponding to 4212
  and 3042 Å, respectively, rather than from spectroscopy.\r\n\r\nZoom InZoom OutReset
  image size\r\nFigure 1. SED of PAN-BH*-1 Top: cutouts from all the HST and JWST
  images in which PAN-BH*-1 is covered. It shows a remarkably compact morphology in
  all the wavelengths, resolved only in the HST F606W and F814W bands (Section 3.3).
  Bottom: photometry from JWST/NIRCam (blue squares), HST/ACS (purple pentagons),
  and Spitzer/IRAC+MIPS (red hexagons, and red triangle for the 5σ upper limit). The
  empty square is the F200W flux after subtracting the Hα flux measured from X-Shooter
  spectroscopy. We show the spectrum of The Cliff for comparison (gray line), shifted
  to z = 1.73 and normalized to the F150W flux of PAN-BH*-1. We also show the best-fitting
  blackbody spectrum (blue dashed line) and the best model from the synthetic LRD
  atmosphere models from H. Liu et al. (2026), shifted to z = 1.73 (green line), undersampled
  by a factor of 500 for clarity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
  image\r\nZoom InZoom OutReset image size\r\nFigure 2. Spectroscopic sample of LRDs
  by redshift and Balmer break strength. We plot the redshift and Balmer break strength
  of PAN-BH*-1, and the JWST sample from A. de Graaff et al. (2025b) (purple diamonds),
  and three local LRDs in X. Lin et al. (2026), for comparison. We also highlight
  three sources with a particularly strong Balmer break: The Cliff (A. de Graaff et
  al. 2025a), MoM-BH* (R. P. Naidu et al. 2025), and CAPERS-LRDz9 (A. J. Taylor et
  al. 2025). The Balmer break strength of the JWST spectroscopic sample is computed
  as fν,4000–4100/fν,3620–3720, whereas the value for PAN-BH*-1 is directly obtained
  from the F115W/F814W photometry.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
  image\r\n3.2. Hα and Hβ Emission Lines\r\nThe Hα profile appears as a complex combination
  of a broad line with strong absorption close to the systemic redshift. We fit the
  Hα emission line with a similar model as the one used in A. Torralba et al. (2026)
  and J. Matthee et al. (2026). The Hα model consists of two Gaussian emission components
  (with narrow and intermediate line widths), and a broad symmetric exponential convolved
  with the intermediate profile and parameterized as in F. D’Eugenio et al. (2025a).
  The absorption is implemented as an opacity law defined as e−τ(λ), where τ(λ) also
  follows a single Gaussian velocity distribution (F. D’Eugenio et al. 2025a, 2025b;
  A. Torralba et al. 2026). For simplicity, we assume a covering factor of Cf = 1
  for the absorbing gas. In previous works, the width of the narrow component is tied
  to that of [O iii], assuming both components come from the same region, often interpreted
  as the interstellar medium (ISM) of the host galaxy. In this case, we have no information
  about [O iii] due to this doublet falling in a wavelength range heavily affected
  by strong telluric absorption. We fit the Hα line after masking relevant skylines
  and strong telluric absorption bands. The fitted Hα parameters are listed in Table
  1 and the best-fit model is shown in Figure 3. The absorption feature is notably
  strong, with an equivalent width of EWabs = −148 ± 12 Å with respect to the fitted
  continuum and 12.2 ± 0.2 Å if including the broad emission component. The absorption
  corresponds to a Balmer optical depth at the line center of , reaching roughly the
  continuum level. The FWHM of the single Gaussian fitted to the absorber is 283  ±
  \ 8 km s−1, and is offset from the systemic redshift by −94 ± 4 km s−1. We note
  that this parameterization is somewhat arbitrary, and we discuss in detail the absorber
  properties in Section 4.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Hα
  spectrum, and the best fit to our fiducial model. We show the X-Shooter R ∼ 5600
  spectrum of the Hα line of PAN-BH*-1, along with the best-fit to the model described
  in Section 3.2; total model (red solid line) and individual components (discontinuous
  color lines). The red wing of the line is severely affected by telluric absorption,
  thus the large uncertainties.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
  image\r\nTable 1. Properties of PAN-BH*-1\r\n\r\nParameter\tValue\tUnit\r\nWidth
  (FWHM; Hα)\r\nExponential\t1257 ± 27\tkm s−1\r\nIntermediate\t687 ± 43\tkm s−1\r\nNarrow\t184
  ± 12\tkm s−1\r\nAbsorption\t283 ± 8\tkm s−1\r\nFlux (Hα)\r\nExponential\t643 ± 7\t10−18
  erg s−1 cm−2\r\nIntermediate\t19 ± 5\t10−18 erg s−1 cm−2\r\nNarrow\t38 ± 3\t10−18
  erg s−1 cm−2\r\nTotal\t522 ± 7\t10−18 erg s−1 cm−2\r\nGeneral properties\r\n(LHα/erg
  s−1)\t43.046 ± 0.006\t⋯\r\nEW0(Hα)\t520 ± 20\tÅ\r\nSFR(Hα, narrow)a\t2.1 ± 0.2\tM⊙
  yr−1\r\nSFR(Hα, narrow)b\t3.3 ± 0.3\tM⊙ yr−1\r\nreff,UV (F606W+F814W)\t\tkpc\r\nreff,opt
  (F200W)\t<0.047\tkpc\r\nHα/Hβ (total)\t>9.4\t⋯\r\nHα/Hβ (narrow)\t5 ± 1\t⋯\r\nNotes.
  aCalibration from I. G. Kramarenko et al. (2026). bCalibration from R. C. Kennicutt
  & N. J. Evans (2012). SFR values calculated assuming no dust attenuation.\r\n\r\nDownload
  table as: \r\nASCIITypeset image\r\n\r\nThe Hβ line is marginally detected. After
  undersampling the spectrum by a factor 5, a hint of a weak narrow component can
  be identified (Figure 4), along with a tentative absorption at the same mean velocity
  as in Hα. We fit the best Hα model to the Hβ spectrum, only rescaling it by a multiplicative
  factor, and adding a flat continuum component. By doing this, we find an Hβ flux
  of (47 ± 8) × 10−18 erg s−1 cm−2 (S/N ≈ 6). Conservatively, we obtain a Balmer decrement
  of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with the high decrements found
  for the LRD population (e.g., G. P. Nikopoulos et al. 2026; A. de Graaff et al.
  2025b; J. Matthee et al. 2026). In Figure 5, we show the Hβ spectrum compared to
  the rescaled Hα model. By matching the best-fit Hα profile with the data at the
  expected observed wavelength for Hβ (±5000 km s−1), we obtain a better agreement
  (, BIC = 1537) than fitting a flat continuum only (, BIC = 1658) with ΔBIC = 121
  ≫ 10, strongly favoring a detection of a broad Hβ emission line, and securing the
  spectroscopic redshift. Similarly, we fit a narrow Gaussian to Hβ with the same
  width and velocity as the Hα best-fit model, assuming a completely saturated absorption.
  We obtain a Balmer decrement for the narrow component of Hα/Hβ = 5 ± 1, which would
  imply a dust extinction of using a J. A. Cardelli et al. (1989) attenuation law,
  under the assumption of case B recombination. However, due to the low S/N of Hβ
  this result is only tentative, and compatible with a standard Case B value within
  ∼2σ.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. X-Shooter spectrum of Hα
  and Hβ of PAN-BH*-1 (blue). We compare to the spectrum of The Cliff (gray; data
  from JWST DDT #9433), normalized in each panel to the flux of PAN-BH*-1 in the range
  v ∈ (−3000, −2000) km s−1. Due to the low S/N, the Hβ spectrum of PAN-BH*-1 is rebinned
  to a coarser grid by a factor 5, after masking the most relevant skylines.\r\n\r\nDownload
  figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image
  size\r\nFigure 5. Hβ spectrum. The spectrum is rebinned by a factor of 10 with inverse
  variance flux weighting for visual clarity, due to the low S/N. We compare to the
  best-fit Hα model, scaled by a factor of 0.112. In the bottom panel, we show the
  χ residuals between the spectrum and the rescaled Hα model in black, and for only
  the continuum in pink (ΔBIC = 121 strongly favoring the presence of a broad Hβ line).\r\n\r\nDownload
  figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.3. Spatial Morphology\r\nIn
  order to assess whether PAN-BH*-1 is spatially resolved, we use the Bayesian profile
  fitting software pysersic (I. Pasha & T. B. Miller 2023)18 to fit a single Sérsic
  profile to the JWST and HST imaging data of PAN-BH*-1. For JWST/NIRCam, we choose
  F200W as the filter with the highest S/N in the short wavelength channel, benefiting
  from a high spatial resolution and probing rest-frame optical wavelengths. To model
  its PSF, we use version 2.2.0 of the stpsf software (formerly webbpsf, M. D. Perrin
  et al. 2014). For the two HST bands F606W and F814W, we instead construct empirical
  PSFs from public imaging data in the GOODS-S field following A. Weibel et al. (2024).
  In all three bands, we sample the posterior with the No U-turn sampler in two chains
  with 1000 warm-up and 2000 sampling steps each. We find that PAN-BH*-1 is unresolved
  with NIRCam in F200W where the effective radius converges toward the edge of the
  prior at 0.25 pixels. Using the 95th percentile of the posterior chains as an upper
  limit on the effective radius, we find a rest-optical size of reff < 47 pc.\r\n\r\nPAN-BH*-1
  appears to be resolved in the HST images corresponding to rest-frame pivot 0.2 and
  0.3 μm, respectively. Due to the low signal-to-noise of the F606W and F814W photometry,
  we fit both bands simultaneously fixing all the morphological parameters in both
  images. We measure physical effective radii of  kpc (see Appendix B). The modest
  stretching by the foreground A370 lensing cluster could imply a correction of ∼10%
  to the measured radius (A. Niemiec et al. 2023), which we disregard given the uncertainties.
  These measured sizes are consistent with the typical sizes for galaxies with a stellar
  mass ≲ 109 M⊙ at z = 1.75 (A. van der Wel et al. 2014). These findings are consistent
  with the scenario of a compact LRD “engine” dominating the rest-optical light embedded
  in a host galaxy, whose contribution becomes significant blueward of the Balmer
  break (see A. P. Cloonan et al. 2026, for a relevant discussion).\r\n\r\n4. Absorber
  Kinematics\r\nAs described in Section 3.2, the velocity distribution of the absorber
  is empirically modeled with a Gaussian, which we find has a central velocity of
  −94 ± 4 km s−1 relative to the redshift of the narrow emission component (adopted
  as systemic). The absorption trough extends from negative to positive velocities
  with respect to the redshift of the narrow component, but also with respect to the
  center of the symmetric exponential wings. However, there are several degeneracies
  between the shape of the absorber and other components of the emission line, such
  as the narrow central emission (see Section 3.2). Furthermore, direct interpretation
  of the absorber center velocity shift is challenging in an optically thick gas with
  presumably complex dynamics, and it does not necessarily trace bulk motion. A more
  robust, physically motivated pair of quantities is the minimum and maximum absorber
  velocities. We define them as the values where the transmission of the Balmer absorber
  increases to 99%,  km s−1 and  km s−1. These values trace the largest velocities
  in the line of sight of gas with significant Balmer absorption. The absorbing trough
  extends over 787 ± 17 km s−1 under this definition. The values of and are relatively
  agnostic to the choice of the shape of the absorber, since they are determined by
  the wavelength where the line profile deviates from a broad, symmetric exponential
  profile. In Figure 6, we illustrate three proposed configurations of the velocity
  distribution of the absorbing gas that could explain the shape of the observed Balmer
  absorption, and we discuss these scenarios below.\r\n\r\nZoom InZoom OutReset image
  size\r\nFigure 6. Geometric configurations for the absorber. We illustrate three
  scenarios that could give rise to the observed Balmer absorption in PAN-BH*-1. In
  scenario (a), the obscuring agent is a thick screen of gas with a certain bulk velocity,
  and turbulent motions produce the broadening of the absorption trough. In (b), there
  are two (or more) absorbers with opposite velocities in the line of sight. These
  first two scenarios are dynamically unstable; therefore, variability is expected
  in the absorption. Lastly, in (c), we observed an extended source through a disk
  wind with a rotational component (vϕ) in addition to the poloidal (nonazimuthal)
  velocity (vp). In the last scenario, the redshifted absorption is produced by streamlines
  that oppose the observer when projected along the line of sight, despite the fact
  that the gas is outflowing from the central source.\r\n\r\nDownload figure:\r\n\r\nStandard
  imageHigh-resolution image\r\n4.1. Unstable Gas Flows?\r\nThe fact that there is
  significant absorption at both negative and positive velocities with respect to
  the systemic redshift cannot be simply explained by an axisymmetric outflowing or
  inflowing wind. In the case of observing a compact object through a spherically
  symmetric, nonturbulent bulk flow, a classical P Cygni profile is expected, with
  a purely blueshifted absorption (or redshifted if the wind is infalling). The fact
  that we also see redshifted absorption rules out this simple scenario. In principle,
  turbulent motions could also produce broadening of the absorbing medium (scenario
  a in Figure 6). However, the required turbulent velocity dispersion σturb ≈ 120
  km s−1 (from the Gaussian fit in Section 3.2) is comparable to the mean velocity
  of the absorption trough, meaning that turbulence dominates the gas flow. In such
  a case, strong variability of the absorption profile would be expected, given the
  typical dynamical crossing times (see Sect. 4.1 in F. D’Eugenio et al. 2025b). For
  example, for a radius of 1016 cm (e.g., A. Torralba et al. 2026) and a mass of 106
  M⊙, the dynamical freefall time is  yr. Moreover, the turbulent velocity would be
  highly supersonic, and the dissipation timescale would be comparable to the dynamical
  time (e.g., M.-M. Mac Low 1999). Alternatively, in the context of a strong Balmer
  absorber at z ∼ 7, F. D’Eugenio et al. (2026) recently discussed a “breathing mode”
  scenario with cyclic inflows and outflows along the same line of sight, with the
  gas being in different phases at different depths (scenario b in Figure 6; see also
  K. Park et al. 2017). In this case, the same arguments regarding the stability of
  the absorber would apply, and absorber variability is expected on observed timescales
  of ∼5 yr (for a source at z = 1.7), which is testable with future observations.\r\n\r\n4.2.
  The Case for the Disk Wind Hypothesis\r\nAn alternative, dynamically stable scenario
  is a disk wind configuration (scenario c in Figure 6). Here, the wind would be launched
  from a thick disk near the central engine, which we speculate could be the source
  of the optical continuum emission (e.g., H. Liu et al. 2025, 2026; L. Zwick et al.
  2025; Y.-X. Chen et al. 2026). A rotating disk would imprint to the wind an azimuthal
  velocity component (vϕ). Observations at specific lines of sight, particularly for
  high inclination angles (close to edge-on) where the rotational component dominates
  the poloidal velocity, can give rise to both blueshifted and redshifted absorption
  features (D. Proga et al. 2000; P. B. Hall et al. 2002, 2013; D. Proga & T. R. Kallman
  2004; M. Giustini & D. Proga 2012). Most observed LRDs have blueshifted P Cygni–like
  absorbers (J. Matthee et al. 2026), which can be naively interpreted as a uniformly
  expanding shell. The low incidence of redshifted Balmer absorbers in LRD spectra
  (e.g., I. Labbe et al. 2024; A. de Graaff et al. 2025a; F. D’Eugenio et al. 2025b,
  2026; Y. Ma et al. 2026) can therefore be explained by the requirement of high inclination
  angles to observe such features (see also A. Sneppen et al. 2026). Such a picture
  is broadly in line with disk wind models for AGN with broad absorption lines (e.g.,
  P. B. Hall et al. 2002; H. Zhou et al. 2019) and around stars with circumstellar
  disks (e.g., J. Erkal et al. 2022), such as accreting T Tauri stars (S. Edwards
  et al. 2006) or cataclysmic variables (D. Proga 2003).\r\n\r\n4.3. Implications
  of Rotating Winds for the Emission Lines of LRDs\r\nThe disk wind hypothesis would
  imply that a photosphere in the shape of a rotating disk is the source of the optical
  continuum emission, and drives winds that can explain the observed absorption trough.
  Emission lines originating in a thin rotating disk would have a double-peaked profile
  in the idealized case (for most inclination angles), but this is not necessarily
  true if the disk is not sufficiently thin (e.g., N. Murray & J. Chiang 1997), for
  instance, in the case of a puffed-up disk associated with super-Eddington accretion
  (e.g., H. Liu et al. 2026). In addition, most line emission would not be produced
  directly at the base of the disk, but slightly outside (e.g., via collisional cooling
  or residual recombination; A. Torralba et al. 2026), where the rotational velocity
  is lower, and the dynamics are complex (e.g., G. A. Shields 1977).\r\n\r\nThe Balmer
  lines of most LRDs are dominated by broad, symmetric exponential components that
  are associated with broadening by electron scattering (e.g., V. Rusakov et al. 2026;
  J. Matthee et al. 2026). For PAN-BH*-1, the Hα line profile of PAN-BH*-1 is compatible
  with a broad exponential profile emerging through a dense wind where the absorption
  trough is produced. In dense gas with a large column density of neutral hydrogen,
  and optically thick to Balmer transitions (NHI,2s ≳ 1014 cm−2), resonant scattering
  effects become important. Crucially, resonant scattering impacts Hα and Hβ differently
  (e.g., S.-J. Chang et al. 2026), hence the 3D radiative transfer and photon redistribution
  of both lines may produce different profiles (see, e.g., Figure 2 in D. Proga 2003).
  Therefore, the empirical fitting and interpretation of the absorption profiles becomes
  nontrivial. Dedicated radiative transfer modeling is necessary to study such effects,
  and they can be tested in other emission lines with high optical depth, such as
  He i λ10830 Å, or resonant lines like C iv λ1550.\r\n\r\n5. Implications for the
  Galaxy and Black Hole Masses\r\n5.1. Properties of the Host Galaxy\r\nAssuming that
  the narrow component of Hα corresponds to ISM emission in the host galaxy, we compute
  the associated star formation rate using the local calibration from R. C. Kennicutt
  & N. J. Evans (2012) and assuming no dust attenuation. We obtain SFR(Hα) = 3.3 ±
  0.3 M⊙ yr−1. A somewhat lower value of SFR(Hα) = 2.1 ± 0.2 M⊙ yr−1 is obtained using
  the high-redshift (z ≳ 4) calibrations in I. G. Kramarenko et al. (2026), which
  might be more appropriate for a young dwarf galaxy with a bursty star formation
  history. The star formation rates are low, but in line with a main-sequence galaxy
  with (extrapolating the relation from J. S. Speagle et al. 2014). Assuming zero
  dust attenuation, the UV absolute magnitude (MUV = −16.7 ± 0.7; Section 3.1) would
  imply SFR(UV) = 0.18 ± 0.12 M⊙ yr−1 (R. C. Kennicutt & N. J. Evans 2012). The discrepancy
  between the UV and Hα inferred star formation rate suggests there is some amount
  of dust attenuation in the host galaxy.\r\n\r\nWe derive a dynamical mass from the
  width of the narrow component Hα line and the estimated UV size as , adopting the
  empirical virial correction K(n)K(q) from A. van der Wel et al. (2022), where K(n)
  and K(q) are functions of the best-fit ellipticity and Sérsic index (see Appendix
  B). Adopting a Mdyn/M* factor of 40 as found by A. de Graaff et al. (2024) for dwarf
  galaxies at high redshift, we infer a stellar mass of . However, the Mdyn/M* is
  very uncertain in this regime, and the uncertainty can span over 1 dex (A. Saldana-Lopez
  et al. 2025). We advise caution in interpreting this result, as there are large
  uncertainties in the measurements of the narrow Hα component, the HST morphology,
  and the empirical relations used.\r\n\r\nAs discussed in Section 4, the absorption
  profile is compatible with broadening by a rotating disk wind, and numerical modeling
  of such configurations often predicts a narrow component arising from increased
  transmission due to purely kinematic effects in the wind geometry (D. Proga et al.
  2000; D. Proga 2003; D. Proga & T. R. Kallman 2004). This would be an alternative
  explanation for at least part of the narrow component flux. On the other hand, most
  LRDs present narrow [O iii] emission that is often associated with the host galaxy.
  Indeed, the ionized gas producing [O iii] emission should have associated emission
  in the Hα and higher-order Balmer lines. However, constraining this component largely
  depends on the assumptions on dust attenuation or ISM conditions, and requires very
  high S/N and resolution data. Deep, space-based follow-up observations of PAN-BH*-1
  would be very constraining for the wind kinematics (e.g., by the joint analysis
  of Hβ) and to assess whether a narrow component comes from a host galaxy (e.g.,
  by comparing to a narrow Hβ component or [O iii] λλ4960, 5008).\r\n\r\n5.2. Black
  Hole Mass From Photosphere Models\r\nThe general physical setup of LRDs is an open
  debate, and their masses are a major unknown. Due to the multiple differences with
  respect to the classical AGN population, the validity of standard virial calibrations
  has been questioned (e.g., V. Rusakov et al. 2026; J. E. Greene et al. 2026; A.
  Sneppen et al. 2026; A. Torralba et al. 2026, although see, e.g., M. Brazzini et
  al. 2025, 2026; J. Scholtz et al. 2026 for an alternative interpretation).\r\n\r\nOne
  can obtain a mass estimate assuming a system in radiative equilibrium with Lbol/LEdd
  = 1 (e.g., H. Umeda et al. 2026); this yields a total mass of ≈106 M⊙, using the
  bolometric luminosity from integrating the best-fit blackbody in Section 3.1. Recently,
  H. Liu et al. (2026) developed a synthetic spectral library of LRD atmosphere models.
  In these models, the density of the photosphere is regulated by the net surface
  gravity of an optically thick atmosphere, enabling constraints on the mass of the
  system. We fit the JWST photometry of PAN-BH*-1 using the models from H. Liu et
  al. (2026), assuming a negligible contribution from a host galaxy to the optical
  continuum. The best-fit model has effective temperature Teff = 4800 K, surface gravity
  , and metallicity (; see Figure 1). The best-fit implies a total mass of the system
  (BH plus gas) of (Equation (6) in H. Liu et al. 2026, assuming hydrostatic equilibrium).
  For the second and third best fits, we obtain and −2, respectively (, respectively;
  with the same metallicity and effective temperature), which would imply lower limits
  to the system mass between and 4. The bolometric luminosity of PAN-BH*-1 (from the
  integral of the best-fit green curve in Figure 1) implies an Eddington luminosity
  ratio of L/LEdd ≲ 13, assuming the best-fit mass from the H. Liu et al. (2026) models.
  The elevated Eddington ratio is in line with the hypothesis of a radiation-driven
  wind discussed in Section 4, and allows for somewhat larger system masses. The low
  masses obtained with this model, combined with the stellar mass inferred from dynamical
  arguments for the host galaxy (Section 3.3) set lower limits to the BH-to-stellar
  mass ratio of MBH/M* ≳ 10−4–10−2, which are compatible with the relations observed
  in the Local Universe, within the large uncertainties (A. E. Reines & M. Volonteri
  2015).\r\n\r\n6. Conclusions\r\nIn this Letter, we presented the discovery and spectroscopic
  confirmation of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.731. The
  strength of the Balmer break (F115W/F814W = 7 ± 1) is comparable to the most extreme
  LRDs known, The Cliff (A. de Graaff et al. 2025a) and MoM-BH* (R. P. Naidu et al.
  2025). We summarize the observations and our main conclusions as follows.\r\n\r\n\r\n1.
  \ \r\nWe obtained deep VLT/X-Shooter spectroscopy of PAN-BH*-1. The Hα emission
  line is luminous and broad (LHα = 1043 erg s−1), and has an unusually strong absorption.
  Hβ is detected with an S/N ≈ 6, and we conservatively estimate a lower limit for
  the Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with other
  LRDs in the literature (e.g., A. de Graaff et al. 2025b; G. P. Nikopoulos et al.
  2026).\r\n2.  \r\nThe absorption trough spans from −520 to 267 km s−1 (at a transmission
  level of 99%). We interpret the presence of blue- and redshifted absorption as produced
  by a disk wind, analogous to those analyzed in the context of broad absorption line
  quasars or accreting stars. This hypothesis would imply that the source of the optical
  continuum is likely a thick photospheric disk.\r\n3.  \r\nWe detect a narrow Hα
  component (FWHM = 184 ± 12 km s−1), which we interpret as probing a host galaxy
  with M* ≈ 108 M⊙ and SFR = 2–3 M⊙. This interpretation is in line with the extended
  rest-NUV morphology measured in the HST bands (\r\n kpc).\r\n4.  \r\nBy fitting
  the synthetic atmosphere models of H. Liu et al. (2026), we estimate a system mass
  (BH+envelope) of 104–106 M⊙. The inferred masses, together with the stellar mass
  inferred from morphology and narrow emission line dynamics, imply BH-to-stellar
  mass ratios of 10−2–10−4, close to the extrapolated trend in the local Universe
  (A. E. Reines & M. Volonteri 2015).\r\n5.  \r\nThe confirmation of this source at
  cosmic noon (magnitude of ≈22 in the K band, Hα flux ≈5 × 10−16 erg s−1 cm−2) proves
  the feasibility of detecting extreme LRDs at such epochs with wide-area spectroscopic
  surveys like Euclid or the forthcoming Nancy Grace Roman Space Telescope.\r\n\r\nAcknowledgments\r\nA.T.
  thanks Debasish Dutta and Tamara Bogdanović for useful conversations about stellar
  and AGN winds.\r\n\r\nWe thank the scientific referee for the useful and constructive
  feedback, which helped improve the quality of this paper.\r\n\r\nJ.M. and A.T. acknowledge
  funding by the European Union (ERC, AGENTS, 101076224). The work of CCW is supported
  by NOIRLab, which is managed by the Association of Universities for Research in
  Astronomy (AURA) under a cooperative agreement with the National Science Foundation.
  A.P.C. warmly acknowledges the support of the National Science Foundation through
  the NSF Graduate Research Fellowship Program. A.d.G. acknowledges support from a
  Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.\r\n\r\nBased
  on observations made with ESO Telescopes at the Paranal Observatory under program
  IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is based in part on observations made
  with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
  Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
  with programs #2514 and #9433. C.C.W. gratefully acknowledges support for program
  JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs
  R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access
  period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble
  Space Telescope obtained from the Space 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 program #15117.\r\n\r\nThe JWST
  and HST data presented in this article were obtained from the Mikulski Archive for
  Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations
  analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis work is based in
  part on observations made with the Spitzer Space Telescope, which was operated by
  the Jet Propulsion Laboratory, California Institute of Technology under a contract
  with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis
  work was supported by the International Space Science Institute (ISSI) in Bern,
  through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST
  cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope
  (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam,
  NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space
  Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration
  et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al.
  2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023),
  stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL
  Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP
  (K. Barbary 2016)."
article_number: L37
article_processing_charge: Yes
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: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: Yilun
  full_name: Ma, Yilun
  last_name: Ma
- first_name: Aidan P.
  full_name: Cloonan, Aidan P.
  last_name: Cloonan
- first_name: Aayush A
  full_name: Desai, Aayush A
  id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
  last_name: Desai
- first_name: Anna
  full_name: De Graaff, Anna
  last_name: De Graaff
- first_name: Jenny E.
  full_name: Greene, Jenny E.
  last_name: Greene
- first_name: Christian Kragh
  full_name: Jespersen, Christian Kragh
  last_name: Jespersen
- first_name: Ivan
  full_name: Kramarenko, Ivan
  id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
  last_name: Kramarenko
  orcid: 0000-0001-5346-6048
- first_name: Sara
  full_name: Mascia, Sara
  id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
  last_name: Mascia
- first_name: Pascal A.
  full_name: Oesch, Pascal A.
  last_name: Oesch
- first_name: Wendy Q.
  full_name: Sun, Wendy Q.
  last_name: Sun
- first_name: Christina C.
  full_name: Williams, Christina C.
  last_name: Williams
citation:
  ama: 'Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic
    noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick
    winds in a Little Red Dot at z = 1.7. <i>The Astrophysical Journal Letters</i>.
    2026;1005(2). doi:<a href="https://doi.org/10.3847/2041-8213/ae7bfd">10.3847/2041-8213/ae7bfd</a>'
  apa: 'Torralba Torregrosa, A., Matthee, J. J., Weibel, A., Naidu, R. P., Ma, Y.,
    Cloonan, A. P., … Williams, C. C. (2026). A black hole star at cosmic noon: Extreme
    Balmer break, photospheric continuum, and broad absorption by thick winds in a
    Little Red Dot at z = 1.7. <i>The Astrophysical Journal Letters</i>. IOP Publishing.
    <a href="https://doi.org/10.3847/2041-8213/ae7bfd">https://doi.org/10.3847/2041-8213/ae7bfd</a>'
  chicago: 'Torralba Torregrosa, Alberto, Jorryt J Matthee, Andrea Weibel, Rohan P.
    Naidu, Yilun Ma, Aidan P. Cloonan, Aayush A Desai, et al. “A Black Hole Star at
    Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption
    by Thick Winds in a Little Red Dot at z = 1.7.” <i>The Astrophysical Journal Letters</i>.
    IOP Publishing, 2026. <a href="https://doi.org/10.3847/2041-8213/ae7bfd">https://doi.org/10.3847/2041-8213/ae7bfd</a>.'
  ieee: 'A. Torralba Torregrosa <i>et al.</i>, “A black hole star at cosmic noon:
    Extreme Balmer break, photospheric continuum, and broad absorption by thick winds
    in a Little Red Dot at z = 1.7,” <i>The Astrophysical Journal Letters</i>, vol.
    1005, no. 2. IOP Publishing, 2026.'
  ista: 'Torralba Torregrosa A, Matthee JJ, Weibel A, Naidu RP, Ma Y, Cloonan AP,
    Desai AA, De Graaff A, Greene JE, Jespersen CK, Kramarenko I, Mascia S, Oesch
    PA, Sun WQ, Williams CC. 2026. A black hole star at cosmic noon: Extreme Balmer
    break, photospheric continuum, and broad absorption by thick winds in a Little
    Red Dot at z = 1.7. The Astrophysical Journal Letters. 1005(2), L37.'
  mla: 'Torralba Torregrosa, Alberto, et al. “A Black Hole Star at Cosmic Noon: Extreme
    Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a
    Little Red Dot at z = 1.7.” <i>The Astrophysical Journal Letters</i>, vol. 1005,
    no. 2, L37, IOP Publishing, 2026, doi:<a href="https://doi.org/10.3847/2041-8213/ae7bfd">10.3847/2041-8213/ae7bfd</a>.'
  short: A. Torralba Torregrosa, J.J. Matthee, A. Weibel, R.P. Naidu, Y. Ma, A.P.
    Cloonan, A.A. Desai, A. De Graaff, J.E. Greene, C.K. Jespersen, I. Kramarenko,
    S. Mascia, P.A. Oesch, W.Q. Sun, C.C. Williams, The Astrophysical Journal Letters
    1005 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: "Based on observations made with ESO Telescopes at the
  Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is
  based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope.
  The data were obtained from the Mikulski Archive for Space Telescopes at the Space
  Telescope Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These
  observations are associated with programs #2514 and #9433. C.C.W. gratefully acknowledges
  support for program JWST-GO-2514 provided by NASA through a grant from the Space
  Telescope Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge
  the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing
  program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations
  made with the NASA/ESA Hubble Space Telescope obtained from the Space 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 program #15117.\r\n\r\nThe JWST and HST data presented in this article were
  obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope
  Science Institute. The specific observations analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis
  work is based in part on observations made with the Spitzer Space Telescope, which
  was operated by the Jet Propulsion Laboratory, California Institute of Technology
  under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis
  work was supported by the International Space Science Institute (ISSI) in Bern,
  through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST
  cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope
  (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam,
  NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space
  Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration
  et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al.
  2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023),
  stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL
  Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP
  (K. Barbary 2016)."
date_created: 2026-07-12T22:02:17Z
date_published: 2026-07-10T00:00:00Z
date_updated: 2026-07-13T08:08:41Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
- _id: IlCa
- _id: GradSch
doi: 10.3847/2041-8213/ae7bfd
external_id:
  arxiv:
  - '2603.28335'
file:
- access_level: open_access
  checksum: 7600db260d799ddea45cf3bd01effe41
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T07:46:22Z
  date_updated: 2026-07-13T07:46:22Z
  file_id: '22274'
  file_name: 2026_AstrophysicalJourLetters_Torralba.pdf
  file_size: 5419071
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T07:46:22Z
has_accepted_license: '1'
intvolume: '      1005'
issue: '2'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal Letters
publication_identifier:
  eissn:
  - 2041-8213
  issn:
  - 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: 'A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum,
  and broad absorption by thick winds in a Little Red Dot at z = 1.7'
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: 1005
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22264'
abstract:
- lang: eng
  text: 'The correlation between galaxy stellar mass and gas-phase metallicity, known
    as the mass–metallicity relation (MZR), gives key insights into the processes
    that govern galaxy evolution. However, unquantified observational and selection
    biases can result in systematic errors in attempts to recover the intrinsic MZR,
    particularly at higher redshifts. We characterize the MZR at z ∼ 3–6 within a
    fully Bayesian framework using JWST/NIRSpec spectra of 191 galaxies from the RUBIES
    survey. We forward model the observed mass–metallicity surface using prospector-generated
    spectra to account for two selection biases: the survey selection function and
    the success in observing high signal-to-noise ratio emission lines. We demonstrate
    that the RUBIES selection function, based on F444W magnitude and F150W – F444W
    color, has a negligible effect on our measured MZR. A correct treatment of the
    non-Gaussian metallicity uncertainties from strong-line calibrations lowers the
    derived MZR normalization by 0.2 dex and flattens the slope by ∼20%; forward modeling
    the effect of emission line observability steepens the slope by ∼15%. Both of
    these biases must be taken into account in order to properly measure the intrinsic
    MZR. This novel forward-modeling process motivates careful consideration of selection
    functions in future surveys, and paves the way for robust, high-redshift chemical
    enrichment studies that trace the evolution of the MZR across cosmic time.'
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 program ID 4233. This material
  is based upon work supported by the National Science Foundation Graduate Research
  Fellowship under grant No. 2137424 as well as work supported by NASA under Award
  No. 2025_3-0, issued through the Wisconsin Space Grant Consortium, and JWST-GO-4233.
  Any opinions, findings, and conclusions or recommendations expressed in this material
  are those of the author(s) and do not necessarily reflect the views of the National
  Aeronautics and Space Administration. Support for program ID 4233 was provided by
  NASA through a grant from the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc., under NASA contract
  NAS 5-03127. M.V.M. is supported by the National Science Foundation via grant AAG
  2205519. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian
  Astrophysical Observatory. T.B.M. was supported by a CIERA Fellowship. Part of the
  computations for this research were performed on the Pennsylvania State University’s
  Institute for Computational and Data Sciences’ Roar supercomputer. Some/all of the
  data presented in this article were obtained from the Mikulski Archive for Space
  Telescopes (MAST) at the Space Telescope Science Institute. The specific observations
  analyzed can be accessed via doi:10.17909/qk5z-7p30. The scripts used to generate
  the data and results in this work can be found in Zenodo at doi:10.5281/zenodo.20513668
  and GitHub  \r\nhttps://github.com/zachlewis99/rubies_mzr "
article_number: '159'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zach
  full_name: Lewis, Zach
  last_name: Lewis
- first_name: Michael V.
  full_name: Maseda, Michael V.
  last_name: Maseda
- first_name: Anna
  full_name: De Graaff, Anna
  last_name: De Graaff
- first_name: Joel
  full_name: Leja, Joel
  last_name: Leja
- first_name: Bingjie
  full_name: Wang, Bingjie
  last_name: Wang
- first_name: Hans Walter
  full_name: Rix, Hans Walter
  last_name: Rix
- first_name: Ian
  full_name: Mcconachie, Ian
  last_name: Mcconachie
- first_name: Nikko J.
  full_name: Cleri, Nikko J.
  last_name: Cleri
- first_name: Rachel
  full_name: Bezanson, Rachel
  last_name: Bezanson
- first_name: Leindert A.
  full_name: Boogaard, Leindert A.
  last_name: Boogaard
- first_name: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Jenny E.
  full_name: Greene, Jenny E.
  last_name: Greene
- first_name: Michaela
  full_name: Hirschmann, Michaela
  last_name: Hirschmann
- first_name: Harley
  full_name: Katz, Harley
  last_name: Katz
- first_name: Ivo
  full_name: Labbé, Ivo
  last_name: Labbé
- 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: Tim B.
  full_name: Miller, Tim B.
  last_name: Miller
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: Pascal A.
  full_name: Oesch, Pascal A.
  last_name: Oesch
- first_name: David J.
  full_name: Setton, David J.
  last_name: Setton
- first_name: Katherine A.
  full_name: Suess, Katherine A.
  last_name: Suess
- first_name: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Katherine E.
  full_name: Whitaker, Katherine E.
  last_name: Whitaker
- first_name: Christina C.
  full_name: Williams, Christina C.
  last_name: Williams
citation:
  ama: Lewis Z, Maseda MV, De Graaff A, et al. The mass–metallicity relation and its
    observational effects at z ∼ 3–6. <i>The Astrophysical Journal</i>. 2026;1005(2).
    doi:<a href="https://doi.org/10.3847/1538-4357/ae7bfc">10.3847/1538-4357/ae7bfc</a>
  apa: Lewis, Z., Maseda, M. V., De Graaff, A., Leja, J., Wang, B., Rix, H. W., …
    Williams, C. C. (2026). The mass–metallicity relation and its observational effects
    at z ∼ 3–6. <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae7bfc">https://doi.org/10.3847/1538-4357/ae7bfc</a>
  chicago: Lewis, Zach, Michael V. Maseda, Anna De Graaff, Joel Leja, Bingjie Wang,
    Hans Walter Rix, Ian Mcconachie, et al. “The Mass–Metallicity Relation and Its
    Observational Effects at z ∼ 3–6.” <i>The Astrophysical Journal</i>. IOP Publishing,
    2026. <a href="https://doi.org/10.3847/1538-4357/ae7bfc">https://doi.org/10.3847/1538-4357/ae7bfc</a>.
  ieee: Z. Lewis <i>et al.</i>, “The mass–metallicity relation and its observational
    effects at z ∼ 3–6,” <i>The Astrophysical Journal</i>, vol. 1005, no. 2. IOP Publishing,
    2026.
  ista: Lewis Z, Maseda MV, De Graaff A, Leja J, Wang B, Rix HW, Mcconachie I, Cleri
    NJ, Bezanson R, Boogaard LA, Brammer G, Greene JE, Hirschmann M, Katz H, Labbé
    I, Matthee JJ, Miller TB, Naidu RP, Oesch PA, Setton DJ, Suess KA, Weibel A, Whitaker
    KE, Williams CC. 2026. The mass–metallicity relation and its observational effects
    at z ∼ 3–6. The Astrophysical Journal. 1005(2), 159.
  mla: Lewis, Zach, et al. “The Mass–Metallicity Relation and Its Observational Effects
    at z ∼ 3–6.” <i>The Astrophysical Journal</i>, vol. 1005, no. 2, 159, IOP Publishing,
    2026, doi:<a href="https://doi.org/10.3847/1538-4357/ae7bfc">10.3847/1538-4357/ae7bfc</a>.
  short: Z. Lewis, M.V. Maseda, A. De Graaff, J. Leja, B. Wang, H.W. Rix, I. Mcconachie,
    N.J. Cleri, R. Bezanson, L.A. Boogaard, G. Brammer, J.E. Greene, M. Hirschmann,
    H. Katz, I. Labbé, J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, D.J. Setton,
    K.A. Suess, A. Weibel, K.E. Whitaker, C.C. Williams, The Astrophysical Journal
    1005 (2026).
das_tickbox: '1'
dataavailabilitystatement: The specific observations analyzed can be accessed via
  doi:10.17909/qk5z-7p30. The scripts used to generate the data and results in this
  work can be found in Zenodo at doi:10.5281/zenodo.20513668 and GitHub https://github.com/zachlewis99/rubies_mzr
date_created: 2026-07-12T22:02:17Z
date_published: 2026-07-10T00:00:00Z
date_updated: 2026-07-13T07:40:41Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae7bfc
external_id:
  arxiv:
  - '2512.03134'
file:
- access_level: open_access
  checksum: 9b13fbbc5e5e921c04676ebc532d9c42
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T07:35:16Z
  date_updated: 2026-07-13T07:35:16Z
  file_id: '22273'
  file_name: 2026_AstrophysicalJour_Lewis.pdf
  file_size: 1854628
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T07:35:16Z
has_accepted_license: '1'
intvolume: '      1005'
issue: '2'
keyword:
- Galaxy evolution
- Chemical enrichment
- Metallicity
- Galaxy abundances
- Scaling relations
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: no
title: The mass–metallicity relation and its observational effects at z ∼ 3–6
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: 1005
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22262'
abstract:
- lang: eng
  text: Mixed modes are observed in many low-mass evolved stars. They provide information
    about core rotation rates of these stars, which are lower than predicted by stellar
    evolution models. The mixed modes themselves have been invoked as an angular momentum
    (AM) transport mechanism, but estimating their transport efficiency requires knowledge
    of their amplitudes. We constrain, for the first time, the mixed-mode amplitudes
    in 2D hydrodynamical simulations of a 1.3M⊙ red giant using the code MUSIC. We
    perform two simulations with outer radial truncations at fractional radii ro/r⋆
    = 0.90 and 0.98. We compare the modes in the simulation with those found using
    both GYRE and a Dedalus eigenvalue solver. Excellent frequency agreement is found
    for all p-dominated modes, with minor discrepancies for g-dominated modes, especially
    in the frequency range [60, 240] μHz. We find excellent eigenfunction agreement
    for all modes except those in this frequency range. According to empirical predictions,
    the largest kinetic energies are located around Vmax= 312.μHz, but in both simulations,
    the modes with frequencies of ν < 50 μHz have the largest kinetic energies. In
    the simulation with r/r⋆ = 0.98, the simulated modes have extrapolated surface
    velocities comparable to the empirical predictions, with the highest surface velocities
    in a bell-shaped curve peaking around ν = 700 μHz. The extrapolated surface velocities
    of the low-frequency modes are small and thus hard to observe, but their large
    kinetic energies deeper in the interior could significantly impact AM transport,
    which has not yet been investigated.
acknowledgement: 'We would like to thank the referee for their careful reading of
  the manuscript and their constructive comments that helped improve the paper. N.B.V.
  would like to thank K. Belkacem and J. Philidet for helpful discussions. N.B.V.
  is supported by STFC grant ST/Y002164/1. A.L.S. acknowledges 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
  ATPS (CNRS/INSU). Part of this work was supported by the ERC grant No. 787361-COBOM.
  R.H.D.T. acknowledges support from NASA grants 80NSSC24K0895 and 80NSSC23K1517,
  and NSF grant 2407636. A.L. is supported by ERC Starting Grant 101165631 (“Calcifer”).
  The authors would like to acknowledge the use of the University of Exeter High-Performance
  Computing (HPC) facility, ISCA, in carrying out this work. This work used the DiRAC
  Memory Intensive service (Cosma8) at Durham University, managed by the Institute
  for Computational Cosmology, and the DiRAC Data Intensive service (DIaL3) at the
  University of Leicester, managed by the University of Leicester Research Computing
  Service. These facilities are managed on behalf of the STFC DiRAC HPC (www.dirac.ac.uk).
  The DiRAC services at Durham and Leicester were funded by BEIS, UKRI, and STFC capital
  funding, and STFC operations grants. The service at Durham received funding from
  Durham University. DiRAC is part of the UKRI Digital Research Infrastructure.'
article_number: '154'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Nils B.
  full_name: De Vries, Nils B.
  last_name: De Vries
- first_name: Arthur
  full_name: Le Saux, Arthur
  last_name: Le Saux
- first_name: Isabelle
  full_name: Baraffe, Isabelle
  last_name: Baraffe
- first_name: Thomas
  full_name: Guillet, Thomas
  last_name: Guillet
- first_name: Richard H.D.
  full_name: Townsend, Richard H.D.
  last_name: Townsend
- first_name: Armand
  full_name: Leclerc, Armand
  id: 2a1fb1fc-f373-11ef-901a-87cee43a1217
  last_name: Leclerc
- first_name: Adrien
  full_name: Morison, Adrien
  last_name: Morison
citation:
  ama: De Vries NB, Le Saux A, Baraffe I, et al. Revealing mixed modes in compressible
    hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>.
    2026;1005(2). doi:<a href="https://doi.org/10.3847/1538-4357/ae7a3c">10.3847/1538-4357/ae7a3c</a>
  apa: De Vries, N. B., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D.,
    Leclerc, A., &#38; Morison, A. (2026). Revealing mixed modes in compressible hydrodynamical
    simulations of red giant stars. <i>The Astrophysical Journal</i>. IOP Publishing.
    <a href="https://doi.org/10.3847/1538-4357/ae7a3c">https://doi.org/10.3847/1538-4357/ae7a3c</a>
  chicago: De Vries, Nils B., Arthur Le Saux, Isabelle Baraffe, Thomas Guillet, Richard
    H.D. Townsend, Armand Leclerc, and Adrien Morison. “Revealing Mixed Modes in Compressible
    Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>.
    IOP Publishing, 2026. <a href="https://doi.org/10.3847/1538-4357/ae7a3c">https://doi.org/10.3847/1538-4357/ae7a3c</a>.
  ieee: N. B. De Vries <i>et al.</i>, “Revealing mixed modes in compressible hydrodynamical
    simulations of red giant stars,” <i>The Astrophysical Journal</i>, vol. 1005,
    no. 2. IOP Publishing, 2026.
  ista: De Vries NB, Le Saux A, Baraffe I, Guillet T, Townsend RHD, Leclerc A, Morison
    A. 2026. Revealing mixed modes in compressible hydrodynamical simulations of red
    giant stars. The Astrophysical Journal. 1005(2), 154.
  mla: De Vries, Nils B., et al. “Revealing Mixed Modes in Compressible Hydrodynamical
    Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>, vol. 1005,
    no. 2, 154, IOP Publishing, 2026, doi:<a href="https://doi.org/10.3847/1538-4357/ae7a3c">10.3847/1538-4357/ae7a3c</a>.
  short: N.B. De Vries, A. Le Saux, I. Baraffe, T. Guillet, R.H.D. Townsend, A. Leclerc,
    A. Morison, The Astrophysical Journal 1005 (2026).
das_tickbox: '1'
dataavailabilitystatement: The kinetic energies and surface velocities shown in Figure
  4, as well as the underlying spectral data of this work, can be found in a Zenodo
  repository at doi:10.5281/zenodo.18661976.
date_created: 2026-07-12T22:02:17Z
date_published: 2026-07-10T00:00:00Z
date_updated: 2026-07-13T08:16:25Z
day: '10'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/1538-4357/ae7a3c
external_id:
  arxiv:
  - '2606.07125'
file:
- access_level: open_access
  checksum: d32061d2341bac3adeb404975c6bd59e
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T08:14:01Z
  date_updated: 2026-07-13T08:14:01Z
  file_id: '22275'
  file_name: 2026_AstrophysicalJour_deVries.pdf
  file_size: 14866194
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T08:14:01Z
has_accepted_license: '1'
intvolume: '      1005'
issue: '2'
keyword:
- Stellar physics
- Stellar interiors
- Asteroseismology
- Stellar oscillations
- Hydrodynamical simulations
language:
- iso: eng
month: '07'
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: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Revealing mixed modes in compressible hydrodynamical simulations of red giant
  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: 1005
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '22261'
abstract:
- lang: eng
  text: 'Climate change is significantly altering regional precipitation patterns
    across Europe and the Mediterranean. We analyze daily precipitation distribution
    changes in a 15-member Euro-CORDEX ensemble, through a diagnostic framework that
    separates occurrence changes, wet-days intensity shifts and distortions. At +4
    ∘C global warming, Northern Europe shows a robust intensification of precipitation,
    driven by both higher occurrence and stronger events. Conversely, the Mediterranean
    exhibits a dominant drying signal, primarily due to fewer wet-days, which impacts
    daily precipitation distribution even for heavy rainfall. Transitional zones in
    the northern Mediterranean reveal “U-shape” regimes, with rising extremes but
    declining moderate rain. Comparing with ERA5 reanalysis over the past, low model
    agreement in the south highlights higher uncertainty in the Mediterranean region.
    The timing of robust signal emergence varies: Northern Europe shows robust patterns
    from +1 ∘C, while the Mediterranean exhibits delays until +3-4 ∘C. These findings
    are essential for informing risk-based adaptation strategies.'
acknowledgement: J.A. gratefully acknowledges the JSPS postdoctoral fellowship (Japan
  Society for Promotion of Science, grant number P25709). C.J.M. gratefully acknowledges
  funding from the European Research Council (ERC) under the European Union’s Horizon
  2020 research and innovation program (Project CLUSTER, Grant Agreement No. 805041).
  The authors also thank Samuel Somot (Centre National de Recherches Météorologiques,
  Toulouse) and Juliette Blanchet (Institut des Géosciences de l’Environnement, Grenoble)
  for their fruitful discussions on the project.
article_number: '572'
article_processing_charge: Yes
article_type: original
author:
- first_name: Julie
  full_name: André, Julie
  last_name: André
- first_name: Nicolas
  full_name: Chiabrando, Nicolas
  last_name: Chiabrando
- first_name: Caroline J
  full_name: Muller, Caroline J
  id: f978ccb0-3f7f-11eb-b193-b0e2bd13182b
  last_name: Muller
  orcid: 0000-0001-5836-5350
- first_name: Philippe
  full_name: Drobinski, Philippe
  last_name: Drobinski
- first_name: Fabio
  full_name: D’Andrea, Fabio
  last_name: D’Andrea
citation:
  ama: André J, Chiabrando N, Muller CJ, Drobinski P, D’Andrea F. Distinct regimes
    of precipitation changes across Europe and the Mediterranean under global warming.
    <i>Communications Earth and Environment</i>. 2026;7. doi:<a href="https://doi.org/10.1038/s43247-026-03519-7">10.1038/s43247-026-03519-7</a>
  apa: André, J., Chiabrando, N., Muller, C. J., Drobinski, P., &#38; D’Andrea, F.
    (2026). Distinct regimes of precipitation changes across Europe and the Mediterranean
    under global warming. <i>Communications Earth and Environment</i>. Springer Nature.
    <a href="https://doi.org/10.1038/s43247-026-03519-7">https://doi.org/10.1038/s43247-026-03519-7</a>
  chicago: André, Julie, Nicolas Chiabrando, Caroline J Muller, Philippe Drobinski,
    and Fabio D’Andrea. “Distinct Regimes of Precipitation Changes across Europe and
    the Mediterranean under Global Warming.” <i>Communications Earth and Environment</i>.
    Springer Nature, 2026. <a href="https://doi.org/10.1038/s43247-026-03519-7">https://doi.org/10.1038/s43247-026-03519-7</a>.
  ieee: J. André, N. Chiabrando, C. J. Muller, P. Drobinski, and F. D’Andrea, “Distinct
    regimes of precipitation changes across Europe and the Mediterranean under global
    warming,” <i>Communications Earth and Environment</i>, vol. 7. Springer Nature,
    2026.
  ista: André J, Chiabrando N, Muller CJ, Drobinski P, D’Andrea F. 2026. Distinct
    regimes of precipitation changes across Europe and the Mediterranean under global
    warming. Communications Earth and Environment. 7, 572.
  mla: André, Julie, et al. “Distinct Regimes of Precipitation Changes across Europe
    and the Mediterranean under Global Warming.” <i>Communications Earth and Environment</i>,
    vol. 7, 572, Springer Nature, 2026, doi:<a href="https://doi.org/10.1038/s43247-026-03519-7">10.1038/s43247-026-03519-7</a>.
  short: J. André, N. Chiabrando, C.J. Muller, P. Drobinski, F. D’Andrea, Communications
    Earth and Environment 7 (2026).
das_tickbox: '1'
dataavailabilitystatement: ERA5 reanalysis and Euro-CORDEX simulations are publicly
  available from https://doi.org/10.24381/cds.143582cf and https://cordex.org/data-access/esgf/.
  The custom code developed and used for this paper can be accessed through Zenodo,
  https://doi.org/10.5281/zenodo.18995401.
date_created: 2026-07-12T22:02:16Z
date_published: 2026-07-06T00:00:00Z
date_updated: 2026-07-13T07:13:21Z
day: '06'
ddc:
- '550'
department:
- _id: CaMu
doi: 10.1038/s43247-026-03519-7
ec_funded: 1
file:
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  checksum: fd8f57cbe180f7a4d49ab17b3571ad2b
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  creator: dernst
  date_created: 2026-07-13T07:12:35Z
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language:
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month: '07'
oa: 1
oa_version: Published Version
project:
- _id: 629205d8-2b32-11ec-9570-e1356ff73576
  call_identifier: H2020
  grant_number: '805041'
  name: Organization of CLoUdS, and implications of Tropical  cyclones and for the
    Energetics of the tropics, in current and waRming climate
publication: Communications Earth and Environment
publication_identifier:
  eissn:
  - 2662-4435
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Distinct regimes of precipitation changes across Europe and the Mediterranean
  under global warming
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: 7
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
_id: '22267'
abstract:
- lang: eng
  text: Thermal pollution, whether local or driven by global warming, threatens biodiversity
    in part through its detrimental effects on reproduction. Non-coding small RNAs
    (sRNAs) are crucial for maintaining germline developmental robustness under heat
    stress. Remarkably, we uncovered that neuronal sRNAs regulate germ cells’ thermotolerance,
    affecting both spermatogenic and oogenic germlines in a cell-non-autonomous manner.
    Furthermore, we demonstrate that, in RNAi mutants, an oxygen-sensing neural circuit,
    modulated by neuropeptide signaling, antagonizes germline maintenance, likely
    reflecting the nematode’s innate association of reduced oxygen levels with food
    availability and reproductive permissive environments. Finally, we provide evidence
    that laboratory-domesticated alleles of oxygen-response genes encoding neuropeptide
    receptor NPR-1 and hexacoordinated globin GLB-5 compromise germline thermotolerance.
    Hence, our findings raise the possibility that sensory perception, independent
    of direct environmental change, modulates germline integrity, highlighting a novel
    mechanism by which neural circuits integrate environmental information to safeguard
    reproductive fitness in fluctuating environments.
acknowledgement: We thank Itai Reiger for their assistance with experiments. We thank
  Cori Bargmann (Rockefeller University) for providing introgressed strains carrying
  HW alleles of npr-1 and glb-5. Some graphics were created with Biorender.com. We
  are grateful to WormBase for providing valuable data and resources. Some strains
  were provided by the Caenorhabditis Genetics Center (CGC), which is funded by NIH
  Office of Research Infrastructure Programs (P40 OD010440). O.R. is grateful for
  the support of the Morris Kahn Foundation. C.K.E. was supported by an EMBO fellowship
  ALTF 6-2022. This work is funded by Eric and Wendy Schmidt Fund for Strategic Innovation
  Polymath Award 0140001000 (O.R.); European Research Council grant 335624 (O.R.);
  Israel Science Foundation 979/21 (Y.B.T.); and the US-Israel Binational Science
  Foundation 2023036 (Y.B.T.).
article_processing_charge: Yes (in subscription journal)
article_type: original
author:
- first_name: Chee Kiang
  full_name: Ewe, Chee Kiang
  last_name: Ewe
- first_name: Hanna
  full_name: Achache, Hanna
  last_name: Achache
- first_name: Hanna
  full_name: Schön, Hanna
  id: C8E17EDC-D7AA-11E9-B7B7-45ECE5697425
  last_name: Schön
- first_name: Leonid
  full_name: Kontorovich, Leonid
  last_name: Kontorovich
- first_name: Guy
  full_name: Teichman, Guy
  last_name: Teichman
- first_name: Shir
  full_name: Weiss, Shir
  last_name: Weiss
- first_name: Anna
  full_name: Mogilevskaya, Anna
  last_name: Mogilevskaya
- first_name: Myriam
  full_name: Valenski, Myriam
  last_name: Valenski
- first_name: Sarit
  full_name: Anava, Sarit
  last_name: Anava
- first_name: Rutwik
  full_name: Bardapurkar, Rutwik
  last_name: Bardapurkar
- first_name: Hila
  full_name: Gingold, Hila
  last_name: Gingold
- first_name: Rachel
  full_name: Posner, Rachel
  last_name: Posner
- first_name: Olga
  full_name: Antonova, Olga
  last_name: Antonova
- first_name: Mario
  full_name: De Bono, Mario
  id: 4E3FF80E-F248-11E8-B48F-1D18A9856A87
  last_name: De Bono
  orcid: 0000-0001-8347-0443
- first_name: Yonatan B.
  full_name: Tzur, Yonatan B.
  last_name: Tzur
- first_name: Oded
  full_name: Rechavi, Oded
  last_name: Rechavi
citation:
  ama: Ewe CK, Achache H, Schön H, et al. Neuronal RNAi and oxygen-sensing circuit
    shape germline resilience to heat stress. <i>Current Biology</i>. doi:<a href="https://doi.org/10.1016/j.cub.2026.06.016">10.1016/j.cub.2026.06.016</a>
  apa: Ewe, C. K., Achache, H., Schön, H., Kontorovich, L., Teichman, G., Weiss, S.,
    … Rechavi, O. (n.d.). Neuronal RNAi and oxygen-sensing circuit shape germline
    resilience to heat stress. <i>Current Biology</i>. Elsevier. <a href="https://doi.org/10.1016/j.cub.2026.06.016">https://doi.org/10.1016/j.cub.2026.06.016</a>
  chicago: Ewe, Chee Kiang, Hanna Achache, Hanna Schön, Leonid Kontorovich, Guy Teichman,
    Shir Weiss, Anna Mogilevskaya, et al. “Neuronal RNAi and Oxygen-Sensing Circuit
    Shape Germline Resilience to Heat Stress.” <i>Current Biology</i>. Elsevier, n.d.
    <a href="https://doi.org/10.1016/j.cub.2026.06.016">https://doi.org/10.1016/j.cub.2026.06.016</a>.
  ieee: C. K. Ewe <i>et al.</i>, “Neuronal RNAi and oxygen-sensing circuit shape germline
    resilience to heat stress,” <i>Current Biology</i>. Elsevier.
  ista: Ewe CK, Achache H, Schön H, Kontorovich L, Teichman G, Weiss S, Mogilevskaya
    A, Valenski M, Anava S, Bardapurkar R, Gingold H, Posner R, Antonova O, de Bono
    M, Tzur YB, Rechavi O. Neuronal RNAi and oxygen-sensing circuit shape germline
    resilience to heat stress. Current Biology.
  mla: Ewe, Chee Kiang, et al. “Neuronal RNAi and Oxygen-Sensing Circuit Shape Germline
    Resilience to Heat Stress.” <i>Current Biology</i>, Elsevier, doi:<a href="https://doi.org/10.1016/j.cub.2026.06.016">10.1016/j.cub.2026.06.016</a>.
  short: C.K. Ewe, H. Achache, H. Schön, L. Kontorovich, G. Teichman, S. Weiss, A.
    Mogilevskaya, M. Valenski, S. Anava, R. Bardapurkar, H. Gingold, R. Posner, O.
    Antonova, M. de Bono, Y.B. Tzur, O. Rechavi, Current Biology (n.d.).
das_tickbox: '1'
dataavailabilitystatement: "* All NGS data are available through GEO under accession
  number GSE331410.\r\n* This paper does not report original code.\r\n* Any additional
  information required to reanalyze the data reported in this paper is available from
  the lead contact upon request."
date_created: 2026-07-12T22:02:18Z
date_published: 2026-07-06T00:00:00Z
date_updated: 2026-07-13T08:23:09Z
day: '06'
ddc:
- '570'
department:
- _id: MaDe
doi: 10.1016/j.cub.2026.06.016
external_id:
  pmid:
  - '42409014'
has_accepted_license: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1016/j.cub.2026.06.016
month: '07'
oa: 1
oa_version: Published Version
pmid: 1
publication: Current Biology
publication_identifier:
  eissn:
  - 1879-0445
  issn:
  - 0960-9822
publication_status: inpress
publisher: Elsevier
quality_controlled: '1'
researchdata_availability: upon request
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Neuronal RNAi and oxygen-sensing circuit shape germline resilience to heat
  stress
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
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22270'
abstract:
- lang: eng
  text: "The explosion of a white dwarf (WD) in a close binary can launch a surviving
    runaway star at\r\nvelocities of ≳ 1000 km s−1\r\n. Such runaways provide a direct
    probe of thermonuclear supernovae (SNe)\r\nin double-degenerate binaries. Several
    candidate runaways are known, but their evolutionary states\r\nand the demographics
    of the broader population are uncertain. To enable robust population inference,\r\nwe
    carry out a systematic survey for hypervelocity runaways with a simple selection
    function, selecting\r\ncandidates based on large Gaia-inferred tangential velocities
    and blue colors. We classify 100% of the\r\nresulting 92 candidates using a combination
    of spectroscopic follow-up and archival data. The search\r\nyields ten suspected
    D6\r\nstars and three LP 40-365 stars. Three D6\r\nstars are new discoveries,
    including\r\ntwo hot (Teff ≳ 50,000 K) objects and one cool (Teff ≈ 7,000 K) object.
    We forward-model our survey\r\nunder several proposed D6\r\nstar evolutionary
    models, coupling each to a Galactic model and the survey\r\nselection function.
    No single model reproduces the observed diversity of D6\r\nstars, which likely
    reflects\r\na range of remnant masses, ages, and heating mechanisms. Models in
    which runaway companions\r\nare heated by SN shocks alone are too faint and short-lived
    to explain most of the observed sample,\r\nwhile fully reheated models are too
    luminous and long-lived. Models with intermediate heating,\r\nas occurs in some
    simulations of violent mergers and partially disrupted remnants, best match the\r\nobserved
    magnitude, distance, and kinematic-age distributions. The inferred D6\r\nstar
    birth rate is\r\nmodel dependent, but the models that best match the observed
    population require rates of only a\r\nfew percent of the Galactic SN Ia rate,
    perhaps implying that most SNe Ia result from WD binaries\r\nin which both components
    explode. If most SNe Ia do produce surviving runaways, these must be\r\nfainter
    or shorter-lived than the currently known runaways."
acknowledgement: "We thank Lars Bildsten, Evan Bauer, Ruediger Pakmor, Jim Fuller,
  Logan Proust, Abinaya Rajamuthukumar, and Stephan Geier for useful discussion related
  to\r\nthis work.\r\nThis work was supported by NSF grants AST-2508988\r\nand AST-2205631,
  NASA/ESA Hubble Space Telescope\r\nprogram No. 17441, and Scialog grant #SA-LSST-2024-\r\n114c
  from the Research Corporation for Science Advancement. The Kavli Institute for Theoretical
  Physics\r\n(KITP) hosted the program, “White Dwarfs as Probes of\r\nthe Evolution
  of Planets, Stars, the Milky Way, and the\r\nExpanding Universe,” during which this
  project was initiated. This research was supported in part by the U.S.\r\nNational
  Science Foundation (NSF) under grants PHY1748958. This research benefited from discussions
  that\r\nwere funded by the Gordon and Betty Moore Foundation\r\nthrough Grant GBMF5076.\r\nWe
  thank the staffs of the various observatories at\r\nwhich data were obtained. This
  work is partially based\r\non observations obtained at the Southern Astrophysical
  Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia,
  Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s
  NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan
  State University\r\n(MSU). Some of the data presented herein were obtained\r\nat
  the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among
  the California Institute of\r\nTechnology, the University of California, and NASA;
  the observatory was made possible by the generous financial\r\nsupport of the W.
  M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive
  (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet
  Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand
  Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space
  Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby
  the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium).
  Funding for the DPAC has been\r\nprovided by national institutions, in particular
  the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Kareem
  full_name: El-Badry, Kareem
  last_name: El-Badry
- first_name: Klaus
  full_name: Werner, Klaus
  last_name: Werner
- first_name: Ken J.
  full_name: Shen, Ken J.
  last_name: Shen
- first_name: Jay
  full_name: Strader, Jay
  last_name: Strader
- first_name: Antonio C.
  full_name: Rodriguez, Antonio C.
  last_name: Rodriguez
- first_name: Jiwon Jesse
  full_name: Han, Jiwon Jesse
  last_name: Han
- first_name: Vedant
  full_name: Chandra, Vedant
  last_name: Chandra
- first_name: Laura
  full_name: Chomiuk, Laura
  last_name: Chomiuk
- first_name: Zachary P.
  full_name: Vanderbosch, Zachary P.
  last_name: Vanderbosch
- first_name: Lisa
  full_name: Blomberg, Lisa
  last_name: Blomberg
- first_name: Natsuko
  full_name: Yamaguchi, Natsuko
  last_name: Yamaguchi
- first_name: Pranav
  full_name: Nagarajan, Pranav
  last_name: Nagarajan
- first_name: Ilaria
  full_name: Caiazzo, Ilaria
  id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
  last_name: Caiazzo
  orcid: 0000-0002-4770-5388
- first_name: Joannes C
  full_name: van Roestel, Joannes C
  id: 4d122fc8-6083-11f0-87a5-97d68b860333
  last_name: van Roestel
- first_name: Hila
  full_name: Glanz, Hila
  last_name: Glanz
- first_name: Tin Long Sunny
  full_name: Wong, Tin Long Sunny
  last_name: Wong
- first_name: Aakash
  full_name: Bhat, Aakash
  last_name: Bhat
- first_name: Mark A.
  full_name: Hollands, Mark A.
  last_name: Hollands
citation:
  ama: El-Badry K, Werner K, Shen KJ, et al. A systematic survey for hypervelocity
    runaways from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>.
    2026;9. doi:<a href="https://doi.org/10.33232/001c.164326">10.33232/001c.164326</a>
  apa: El-Badry, K., Werner, K., Shen, K. J., Strader, J., Rodriguez, A. C., Han,
    J. J., … Hollands, M. A. (2026). A systematic survey for hypervelocity runaways
    from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>. Maynooth
    Academic Publishing. <a href="https://doi.org/10.33232/001c.164326">https://doi.org/10.33232/001c.164326</a>
  chicago: El-Badry, Kareem, Klaus Werner, Ken J. Shen, Jay Strader, Antonio C. Rodriguez,
    Jiwon Jesse Han, Vedant Chandra, et al. “A Systematic Survey for Hypervelocity
    Runaways from Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>.
    Maynooth Academic Publishing, 2026. <a href="https://doi.org/10.33232/001c.164326">https://doi.org/10.33232/001c.164326</a>.
  ieee: K. El-Badry <i>et al.</i>, “A systematic survey for hypervelocity runaways
    from thermonuclear supernovae,” <i>The Open Journal of Astrophysics</i>, vol.
    9. Maynooth Academic Publishing, 2026.
  ista: El-Badry K, Werner K, Shen KJ, Strader J, Rodriguez AC, Han JJ, Chandra V,
    Chomiuk L, Vanderbosch ZP, Blomberg L, Yamaguchi N, Nagarajan P, Caiazzo I, van
    Roestel JC, Glanz H, Wong TLS, Bhat A, Hollands MA. 2026. A systematic survey
    for hypervelocity runaways from thermonuclear supernovae. The Open Journal of
    Astrophysics. 9.
  mla: El-Badry, Kareem, et al. “A Systematic Survey for Hypervelocity Runaways from
    Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth
    Academic Publishing, 2026, doi:<a href="https://doi.org/10.33232/001c.164326">10.33232/001c.164326</a>.
  short: K. El-Badry, K. Werner, K.J. Shen, J. Strader, A.C. Rodriguez, J.J. Han,
    V. Chandra, L. Chomiuk, Z.P. Vanderbosch, L. Blomberg, N. Yamaguchi, P. Nagarajan,
    I. Caiazzo, J.C. van Roestel, H. Glanz, T.L.S. Wong, A. Bhat, M.A. Hollands, The
    Open Journal of Astrophysics 9 (2026).
das_tickbox: '1'
dataavailabilitystatement: "We thank the staffs of the various observatories at\r\nwhich
  data were obtained. This work is partially based\r\non observations obtained at
  the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof
  the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the
  US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat
  Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented
  herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific
  partnership among the California Institute of\r\nTechnology, the University of California,
  and NASA; the\r\nobservatory was made possible by the generous financial\r\nsupport
  of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive
  (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet
  Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand
  Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space
  Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby
  the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium).
  Funding for the DPAC has been\r\nprovided by national institutions, in particular
  the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement."
date_created: 2026-07-12T22:02:19Z
date_published: 2026-06-30T00:00:00Z
date_updated: 2026-07-13T09:09:34Z
day: '30'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.33232/001c.164326
external_id:
  arxiv:
  - '2606.11293'
file:
- access_level: open_access
  checksum: 6320fd19e5ea3399f332be5aab022736
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T09:05:36Z
  date_updated: 2026-07-13T09:05:36Z
  file_id: '22282'
  file_name: 2026_OpenJourAstrophysics_ElBadry.pdf
  file_size: 1994596
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T09:05:36Z
has_accepted_license: '1'
intvolume: '         9'
keyword:
- white dwarfs
- 'binaries: close'
- 'stars: chemically peculiar'
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: The Open Journal of Astrophysics
publication_identifier:
  eissn:
  - 2565-6120
publication_status: published
publisher: Maynooth Academic Publishing
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: no
title: A systematic survey for hypervelocity runaways from thermonuclear supernovae
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 9
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '22268'
abstract:
- lang: eng
  text: AlphaFold3 predicts highly accurate protein structures from sequence but tends
    to collapse to a single dominant conformation, even when the underlying structure
    is inherently heterogeneous. Moreover, its predictions are oblivious to experimental
    conditions that can alter local sequence conformation. In this work, we show that
    AlphaFold3 can be guided to match data obtained by nuclear magnetic resonance
    (NMR) spectroscopy, X-ray crystallography and cryogenic electron microscopy (cryo-EM)
    experiments and combinations thereof. Our approach can also incorporate data that
    explicitly report on dynamics, such as site-resolved order parameters. We demonstrate
    that this methodology generates compact structural ensembles whose ensemble-averaged
    observables agree with experiment, with fewer distance restraint violations than
    traditionally resolved NMR structures and with unmodeled alternate conformations
    uncovered in electron density. This methodology paves the way for experimentally
    aware predictive models that generate structural ensembles consistent with the
    measurements, potentially over multiple modalities, and that can be further refined
    toward thermodynamically grounded ensembles by incorporating energetics.
acknowledgement: A. Marx acknowledges the financial support of the Helmsley Fellowships
  Program for Sustainability and Health. A.M.B. and P.S. are supported by the Institute
  of Science and Technology Austria Internal Project Call grant Generative Protein
  NMR. S.V. was supported in part by funding from the Eric and Wendy Schmidt Center
  at the Broad Institute of MIT and Harvard. Open access funding provided by Institute
  of Science and Technology (IST Austria).
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Sai A
  full_name: Maddipatla, Sai A
  id: e957f5e5-91c9-11f0-a95f-e090f66ecb4d
  last_name: Maddipatla
- first_name: Nadav E
  full_name: Sellam, Nadav E
  id: ef280fe0-91c9-11f0-a95f-8dea3f5bc513
  last_name: Sellam
- first_name: Meital I
  full_name: Bojan, Meital I
  id: 11d88cf5-91ca-11f0-a95f-edf9f08f47b7
  last_name: Bojan
- first_name: Vova
  full_name: Masalitin, Vova
  id: ff7958eb-91c9-11f0-a95f-f3bf65828cf6
  last_name: Masalitin
- first_name: Sanketh
  full_name: Vedula, Sanketh
  last_name: Vedula
- first_name: Paul
  full_name: Schanda, Paul
  id: 7B541462-FAF6-11E9-A490-E8DFE5697425
  last_name: Schanda
  orcid: 0000-0002-9350-7606
- first_name: Ailie
  full_name: Marx, Ailie
  last_name: Marx
- first_name: Alexander
  full_name: Bronstein, Alexander
  id: 58f3726e-7cba-11ef-ad8b-e6e8cb3904e6
  last_name: Bronstein
  orcid: 0000-0001-9699-8730
citation:
  ama: Maddipatla SA, Sellam NE, Bojan MI, et al. Experiment-guided AlphaFold3 resolves
    measurement-consistent protein ensembles. <i>Nature Biotechnology</i>. 2026. doi:<a
    href="https://doi.org/10.1038/s41587-026-03166-5">10.1038/s41587-026-03166-5</a>
  apa: Maddipatla, S. A., Sellam, N. E., Bojan, M. I., Masalitin, V., Vedula, S.,
    Schanda, P., … Bronstein, A. M. (2026). Experiment-guided AlphaFold3 resolves
    measurement-consistent protein ensembles. <i>Nature Biotechnology</i>. Springer
    Nature. <a href="https://doi.org/10.1038/s41587-026-03166-5">https://doi.org/10.1038/s41587-026-03166-5</a>
  chicago: Maddipatla, Sai A, Nadav E Sellam, Meital I Bojan, Vova Masalitin, Sanketh
    Vedula, Paul Schanda, Ailie Marx, and Alex M. Bronstein. “Experiment-Guided AlphaFold3
    Resolves Measurement-Consistent Protein Ensembles.” <i>Nature Biotechnology</i>.
    Springer Nature, 2026. <a href="https://doi.org/10.1038/s41587-026-03166-5">https://doi.org/10.1038/s41587-026-03166-5</a>.
  ieee: S. A. Maddipatla <i>et al.</i>, “Experiment-guided AlphaFold3 resolves measurement-consistent
    protein ensembles,” <i>Nature Biotechnology</i>. Springer Nature, 2026.
  ista: Maddipatla SA, Sellam NE, Bojan MI, Masalitin V, Vedula S, Schanda P, Marx
    A, Bronstein AM. 2026. Experiment-guided AlphaFold3 resolves measurement-consistent
    protein ensembles. Nature Biotechnology.
  mla: Maddipatla, Sai A., et al. “Experiment-Guided AlphaFold3 Resolves Measurement-Consistent
    Protein Ensembles.” <i>Nature Biotechnology</i>, Springer Nature, 2026, doi:<a
    href="https://doi.org/10.1038/s41587-026-03166-5">10.1038/s41587-026-03166-5</a>.
  short: S.A. Maddipatla, N.E. Sellam, M.I. Bojan, V. Masalitin, S. Vedula, P. Schanda,
    A. Marx, A.M. Bronstein, Nature Biotechnology (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: All structures and metrics reported in this paper are openly
  available on Harvard Dataverse - https://doi.org/10.7910/DVN/PLYUHN. All code is
  openly available on GitHub (https://github.com/sai-advaith/guided_alphafold); the
  version used for this paper (version 0.9.1) is permanently archived on Zenodo https://doi.org/10.5281/zenodo.17307005
date_created: 2026-07-12T22:02:19Z
date_published: 2026-06-29T00:00:00Z
date_updated: 2026-07-13T09:34:36Z
day: '29'
ddc:
- '570'
department:
- _id: PaSc
- _id: AlBr
- _id: GradSch
doi: 10.1038/s41587-026-03166-5
external_id:
  pmid:
  - '42374114'
has_accepted_license: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1038/s41587-026-03166-5
month: '06'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Biotechnology
publication_identifier:
  eissn:
  - 1546-1696
  issn:
  - 1087-0156
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles
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
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
_id: '22269'
abstract:
- lang: eng
  text: The divisome apparatus synthesizes septal peptidoglycan (PG) during bacterial
    division. In Escherichia coli, the class A penicillin-binding protein (aPBP) called
    PBP1b has been implicated in division, but its role in the process has remained
    unclear. Here we show using in situ cryo-electron tomography, genetics and other
    imaging methods that PBP1b is required to produce a wedge-like density of PG at
    the division site and that loss of this structure weakens the division site, making
    it hypersusceptible to osmotic lysis. Surprisingly, the activator LpoB needed
    for general PBP1b function was not required for its role in division. Of the two
    PBP1b isoforms produced in cells, we show that the one with an extended cytoplasmic
    N terminus localizes to and functions at the division site, probably via recruitment
    by the FtsA component of the divisome. The conservation of aPBPs with extended
    cytoplasmic N termini suggests that other Gram-negative bacteria may use similar
    mechanisms for division site reinforcement.
acknowledgement: We thank all members of the Bernhardt, Rudner, Navarro and Vettiger
  Laboratories for support and helpful conversations. We thank C. Genoud, J. Daraspe,
  A. Mucciolo and D. de Bellis at the Electron Microscopy Facility of the University
  of Lausanne and E. Jeanvoine for providing access to workstations for cryo-ET image
  processing; S. Sterling, C. Borsa, J. Podgorski, P. Vinh Dip, E. Brignole and A.
  Osherov at the MIT.nano cryo-EM facility, K. Song and C. Xu at the University of
  Massachusetts cryo-EM facility, and R. Walsh and Z. Li at the cryo-EM at Harvard
  Medical School facility for providing access to the cryo-EM microscopes and for
  all their help, advice and maintenance of cryo-EM equipment. AFM was performed at
  the Harvard University Center for Nanoscale Systems (CNS), a member of the National
  Nanotechnology Coordinated Infrastructure Network (NNCI), which is supported by
  the National Science Foundation under NSF award no. ECCS-2025158. We thank N. S.
  Colella for excellent advice on AFM data acquisition and analysis; the MicRoN imaging
  core at Harvard Medical School for excellent advice on live cell imaging and maintenance
  of fluorescence microscopes; B. Krautz for creating the cartoon illustrations (www.sciencecommunicated.com);
  and L. Miles and R. Aeschimann for assistance with strain construction. A.V. was
  supported by an EMBO long-term postdoctoral fellowship ALTF_89-2019, the Swiss National
  Science Foundation (SNSF) Postdoc.Mobility fellowship P500PB_203143. P.P.N. was
  a recipient of early postdoc.mobility and postdoc.mobility fellowships (P2BSP3_188112
  and P400PB_199252). This work was also supported by funding from the National Institutes
  of Health (R35GM142553 to L.H.C. and R01AI083365 to T.G.B.), investigator funds
  from the Howard Hughes Medical Institute (T.G.B.), an SNSF project grant (320030-236243
  to A.V.), an SNSF Starting Grant (TMSGI3_218251 to P.P.N.), an SNSF Project grant
  (320030-236069 to P.P.N), an SNSF SPARK grant (CRSK-3_237167 to P.P.N.), cryo-EM
  funds from the Faculty of Biology and Medicine at University of Lausanne to P.P.N.
  and the Foundation Pierre Mercier pour la Science (to P.P.N.).
article_processing_charge: Yes (in subscription journal)
article_type: original
author:
- first_name: Paula P.
  full_name: Navarro, Paula P.
  last_name: Navarro
- first_name: Andrea
  full_name: Vettiger, Andrea
  last_name: Vettiger
- first_name: Roman
  full_name: Hajdu, Roman
  id: ffab949d-133f-11ed-8f02-94de21ace503
  last_name: Hajdu
- first_name: Virly Y.
  full_name: Ananda, Virly Y.
  last_name: Ananda
- first_name: Alejandro
  full_name: López-Tavares, Alejandro
  last_name: López-Tavares
- first_name: Ernst W.
  full_name: Schmid, Ernst W.
  last_name: Schmid
- first_name: Johannes C.
  full_name: Walter, Johannes C.
  last_name: Walter
- first_name: Martin
  full_name: Loose, Martin
  id: 462D4284-F248-11E8-B48F-1D18A9856A87
  last_name: Loose
  orcid: 0000-0001-7309-9724
- first_name: Luke H.
  full_name: Chao, Luke H.
  last_name: Chao
- first_name: Thomas G.
  full_name: Bernhardt, Thomas G.
  last_name: Bernhardt
citation:
  ama: Navarro PP, Vettiger A, Hajdu R, et al. The penicillin-binding protein PBP1b
    fortifies the Escherichia coli division site against osmotic rupture. <i>Nature
    Microbiology</i>. 2026. doi:<a href="https://doi.org/10.1038/s41564-026-02403-6">10.1038/s41564-026-02403-6</a>
  apa: Navarro, P. P., Vettiger, A., Hajdu, R., Ananda, V. Y., López-Tavares, A.,
    Schmid, E. W., … Bernhardt, T. G. (2026). The penicillin-binding protein PBP1b
    fortifies the Escherichia coli division site against osmotic rupture. <i>Nature
    Microbiology</i>. Springer Nature. <a href="https://doi.org/10.1038/s41564-026-02403-6">https://doi.org/10.1038/s41564-026-02403-6</a>
  chicago: Navarro, Paula P., Andrea Vettiger, Roman Hajdu, Virly Y. Ananda, Alejandro
    López-Tavares, Ernst W. Schmid, Johannes C. Walter, Martin Loose, Luke H. Chao,
    and Thomas G. Bernhardt. “The Penicillin-Binding Protein PBP1b Fortifies the Escherichia
    Coli Division Site against Osmotic Rupture.” <i>Nature Microbiology</i>. Springer
    Nature, 2026. <a href="https://doi.org/10.1038/s41564-026-02403-6">https://doi.org/10.1038/s41564-026-02403-6</a>.
  ieee: P. P. Navarro <i>et al.</i>, “The penicillin-binding protein PBP1b fortifies
    the Escherichia coli division site against osmotic rupture,” <i>Nature Microbiology</i>.
    Springer Nature, 2026.
  ista: Navarro PP, Vettiger A, Hajdu R, Ananda VY, López-Tavares A, Schmid EW, Walter
    JC, Loose M, Chao LH, Bernhardt TG. 2026. The penicillin-binding protein PBP1b
    fortifies the Escherichia coli division site against osmotic rupture. Nature Microbiology.
  mla: Navarro, Paula P., et al. “The Penicillin-Binding Protein PBP1b Fortifies the
    Escherichia Coli Division Site against Osmotic Rupture.” <i>Nature Microbiology</i>,
    Springer Nature, 2026, doi:<a href="https://doi.org/10.1038/s41564-026-02403-6">10.1038/s41564-026-02403-6</a>.
  short: P.P. Navarro, A. Vettiger, R. Hajdu, V.Y. Ananda, A. López-Tavares, E.W.
    Schmid, J.C. Walter, M. Loose, L.H. Chao, T.G. Bernhardt, Nature Microbiology
    (2026).
das_tickbox: '1'
dataavailabilitystatement: 'The data, plasmids and strains that support the findings
  of this study are available from the corresponding authors by request. Representative
  tomograms are deposited in EMDB: EMD-27479 (wild-type), EMD-53351 (∆ponB), EMD-53357(∆lpoB)
  and EMD-53363 (∆ponA). Corresponding raw movie frames and stacks of tilt series
  are deposited as EMPIAR-11090 (wild type), EMPIAR-13502 (∆ponB), EMPIAR-13513 (∆lpoB)
  and EMPIAR-13512 (∆ponA), and will be released upon publication. Other data related
  to this manuscript (for example, AFM, light microscopy, growth curves and so on)
  can be found on Zenodo at https://doi.org/10.5281/zenodo.20841819 (ref. 101). Source
  data are provided with this paper. Scripts used in this study were deposited on
  GitHub at https://github.com/NavarroVettiger/Navarro-et-al_2022 and https://github.com/virlyananda/EM-ImageProcessing.'
date_created: 2026-07-12T22:02:19Z
date_published: 2026-07-03T00:00:00Z
date_updated: 2026-07-13T09:22:49Z
day: '03'
ddc:
- '570'
department:
- _id: MaLo
- _id: GradSch
doi: 10.1038/s41564-026-02403-6
external_id:
  pmid:
  - '42399561'
has_accepted_license: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1038/s41564-026-02403-6
month: '07'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Microbiology
publication_identifier:
  eissn:
  - 2058-5276
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: The penicillin-binding protein PBP1b fortifies the Escherichia coli division
  site against osmotic rupture
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
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22288'
abstract:
- lang: eng
  text: Soft solids and their surface deformations control the response of many natural
    and artificial systems. Yet, their underlying properties are vigorously debated,
    particularly for polymer networks. While molecular-scale theories predict no interfacial
    changes with macroscopic deformation, multiple experiments suggest otherwise.
    To settle this issue, we measure displacement fields near the interface of a silicone
    gel, in the limit of small deformations. We discover an unexpected multiscale
    response. The shear modulus decreases smoothly by half with 20  μ⁢m of the interface.
    At the same time we observe a surface excess elasticity, that depends on history
    and outer medium composition. These results reveal the fundamentally multiscale
    nature of polymeric surfaces, and call for further experimental and theoretical
    investigations into the basic understanding of soft solid interfaces.
acknowledgement: The authors thank Katharine Jensen, Stefanie Heyden, Thomas Salez,
  Francesco Stellacci, Denis Bartolo, Francesco Picella, Hélène Delanoë-Ayari, Mathieu
  Leocmach, Antoine Bérut, Cécile Cottin-Bizonne, Anne-Laure Biance, and Oriane Talabart
  for useful discussions. We also thank the reviewers for excellent suggestions that
  substantively improved the manuscript.
article_number: '021063'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Nicolas
  full_name: Bain, Nicolas
  last_name: Bain
- first_name: Lawrence A.
  full_name: Wilen, Lawrence A.
  last_name: Wilen
- first_name: Dominic
  full_name: Gerber, Dominic
  last_name: Gerber
- first_name: Mengjie
  full_name: Zu, Mengjie
  id: 26dd9e7c-e86a-11eb-a854-82ac731c9ae2
  last_name: Zu
- first_name: Carl Peter
  full_name: Goodrich, Carl Peter
  id: EB352CD2-F68A-11E9-89C5-A432E6697425
  last_name: Goodrich
  orcid: 0000-0002-1307-5074
- first_name: Senthilkumar
  full_name: Duraivel, Senthilkumar
  last_name: Duraivel
- first_name: Kaarthik
  full_name: Varma, Kaarthik
  last_name: Varma
- first_name: Harsha
  full_name: Koganti, Harsha
  last_name: Koganti
- first_name: Robert W.
  full_name: Style, Robert W.
  last_name: Style
- first_name: Eric R.
  full_name: Dufresne, Eric R.
  last_name: Dufresne
citation:
  ama: Bain N, Wilen LA, Gerber D, et al. Multiscale interfacial mechanics of soft
    solids. <i>Physical Review X</i>. 2026;16(2). doi:<a href="https://doi.org/10.1103/8msx-l8s7">10.1103/8msx-l8s7</a>
  apa: Bain, N., Wilen, L. A., Gerber, D., Zu, M., Goodrich, C. P., Duraivel, S.,
    … Dufresne, E. R. (2026). Multiscale interfacial mechanics of soft solids. <i>Physical
    Review X</i>. American Physical Society. <a href="https://doi.org/10.1103/8msx-l8s7">https://doi.org/10.1103/8msx-l8s7</a>
  chicago: Bain, Nicolas, Lawrence A. Wilen, Dominic Gerber, Mengjie Zu, Carl Peter
    Goodrich, Senthilkumar Duraivel, Kaarthik Varma, Harsha Koganti, Robert W. Style,
    and Eric R. Dufresne. “Multiscale Interfacial Mechanics of Soft Solids.” <i>Physical
    Review X</i>. American Physical Society, 2026. <a href="https://doi.org/10.1103/8msx-l8s7">https://doi.org/10.1103/8msx-l8s7</a>.
  ieee: N. Bain <i>et al.</i>, “Multiscale interfacial mechanics of soft solids,”
    <i>Physical Review X</i>, vol. 16, no. 2. American Physical Society, 2026.
  ista: Bain N, Wilen LA, Gerber D, Zu M, Goodrich CP, Duraivel S, Varma K, Koganti
    H, Style RW, Dufresne ER. 2026. Multiscale interfacial mechanics of soft solids.
    Physical Review X. 16(2), 021063.
  mla: Bain, Nicolas, et al. “Multiscale Interfacial Mechanics of Soft Solids.” <i>Physical
    Review X</i>, vol. 16, no. 2, 021063, American Physical Society, 2026, doi:<a
    href="https://doi.org/10.1103/8msx-l8s7">10.1103/8msx-l8s7</a>.
  short: N. Bain, L.A. Wilen, D. Gerber, M. Zu, C.P. Goodrich, S. Duraivel, K. Varma,
    H. Koganti, R.W. Style, E.R. Dufresne, Physical Review X 16 (2026).
das_tickbox: '1'
dataavailabilitystatement: The data that support the findings of this article are
  openly available https://github.com/nicobain/Multiscale_interfacial_mechanics_soft_solids_data
date_created: 2026-07-13T09:40:54Z
date_published: 2026-06-30T00:00:00Z
date_updated: 2026-07-13T11:17:51Z
day: '30'
ddc:
- '530'
department:
- _id: CaGo
doi: 10.1103/8msx-l8s7
external_id:
  arxiv:
  - '2410.09158'
file:
- access_level: open_access
  checksum: 47354f40981223fb0c9afe292f16ead1
  content_type: application/pdf
  creator: dernst
  date_created: 2026-07-13T11:16:47Z
  date_updated: 2026-07-13T11:16:47Z
  file_id: '22309'
  file_name: 2026_PhysicalReviewX_Bain.pdf
  file_size: 4367284
  relation: main_file
  success: 1
file_date_updated: 2026-07-13T11:16:47Z
has_accepted_license: '1'
intvolume: '        16'
issue: '2'
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: Physical Review X
publication_identifier:
  issn:
  - 2160-3308
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Multiscale interfacial mechanics of soft solids
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: 16
year: '2026'
...
---
OA_type: closed access
_id: '22286'
abstract:
- lang: eng
  text: Plants are remarkable organisms. Unlike animals, they cannot flee and, rooted
    in one place, they must cope with whatever challenges arise — nutrient scarcity,
    drought, shade, wind or obstacles in the soil. Their extraordinary ability to
    survive in such unstable environmental conditions lies in their capacity to adapt.
    In response to environmental signals, plants can rapidly adjust the rate of organ
    growth, change the direction of growth, bend toward resources, or remodel their
    body architecture by promoting or suppressing the formation of new organs such
    as lateral roots, branches, leaves, or flowers. This unique developmental plasticity
    depends on chemical signals, plant hormones that serve as regulators and coordinators
    of endogenous molecular and cellular processes. Chief among these signals is auxin,
    a plant hormone central to nearly every aspect of plant life.
article_processing_charge: No
article_type: original
author:
- first_name: Valentin
  full_name: Leitner, Valentin
  id: 4c665ce3-0016-11ec-bea0-e44de7a4fa3d
  last_name: Leitner
- first_name: Eva
  full_name: Benková, Eva
  id: 38F4F166-F248-11E8-B48F-1D18A9856A87
  last_name: Benková
  orcid: 0000-0002-8510-9739
citation:
  ama: Leitner V, Benková E. Auxin and the control of plant growth and development.
    <i>Current Biology</i>. 2026;36(13):R739-R744. doi:<a href="https://doi.org/10.1016/j.cub.2026.04.047">10.1016/j.cub.2026.04.047</a>
  apa: Leitner, V., &#38; Benková, E. (2026). Auxin and the control of plant growth
    and development. <i>Current Biology</i>. Elsevier. <a href="https://doi.org/10.1016/j.cub.2026.04.047">https://doi.org/10.1016/j.cub.2026.04.047</a>
  chicago: Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth
    and Development.” <i>Current Biology</i>. Elsevier, 2026. <a href="https://doi.org/10.1016/j.cub.2026.04.047">https://doi.org/10.1016/j.cub.2026.04.047</a>.
  ieee: V. Leitner and E. Benková, “Auxin and the control of plant growth and development,”
    <i>Current Biology</i>, vol. 36, no. 13. Elsevier, pp. R739–R744, 2026.
  ista: Leitner V, Benková E. 2026. Auxin and the control of plant growth and development.
    Current Biology. 36(13), R739–R744.
  mla: Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth
    and Development.” <i>Current Biology</i>, vol. 36, no. 13, Elsevier, 2026, pp.
    R739–44, doi:<a href="https://doi.org/10.1016/j.cub.2026.04.047">10.1016/j.cub.2026.04.047</a>.
  short: V. Leitner, E. Benková, Current Biology 36 (2026) R739–R744.
corr_author: '1'
das_tickbox: '0'
date_created: 2026-07-13T09:39:40Z
date_published: 2026-07-06T00:00:00Z
date_updated: 2026-07-13T11:11:56Z
day: '06'
department:
- _id: EvBe
- _id: GradSch
doi: 10.1016/j.cub.2026.04.047
external_id:
  pmid:
  - '42407441'
intvolume: '        36'
issue: '13'
language:
- iso: eng
month: '07'
oa_version: None
page: R739-R744
pmid: 1
publication: Current Biology
publication_identifier:
  issn:
  - 0960-9822
publication_status: published
publisher: Elsevier
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: no
title: Auxin and the control of plant growth and development
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 36
year: '2026'
...