---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23087'
abstract:
- lang: eng
text: Disordered materials such as glasses are promising candidates as solid-state
electrolytes for batteries, but they tend to exhibit low ionic conductivity and
current methods for investigating and predicting the ionic conductivity of electrolyte
materials are inefficient. Here, we propose a framework that summarizes the topological
properties of the electrolyte material’s atomic structure with a weighted graph
based on periodic boundary conditions. We then compute a variation of the max-flow
algorithm, a commonly used model in continuum models of transportation and liquid
flow, on this summary and show that it is compatible with the simulated periodic
atomic structures. Using molecular dynamics simulations of various glassy solid-state
electrolyte families including both mobile lithium and sodium ions, we validate
the approach by showing a positive correlation between the area-normalized maximum
flow predicted from the static glass structures and the ionic conductivity as
obtained from the simulations, especially in the case of high-conductivity sulfide
glass electrolytes. We envision that the developed methodology, which only relies
on static atomic structure, will accelerate the discovery of highly conductive
sulfide glassy electrolytes for high-performance all-solid-state batteries.
acknowledgement: We thank the Danish e-Infrastructure Cooperation (DeiC) for access
to computational resources at Sophia and LUMI-C (DeiC-AAU-N5-202200005). This work
was supported by the Independent Research Fund Denmark (1026-00037), European Union
(ERC, NewGLASS, 101044664), and Danish Data Science Academy, which in turn is funded
by the Novo Nordisk Foundation (NNF21SA0069429) and VILLUM FONDEN (40516). Y.B.B.
acknowledges support from the Austrian Science Fund (FWF) 10.55776/ESP9584724.
article_number: '10343'
article_processing_charge: Yes
article_type: original
author:
- first_name: Matteo
full_name: Pegoraro, Matteo
last_name: Pegoraro
- first_name: Rasmus
full_name: Christensen, Rasmus
last_name: Christensen
- first_name: Søren S.
full_name: Sørensen, Søren S.
last_name: Sørensen
- first_name: Anders R.
full_name: Lindbjerg, Anders R.
last_name: Lindbjerg
- first_name: Tao
full_name: Du, Tao
last_name: Du
- first_name: Yossi
full_name: Bleile, Yossi
id: 920a7385-7995-11ef-9bfd-8c434cd8f3c2
last_name: Bleile
orcid: 0000-0002-4861-9174
- first_name: Anne Marie
full_name: Svane, Anne Marie
last_name: Svane
- first_name: Christophe A.N.
full_name: Biscio, Christophe A.N.
last_name: Biscio
- first_name: Lisbeth
full_name: Fajstrup, Lisbeth
last_name: Fajstrup
- first_name: Morten M.
full_name: Smedskjaer, Morten M.
last_name: Smedskjaer
citation:
ama: Pegoraro M, Christensen R, Sørensen SS, et al. Predicting ionic conductivity
of sulfide glass solid-state electrolytes using max-flow methodology. Nature
Communications. 2026;17. doi:10.1038/s41467-026-77363-w
apa: Pegoraro, M., Christensen, R., Sørensen, S. S., Lindbjerg, A. R., Du, T., Bokor
Bleile, Y., … Smedskjaer, M. M. (2026). Predicting ionic conductivity of sulfide
glass solid-state electrolytes using max-flow methodology. Nature Communications.
Springer Nature. https://doi.org/10.1038/s41467-026-77363-w
chicago: Pegoraro, Matteo, Rasmus Christensen, Søren S. Sørensen, Anders R. Lindbjerg,
Tao Du, Yossi Bokor Bleile, Anne Marie Svane, Christophe A.N. Biscio, Lisbeth
Fajstrup, and Morten M. Smedskjaer. “Predicting Ionic Conductivity of Sulfide
Glass Solid-State Electrolytes Using Max-Flow Methodology.” Nature Communications.
Springer Nature, 2026. https://doi.org/10.1038/s41467-026-77363-w.
ieee: M. Pegoraro et al., “Predicting ionic conductivity of sulfide glass
solid-state electrolytes using max-flow methodology,” Nature Communications,
vol. 17. Springer Nature, 2026.
ista: Pegoraro M, Christensen R, Sørensen SS, Lindbjerg AR, Du T, Bokor Bleile Y,
Svane AM, Biscio CAN, Fajstrup L, Smedskjaer MM. 2026. Predicting ionic conductivity
of sulfide glass solid-state electrolytes using max-flow methodology. Nature Communications.
17, 10343.
mla: Pegoraro, Matteo, et al. “Predicting Ionic Conductivity of Sulfide Glass Solid-State
Electrolytes Using Max-Flow Methodology.” Nature Communications, vol. 17,
10343, Springer Nature, 2026, doi:10.1038/s41467-026-77363-w.
short: M. Pegoraro, R. Christensen, S.S. Sørensen, A.R. Lindbjerg, T. Du, Y. Bokor
Bleile, A.M. Svane, C.A.N. Biscio, L. Fajstrup, M.M. Smedskjaer, Nature Communications
17 (2026).
das_tickbox: '1'
dataavailabilitystatement: All data supporting the findings of this study are available
within the article and Supplementary Information files. Source data are provided
with this paper. The developed code to perform the max-flow calculations is available
as part of the Topological Materials Analysis (ToMA) library, which is available
at Zenodo (https://doi.org/10.5281/zenodo.10781424) and Github (https://github.com/yossibokorbleile/TopologicalMaterialAnalysis),
with documentation available at https://yossi.eu/toma/. To enhance usability, we
have included a brief documentation on how to compile ToMA as well as a minimal
working example of the code together with an example trajectory directly in the
ToMA repository. LAMMPS is an open-source code available at https://lammps.sandia.gov.
date_created: 2026-10-11T22:02:03Z
date_published: 2026-09-30T00:00:00Z
date_updated: 2026-10-12T09:03:58Z
day: '30'
ddc:
- '500'
department:
- _id: HeEd
doi: 10.1038/s41467-026-77363-w
external_id:
pmid:
- '42811056'
file:
- access_level: open_access
checksum: eba760f5982a89f59664957e00c5d2d6
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T09:00:06Z
date_updated: 2026-10-12T09:00:06Z
file_id: '23104'
file_name: 2026_NatureComm_Pegoraro.pdf
file_size: 1889857
relation: main_file
success: 1
file_date_updated: 2026-10-12T09:00:06Z
fulldoi: https://doi.org/10.1038/s41467-026-77363-w
has_accepted_license: '1'
intvolume: ' 17'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
pmid: 1
project:
- _id: 9106a876-16d5-11f0-9cad-bbf11c9952f9
grant_number: ESP 9584724
name: Quantitative Unbiased Shape Analysis with Geometry & Topology
publication: Nature Communications
publication_identifier:
eissn:
- 2041-1723
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Predicting ionic conductivity of sulfide glass solid-state electrolytes using
max-flow methodology
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'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23091'
abstract:
- lang: eng
text: Glaciers worldwide are becoming increasingly debris-covered, yet many aspects
within the coupled glacier-debris system are not well-understood. While the insulating
effect of continuous debris layers is well-known, the transient feedbacks with
glacier dynamics are poorly understood. The main aim of this study is to better
understand the complex transient glacier response and debris-induced feedbacks
through numerical flow modelling. We present an improved flowline model that couples
ice flow, depth-resolved debris transport, and debris cover impact on mass balance.
This approach allows for a detailed examination of the dynamics of debris-covered
glaciers under transient forcing conditions of climate and debris input over extended
timescales. Our results indicate that low-amplitude, decade-scale variability
in debris or climate forcing does not substantially impact glacier evolution.
However, large debris supply events can have a sustained impact. We find that
debris-covered glacier response to warming climate forcing is non-monotonic, with
distinct phases of thinning, retreat, and long-term re-advance. We attribute this
to a separate, longer timescale process of englacial debris transport. Additionally,
feedbacks in the englacial debris trajectory and complex bed topography further
amplify the non-linear pattern of retreat in the transient glacier response to
warming.
acknowledgement: We thank Evan Miles, Ramachandran Shankar, and Argha Banerjee for
valuable discussions and inputs on experiment design and analysis. This research
has been mainly funded by the SNSF (grant no. IZINZ2_209521) within the Indo-Swiss
joint trilateral SNSF-ICSSR-MoES scheme and the earlier SNSF (grant no. 200021_169775).
article_processing_charge: Yes
article_type: original
author:
- first_name: Florian
full_name: Hardmeier, Florian
last_name: Hardmeier
- first_name: James
full_name: Ferguson, James
id: 05fd8d9b-bd43-11eb-8d36-f8fb1cc98040
last_name: Ferguson
- first_name: Andreas
full_name: Vieli, Andreas
last_name: Vieli
citation:
ama: Hardmeier F, Ferguson J, Vieli A. Feedbacks and timescales in the modelled
transient response of debris-covered glaciers. The Cryosphere. 2026;20(9):5365-5392.
doi:10.5194/tc-20-5365-2026
apa: Hardmeier, F., Ferguson, J., & Vieli, A. (2026). Feedbacks and timescales
in the modelled transient response of debris-covered glaciers. The Cryosphere.
Copernicus Publications. https://doi.org/10.5194/tc-20-5365-2026
chicago: Hardmeier, Florian, James Ferguson, and Andreas Vieli. “Feedbacks and Timescales
in the Modelled Transient Response of Debris-Covered Glaciers.” The Cryosphere.
Copernicus Publications, 2026. https://doi.org/10.5194/tc-20-5365-2026.
ieee: F. Hardmeier, J. Ferguson, and A. Vieli, “Feedbacks and timescales in the
modelled transient response of debris-covered glaciers,” The Cryosphere,
vol. 20, no. 9. Copernicus Publications, pp. 5365–5392, 2026.
ista: Hardmeier F, Ferguson J, Vieli A. 2026. Feedbacks and timescales in the modelled
transient response of debris-covered glaciers. The Cryosphere. 20(9), 5365–5392.
mla: Hardmeier, Florian, et al. “Feedbacks and Timescales in the Modelled Transient
Response of Debris-Covered Glaciers.” The Cryosphere, vol. 20, no. 9, Copernicus
Publications, 2026, pp. 5365–92, doi:10.5194/tc-20-5365-2026.
short: F. Hardmeier, J. Ferguson, A. Vieli, The Cryosphere 20 (2026) 5365–5392.
das_tickbox: '1'
dataavailabilitystatement: 'The model presented in this study as well as the code
and synthetic data (generated from model runs) are available on Zenodo: https://doi.org/10.5281/zenodo.22687411
(Hardmeier et al., 2026). Two animations, referenced to in the text as Video Supplement
1 and 2, are available on Zenodo: https://doi.org/10.5281/zenodo.22687411 (Hardmeier
et al., 2026).'
date_created: 2026-10-11T22:02:04Z
date_published: 2026-09-21T00:00:00Z
date_updated: 2026-10-12T09:21:04Z
day: '21'
ddc:
- '550'
- '000'
department:
- _id: TiVo
doi: 10.5194/tc-20-5365-2026
file:
- access_level: open_access
checksum: b934b69f66efac91c08680a513bf74d9
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T09:17:51Z
date_updated: 2026-10-12T09:17:51Z
file_id: '23105'
file_name: 2026_Cryosphere_Hardmeier.pdf
file_size: 9284677
relation: main_file
success: 1
file_date_updated: 2026-10-12T09:17:51Z
fulldoi: https://doi.org/10.5194/tc-20-5365-2026
has_accepted_license: '1'
intvolume: ' 20'
issue: '9'
language:
- iso: eng
month: '09'
oa: 1
oa_version: None
page: 5365-5392
publication: The Cryosphere
publication_identifier:
eissn:
- 1994-0424
issn:
- 1994-0416
publication_status: published
publisher: Copernicus Publications
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Feedbacks and timescales in the modelled transient response of debris-covered
glaciers
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: 20
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '23057'
abstract:
- lang: eng
text: "We recently showed that macroscopic nuclear spin ensembles prepared in coherent
spin states can dramatically enhance the interaction rates of weakly interacting
cosmic relics, such as dark matter and the cosmic neutrino background, through
collective quantum effects analogous to Dicke superradiance, where the deexcitation
and excitation rates scale as the square of the number of spins \U0001D4412. We
thus coined these processes superradiant interactions. In this paper, we propose
a protocol to realize this enhancement and boost the discovery potential for such
relics. We show how concepts from quantum optics can be adapted to nuclear spins
coupled to superconducting circuits, enabling high-sensitivity systems. The spins
are first initialized into a coherent spin state via a \U0001D70B/2 Rabi pulse
from the ground state. When the circuit is sufficiently detuned from resonance,
the spin-circuit interaction implements a squeezing Hamiltonian. Because squeezing
must outpace spin relaxation and dephasing, the protocol favors macroscopic ensembles
and high-quality superconducting circuits. During this squeezing phase, the standard
quantum variance is reduced by up to 4.8 orders of magnitude, equivalent to 48
dB of squeezing, for circuits with quality factors \U0001D444∼10^8–10^9. The signal
imprinted on the spins during the squeezing protocol can be magnified by further
utilizing the squeezing interactions, easing the requirement for shot-noise-limited
readout. This protocol has the potential to significantly accelerate axion and
dark photon dark matter searches and extend the reach of existing axion experiments
to probe QCD axion-nuclear spin couplings. More broadly, it paves the way for
detecting coherent inelastic interactions from other cosmic relics, most notably
the cosmic neutrino background, and establishes nuclear-spin-based systems as
a class of quantum, ultra-low-threshold detectors."
acknowledgement: We are grateful to K. Irwin for illuminating discussions, and M.
Schleier-Smith, M. Kasevich, J. Hogan, N. Rapidis, M. Fedderke, A. Geraci, G. Gratta,
D. Schuster, D. Budker, and A. Sushkov for very valuable conversations. O.H. acknowledges
support by the Institute of Science and Technology Austria (ISTA). A.A., S.D., and
M.G. acknowledge the hospitality provided by ISTA, where part of this work was being
completed. A.A., M.G., and O.H. acknowledge the hospitality provided by the Leinweber
Institute for Theoretical Physics at Stanford, where part of this work was being
completed. S.D. acknowledges support by NSF Grant No. PHY-2310429 and the Gordon
and Betty Moore Foundation Grant No. GBMF7946, and Perimeter Institute and its hospitality.
Research at Perimeter Institute is supported in part by the Government of Canada
through the Department of Innovation, Science and Economic Development and by the
Province of Ontario through the Ministry of Colleges and Universities. A.A. is grateful
for the support of the Stavros Niarchos Foundation.
article_number: '063714'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Marios
full_name: Galanis, Marios
last_name: Galanis
- first_name: Onur
full_name: Hosten, Onur
id: 4C02D85E-F248-11E8-B48F-1D18A9856A87
last_name: Hosten
orcid: 0000-0002-2031-204X
- first_name: Asimina
full_name: Arvanitaki, Asimina
last_name: Arvanitaki
- first_name: Savas
full_name: Dimopoulos, Savas
last_name: Dimopoulos
citation:
ama: Galanis M, Hosten O, Arvanitaki A, Dimopoulos S. Superradiant interactions
for relic detection with entangled nuclear spins. Physical Review A. 2026;113(6).
doi:10.1103/Z2D9-4GV6
apa: Galanis, M., Hosten, O., Arvanitaki, A., & Dimopoulos, S. (2026). Superradiant
interactions for relic detection with entangled nuclear spins. Physical Review
A. American Physical Society. https://doi.org/10.1103/Z2D9-4GV6
chicago: Galanis, Marios, Onur Hosten, Asimina Arvanitaki, and Savas Dimopoulos.
“Superradiant Interactions for Relic Detection with Entangled Nuclear Spins.”
Physical Review A. American Physical Society, 2026. https://doi.org/10.1103/Z2D9-4GV6.
ieee: M. Galanis, O. Hosten, A. Arvanitaki, and S. Dimopoulos, “Superradiant interactions
for relic detection with entangled nuclear spins,” Physical Review A, vol.
113, no. 6. American Physical Society, 2026.
ista: Galanis M, Hosten O, Arvanitaki A, Dimopoulos S. 2026. Superradiant interactions
for relic detection with entangled nuclear spins. Physical Review A. 113(6), 063714.
mla: Galanis, Marios, et al. “Superradiant Interactions for Relic Detection with
Entangled Nuclear Spins.” Physical Review A, vol. 113, no. 6, 063714, American
Physical Society, 2026, doi:10.1103/Z2D9-4GV6.
short: M. Galanis, O. Hosten, A. Arvanitaki, S. Dimopoulos, Physical Review A 113
(2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: The data that support the findings of this article are
not publicly available. The data are available from the authors upon reasonable
request.
date_created: 2026-10-04T22:01:57Z
date_published: 2026-06-01T00:00:00Z
date_updated: 2026-10-12T08:36:40Z
day: '01'
department:
- _id: OnHo
doi: 10.1103/Z2D9-4GV6
external_id:
arxiv:
- '2508.20520'
fulldoi: https://doi.org/10.1103/Z2D9-4GV6
intvolume: ' 113'
issue: '6'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2508.20520
month: '06'
oa: 1
oa_version: Preprint
publication: Physical Review A
publication_identifier:
eissn:
- 2469-9934
issn:
- 2469-9926
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
researchdata_availability: upon request
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Superradiant interactions for relic detection with entangled nuclear spins
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 113
year: '2026'
...
---
OA_type: closed access
_id: '23086'
abstract:
- lang: eng
text: The division of a mother cell into two daughter cells is a fundamental process
in biology, involving the transfer of genomic information to the next generation
of cells. In plant roots, cell divisions occur in the root apical meristem, a
specialized tissue located at the plant’s root tip. Cell proliferation rates in
the root apical meristem shape root growth, thereby contributing to general development
as well as the acclimatization to stressful environmental conditions through phenotypic
plasticity. Here, we present a protocol for the microscopical analysis of cell
proliferation in Arabidopsis thaliana root meristems by 5-ethynyl-2ʹ-deoxyuridine
(EdU) staining. EdU, a thymine-analog, is incorporated into newly synthesized
DNA of proliferative cells during the S-phase of the cell cycle. Subsequently,
EdU-containing nuclei can be labeled with a fluorophore and detected by confocal
laser scanning microscopy. The combination of the EdU assay with cell wall staining
enables the quantification of root meristem architecture parameters and cell division
activity from microscopic images. Together, this can elucidate how root meristems
respond to changes in environmental conditions or address fundamental questions
of developmental plant biology.
alternative_title:
- Methods in Molecular Biology
article_processing_charge: No
author:
- first_name: Tilman
full_name: Jacob, Tilman
last_name: Jacob
- first_name: Haiyue
full_name: Ai, Haiyue
id: 71a6871f-c08f-11ee-886c-c975579c368c
last_name: Ai
- first_name: Marcel
full_name: Quint, Marcel
last_name: Quint
citation:
ama: 'Jacob T, Ai H, Quint M. EdU-Based Quantitative Analysis of Cell Proliferation
in Arabidopsis Root Meristems. In: Root Development. Vol 3086. MIMB. New
York: Springer; 2026:165-176. doi:10.1007/978-1-0716-5603-7_13'
apa: 'Jacob, T., Ai, H., & Quint, M. (2026). EdU-Based Quantitative Analysis
of Cell Proliferation in Arabidopsis Root Meristems. In Root Development
(Vol. 3086, pp. 165–176). New York: Springer. https://doi.org/10.1007/978-1-0716-5603-7_13'
chicago: 'Jacob, Tilman, Haiyue Ai, and Marcel Quint. “EdU-Based Quantitative Analysis
of Cell Proliferation in Arabidopsis Root Meristems.” In Root Development,
3086:165–76. MIMB. New York: Springer, 2026. https://doi.org/10.1007/978-1-0716-5603-7_13.'
ieee: 'T. Jacob, H. Ai, and M. Quint, “EdU-Based Quantitative Analysis of Cell Proliferation
in Arabidopsis Root Meristems,” in Root Development, vol. 3086, New York:
Springer, 2026, pp. 165–176.'
ista: 'Jacob T, Ai H, Quint M. 2026.EdU-Based Quantitative Analysis of Cell Proliferation
in Arabidopsis Root Meristems. In: Root Development. Methods in Molecular Biology,
vol. 3086, 165–176.'
mla: Jacob, Tilman, et al. “EdU-Based Quantitative Analysis of Cell Proliferation
in Arabidopsis Root Meristems.” Root Development, vol. 3086, Springer,
2026, pp. 165–76, doi:10.1007/978-1-0716-5603-7_13.
short: T. Jacob, H. Ai, M. Quint, in:, Root Development, Springer, New York, 2026,
pp. 165–176.
date_created: 2026-10-11T22:02:03Z
date_published: 2026-10-01T00:00:00Z
date_updated: 2026-10-12T09:13:28Z
day: '01'
department:
- _id: JiFr
doi: 10.1007/978-1-0716-5603-7_13
external_id:
pmid:
- '42814359'
fulldoi: https://doi.org/10.1007/978-1-0716-5603-7_13
intvolume: ' 3086'
keyword:
- Root growth
- Root development
- Root meristem
- Cell cycle
- Cell division
- S-phase
- EdU
- Arabidopsis thaliana
- Microscopy
language:
- iso: eng
month: '10'
oa_version: None
page: 165-176
place: New York
pmid: 1
publication: Root Development
publication_identifier:
eisbn:
- '9781071656037'
eissn:
- 1940-6029
publication_status: published
publisher: Springer
quality_controlled: '1'
scopus_import: '1'
series_title: MIMB
status: public
title: EdU-Based Quantitative Analysis of Cell Proliferation in Arabidopsis Root Meristems
type: book_chapter
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 3086
year: '2026'
...
---
OA_type: closed access
_id: '23056'
abstract:
- lang: eng
text: Superconducting qubits face scaling challenges due to millikelvin temperature
requirements. Here we demonstrate the generation and low-noise upconversion of
single microwave photons to telecom frequencies, paving the way for quantum networks
with superconducting qubits.
alternative_title:
- Technical Digest Series
article_number: QM2A.1
article_processing_charge: No
author:
- first_name: Andrei
full_name: Militaru, Andrei
id: d67706f8-8eb1-11ee-ad1b-9c30dfa19e0b
last_name: Militaru
- first_name: Thomas
full_name: Werner, Thomas
id: 1fcd8497-dba3-11ea-a45e-c6fbd715f7c7
last_name: Werner
orcid: 0009-0001-2346-5236
- first_name: Erfan
full_name: Riyazi, Erfan
id: 53322f94-5355-11ee-ae5a-ff6f81c87d51
last_name: Riyazi
- first_name: Samarth
full_name: Hawaldar, Samarth
id: 221708e1-1ff6-11ee-9fa6-85146607433e
last_name: Hawaldar
orcid: 0000-0002-1965-4309
- first_name: Rishabh
full_name: Sahu, Rishabh
id: 47D26E34-F248-11E8-B48F-1D18A9856A87
last_name: Sahu
orcid: 0000-0001-6264-2162
- first_name: Georg M
full_name: Arnold, Georg M
id: 3770C838-F248-11E8-B48F-1D18A9856A87
last_name: Arnold
orcid: 0000-0003-1397-7876
- first_name: Paul
full_name: Falthansl-Scheinecker, Paul
id: 85b43b21-15b2-11ec-abd3-e2c252cc2285
last_name: Falthansl-Scheinecker
- first_name: Jennifer Anais
full_name: Sanchez Naranjo, Jennifer Anais
id: 0fd10295-ebd4-11ec-b0f1-c1c8465143f9
last_name: Sanchez Naranjo
- first_name: Dante
full_name: Loi, Dante
id: a24803ec-c619-11f1-873b-95804e96f22f
last_name: Loi
- first_name: Lucky
full_name: Kapoor, Lucky
id: 84b9700b-15b2-11ec-abd3-831089e67615
last_name: Kapoor
orcid: 0000-0001-8319-2148
- first_name: Martin
full_name: Zemlicka, Martin
id: 2DCF8DE6-F248-11E8-B48F-1D18A9856A87
last_name: Zemlicka
orcid: 0009-0005-0878-3032
- first_name: Liu
full_name: Qiu, Liu
id: 45e99c0d-1eb1-11eb-9b96-ed8ab2983cac
last_name: Qiu
orcid: 0000-0003-4345-4267
- first_name: Johannes M
full_name: Fink, Johannes M
id: 4B591CBA-F248-11E8-B48F-1D18A9856A87
last_name: Fink
orcid: 0000-0001-8112-028X
citation:
ama: 'Militaru A, Werner T, Riyazi E, et al. Electro-optic conversion of itinerant
Fock states. In: Quantum 2.0 Conference and Exhibition. Optica Publishing
Group; 2026.'
apa: 'Militaru, A., Werner, T., Riyazi, E., Hawaldar, S., Sahu, R., Arnold, G. M.,
… Fink, J. M. (2026). Electro-optic conversion of itinerant Fock states. In Quantum
2.0 Conference and Exhibition. Glasgow, United Kingdom: Optica Publishing
Group.'
chicago: Militaru, Andrei, Thomas Werner, Erfan Riyazi, Samarth Hawaldar, Rishabh
Sahu, Georg M Arnold, Paul Falthansl-Scheinecker, et al. “Electro-Optic Conversion
of Itinerant Fock States.” In Quantum 2.0 Conference and Exhibition. Optica
Publishing Group, 2026.
ieee: A. Militaru et al., “Electro-optic conversion of itinerant Fock states,”
in Quantum 2.0 Conference and Exhibition, Glasgow, United Kingdom, 2026.
ista: Militaru A, Werner T, Riyazi E, Hawaldar S, Sahu R, Arnold GM, Falthansl-Scheinecker
P, Sanchez Naranjo JA, Loi D, Kapoor L, Zemlicka M, Qiu L, Fink JM. 2026. Electro-optic
conversion of itinerant Fock states. Quantum 2.0 Conference and Exhibition. Quantum
2.0, Technical Digest Series, , QM2A.1.
mla: Militaru, Andrei, et al. “Electro-Optic Conversion of Itinerant Fock States.”
Quantum 2.0 Conference and Exhibition, QM2A.1, Optica Publishing Group,
2026.
short: A. Militaru, T. Werner, E. Riyazi, S. Hawaldar, R. Sahu, G.M. Arnold, P.
Falthansl-Scheinecker, J.A. Sanchez Naranjo, D. Loi, L. Kapoor, M. Zemlicka, L.
Qiu, J.M. Fink, in:, Quantum 2.0 Conference and Exhibition, Optica Publishing
Group, 2026.
conference:
end_date: 2026-06-18
location: Glasgow, United Kingdom
name: Quantum 2.0
start_date: 2026-06-15
corr_author: '1'
date_created: 2026-10-04T22:01:57Z
date_published: 2026-09-01T00:00:00Z
date_updated: 2026-10-12T08:53:25Z
day: '01'
department:
- _id: JoFi
- _id: GradSch
- _id: GeKa
language:
- iso: eng
month: '09'
oa_version: None
publication: Quantum 2.0 Conference and Exhibition
publication_identifier:
isbn:
- '9781957171616'
publication_status: published
publisher: Optica Publishing Group
scopus_import: '1'
status: public
title: Electro-optic conversion of itinerant Fock states
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23092'
abstract:
- lang: eng
text: We present the number density of massive (log(M*/Mo)> 10.3) quiescent galaxies
at 2 < z < 5 using JWST NIRSpec PRISM spectra. This work relies on spectra from
RUBIES, which provides excellent data quality and an unparalleled, well-defined
targeting strategy to robustly infer physical properties and number densities.
We identify quiescent galaxy candidates within RUBIES through principal component
analysis and construct a final sample using star formation histories derived from
spectrophotometric fitting of the NIRSpec PRISM spectra and NIRCam photometry.
By inverting the RUBIES selection function, we correct for survey incompleteness
and calculate the number density of massive quiescent galaxies at these redshifts,
providing the most complete spectroscopic estimates prior to cosmic noon to date.
We find that early massive quiescent galaxies are surprisingly common (≳10−5 Mpc−3
by 4 < z < 5), which is consistent with previous studies based on JWST photometry
alone and/or in smaller survey areas. We compare our number densities with predictions
from six state-of-the-art cosmological galaxy formation simulations. At z > 3,
most simulations fail to produce enough massive quiescent galaxies, suggesting
the treatment of feedback and/or the channels for early efficient formation are
incomplete in most galaxy evolution models.
acknowledgement: "We thank Alan Pearl for his contribution to estimating the cosmic
variance contribution to the number density uncertainties in this work. We thank
Hans-Walter Rix for the valuable discussion on the selection function and correcting
the spectroscopic incompleteness of massive quiescent galaxies in RUBIES.\r\n\r\nSome
of the data products presented herein were retrieved from the Dawn JWST Archive
(DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by
the Danish National Research Foundation under grant DNRF140.\r\n\r\nThe Cosmic Dawn
Center is funded by the Danish National Research Foundation (DNRF) under grant #140.\r\n\r\nSupport
for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship
grant.\r\n\r\nR.B. gratefully acknowledges support from the Research Corporation
for Scientific Advancement (RCSA) Cottrell Scholar Award ID No: 27587.\r\n\r\nThe
work of C.C.W. 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.\r\n\r\nT.B.M. was supported by a CIERA Postdoctoral Fellowship.\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 program numbers 1180, 1181, 1210, 1211,
1213, 1214, 1215, 1286, 1345, 1433, 1747, 2028, 2073, 2198, 2282, 2561, 2565, 2750,
2756, 2767, 3073, 3215, 4233, 4446, 4557, 6368, 6541, and 6585. The specific observations
analyzed can be accessed via DOI: 10.17909/sjsj-8p46.\r\n\r\nSupport for program
No. 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.\r\n\r\nThe authors acknowledge the CEERS
and PRIMER teams for developing their observing program with a zero-exclusive access
period.\r\n\r\nFacility: JWST - James Webb Space Telescope.\r\n\r\nSoftware: Astropy
(Astropy Collaboration et al. 2013, 2018, 2022), Scipy (P. Virtanen et al. 2020),
Photutils (L. Bradley 2023), SpectRes (A. C. Carnall 2017), Scikit-learn (F. Pedregosa
et al. 2011), Prospector (B. Johnson & J. Leja 2017; J. Leja et al. 2017; B. Johnson
et al. 2021)."
article_number: '252'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Yunchong
full_name: Zhang, Yunchong
last_name: Zhang
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Claudia
full_name: Del P. Lagos, Claudia
last_name: Del P. Lagos
- first_name: Sam E.
full_name: Cutler, Sam E.
last_name: Cutler
- first_name: Ian
full_name: Mcconachie, Ian
last_name: Mcconachie
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Olivia R.
full_name: Cooper, Olivia R.
last_name: Cooper
- first_name: Rashmi
full_name: Gottumukkala, Rashmi
last_name: Gottumukkala
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Gourav
full_name: Khullar, Gourav
last_name: Khullar
- first_name: Ivo
full_name: Labbe, Ivo
last_name: Labbe
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- 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: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: Zhang Y, De Graaff A, Setton DJ, et al. RUBIES spectroscopically confirms the
high number density of quiescent galaxies from2<z<5. The Astrophysical
Journal. 2026;997(2). doi:10.3847/1538-4357/ae24e1
apa: Zhang, Y., De Graaff, A., Setton, D. J., Price, S. H., Bezanson, R., Del P.
Lagos, C., … Williams, C. C. (2026). RUBIES spectroscopically confirms the high
number density of quiescent galaxies from2<z<5. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ae24e1
chicago: Zhang, Yunchong, Anna De Graaff, David J. Setton, Sedona H. Price, Rachel
Bezanson, Claudia Del P. Lagos, Sam E. Cutler, et al. “RUBIES Spectroscopically
Confirms the High Number Density of Quiescent Galaxies From2<z<5.” The
Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae24e1.
ieee: Y. Zhang et al., “RUBIES spectroscopically confirms the high number
density of quiescent galaxies from2<z<5,” The Astrophysical Journal,
vol. 997, no. 2. IOP Publishing, 2026.
ista: Zhang Y, De Graaff A, Setton DJ, Price SH, Bezanson R, Del P. Lagos C, Cutler
SE, Mcconachie I, Cleri NJ, Cooper OR, Gottumukkala R, Greene JE, Hirschmann M,
Khullar G, Labbe I, Leja J, Maseda MV, Matthee JJ, Miller TB, Nanayakkara T, Suess
KA, Wang B, Whitaker KE, Williams CC. 2026. RUBIES spectroscopically confirms
the high number density of quiescent galaxies from2<z<5. The Astrophysical
Journal. 997(2), 252.
mla: Zhang, Yunchong, et al. “RUBIES Spectroscopically Confirms the High Number
Density of Quiescent Galaxies From2<z<5.” The Astrophysical Journal,
vol. 997, no. 2, 252, IOP Publishing, 2026, doi:10.3847/1538-4357/ae24e1.
short: Y. Zhang, A. De Graaff, D.J. Setton, S.H. Price, R. Bezanson, C. Del P. Lagos,
S.E. Cutler, I. Mcconachie, N.J. Cleri, O.R. Cooper, R. Gottumukkala, J.E. Greene,
M. Hirschmann, G. Khullar, I. Labbe, J. Leja, M.V. Maseda, J.J. Matthee, T.B.
Miller, T. Nanayakkara, K.A. Suess, B. Wang, K.E. Whitaker, C.C. Williams, The
Astrophysical Journal 997 (2026).
date_created: 2026-10-11T22:02:05Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-10-12T11:55:05Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae24e1
external_id:
arxiv:
- '2508.08577'
file:
- access_level: open_access
checksum: 547c63f9265be5d41efdc555a25423cc
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T11:51:24Z
date_updated: 2026-10-12T11:51:24Z
file_id: '23110'
file_name: 2026_AstrophysicalJour_Zhang.pdf
file_size: 5995619
relation: main_file
success: 1
file_date_updated: 2026-10-12T11:51:24Z
fulldoi: https://doi.org/10.3847/1538-4357/ae24e1
has_accepted_license: '1'
intvolume: ' 997'
issue: '2'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: RUBIES spectroscopically confirms the high number density of quiescent galaxies
from2Plos One. 2026;21(10):e0351518. doi:10.1371/journal.pone.0351518'
apa: 'Garcia Castillo, D. F. (2026). Generalism vs. specialization: Does niche breadth
influence species responses to anthropogenic land-use change in Neotropical leaf-cutter
ants? Plos One. Public Library of Science. https://doi.org/10.1371/journal.pone.0351518'
chicago: 'Garcia Castillo, Diego Fernando. “Generalism vs. Specialization: Does
Niche Breadth Influence Species Responses to Anthropogenic Land-Use Change in
Neotropical Leaf-Cutter Ants?” Plos One. Public Library of Science, 2026.
https://doi.org/10.1371/journal.pone.0351518.'
ieee: 'D. F. Garcia Castillo, “Generalism vs. specialization: Does niche breadth
influence species responses to anthropogenic land-use change in Neotropical leaf-cutter
ants?,” Plos One, vol. 21, no. 10. Public Library of Science, p. e0351518,
2026.'
ista: 'Garcia Castillo DF. 2026. Generalism vs. specialization: Does niche breadth
influence species responses to anthropogenic land-use change in Neotropical leaf-cutter
ants? Plos One. 21(10), e0351518.'
mla: 'Garcia Castillo, Diego Fernando. “Generalism vs. Specialization: Does Niche
Breadth Influence Species Responses to Anthropogenic Land-Use Change in Neotropical
Leaf-Cutter Ants?” Plos One, vol. 21, no. 10, Public Library of Science,
2026, p. e0351518, doi:10.1371/journal.pone.0351518.'
short: D.F. Garcia Castillo, Plos One 21 (2026) e0351518.
corr_author: '1'
das_tickbox: '0'
date_created: 2026-10-11T22:02:05Z
date_published: 2026-10-01T00:00:00Z
date_updated: 2026-10-12T11:43:26Z
day: '01'
ddc:
- '570'
department:
- _id: NiBa
doi: 10.1371/journal.pone.0351518
external_id:
pmid:
- '42821535'
file:
- access_level: open_access
checksum: 06ccc9f8806de407b21a168525e324de
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T11:42:06Z
date_updated: 2026-10-12T11:42:06Z
file_id: '23109'
file_name: 2026_PlosOne_GarciaCastillo.pdf
file_size: 1166607
relation: main_file
success: 1
file_date_updated: 2026-10-12T11:42:06Z
fulldoi: https://doi.org/10.1371/journal.pone.0351518
has_accepted_license: '1'
intvolume: ' 21'
issue: '10'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
page: e0351518
pmid: 1
publication: Plos One
publication_identifier:
eissn:
- 1932-6203
publication_status: published
publisher: Public Library of Science
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: 'Generalism vs. specialization: Does niche breadth influence species responses
to anthropogenic land-use change in Neotropical leaf-cutter ants?'
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: 21
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '23089'
abstract:
- lang: eng
text: The location of the hydrogen-helium (H/He) immiscibility boundary controls
whether and where helium rain occurs in giant planets, yet it remains uncertain
because high-pressure experiments are challenging and ab initio simulations are
limited in system size and simulation time. We map this boundary by computing
composition-dependent chemical potentials from large-scale molecular dynamics
driven by machine learning potentials trained on three density functional approximations
(PBE, vdW-DF, and the hybrid HSE). Across the pressure range of 100-1000 GPa,
the demixing temperatures are typically ~ 2000 K lower than previous ab initio
simulations using small system sizes, and this discrepancy is larger than the
estimated error from the chosen density functionals, machine learning potentials,
neglect of nuclear quantum effects, and statistical uncertainties. Fitting the
H/He mixing free energy to a Redlich-Kister regular solution model rationalizes
the thermodynamic driving force for phase separation, and provides a predictive
representation of the boundary. Comparing with current planetary interior profiles
indicates that helium rain is plausible in Saturn but unlikely in the warmer interior
of Jupiter. Our results narrow the uncertainty in the H/He immiscibility boundary
and provide inputs for planetary models that couple demixing, heat transport,
and composition gradients in gas giants.
acknowledged_ssus:
- _id: ScienComp
acknowledgement: The authors are thankful to Armin Bergermann and Ronald Redmer for
generously sharing AIMD trajectories and data, and for valuable discussions and
feedback on the manuscript. The authors also acknowledge the research computing
facilities provided by the high-performance computing (HPC) cluster at the Institute
of Science and Technology Austria (ISTA), Berkeley Research Computing (BRC) at the
University of California, Berkeley (UCB), and Lawrence Livermore National Laboratory
(LLNL). B.C. was supported by the Laboratory Directed Research and Development (LDRD)
Program at Lawrence Berkeley National Laboratory (LBNL) under project ID 110990-001.
Part of this work was performed under the auspices of the U.S. Department of Energy
by LLNL under Contract DE-AC52-07NA27344. S.H. was supported by the LDRD Program
at LLNL under project tracking code 23-SI-006.
article_number: '10382'
article_processing_charge: Yes
article_type: original
author:
- first_name: Xiaoyu
full_name: Wang, Xiaoyu
id: 8dff9c62-32b0-11ee-9fa8-fc73025e10f3
last_name: Wang
- first_name: Sebastien
full_name: Hamel, Sebastien
last_name: Hamel
- first_name: Bingqing
full_name: Cheng, Bingqing
id: cbe3cda4-d82c-11eb-8dc7-8ff94289fcc9
last_name: Cheng
orcid: 0000-0002-3584-9632
citation:
ama: Wang X, Hamel S, Cheng B. Hydrogen-helium immiscibility boundary in gas-giant
planetary interiors from machine-learning molecular dynamics. Nature Communications.
2026;17. doi:10.1038/s41467-026-77117-8
apa: Wang, X., Hamel, S., & Cheng, B. (2026). Hydrogen-helium immiscibility
boundary in gas-giant planetary interiors from machine-learning molecular dynamics.
Nature Communications. Springer Nature. https://doi.org/10.1038/s41467-026-77117-8
chicago: Wang, Xiaoyu, Sebastien Hamel, and Bingqing Cheng. “Hydrogen-Helium Immiscibility
Boundary in Gas-Giant Planetary Interiors from Machine-Learning Molecular Dynamics.”
Nature Communications. Springer Nature, 2026. https://doi.org/10.1038/s41467-026-77117-8.
ieee: X. Wang, S. Hamel, and B. Cheng, “Hydrogen-helium immiscibility boundary in
gas-giant planetary interiors from machine-learning molecular dynamics,” Nature
Communications, vol. 17. Springer Nature, 2026.
ista: Wang X, Hamel S, Cheng B. 2026. Hydrogen-helium immiscibility boundary in
gas-giant planetary interiors from machine-learning molecular dynamics. Nature
Communications. 17, 10382.
mla: Wang, Xiaoyu, et al. “Hydrogen-Helium Immiscibility Boundary in Gas-Giant Planetary
Interiors from Machine-Learning Molecular Dynamics.” Nature Communications,
vol. 17, 10382, Springer Nature, 2026, doi:10.1038/s41467-026-77117-8.
short: X. Wang, S. Hamel, B. Cheng, Nature Communications 17 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: 'The training data, fitted MLPs, MLP molecular dynamics
results, and source data underlying all figures and tables in the main text and
Supplementary Information have been deposited in the Zenodo repository: https://doi.org/10.5281/zenodo.21632034.
The data-analysis and plotting scripts used to generate the figures and tables in
the main text and Supplementary Information are available in the GitHub repository:
https://github.com/ChengUCB/HighPressure_HHe.'
date_created: 2026-10-11T22:02:04Z
date_published: 2026-09-01T00:00:00Z
date_updated: 2026-10-12T11:00:16Z
day: '01'
ddc:
- '540'
department:
- _id: GradSch
- _id: BiCh
doi: 10.1038/s41467-026-77117-8
external_id:
pmid:
- '42816492'
file:
- access_level: open_access
checksum: f39b50a550623a65aea2405b527e068c
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T10:57:42Z
date_updated: 2026-10-12T10:57:42Z
file_id: '23107'
file_name: 2026_NatureComm_Wang.pdf
file_size: 1559219
relation: main_file
success: 1
file_date_updated: 2026-10-12T10:57:42Z
fulldoi: https://doi.org/10.1038/s41467-026-77117-8
has_accepted_license: '1'
intvolume: ' 17'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Communications
publication_identifier:
eissn:
- 2041-1723
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Hydrogen-helium immiscibility boundary in gas-giant planetary interiors from
machine-learning molecular dynamics
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'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '23090'
abstract:
- lang: eng
text: 'Homologous recombination is ubiquitous across evolution, generating variation
through genetic reshuffling. Although bacteria lack meiotic recombination, homologous
recombination has been known to extensively shape their genomes. However, the
mechanisms and ecological conditions sustaining frequent recombination in bacteria
remain unclear. Using an Escherichia coli–P1 phage model system, we reveal how
frequent recombination emerges from CRISPR-based herd immunity to a generalized
transducing phage (DNA vector). Herd immunity maintains phage-susceptible donor
bacteria, recipient immune bacteria, and transducing phage, which promotes chromosomal
gene flow that exceeds spontaneous mutation by up to two orders of magnitude.
Notably, recombination begins as bacterial cultures enter stationary phase, when
canonical mutation supply through population growth and DNA replication is strongly
reduced, and recombination can be reinitiated by brief fresh nutrient pulses.
Genetic analysis showed that stationary-phase recombination requires recA, recB,
and recG, connecting this process to a defined homologous recombination pathway,
and suggests a plausible transcriptional regulatory link to transition to nutrient
limitation. Bacterial herd immunity therefore has an unexpected evolutionary consequence:
it can promote homologous recombination by turning phages into de facto pollinators.
This mechanism can help explain how high rates of homologous recombination may
be sustained across bacterial populations and suggests that bacterial immune systems
can shape molecular evolution not only by blocking infection but also by regulating
genetic exchange.'
acknowledgement: We thank Stuart Baird, Nick Barton, Max Joesch, Meriem El Karoui,
Mato Lagator, Ivana Mašlaňová, Stepan Ovchinnikov, Roman Pantůček, Maroš Pleška,
Jitka Polechová, and Bryan Wu for their feedback on the manuscript. We are grateful
to the Redlinger Hut for hosting many discussions about the project away from the
daily buzz. We acknowledge the core facility CELLIM supported by the Czech-BioImaging
large RI project (LM2023050 funded by MEYS CR) for their support. This work was
supported by H2020 European Research Council EVOLHGT No. 648440 to JPB, European
Commission Programme EXCELES project LX22NPO5103 “National Institute of Virology
and Bacteriology” to PPl, and a bilateral Czech-Austrian mobility grant 8J3AT003
funded by MEYS CR and OeAD AT to PPa and CCG.
article_number: msag238
article_processing_charge: Yes
article_type: original
author:
- first_name: Pavel
full_name: Payne, Pavel
id: 35F78294-F248-11E8-B48F-1D18A9856A87
last_name: Payne
orcid: 0000-0002-2711-9453
- first_name: Pavel
full_name: Plevka, Pavel
last_name: Plevka
- first_name: Jonathan P
full_name: Bollback, Jonathan P
id: 2C6FA9CC-F248-11E8-B48F-1D18A9856A87
last_name: Bollback
orcid: 0000-0002-4624-4612
- first_name: Calin C
full_name: Guet, Calin C
id: 47F8433E-F248-11E8-B48F-1D18A9856A87
last_name: Guet
orcid: 0000-0001-6220-2052
citation:
ama: Payne P, Plevka P, Bollback JP, Guet CC. Herd immunity underlies homologous
recombination in stationary phase bacteria. Molecular Biology and Evolution.
2026;43(10). doi:10.1093/molbev/msag238
apa: Payne, P., Plevka, P., Bollback, J. P., & Guet, C. C. (2026). Herd immunity
underlies homologous recombination in stationary phase bacteria. Molecular
Biology and Evolution. Oxford University Press. https://doi.org/10.1093/molbev/msag238
chicago: Payne, Pavel, Pavel Plevka, Jonathan P Bollback, and Calin C Guet. “Herd
Immunity Underlies Homologous Recombination in Stationary Phase Bacteria.” Molecular
Biology and Evolution. Oxford University Press, 2026. https://doi.org/10.1093/molbev/msag238.
ieee: P. Payne, P. Plevka, J. P. Bollback, and C. C. Guet, “Herd immunity underlies
homologous recombination in stationary phase bacteria,” Molecular Biology and
Evolution, vol. 43, no. 10. Oxford University Press, 2026.
ista: Payne P, Plevka P, Bollback JP, Guet CC. 2026. Herd immunity underlies homologous
recombination in stationary phase bacteria. Molecular Biology and Evolution. 43(10),
msag238.
mla: Payne, Pavel, et al. “Herd Immunity Underlies Homologous Recombination in Stationary
Phase Bacteria.” Molecular Biology and Evolution, vol. 43, no. 10, msag238,
Oxford University Press, 2026, doi:10.1093/molbev/msag238.
short: P. Payne, P. Plevka, J.P. Bollback, C.C. Guet, Molecular Biology and Evolution
43 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: The data underlying this article are available in the article
and in its online material.
date_created: 2026-10-11T22:02:04Z
date_published: 2026-10-03T00:00:00Z
date_updated: 2026-10-12T10:51:54Z
day: '03'
ddc:
- '570'
department:
- _id: CaGu
doi: 10.1093/molbev/msag238
external_id:
pmid:
- '42827080'
fulldoi: https://doi.org/10.1093/molbev/msag238
has_accepted_license: '1'
intvolume: ' 43'
issue: '10'
keyword:
- homologous recombination
- defense systems
- CRISPR-Cas
- herd immunity
- stationary phase
- bacterial evolution
language:
- iso: eng
license: https://creativecommons.org/licenses/by-nc/4.0/
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/molbev/msag238
month: '10'
oa: 1
oa_version: Published Version
pmid: 1
publication: Molecular Biology and Evolution
publication_identifier:
eissn:
- 1537-1719
issn:
- 0737-4038
publication_status: epub_ahead
publisher: Oxford University Press
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Herd immunity underlies homologous recombination in stationary phase bacteria
tmp:
image: /images/cc_by_nc.png
legal_code_url: https://creativecommons.org/licenses/by-nc/4.0/legalcode
name: Creative Commons Attribution-NonCommercial 4.0 International (CC BY-NC 4.0)
short: CC BY-NC (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 43
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '23088'
abstract:
- lang: eng
text: In this review, we provide an engineering assessment of prevalent blood-wetted
cardiovascular devices, their hematologic complications, and their interconnections
to identify key areas for future research. In fact, the incidence of cardiovascular
diseases has promoted the development of various devices to treat these conditions,
including mechanical circulatory supports (mechanical pumps that assist or replace
failing hearts), artificial valves to replace faulty heart valves, stents to relieve
obstructions in blood vessels, vascular grafts to repair/reconstruct damaged vessels,
patches to reinforce or reconstruct cardiovascular tissues, and other implants.
The hemocompatibility of these cardiovascular devices, namely their ability to
interact with blood flow without causing adverse reactions, remains unsatisfactory,
and recurrent complications include thrombosis, hemolysis, and bleeding. Therefore,
the discussion provided herein will support readers approaching cardiovascular
technologies in building a solid foundation and provide everyone with an up-to-date
overview of ongoing research in this multidisciplinary field.
article_number: '167'
article_processing_charge: Yes
article_type: original
author:
- first_name: Damiano
full_name: Padovani, Damiano
last_name: Padovani
- first_name: Nasima S
full_name: Afsharimani, Nasima S
id: fe7df522-678a-11eb-9fb9-a37ecf42528e
last_name: Afsharimani
- first_name: Andrea
full_name: Cioncolini, Andrea
last_name: Cioncolini
- first_name: Yu
full_name: Ding, Yu
last_name: Ding
citation:
ama: Padovani D, Afsharimani NS, Cioncolini A, Ding Y. Hematologic complications
and design challenges in cardiovascular devices. Communications Engineering.
2026;5. doi:10.1038/s44172-026-00771-9
apa: Padovani, D., Afsharimani, N. S., Cioncolini, A., & Ding, Y. (2026). Hematologic
complications and design challenges in cardiovascular devices. Communications
Engineering. Springer Nature. https://doi.org/10.1038/s44172-026-00771-9
chicago: Padovani, Damiano, Nasima S Afsharimani, Andrea Cioncolini, and Yu Ding.
“Hematologic Complications and Design Challenges in Cardiovascular Devices.” Communications
Engineering. Springer Nature, 2026. https://doi.org/10.1038/s44172-026-00771-9.
ieee: D. Padovani, N. S. Afsharimani, A. Cioncolini, and Y. Ding, “Hematologic complications
and design challenges in cardiovascular devices,” Communications Engineering,
vol. 5. Springer Nature, 2026.
ista: Padovani D, Afsharimani NS, Cioncolini A, Ding Y. 2026. Hematologic complications
and design challenges in cardiovascular devices. Communications Engineering. 5,
167.
mla: Padovani, Damiano, et al. “Hematologic Complications and Design Challenges
in Cardiovascular Devices.” Communications Engineering, vol. 5, 167, Springer
Nature, 2026, doi:10.1038/s44172-026-00771-9.
short: D. Padovani, N.S. Afsharimani, A. Cioncolini, Y. Ding, Communications Engineering
5 (2026).
das_tickbox: '0'
date_created: 2026-10-11T22:02:04Z
date_published: 2026-09-30T00:00:00Z
date_updated: 2026-10-12T11:34:48Z
day: '30'
ddc:
- '570'
- '610'
department:
- _id: NanoFab
doi: 10.1038/s44172-026-00771-9
external_id:
pmid:
- '42816513'
file:
- access_level: open_access
checksum: 770d3ef015bc3a8a81017f07a3225ab6
content_type: application/pdf
creator: dernst
date_created: 2026-10-12T11:33:01Z
date_updated: 2026-10-12T11:33:01Z
file_id: '23108'
file_name: 2026_CommunicationsEngineering_Padovani.pdf
file_size: 9201511
relation: main_file
success: 1
file_date_updated: 2026-10-12T11:33:01Z
fulldoi: https://doi.org/10.1038/s44172-026-00771-9
has_accepted_license: '1'
intvolume: ' 5'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
pmid: 1
publication: Communications Engineering
publication_identifier:
eissn:
- 2731-3395
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Hematologic complications and design challenges in cardiovascular devices
tmp:
image: /images/cc_by_nc_nd.png
legal_code_url: https://creativecommons.org/licenses/by-nc-nd/4.0/legalcode
name: Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International
(CC BY-NC-ND 4.0)
short: CC BY-NC-ND (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 5
year: '2026'
...
---
OA_place: publisher
_id: '23072'
abstract:
- lang: eng
text: "Inferring signal from large quantities of data is one of the most important
problems in today’s\r\nworld, with neural networks emerging as the most powerful
solution. While there have been\r\nmassive breakthroughs in the ML space, there
are two main drawbacks. The first is that\r\nmost of these models are “black boxes”,
with very little understanding of why they work,\r\nwhich makes it hard to find
the correct architecture for a given problem. The architecture is\r\ncrucial,
as the widely used training algorithms are “local” and thus rely on the loss landscape\r\nbeing
benign enough to find a global optimum. This brings us to the second problem:
while\r\nthere is a lot of evidence that this can be overcome with large enough
data, this is less clear\r\nfor datasets which are noisy, do not have enough samples,
or have a non-standard structure.\r\nHistorically, on a smaller scale, the alternative
has been simple (Bayesian) statistical methods,\r\nwhich also have the advantage
of being interpretable and adaptable. However, many of the\r\nclassical results
cannot be easily extended to the high-dimensional regime in which modern\r\ndata
lives.\r\nIn this work we want to consider two different settings relating to
the above. The first is\r\napproximate message passing (AMP), an iterative algorithm
for high-dimensional (generalized)\r\nlinear models that easily lends itself to
Bayesian setups, and which in many cases is provably\r\nBayes-optimal. The second
is an autoencoder with a shallow encoder, for which we can\r\nanalyze the weights
along the training trajectory of gradient descent. Surprisingly, we will find\r\na
connection between the two, as we recover certain structures of AMP.\r\nWe will
first introduce the AMP framework by studying an extension that can be applied\r\nto
a wider variety of data: rotationally invariant generalized approximate message
passing\r\n(RI-GAMP). This shows that one can extend the AMP framework to a much
wider class of\r\nalgorithms, relevant to more practical settings. The results
are then also confirmed on real\r\ndata that go beyond the theoretical setting.\r\nWe
then move to the setup of an autoencoder with a shallow encoder and a Bayesian
prior in\r\nthe high-dimensional regime, in which the input and compression dimensions
are large and\r\nproportional; this is also a first step towards opening one of
the black boxes above, as we\r\ncan say precisely when and why the network works.
While autoencoders are widely used in\r\nmodern ML architectures, most fundamental
research in this direction has focused on extreme\r\nasymptotic regimes, where
the autoencoder is either severely over- or under-parameterized,\r\nand which
do not extend to the proportional high-dimensional regime. We show that for\r\nGaussian
priors the network finds the global optimum, and these theoretical findings extrapolate\r\nstrikingly
well to real image data. Next we extend this analysis to more structured priors
and\r\na deeper decoder. For sparse Gaussian inputs in the training regime studied
here, the shallow\r\ndecoder does not exploit sparsity and yields the same dynamics
as in the Gaussian setting.\r\nWe then show how a deeper decoder can break this
behavior, and interestingly, if we treat the\r\nproblem as an AMP problem, the
network eventually learns the same decoding as AMP. This\r\ntoo extrapolates to
real image data.\r\nLastly, we will show that the AMP setup has real practical
use, by using a practical variant,\r\ngenetic vector approximate message passing
(gVAMP), for predicting plasma protein levels\r\nfrom genetic information using
the UKB GWAS data. This is a perfect example of the problems\r\nin the high-dimensional
regime: approximately 8.4 million dimensions and 40,000 samples,\r\nwhere the
high noise, low sample count, and large size make it hard for ML methods to work.\r\nTo
get the optimal prediction accuracy we consider a two-step inference. We first
consider a\r\npre-processed version of the data, of about 880,000 dimensions,
on which we run the gVAMP\r\nalgorithm; this allows us to find predictive regions,
taking into account joint effects between\r\ndifferent regions, and for most proteins
we end up selecting only about 0.1% of the dimensions.\r\nWe then consider the
analogue of this small subset, on which we can now run a standard tree\r\nalgorithm
(XGB) that no longer suffers from the aforementioned problems. This pipeline yields\r\nbetter
prediction accuracy than recent nonlinear deep learning approaches applied to
this data,\r\nas we are able to handle the pre-processing in a principled Bayesian
way."
acknowledged_ssus:
- _id: ScienComp
acknowledgement: "This project was partially supported by the 2019 Lopez-Loreta Prize
and\r\nthe ERC INF2 project (project number 101161364). Furthermore, the candidate
acknowledges\r\nthe support from the Scientific Service Units of the Institute of
Science and Technology Austria\r\nthrough resources provided by Scientific Computing."
alternative_title:
- ISTA Thesis
article_processing_charge: No
author:
- first_name: Kevin
full_name: Kögler, Kevin
id: 94ec913c-dc85-11ea-9058-e5051ab2428b
last_name: Kögler
citation:
ama: 'Kögler K. Compression and inference in high dimensions: An approximate message
passing perspective. 2026. doi:10.15479/AT-ISTA-23072'
apa: 'Kögler, K. (2026). Compression and inference in high dimensions: An approximate
message passing perspective. Institute of Science and Technology Austria.
https://doi.org/10.15479/AT-ISTA-23072'
chicago: 'Kögler, Kevin. “Compression and Inference in High Dimensions: An Approximate
Message Passing Perspective.” Institute of Science and Technology Austria, 2026.
https://doi.org/10.15479/AT-ISTA-23072.'
ieee: 'K. Kögler, “Compression and inference in high dimensions: An approximate
message passing perspective,” Institute of Science and Technology Austria, 2026.'
ista: 'Kögler K. 2026. Compression and inference in high dimensions: An approximate
message passing perspective. Institute of Science and Technology Austria.'
mla: 'Kögler, Kevin. Compression and Inference in High Dimensions: An Approximate
Message Passing Perspective. Institute of Science and Technology Austria,
2026, doi:10.15479/AT-ISTA-23072.'
short: 'K. Kögler, Compression and Inference in High Dimensions: An Approximate
Message Passing Perspective, Institute of Science and Technology Austria, 2026.'
corr_author: '1'
date_created: 2026-10-07T11:20:26Z
date_published: 2026-10-08T00:00:00Z
date_updated: 2026-10-12T13:04:49Z
day: '08'
ddc:
- '519'
degree_awarded: PhD
department:
- _id: MaMo
- _id: GradSch
doi: 10.15479/AT-ISTA-23072
doi_confirm: '1'
file:
- access_level: closed
checksum: 5fb2ff02dc9d8c659b2fb5e0802b06ff
content_type: application/zip
creator: kkoegler
date_created: 2026-10-09T11:20:09Z
date_updated: 2026-10-09T12:22:55Z
file_id: '23084'
file_name: 2026_Koegler_Kevin_Thesis.zip
file_size: 8504109
relation: source_file
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checksum: a6df3b04c97628a1703f63356fb56f96
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creator: kkoegler
date_created: 2026-10-09T13:25:49Z
date_updated: 2026-10-09T13:25:49Z
file_id: '23085'
file_name: 2026_Koegler_Kevin_Thesis.pdf
file_size: 6692605
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success: 1
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fulldoi: https://doi.org/10.15479/AT-ISTA-23072
has_accepted_license: '1'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
page: '222'
project:
- _id: 059876FA-7A3F-11EA-A408-12923DDC885E
name: Prix Lopez-Loretta 2019 - Marco Mondelli
publication_identifier:
issn:
- 2663-337X
publication_status: published
publisher: Institute of Science and Technology Austria
related_material:
record:
- id: '14459'
relation: part_of_dissertation
status: public
- id: '12540'
relation: part_of_dissertation
status: public
- id: '17469'
relation: part_of_dissertation
status: public
status: public
supervisor:
- first_name: Marco
full_name: Mondelli, Marco
id: 27EB676C-8706-11E9-9510-7717E6697425
last_name: Mondelli
orcid: 0000-0002-3242-7020
title: 'Compression and inference in high dimensions: An approximate message passing
perspective'
type: dissertation
user_id: 8b945eb4-e2f2-11eb-945a-df72226e66a9
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '23094'
abstract:
- lang: eng
text: The formation of C(sp2)–heteroatom bonds through cross-coupling catalysis
is central to the synthesis of pharmaceuticals, agrochemicals and materials. Whereas
Pd0/PdII catalysis requires substrate-specific ligand optimization to balance
the competing demands of oxidative addition and reductive elimination, NiI/NiIII
catalysis offers a complementary strategy because the bond-forming step is intrinsically
favourable. However, contemporary NiI/NiIII methodologies suffer from insufficient
oxidative addition reactivity, restricting the aryl halide scope and requiring
high catalyst loadings. Here we show that mechanistically guided ligand design
overcomes these limitations. Together with a non-nucleophilic base additive that
promotes direct visible-light generation of NiI from a bench-stable NiII precatalyst,
this ligand design enables the coupling of electron-rich aryl bromides with N-,
O-, S- and P-based nucleophiles at nickel loadings as low as 100 ppm. The method
is compatible with sterically encumbered nucleophiles and enables gram-scale synthesis
and late-stage functionalization of complex molecules.
acknowledged_ssus:
- _id: LifeSc
- _id: MassSpec
- _id: NMR
- _id: M-Shop
acknowledgement: We acknowledge ISTA for generous financial support. This research
was supported by the Scientific Service Units (SSU) of ISTA through resources provided
by the Lab Support Facility, Mass Spec Facility, NMR facility and the Miba Machine
Shop. We specifically thank A. Paraskevopoulou for high-resolution mass spectrometry
measurements. B.P. acknowledges the Austrian Science Fund (PAT 1250924) and the
ACS GCI Pharmaceutical Roundtable for funding. T.B. thanks the European Union’s
Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie
Grant Agreement No. 101034413. D.B. acknowledges funding from the Czech Science
Foundation (25-17760M). 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: Aleksander
full_name: Bena, Aleksander
id: 4197c39e-e8ec-11ed-86cb-afed934cd664
last_name: Bena
- first_name: Trisha
full_name: Banik, Trisha
id: 506b8e06-c59a-11ee-a1af-ae470719e7d3
last_name: Banik
- first_name: Christos
full_name: Giannoudis, Christos
id: 1bd506c6-e8ec-11ed-86cb-d495f63f2dcd
last_name: Giannoudis
- first_name: Florian
full_name: Ortis, Florian
id: e34c9177-3208-11ee-ac71-a6a15cf2ef29
last_name: Ortis
orcid: 0000-0002-0458-5187
- first_name: Daniel
full_name: Bím, Daniel
last_name: Bím
- first_name: Haralds
full_name: Baunis, Haralds
id: 2eea55ec-e8ec-11ed-86cb-d9c76787acfe
last_name: Baunis
- first_name: Gayathri
full_name: Palissery, Gayathri
id: b02c9d47-50c9-11ef-b52e-b2180bf00ccd
last_name: Palissery
- first_name: Bartholomäus
full_name: Pieber, Bartholomäus
id: 93e5e5b2-0da6-11ed-8a41-af589a024726
last_name: Pieber
orcid: 0000-0001-8689-388X
citation:
ama: Bena A, Banik T, Giannoudis C, et al. Ligand design broadens NiI-catalysed
C(sp2)–heteroatom couplings of aryl bromides at low catalyst loadings. Nature
Catalysis. 2026. doi:10.1038/s41929-026-01616-6
apa: Bena, A., Banik, T., Giannoudis, C., Ortis, F., Bím, D., Baunis, H., … Pieber,
B. (2026). Ligand design broadens NiI-catalysed C(sp2)–heteroatom couplings of
aryl bromides at low catalyst loadings. Nature Catalysis. Springer Nature.
https://doi.org/10.1038/s41929-026-01616-6
chicago: Bena, Aleksander, Trisha Banik, Christos Giannoudis, Florian Ortis, Daniel
Bím, Haralds Baunis, Gayathri Palissery, and Bartholomäus Pieber. “Ligand Design
Broadens NiI-Catalysed C(Sp2)–Heteroatom Couplings of Aryl Bromides at Low Catalyst
Loadings.” Nature Catalysis. Springer Nature, 2026. https://doi.org/10.1038/s41929-026-01616-6.
ieee: A. Bena et al., “Ligand design broadens NiI-catalysed C(sp2)–heteroatom
couplings of aryl bromides at low catalyst loadings,” Nature Catalysis.
Springer Nature, 2026.
ista: Bena A, Banik T, Giannoudis C, Ortis F, Bím D, Baunis H, Palissery G, Pieber
B. 2026. Ligand design broadens NiI-catalysed C(sp2)–heteroatom couplings of aryl
bromides at low catalyst loadings. Nature Catalysis.
mla: Bena, Aleksander, et al. “Ligand Design Broadens NiI-Catalysed C(Sp2)–Heteroatom
Couplings of Aryl Bromides at Low Catalyst Loadings.” Nature Catalysis,
Springer Nature, 2026, doi:10.1038/s41929-026-01616-6.
short: A. Bena, T. Banik, C. Giannoudis, F. Ortis, D. Bím, H. Baunis, G. Palissery,
B. Pieber, Nature Catalysis (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: All data are available from the authors upon request.
date_created: 2026-10-11T22:02:06Z
date_published: 2026-09-29T00:00:00Z
date_updated: 2026-10-14T06:32:42Z
day: '29'
department:
- _id: BaPi
- _id: GradSch
- _id: RaKl
doi: 10.1038/s41929-026-01616-6
ec_funded: 1
fulldoi: https://doi.org/10.1038/s41929-026-01616-6
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1038/s41929-026-01616-6
month: '09'
oa: 1
oa_version: Published Version
project:
- _id: 8f1d607d-16d5-11f0-9cad-ab453295ba5e
grant_number: PAT 1250924
name: Photoactive ligands for transformative nickel catalysis
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
publication: Nature Catalysis
publication_identifier:
eissn:
- 2520-1158
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: upon request
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Ligand design broadens NiI-catalysed C(sp2)–heteroatom couplings of aryl bromides
at low catalyst loadings
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '23095'
abstract:
- lang: eng
text: "The PXP chain was recently shown to exhibit superdiffusive energy transport
with Kardar-Parisi-Zhang-like\r\nscaling, z ≈ 3/2, joining a growing number of
spin chains with this exponent. An understanding of how this\r\nanomalous hydrodynamics
emerges from microscopics is, however, still lacking. In this work, we show that\r\nfinite-temperature
energy transport in this model provides a window into the emergence of superdiffusion.
At\r\nfinite temperature, the energy autocorrelation function exhibits a crossover
from short-time coherent dynamics to\r\nlong-time hydrodynamics. The short-time
behavior is dominated by a single magnon band and can be understood\r\nanalytically.
In momentum space, this regime is characterized by spectral weight near q = π.
The damping time\r\nτ , which separates the short-time magnon-dominated behavior
from the late-time hydrodynamics, grows rapidly\r\nupon cooling, consistent with
an activated form τ (β) ∼ βe\x05β with a gap scale set by the magnon band. At
longer\r\ntimes, the spectral weight transfers to q = 0 and the running decay
exponent drifts toward the superdiffusive\r\nvalue z = 3/2. Finite-temperature
energy transport therefore provides a bridge between microscopic magnon\r\nphysics
and late-time superdiffusion in the PXP model."
acknowledgement: "We thank M. Serbyn, S. White, and T. Iadecola for insightful discussions.
Work by T.S. was supported by the U.S.\r\nDepartment of Energy, Office of Science,
Office of Basic\r\nEnergy Sciences under Early Career Research Program Award\r\nNo.
DE-SC0025568. T.S. gratefully acknowledges the Institute of Science and Technology
Austria (ISTA) for hosting\r\nhim during the initial stages of this project. S.J.
is supported by the U.S. Department of Energy, Office of Science,\r\nBasic Energy
Sciences, Materials Sciences and Engineering\r\nDivision, under Contract No. DE-AC02-76SF00515.
M.L.\r\nacknowledges support by the Deutsche Forschungsgemeinschaft (DFG, German
Research Foundation) under Germany’s\r\nExcellence Strategy—EXC-2111—390814868.
J.-Y.D. acknowledges funding from the European Union’s Horizon\r\n2020 Research
and innovation program under the Marie\r\nSkłodowska-Curie Grant Agreement No. 101034413."
article_number: '084306'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jiang
full_name: Shengtao, Jiang
last_name: Shengtao
- first_name: Jean-Yves Marc
full_name: Desaules, Jean-Yves Marc
id: 6c292945-a610-11ed-9eec-c3be1ad62a80
last_name: Desaules
orcid: 0000-0002-3749-6375
- first_name: Marko
full_name: Ljubotina, Marko
id: F75EE9BE-5C90-11EA-905D-16643DDC885E
last_name: Ljubotina
orcid: 0000-0003-0038-7068
- first_name: Thomas
full_name: Scaffidi, Thomas
last_name: Scaffidi
citation:
ama: Shengtao J, Desaules J-YM, Ljubotina M, Scaffidi T. Finite-temperature crossover
from coherent magnons to energy superdiffusion in the PXP model. Physical Review
B. 2026;114(8). doi:10.1103/mx9k-1mc6
apa: Shengtao, J., Desaules, J.-Y. M., Ljubotina, M., & Scaffidi, T. (2026).
Finite-temperature crossover from coherent magnons to energy superdiffusion in
the PXP model. Physical Review B. American Physical Society. https://doi.org/10.1103/mx9k-1mc6
chicago: Shengtao, Jiang, Jean-Yves Marc Desaules, Marko Ljubotina, and Thomas Scaffidi.
“Finite-Temperature Crossover from Coherent Magnons to Energy Superdiffusion in
the PXP Model.” Physical Review B. American Physical Society, 2026. https://doi.org/10.1103/mx9k-1mc6.
ieee: J. Shengtao, J.-Y. M. Desaules, M. Ljubotina, and T. Scaffidi, “Finite-temperature
crossover from coherent magnons to energy superdiffusion in the PXP model,” Physical
Review B, vol. 114, no. 8. American Physical Society, 2026.
ista: Shengtao J, Desaules J-YM, Ljubotina M, Scaffidi T. 2026. Finite-temperature
crossover from coherent magnons to energy superdiffusion in the PXP model. Physical
Review B. 114(8), 084306.
mla: Shengtao, Jiang, et al. “Finite-Temperature Crossover from Coherent Magnons
to Energy Superdiffusion in the PXP Model.” Physical Review B, vol. 114,
no. 8, 084306, American Physical Society, 2026, doi:10.1103/mx9k-1mc6.
short: J. Shengtao, J.-Y.M. Desaules, M. Ljubotina, T. Scaffidi, Physical Review
B 114 (2026).
das_tickbox: '1'
dataavailabilitystatement: "There are no publicly available research data or software\r\nsupporting
this manuscript. Requests for further information\r\nor data should be sent to the
authors."
date_created: 2026-10-11T22:02:06Z
date_published: 2026-08-21T00:00:00Z
date_updated: 2026-10-14T05:44:58Z
day: '21'
department:
- _id: MaSe
doi: 10.1103/mx9k-1mc6
ec_funded: 1
external_id:
arxiv:
- '2605.19281'
fulldoi: https://doi.org/10.1103/mx9k-1mc6
intvolume: ' 114'
issue: '8'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2605.19281
month: '08'
oa: 1
oa_version: Preprint
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
publication: Physical Review B
publication_identifier:
eissn:
- 2469-9969
issn:
- 2469-9950
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
researchdata_availability: upon request
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Finite-temperature crossover from coherent magnons to energy superdiffusion
in the PXP model
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 114
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23115'
abstract:
- lang: eng
text: "We investigate the association between galaxies and neutral O I absorption
systems at z ∼ 6, which trace metalenriched gas during the epoch of reionization.
We identify 40 galaxies across six quasar fields, residing in 15\r\noverdensities
within 300 kpc of the background sight lines. Five O I absorption systems are
associated with five of\r\nthese overdensities, yielding a covering fraction of\r\n0.27
0.10\r\n+0.13\r\nwithin 300 kpc. The absorption occurs beyond typical\r\nvirial
radii, indicating that the gas traces extended overdensity environments rather
than individual galaxy halos,\r\nunlike the z ∼ 0 circumgalactic medium (CGM),
which is largely bound to halos. These galaxy-associated\r\nabsorbers account
for ∼35% of all O I systems seen in blind quasar surveys, implying the remainder
arise in\r\nlower-mass galaxies below our detection threshold or in dense neutral
intergalactic medium pockets. The CGM\r\naround these galaxies contains ≳ 2 ×
106 M⊙ of oxygen, comparable to the interstellar medium oxygen mass of\r\nthe
galaxies themselves, suggesting that the surrounding environment holds as much
metal mass as the galaxies.\r\nAll five galaxy-associated systems show significantly
higher\r\nlog NCII NOI ( / )\r\nratios than absorbers lacking galaxy\r\nassociations.
Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal that four of the
five exhibit\r\nenrichment patterns consistent with Population III nucleosynthesis
at the outskirts of galaxy overdensities. These\r\nrare systems offer a unique
window into the role of first-generation stars in shaping the early metal enrichment
of\r\ngalaxies and their environments."
acknowledgement: "IOP Science home\r\nAccessibility Help\r\n\r\nJournals\r\nBooks\r\nPublishing
Support\r\nLogin\r\nThe Astrophysical Journal\r\nThe American Astronomical Society,
find out more.\r\n\r\nThe following article isOpen access\r\nEIGER. VIII. First
Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch
of Reionization\r\nJack Higginson, Rongmon Bordoloi, Robert A. Simcoe, Jorryt Matthee,
Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, Simon J. Lilly, Anna-Christina
Eilers, Rohan P. NaiduShow full author list\r\n\r\nPublished 2026 February 24 •
© 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical
Journal, Volume 999, Number 1\r\nCitation Jack Higginson et al 2026 ApJ 999 49\r\nDOI
10.3847/1538-4357/ae3e81\r\n\r\nPDFOpens in a new tab.\r\nePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle
data\r\nPDFOpens in a new tab.\r\nePub\r\nArticle metrics\r\n626 Total downloads\r\n\r\n22
total citations on Dimensions.\r\nShare this article\r\nArticle information\r\nAbstract\r\nWe
investigate the association between galaxies and neutral O i absorption systems
at z ∼ 6, which trace metal-enriched gas during the epoch of reionization. We identify
40 galaxies across six quasar fields, residing in 15 overdensities within 300 kpc
of the background sight lines. Five O i absorption systems are associated with five
of these overdensities, yielding a covering fraction of \r\n within 300 kpc. The
absorption occurs beyond typical virial radii, indicating that the gas traces extended
overdensity environments rather than individual galaxy halos, unlike the z ∼ 0 circumgalactic
medium (CGM), which is largely bound to halos. These galaxy-associated absorbers
account for ∼35% of all O i systems seen in blind quasar surveys, implying the remainder
arise in lower-mass galaxies below our detection threshold or in dense neutral intergalactic
medium pockets. The CGM around these galaxies contains ≳ 2 × 106 M⊙ of oxygen,
comparable to the interstellar medium oxygen mass of the galaxies themselves, suggesting
that the surrounding environment holds as much metal mass as the galaxies. All five
galaxy-associated systems show significantly higher \r\n ratios than absorbers lacking
galaxy associations. Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal
that four of the five exhibit enrichment patterns consistent with Population III
nucleosynthesis at the outskirts of galaxy overdensities. These rare systems offer
a unique window into the role of first-generation stars in shaping the early metal
enrichment of galaxies and their environments.\r\n\r\nExport citation and abstract\r\nBibTeX\r\nRIS\r\n\r\nPrevious
article in issue\r\nNext article in issue\r\nRelated links\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
first generations of stars formed shortly after the Epoch of Recombination within
dark matter overdensities, producing the first significant quantities of metals
and enriching the intergalactic medium (IGM) while reionizing hydrogen and helium
(e.g., R. S. Klessen & S. C. O. Glover 2023). These metals and gas eventually coalesced
into the first galaxies, which over cosmic time evolved into Milky Way–like systems
today. Studying these young galaxies and their environments provides critical insight
into galaxy formation and evolution, constraining models of stellar feedback, gas
accretion, and chemical enrichment (C.-A. Faucher-Giguère & S. P. Oh 2023; C. Peroux
& D. Nelson 2024).\r\n\r\nAt low redshift, decades of observations using deep ground-based
spectroscopy and Hubble Space Telescope (HST) data of background quasars and foreground
galaxies have built a rich understanding of the circumgalactic medium (CGM) and
its interplay with galaxies (e.g., J. Tumlinson et al. 2017). The CGM plays a crucial
role in gas recycling, star formation regulation, and quenching; understanding its
structure and composition informs galaxy growth models (Y. Peng et al. 2015; E.
Zinger et al. 2020).\r\n\r\nHigh-redshift studies, leveraging ground- and space-based
near-infrared (NIR) spectroscopy of quasars, reveal that the early Universe was
already chemically enriched by the epoch of reionization (e.g., T. J. Cooper et
al. 2019; L. Christensen et al. 2023; R. L. Davies et al. 2023a). Among tracers
of neutral and low-ionization gas, O i has emerged as a key probe: surveys report
an increase in O i number density at z ≳ 5–6 (G. D. Becker et al. 2019; L. Christensen
et al. 2023; A. M. Sebastian et al. 2024; A. Sodini et al. 2024), while higher-ionization
species like C iv and Si iv decline, consistent with a softer and evolving UV background
at the end of reionization (T. J. Cooper et al. 2019; V. D’Odorico et al. 2022;
R. L. Davies et al. 2023a, 2023b).\r\n\r\nHistorically, connecting absorption systems
with their host galaxies was challenging due to the difficulty of obtaining deep,
high-redshift galaxy spectroscopy. This has changed with the advent of JWST, providing
unprecedented views of early galaxies and their impact on surrounding gas through
surveys such as EIGER (D. Kashino et al. 2023) and ASPIRE (F. Wang et al. 2023).
First systematic studies of cool, low-ionization CGM traced by Mg ii around z ∼
6 galaxies suggest that high-redshift CGM differs significantly from its low-redshift
counterpart: these galaxies typically have low masses, and strong stellar feedback
can eject metals far beyond the halo’s gravitational potential (R. Bordoloi et al.
2024). Such pioneering studies now allow systematic investigations of the CGM in
the early Universe.\r\n\r\nThe UV background during reionization was inhomogeneous
and rapidly evolving (e.g., S. R. Furlanetto & S. P. Oh 2005; B. D. Oppenheimer
et al. 2009; K. Finlator et al. 2013; G. D. Becker et al. 2015; S. E. I. Bosman
et al. 2022), initially dominated by Population III stars (K. Nakajima & R. Maiolino
2022; K. Nakajima et al. 2025), then by early star-forming galaxies (L. Jiang et
al. 2022; J. Matthee et al. 2022), with active galactic nuclei (AGN) contributing
significantly by z ∼ 5 (A. D’Aloisio et al. 2017; G. Kulkarni et al. 2019; C.-A.
Faucher-Giguère 2020). Modeling indicates that pockets of Population III star formation
may persist throughout the Epoch of Reionization (L. Tornatore et al. 2007; R. H.
Mebane et al. 2018; J. L. Johnson & A. Aykutalp 2019; A. Venditti et al. 2023; O.
Zier et al. 2025).\r\n\r\nThe large reservoir of neutral O i observed in quasar
absorption lines at high redshift is typically self-shielded, providing robust estimates
of chemical abundances. Studying the association of these absorbers with galaxies
offers unique insight into the CGM of early galaxies, and into potential contributions
from Population III stars to early chemical enrichment.\r\n\r\nIn this work, we
study the cool, neutral CGM around galaxies at z ∼ 6, traced by O i absorption from
the EIGER survey (D. Kashino et al. 2023). We focus on O i absorbers associated
with [O iii]5008-emitting galaxies at 5.875 150 kpc, an incidence
of is measured. Within 300 kpc of the primary galaxy, the overall incidence is ,
with values of for 50 ≤ R ≤ 300 kpc and for 100 ≤ R ≤ 300 kpc. These rates are substantially
weaker than the incidence of strong Mg ii absorption at z ∼ 6 (R. Bordoloi et al.
2024), indicating that neutral oxygen preferentially traces a different phase of
the circumgalactic environment.\r\n\r\nPanels (b) and (d) reveal that O i absorbers
are typically located at much larger R/Rvir than strong low-ionization tracers such
as Mg ii. This distinction suggests that O i absorption at z ∼ 6 is not confined
to the CGM of an individual galaxy but instead reflects the larger-scale gaseous
environment of galaxy overdensities—what might be described as “cosmic ecosystems”
rather than isolated halos.\r\n\r\nComparing the stellar mass distributions of overdensities
with and without O i absorption, we find no statistically significant differences.
The mean stellar mass of galaxies in overdensities with absorption is , compared
to for those without.\r\n\r\nWe emphasize that at z ∼ 6, the large R/Rvir values
of these halos imply that O i absorption typically arises at scales well beyond
the typical CGM [R/Rvir ≲ 1] (J. Tumlinson et al. 2017) probed by low-ionization
lines at lower redshift. Unlike the low-z CGM, where metal absorbers are closely
tied to the halo of a single massive galaxy, the O i absorbers studied here appear
to be linked to extended networks of low-mass, young galaxies embedded in shared
overdensities. Over cosmic time, these small systems and their diffuse gaseous environments
are expected to merge and evolve into more massive systems, eventually forming Milky
Way–like galaxies by z = 0. Thus, neutral O i at reionization is best understood
not as a tracer of isolated galactic halos, but as a probe of the extended environments
that connect galaxies, gas, and structure growth in the early Universe.\r\n\r\nBecause
O i absorption traces dense, neutral gas and requires only minimal ionization corrections,
we can place a conservative lower limit on the total oxygen mass associated with
the EIGER galaxies. These estimates are intended as simple, order-of-magnitude calculations
to provide intuition about the amount of neutral oxygen relative to the observed
galaxy properties. Following the formalism of R. Bordoloi et al. (2014), the oxygen
mass contained in an annulus bounded by Rin and Rout is\r\n\r\nwhere Rin and Rout
are the inner and outer radii of the annulus, fc is the covering fraction (the incidence
of O i detections in that bin), 〈NOI〉 is the mean O i column density in the annulus,
and mO = 16 mp is the mass of an oxygen atom, with mp being the mass of a proton.
For a conservative lower limit, we adopt fion = 1, where fion is the ionization
fraction (i.e., we assume that all of the oxygen mass is in the neutral phase).
We justify this assumption as follows: O i is tightly coupled to H i through charge
exchange, and in dense gas, the required ionization correction is minor, even under
strong radiation fields such as the Fermi Bubbles (R. Bordoloi et al. 2017; T. Ashley
et al. 2022). Under a typical metagalactic UV background, it is generally less than
10% and does not significantly alter the inferred oxygen abundance. In addition,
oxygen does not deplete onto dust grains, unlike Si or C. For these reasons, we
consider the approximation NO,total ≈ NOI to be valid for our analysis.\r\n\r\nWe
compute masses in two radial bins: 0–100 kpc and 100–300 kpc, respectively. The
total oxygen mass within radius is obtained by summing the masses of the constituent
annuli. This yields a strict lower limit of ≳ 2 ×106M⊙ on the total oxygen mass
within = 300 kpc.\r\n\r\nWe compare the inferred oxygen mass in the extended environment
of our sample with the total oxygen content in the interstellar medium (ISM) of
a typical z ∼ 6 galaxy. In computing this quantity, we make the following assumptions.
First, we assume that all galaxies in this work lie on the typical z ∼ 6 mass–metallicity
relation, derived by stacking [O iii] emitter galaxies (J. Matthee et al. 2022),
and we adopt the gas-phase metallicity from this relation for each galaxy.\r\n\r\nBecause
direct measurements of the total H2 and H i gas content are not available at these
redshifts, we extrapolate the molecular gas fraction from L. J. Tacconi et al. (2018)
to z ∼ 6 and adopt a conservative H i gas fraction based on local observations (S.
Huang et al. 2012). We note that high-z galaxies are likely more gas-rich than their
local counterparts; therefore, the inferred ISM gas masses should be considered
lower limits.\r\n\r\nWith these caveats in mind, we estimate the total ISM oxygen
mass as\r\n\r\nwhere we define . Here, XO is the gas-phase oxygen abundance derived
from the mass–metallicity relation, and and MHI are the molecular and atomic gas
masses derived as described above. For our galaxy sample, the mean stellar mass
is , corresponding to an ISM oxygen mass of MO,ISM ≳ 6.8 × 105 M⊙. Remarkably,
this indicates that the typical ISM oxygen content is comparable to the oxygen mass
in the extended environment around these galaxies, implying that the circumgalactic
or intergalactic medium at z ∼ 6 contains a substantial reservoir of oxygen. While
these estimates depend on several specific assumptions, the inferred ISM and CGM
oxygen masses appear to be of similar magnitude.\r\n\r\nAt low redshift, both L*
and sub-L* galaxies similarly exhibit substantial metal content in their circumgalactic
medium (CGM), with the CGM containing at least as much metal as the ISM of their
host galaxies (J. Tumlinson et al. 2011; R. Bordoloi et al. 2014). A key difference
is that, whereas the low-z CGM is typically gravitationally bound to its host galaxy,
at high redshift much of the gas exists in the extended environment of galaxy overdensities
rather than being bound to individual galaxies (see also R. Bordoloi et al. 2024).\r\n\r\n4.2.
Expected Incidence of O i Absorbers\r\nIn this section, we report the expected redshift-path
incidence of O i absorbers around [O iii] emitting galaxies detected in the EIGER
survey. We define the number of O i absorbers associated with each galaxy overdensity
per unit absorption distance above a detection threshold (WOI ≥ 0.05Å ) as\r\n\r\n\r\nHere,
Rmax = 300 kpc is the survey radius adopted in this work, and is the mean O i absorber
detection completeness (see Section 3.5; 91.4% for WOI ≥ 0.05 Å). nOD is defined
as\r\n\r\n\r\nngal is the number density of [O iii] emitting galaxies per unit comoving
volume, estimated from the [O iii] luminosity function at z ∼ 6. And 〈overdensity
size〉 is simply the mean number of galaxies in each galaxy overdensity empirically
measured to be 〈overdensity size〉 = 2.67. fc is the O i absorption covering fraction
within 300 kpc for WOI ≥ 0.05 Å (). (The covering fraction within 300 kpc is independent
of the definition of the primary member.)\r\n\r\nTo estimate the number density
of galaxies per unit comoving volume (ngal), we integrate the z ∼ 6 [O iii] luminosity
function derived from the EIGER survey, with a minimum luminosity of Lmin = 1042.2
ergs−1 (J. Matthee et al. 2022):\r\n\r\n\r\nwhere Φ(L) is the [O iii] luminosity
function defined as\r\n\r\n\r\nHere, Φ* is the characteristic number density, L*
is the characteristic luminosity, and α is the faint-end slope. We adopt Φ* = 10−4.02
Mpc−3, L* = 1043.33 ergs−1, and α = −1.92, values derived from detailed completeness
calculations of the EIGER [O iii]-emitting galaxies (R. Mackenzie et al. 2026, in
preparation). This results in ngal = 8.586 × 10−04 Mpc−3. Using these values in
Equation (6) yields , for O i absorption around galaxies at a mean galaxy redshift
of 6.001.\r\n\r\nAll calculations in this section are performed with a detection
threshold of WOI > 0.05Å, since the survey is highly complete down to this equivalent-width
limit and because most of the literature surveys we compare against adopt the same
threshold.\r\n\r\nWe emphasize that this approach differs from blind QSO absorption-line
surveys (e.g., G. D. Becker et al. 2006; L. Christensen et al. 2023; A. M. Sebastian
et al. 2024; A. Sodini et al. 2024), where all O i absorption-line systems along
the full quasar redshift path are counted to compute dN/dX directly, under the assumption
that the absorber cross section is contributed by all galaxies. In contrast, our
method begins by defining the absorber cross section around galaxy overdensities
and then estimating the corresponding contribution to dN/dX from the galaxy overdensities
under study. Comparing these two approaches constrains the fraction of O i (or other
metal) absorption systems that arise in the extended halos of these galaxies. Figure
6 shows these literature measurements as colored circles, while the contribution
to dN/dX around z ∼ 6 galaxy overdensities is indicated by an orange square. To
quantify the relative contribution of galaxy overdensities, we fit a single power
law to all literature values at z > 4 (blue dashed line with shaded region). Comparing
the dN/dX inferred from quasar absorption-line surveys at z ∼ 6 to our measured
value, we find that O i dN/dX around z ∼ 6 EIGER galaxy environments account for
35% ± 16% of all O i absorption-line systems detected in blind quasar surveys. This
implies that [O iii] emitting galaxy environments at z ∼ 6 contribute roughly one-third
of the O i absorption systems at that epoch. Although the EIGER QSOs were selected
to have known absorption systems along their sight lines, the EIGER galaxy survey
around these sight lines is highly complete and independent of this selection. Therefore,
we can create an unbiased measurement of the absorption cross section (dN/dX) around
these galaxy overdensities. We justify this comparison to blind absorption surveys
in Section 2.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Incidence of O
i absorbers per comoving path length, dN/dX. Values are derived from all O i absorption
lines along high-z quasar sight lines. Literature measurements are shown from G.
D. Becker et al. (2019; blue circles), L. Christensen et al. (2023; purple circles),
and A. M. Sebastian et al. (2024; red circles). The blue dashed line shows a power-law
fit to the z > 4 literature data, with the shaded region marking the 1σ uncertainty.
The orange square gives the inferred dN/dX when including only O i absorption associated
with host galaxies (see Section 4.2), indicating that only ∼35% of O i absorbers
at z ∼ 6 arise in galaxy environments.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution
image\r\nThis in turn suggests that ∼65% of the O i absorption systems detected
along quasar sight lines at the epoch of reionization are not associated with [O
iii] emitter galaxy overdensities. Either the bulk of O i absorption resides in
isolated pockets of neutral IGM gas outside extended galaxy halos, or it is contributed
by even lower-luminosity, less massive galaxies () that fall below the EIGER detection
limits. Such systems may also be detected in galaxy halos that are oxygen-poor or
lack strong [O iii] emission features, since our galaxy identifications primarily
rely on [O iii] and Hβ emission lines.\r\n\r\nSimulations suggest that O i absorption
should primarily arise in galactic halos rather than in the diffuse IGM, since metals
are not widely distributed and ionization fronts propagate more quickly than metals
(B. D. Oppenheimer et al. 2009; K. Finlator et al. 2013). Very low-mass protogalaxies
forming their first stars may blur the boundary between IGM and CGM, enriching their
surroundings with metals, especially if their star formation is bursty and prolific.
If sufficiently numerous, such systems could contribute a nonnegligible fraction
of oxygen in the early Universe.\r\n\r\nRecent observations support this possibility.
K. Nakajima et al. (2025) reported a strongly lensed (μ = 98) galaxy at z ≈ 6.6
with a stellar mass upper limit of only ∼2700 M⊙ and a dynamical mass ∼100 times
larger. The source shows emission and may be dominated by Population III stars.
This provides direct evidence of oxygen production in extremely low-mass systems.
A population of such ultralow-mass dwarf galaxies could plausibly account for the
∼65% of O i absorbers detected along quasar sight lines that are not associated
with galaxies in our survey. Our sensitivity limit of (J. Matthee et al. 2022) means
such dwarfs remain undetected. However, these galaxies may lack a dense enough CGM
to shield neutral O i from the UV background; thus, even if they produce oxygen,
neutral O i may not survive (K. Finlator et al. 2013). Interestingly, simulations
by S. Kušmić et al. (2024) showed that the contribution of metal ions, including
O i, is only weakly correlated with the stellar mass of the galaxy, and the contribution
is indistinguishable when comparing across galaxy luminosities. Additionally, they
argue that due to the steep slope of the stellar mass function, lower-mass, lower-luminosity
galaxies contribute the majority of absorbing metal ions in the CGM and IGM.\r\n\r\nLater
simulation works by C. Doughty et al. (2018); C. Doughty & K. Finlator (2019) suggest
that as the Epoch of Reionization continues, O i will reduce overall but be preferentially
found in higher column density regions close to halos, as they have a better ability
to self-shield from ionizing photons. In fact, C. Doughty & K. Finlator (2019) found
that at z = 6 the majority of O i mass was located in the ISM of galaxies and only
∼30% of O i mass was found in the CGM and IGM. In contrast, in this work, we find
that a substantial (comparable to ISM mass) oxygen mass exists outside galaxies;
however, we stress that our mass measurements are order-of-magnitude estimates.
A more direct comparison between these simulations and this work is the covering
fraction. They report ∼5%–25% covering fraction at z = 6 for O i with out to 102
pkpc. In the EIGER survey, we report a covering fraction using a minimum threshold
of WOI ≥ 0.05 Å (or approximately logNOI > 13.7 cm−2) out to 300 kpc. Given the
large measurement uncertainties and different definitions of associated galaxies,
the covering fractions are qualitatively consistent between the two works.\r\n\r\nThe
simulations of K. Finlator et al. (2013) suggest that O i absorbers with are most
likely associated with halos of mass ∼109 M⊙, where self-shielding is efficient.
They further predict that only ∼13% of all O i absorption systems should reside
in halos of 1010–1011.5 M⊙, the mass range of galaxies probed in this work. By contrast,
we measure a higher dN/dX of ∼35%, but qualitatively our results remain consistent
with the idea that roughly two-thirds of O i absorbers are associated with undetected
∼109 M⊙ halos. Future observations targeting lower-luminosity galaxies and higher
redshifts will be essential to test these predictions.\r\n\r\nAfter the initial
posting of this manuscript, G. Pruto et al. (2026) presented a simulation-based
study that adopts the observational compilation shown in Figure 6 as a reference
and explores the corresponding behavior in numerical models. Our minimum Wr threshold
corresponds to ; therefore, the most appropriate comparison is with their sample.
Qualitatively, the two sets of results are in agreement. A key distinction lies
in the definition of galactic environment. We characterize environments in terms
of galaxy overdensities, which we argue is the most appropriate description of where
O i absorbers reside at z ≈ 6, whereas G. Pruto et al. (2026) define the CGM based
on the virial radii of halos with . As a result, a direct quantitative comparison
is not straightforward. Nevertheless, their inferred dN/dX corresponds to an incidence
rate of O i absorbers of ∼58% ± 11%, which is consistent with our measurements within
the uncertainties. This agreement may depend on their tighter constraints on absorber
location and on the adopted minimum Wr or threshold. G. Pruto et al. (2026) further
report that ∼80% of O i absorbers with are predicted to lie outside the CGM, also
in qualitative agreement with our findings.\r\n\r\n4.3. Metal Abundances in O i
absorber population\r\nIn this section, we examine the relative abundances and metal
column density ratios of O i absorbers associated with galaxy overdensities, and
compare them to O i absorbers without any associated galaxies. To enable a fair
comparison, we restrict our analysis to the six quasar sight lines from the EIGER
survey and identify all O i absorption systems in the redshift range where an [O
iii]-emitting galaxy could be detected (5.9 ≤ zOI ≤ zQSO). We detect 10 O i absorption
systems in total, 5 of which have associated galaxy overdensities (Table 1) and
5 are without any identified galaxy association.\r\n\r\nWe first compare the ionic
column density ratios in these two populations. Figure 7 (top panels) shows the
ratios of NSiII/NOI and NCII/NOI as functions of NOI. Systems located near galaxy
overdensities (blue squares) systematically show higher Si ii/O i and C ii/O i ratios
compared to systems without associated overdensities (green crosses). This offset
could reflect differences in metallicity, or alternatively, the effects of ionization.
However, since the majority of these O i systems lack detectable high-ionization
transitions, it is reasonable to assume that neutral oxygen and singly ionized silicon
and carbon dominate the elemental reservoirs (see also L. Christensen et al. 2023).
In those cases, the observed ionic ratios provide direct tracers of relative abundances.
Two exceptions are found along the J0100 and J1148 sight lines, which do exhibit
Si iv and C iv absorption; for these systems, the degeneracy between chemical composition
and ionization corrections cannot be resolved. It is plausible that, on average,
O i absorption found near galaxy overdensities has higher elemental abundance ratios
as the non-galaxy-associated absorbers either have significantly lower-luminosity
and less massive galaxies, which would be expected to produce less metal, or there
are truly no galaxies associated with this population.\r\n\r\nZoom InZoom OutReset
image size\r\nFigure 7. Top panels: ion column density ratios of Si ii to O i (left)
and C ii to O i (right) as a function of the detected O i column densities, shown
in logarithmic units. Absorbers associated with galaxy overdensities (blue squares)
and those not associated with galaxy overdensities (green crosses) exhibit clear
variations in their column density ratios. One sight line with no detected Si ii
absorption is indicated with a downward arrow, where a 2σ upper limit on the column
density is assumed. Bottom panel: relative abundance ratios [Si/O] vs. [C/O] with
respect to solar abundance. The background contours show the IMF-weighted abundance
distributions from Population II and Population III SN models. Orange and pink circles
indicate abundance ratios predicted by low-metallicity Population II SN models.
The abundance ratios of several O i absorbers associated with galaxy overdensities
are consistent with a significant contribution from Population III SNe.\r\n\r\nDownload
figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nWe next compute the relative
abundances [Si/O] and [C/O], presented in the bottom panel of Figure 7. These abundances
are defined as\r\n\r\n\r\nwhere NSi,tot and NC,tot represent the summed ionic column
densities. For systems with detected high-ionization absorption (C iv or Si iv),
we include both low- and high-ionization states (NSiII + NSiIV and NCII + NCIV),
marking these measurements as lower limits (blue upward arrows in the figure) since
additional undetected ionization states may be present. We note that in the two
systems (a and b) exhibiting high-ionization absorption (see Table 1), the low-
and high-ionization absorption components are offset in velocity by Δv = –66 km
s−1 and –69 km s−1, respectively. These offsets are within ≲1.5 resolution elements
of the instrument, and therefore we cannot statistically distinguish whether the
low- and high-ionization components are kinematically distinct. This is suggestive
of a complex, potentially multiphase gaseous environment in the outskirts of these
galaxies. For systems without detected high-ionization transitions, we adopt NSiII
and NCII as the dominant contributions. We assume NO,tot ≈ NOI, as ionization corrections
for O i are typically very small at high O i column densities (see Section 4.1 for
discussion). We adopt solar reference abundances of = −1.18 ± 0.05 and (M. Asplund
et al. 2021).\r\n\r\nFigure 7 (bottom panel) reveals a striking separation between
O i absorbers associated with galaxy overdensities (blue squares) and those without
galaxy associations (green crosses). Systems near galaxies are found in the upper
left of the [Si/O]–[C/O] diagram, with two cases exhibiting high-ionization absorption
(lower abundance limits, blue arrows), which will offset them even farther from
the locus of nongalaxy absorbers.\r\n\r\nWe place these abundance patterns in the
context of chemical enrichment models from different stellar populations (see also
L. Christensen et al. 2023). The contours and colored circles in Figure 7 highlight
predicted [C/O] and [Si/O] yields from representative Population II and Population
III supernova (SN) models, weighted by a Salpeter IMF. The weighting by number of
stars predicted by an IMF is done to represent the typical observational relative
abundance distribution in these models. These are not exhaustive but span the dominant
theoretical expectations.\r\n\r\nPopulation III pair-instability SNe (PISNe; 140–260M⊙;
light green contours) predict narrow [C/O] ≃ –0.7 and high [Si/O] values, inconsistent
with any of our observed systems. Such PISNe are also expected to produce substantial
amounts of iron-peak elements, leading to elevated Fe/O ratios (J. Tumlinson et
al. 2004). We will investigate Mg ii and Fe ii absorption associated with z ∼ 6
galaxies in an upcoming work (J. Higginson et al. 2026, in preparation). Models
of massive Population III stars (10–100 M⊙) produce both hypernovae (gray contours;
E > 1052 erg) and standard core-collapse SNe (light blue contours; A. Heger & S.
E. Woosley 2010), spanning a broader region overlapping some of our measurements.
We also consider Population II models: low-metallicity core-collapse SNe from M.
Limongi & A. Chieffi (2018; orange contours, Population II SNe (L18)) occupy −0.25
≲ [C/O] ≲ 0.5 and −0.4 ≲ [Si/O] ≲ 0.4, overlapping parts of the Population III range,
while the C. Kobayashi et al. (2006) yields (pink and orange circles for hypernovae
and SNe, respectively) tend toward lower [Si/O] and [C/O].\r\n\r\nAgainst these
predictions, the contrast between the two absorber populations is clear. All nongalaxy
O i systems (green crosses) fall at the lower left of the diagram, consistent with
enrichment from both Population II and/or Population III SNe models. This regime
also overlaps with ultra-metal-poor damped Lyman-α absorbers (DLAs) at z ∼ 3 (−0.5
≲ [Si/O] ≲ 0, −0.5 ≲ [C/O] ≲ 0; R. Cooke et al. 2011; R. J. Cooke et al. 2017).
By contrast, three of the five galaxy-associated absorbers lie well outside both
the locus of Population II predictions and the locus of ultra-metal-poor DLA relative
abundances. These systems are best explained if Population III enrichment played
a major role, suggesting that they may represent a distinct population from ultra-metal-poor
DLA host galaxies (see also A. Sodini et al. 2024).\r\n\r\nSimilarly, A. Sodini
et al. (2024) found that the [C/O] and [Si/O] abundance ratios for high-redshift
O i absorber systems are consistent with significant enrichment from Population
III, with the majority explained by ≥ 30% contributions. They also find a large
spread in the implied Population III contribution; several systems require ≥ 60%
contributions, while others fall significantly below the average. This is a strong
indication of heterogeneous chemical enrichment by Population III stars during the
epoch of reionization.\r\n\r\nThe absorber toward J159 at z = 5.91 shows [C/O] =
0.20, [Si/O] = 0.55 (labeled c), and no evidence of high-ionization absorption.
These abundance ratios are best explained by contributions from Population III SNe
or hypernovae. The absorber toward J1030 at z = 6.07 ([C/O] = −0.38, [Si/O] = 0.65,
labeled e) also shows no high-ionization absorption. The relative abundances in
these two predominantly neutral systems are therefore quite robust. Interestingly,
the J1030 system is not reproduced by any single Population II or Population III
model, suggesting that it may have experienced multiple enrichment episodes, producing
unusually high [Si/O] coupled with low [C/O].\r\n\r\nTwo cases require special mention.
The absorber toward J0100 at z = 5.94 shows [C/O] ≥ 0.42 and [Si/O] ≥ 0.67 (labeled
a), with strong C iv and Si iv absorption. Since these are lower limits, ionization
corrections (for carbon and silicon) would push this system further upward, strengthening
the case for Population III contributions. This observation is best explained by
contributions from Population III hypernovae models. The J1148 absorber at z = 6.01
shows [C/O] ≥ 0.02 and [Si/O] ≥ 0.20 (labeled b), again with high-ionization lines;
correcting for ionization would shift it diagonally upward in the diagram. Taken
together, four of the five galaxy-associated absorbers show relative abundances
that cannot be explained by Population II models alone, pointing instead to significant
enrichment from Population III SNe or hypernovae.\r\n\r\nThus, most galaxy-associated
O i systems carry signatures of Population III enrichment. These results suggest
that O i systems tracing galaxy overdensities at z ∼ 6 carry chemical signatures
of Population III enrichment, likely from multiple SNe events rather than a single
explosion. The elevated [Si/O] and [C/O] ratios in these environments imply that
[O iii]—emitting galaxies at this epoch may retain significant Population III contributions,
and that metal-line absorbers around such overdensities provide a powerful probe
of the first generations of stars.\r\n\r\n4.4. Comparison to the z ≈ 0 Universe\r\nAt
z ∼ 6, we cannot directly detect the local environments where O i absorption systems
arise. However, at z ∼ 0, there are instances where the environments giving rise
to O i absorption are well understood. Here, we discuss several such instances and
compare them with z ∼ 6 observations. Such comparisons can provide useful insights
regarding the nature of local environments within which O i systems exist at high
z. We focus on O i absorption associated with local blue compact dwarf (BCD) galaxies
and the Magellanic Stream (MS), owing to their low metallicities and well-characterized
local environments.\r\n\r\nThere is evidence that O i is found preferentially in
the H ii regions of local BCDs, with their H i regions being pristine or showing
very low levels of enrichment (D. Kunth et al. 1994; M. Pettini & K. Lipman 1995;
T. X. Thuan & Y. I. Izotov 1997). In particular, T. X. Thuan & Y. I. Izotov (1997)
report that, to varying degrees, low-ionization metal lines (e.g., O i and Si ii)
reside in the ionized hydrogen regions of BCDs rather than the neutral hydrogen
regions. They report . Compared to the z ∼ 6 measurements in panel (b) of Figure
7, the O i column density of the BCD is comparable, but the Si ii-to-O i ratio is
inconsistent with the z ∼ 6 values. On the other hand, V. Lebouteiller et al. (2004)
find that the H ii region of the BCD I Zw 36 has significantly higher metallicity
than its H i region. However, inferred from velocity offsets, O i in that system
is associated with the H i region. The reported O i column density of that BCD ()
is approximately 2 orders of magnitude higher than the z ∼ 6 sample. Given the available
evidence, we conclude that the observed z ∼ 6 O i absorption systems are not similar
to local BCD systems and are unlikely to originate in H ii regions.\r\n\r\nThe MS
is a filamentary trail of gas in the Local Group. Multiphase absorption-line observations
from A. J. Fox et al. (2013) and P. Richter et al. (2013) support the argument that
the MS was tidally stripped from the Magellanic Clouds approximately 2 Gyr ago.
Inferences from the abundance ratios of alpha elements in the MS are best explained
by contributions from massive stars via Type II SNe when the MS was still part of
the Magellanic Clouds, although the presence of significant dust depletion makes
further inferences into enrichment history difficult. An additional study of the
MS (N. Kumari et al. 2015) reports abundance ratios in a compact high-velocity cloud
(CHVC) that is believed to be associated with the MS. They find [Si/O] = −0.04 ±
0.25 and [C/O] = −0.09 ± 0.23. When comparing these with the z ∼ 6 observations
presented in panel (c) of Figure 7, we see that the CHVC abundance ratios occupy
a different region of parameter space than the z ≈ 6 O i absorbers within identified
galactic overdensities showing Population III enrichment signatures (points a, c,
e). This discrepancy provides evidence that these z ∼ 6 O i absorbers with Population
III enrichment signatures are unlikely to arise in environments similar to the MS.
However, the ionic ratios of O i absorption systems not associated with galaxy overdensities
(green crosses) are consistent with this measurement. With the caveat that MS measurements
do contain dust depletion effects, it is plausible that such O i systems may trace
IGM structures with densities comparable to those of the MS at high z.\r\n\r\n5.
Conclusion\r\nWe have conducted a survey of neutral O i absorption systems associated
with galaxies during the Epoch of Reionization in the EIGER survey, using six high-redshift
quasars as background sight lines. Our study focuses on the distribution of neutral
oxygen around -emitting galaxies within 300 kpc and their connection to galaxy overdensities.
The main results are as follows:\r\n\r\n1. \r\nFive O i absorbers are detected
among 15 galaxy overdensities, spanning z = 5.91–6.16 with a mean redshift 〈z〉 =
6.001.\r\n2. \r\nThe O i covering fraction within 300 kpc of the closest galaxy
is , with for R ≤ 50 kpc and for 50 ≤ R ≤ 300 kpc, where the covering fraction is
calculated using the galaxy in an overdensity with the lowest impact parameter.\r\n3.
\ \r\nWe find ≳ 2 × 106 M⊙ of oxygen within 300 kpc, a mass comparable to the ISM
oxygen content of z ∼ 6 galaxies—assuming minimal ionization correction (see Section
4.1 for justification)—suggesting that the circumgalactic environment already holds
metal reservoirs rivaling those inside galaxies.\r\n4. \r\nO i absorbers are detected
as far as ∼8 R/Rvir from galaxies, in sharp contrast to low-ionization tracers such
as Mg ii, which are typically confined within ≲R/Rvir.\r\n5. \r\nThe incidence
of galaxy-associated O i absorbers is \r\n \r\n. Comparison with blind quasar absorption-line
surveys indicates that these systems represent only ∼35% of all O i absorbers at
z ∼ 6, implying that the majority likely arise in lower-mass galaxies below current
detection limits or in dense neutral IGM pockets that survived reionization.\r\n6.
\ \r\nRelative abundance and ionization ratios ([Si/O], [C/O]) show that galaxy-associated
O i systems are chemically enriched, with signatures in several systems consistent
with contributions from Population III stars. In particular, we identify four galaxy
overdensities whose outskirts exhibit absorption-line abundance ratios consistent
with contributions from Population III nucleosynthesis.\r\n\r\nOverall, these results
indicate that neutral O i at z ∼ 6 primarily traces extended overdensity environments
rather than the CGM of individual halos. Moreover, the chemical abundance patterns
of galaxy-associated O i systems suggest contributions from Population III stars,
likely arising from multiple SNe events rather than a single explosion. The elevated
[Si/O] and [C/O] ratios imply that [O iii]-emitting galaxies at this epoch may retain
significant Population III enrichment. Consequently, metal-line absorbers around
such overdensities offer a powerful probe of the first generations of stars, providing
insight into early chemical enrichment and the role of primordial stellar populations
in shaping galaxy evolution during the Epoch of Reionization.\r\n\r\nAcknowledgments\r\nThis
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 #1243. This paper includes data gathered
with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This
work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet
Science Institute. Data presented herein were obtained at the W. M. Keck Observatory
from telescope time allocated to the National Aeronautics and Space Administration
(NASA) through the agency’s scientific partnership with the California Institute
of Technology and the University of California. The Observatory was made possible
by the generous financial support of the W. M. Keck Foundation. The JWST data presented
in this article were obtained from the Mikulski Archive for Space Telescopes (MAST)
at the Space Telescope Science Institute. The specific observations analyzed can
be accessed via DOI: 10.17909/y94q-h212. This work was partially supported by the
National Science Foundation under grant No. AST-2108931. Jorryt Matthee and Ivan
Kramarenko acknowledge funding from the European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities:
JWST - James Webb Space Telescope (NIRCam), Magellan: Baade - (FIRE), VLT: Kueyen
- (X-shooter), and Keck: I - (HIRES, MOSFIRE).\r\n\r\nSoftware: astropy (Astropy
Collaboration et al. 2013, 2018, 2022), rbcodes (R. Bordoloi et al. 2025), rbvfit
(R. Bordoloi & J. Higginson 2025)."
article_number: '49'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Jack
full_name: Higginson, Jack
last_name: Higginson
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Simon J.
full_name: Lilly, Simon J.
last_name: Lilly
- first_name: Anna-Christina
full_name: Eilers, Anna-Christina
last_name: Eilers
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Minghao
full_name: Yue, Minghao
last_name: Yue
citation:
ama: Higginson J, Bordoloi R, Simcoe RA, et al. EIGER. VIII. First stars signatures
in the connection between O I absorption and galaxies in the epoch of reionization.
The Astrophysical Journal. 2026;999(1). doi:10.3847/1538-4357/ae3e81
apa: Higginson, J., Bordoloi, R., Simcoe, R. A., Matthee, J. J., Kashino, D., Mackenzie,
R., … Yue, M. (2026). EIGER. VIII. First stars signatures in the connection between
O I absorption and galaxies in the epoch of reionization. The Astrophysical
Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae3e81
chicago: Higginson, Jack, Rongmon Bordoloi, Robert A. Simcoe, Jorryt J Matthee,
Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, et al. “EIGER. VIII. First Stars
Signatures in the Connection between O I Absorption and Galaxies in the Epoch
of Reionization.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae3e81.
ieee: J. Higginson et al., “EIGER. VIII. First stars signatures in the connection
between O I absorption and galaxies in the epoch of reionization,” The Astrophysical
Journal, vol. 999, no. 1. IOP Publishing, 2026.
ista: Higginson J, Bordoloi R, Simcoe RA, Matthee JJ, Kashino D, Mackenzie R, Kramarenko
I, Lilly SJ, Eilers A-C, Naidu RP, Yue M. 2026. EIGER. VIII. First stars signatures
in the connection between O I absorption and galaxies in the epoch of reionization.
The Astrophysical Journal. 999(1), 49.
mla: Higginson, Jack, et al. “EIGER. VIII. First Stars Signatures in the Connection
between O I Absorption and Galaxies in the Epoch of Reionization.” The Astrophysical
Journal, vol. 999, no. 1, 49, IOP Publishing, 2026, doi:10.3847/1538-4357/ae3e81.
short: J. Higginson, R. Bordoloi, R.A. Simcoe, J.J. Matthee, D. Kashino, R. Mackenzie,
I. Kramarenko, S.J. Lilly, A.-C. Eilers, R.P. Naidu, M. Yue, The Astrophysical
Journal 999 (2026).
date_created: 2026-10-12T12:15:27Z
date_published: 2026-02-24T00:00:00Z
date_updated: 2026-10-14T07:58:57Z
day: '24'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.3847/1538-4357/ae3e81
external_id:
arxiv:
- '2510.05220'
file:
- access_level: open_access
checksum: 1b8caf640c32d0d27a078bfb27ffcf8a
content_type: application/pdf
creator: dernst
date_created: 2026-10-14T07:50:51Z
date_updated: 2026-10-14T07:50:51Z
file_id: '23136'
file_name: 2026_AstrophysicalJour_Higginson.pdf
file_size: 2808503
relation: main_file
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file_date_updated: 2026-10-14T07:50:51Z
fulldoi: https://doi.org/10.3847/1538-4357/ae3e81
has_accepted_license: '1'
intvolume: ' 999'
issue: '1'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: EIGER. VIII. First stars signatures in the connection between O I absorption
and galaxies in the epoch of reionization
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 999
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23117'
abstract:
- lang: eng
text: 'We present a comprehensive analysis of the relationship between galaxies
and the intergalactic medium (IGM) during the late stages of cosmic reionization,
based on the complete JWST EIGER dataset. Using deep NIRCam 3.5 μm slitless spectroscopy,
we construct a sample of 948 [O iii]λ5008-emitting galaxies with −21.4 ≲ MUV ≲
−17.2 spanning 5.33 < z < 6.97 along six quasar sight lines. We correlate these
galaxies with Lyα and Lyβ transmission measured from high-resolution quasar spectra
across multiple redshift intervals. We find clear redshift evolution in the correlation
between galaxy density and transmission: it is suppressed in overdense regions
at z < 5.50, while enhanced at 5.70 < z < 6.15. The intermediate range exhibits
a transitional behavior. Cross-correlation measurements further reveal excess
absorption within ∼8 cMpc of galaxies at low redshifts, and enhanced transmission
at intermediate scales (∼5–20 cMpc) at z > 5.70. Statistical tests using mock
catalogs with realistic galaxy clustering but no correlation with the transmission
field confirm that the observed correlations are unlikely to arise by chance.
The evolving signals can be explained by stronger absorption in overdense regions,
combined with the competing influences of local radiation fields and the rising
background radiation. While local radiation dominates ionization of the surrounding
IGM at earlier times, the background becomes increasingly important, eventually
surpassing the impact of nearby galaxies. These results support an inside-out
progression of reionization, with ionized regions originating around clustered,
star-forming galaxies and gradually extending into underdense regions.'
acknowledgement: "We thank Enrico Garaldi, Rahul Kannan, Aaron Smith, and the THESAN
team for providing us with their simulation data, and Norbert Pirzkal for helpful
advice on our NIRCam observing program.\r\n\r\nThis 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 were taken under
GTO program No. 1243. The specific observations analyzed can be accessed via doi:10.17909/6grb-j154.\r\n\r\nThe
participation of S.J.L. as an Interdisciplinary Scientist in the JWST Flight Science
Working Group 2002-2022 has been supported by the European Space Agency. His earlier
involvement in the development of the JWST 1996–2001 was supported by the Canadian
Space Agency.\r\n\r\nThis work is partially based on observations collected at the
European Organisation for Astronomical Research in the Southern Hemisphere under
ESO programmes 084.A-0360(A), 084.A-0390(A), 086.A-0162(A), 086.A-0574(A), 087.A-0607(A),
089.A-0814(A), 093.A-0707(A), 098.B-0537(A), and 286.A-5025(A). Some of the data
presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit
organization operated as a scientific partnership among the California Institute
of Technology, the University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous financial support
of the W. M. Keck Foundation. This paper includes data gathered with the 6.5 m Magellan
Telescopes located at Las Campanas Observatory, Chile.\r\n\r\nThis work has been
supported by JSPS KAKENHI grant No. JP21K13956 (D.K.). J.M. is supported by the
European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities: JWST - James Webb Space
Telescope (NIRCam), VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), Magellan:Baade
- Magellan I Walter Baade Telescope (FIRE), Keck:I - KECK I Telescope (MOSFIRE),
Keck:II - KECK II Telescope (ESI).\r\n\r\nSoftware: Python, numpy (C. R. Harris
et al. 2020), scipy (P. Virtanen et al. 2020), Astropy (Astropy Collaboration et
al. 2013), Matplotlib (J. D. Hunter 2007), PypeIt (J. X. Prochaska et al. 2019)."
article_number: '280'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Simon J.
full_name: Lilly, Simon J.
last_name: Lilly
- 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: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Anna-Christina
full_name: Eilers, Anna-Christina
last_name: Eilers
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Minghao
full_name: Yue, Minghao
last_name: Yue
- first_name: Bin
full_name: Liu, Bin
last_name: Liu
citation:
ama: Kashino D, Lilly SJ, Matthee JJ, et al. EIGER. VII. The evolving relationship
between galaxies and the intergalactic medium in the final stages of reionization.
The Astrophysical Journal. 2026;997(2). doi:10.3847/1538-4357/ae2799
apa: Kashino, D., Lilly, S. J., Matthee, J. J., Mackenzie, R., Eilers, A.-C., Bordoloi,
R., … Liu, B. (2026). EIGER. VII. The evolving relationship between galaxies and
the intergalactic medium in the final stages of reionization. The Astrophysical
Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae2799
chicago: Kashino, Daichi, Simon J. Lilly, Jorryt J Matthee, Ruari Mackenzie, Anna-Christina
Eilers, Rongmon Bordoloi, Robert A. Simcoe, Rohan P. Naidu, Minghao Yue, and Bin
Liu. “EIGER. VII. The Evolving Relationship between Galaxies and the Intergalactic
Medium in the Final Stages of Reionization.” The Astrophysical Journal.
IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae2799.
ieee: D. Kashino et al., “EIGER. VII. The evolving relationship between galaxies
and the intergalactic medium in the final stages of reionization,” The Astrophysical
Journal, vol. 997, no. 2. IOP Publishing, 2026.
ista: Kashino D, Lilly SJ, Matthee JJ, Mackenzie R, Eilers A-C, Bordoloi R, Simcoe
RA, Naidu RP, Yue M, Liu B. 2026. EIGER. VII. The evolving relationship between
galaxies and the intergalactic medium in the final stages of reionization. The
Astrophysical Journal. 997(2), 280.
mla: Kashino, Daichi, et al. “EIGER. VII. The Evolving Relationship between Galaxies
and the Intergalactic Medium in the Final Stages of Reionization.” The Astrophysical
Journal, vol. 997, no. 2, 280, IOP Publishing, 2026, doi:10.3847/1538-4357/ae2799.
short: D. Kashino, S.J. Lilly, J.J. Matthee, R. Mackenzie, A.-C. Eilers, R. Bordoloi,
R.A. Simcoe, R.P. Naidu, M. Yue, B. Liu, The Astrophysical Journal 997 (2026).
das_tickbox: '0'
date_created: 2026-10-12T12:17:25Z
date_published: 2026-01-28T00:00:00Z
date_updated: 2026-10-14T08:12:05Z
day: '28'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae2799
external_id:
arxiv:
- '2506.03121'
file:
- access_level: open_access
checksum: c33405da323cac352c0d751f0fe6f021
content_type: application/pdf
creator: dernst
date_created: 2026-10-14T08:09:31Z
date_updated: 2026-10-14T08:09:31Z
file_id: '23138'
file_name: 2026_AstrophysicalJour_Kashino.pdf
file_size: 11393255
relation: main_file
success: 1
file_date_updated: 2026-10-14T08:09:31Z
fulldoi: https://doi.org/10.3847/1538-4357/ae2799
has_accepted_license: '1'
intvolume: ' 997'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: EIGER. VII. The evolving relationship between galaxies and the intergalactic
medium in the final stages of reionization
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 997
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23111'
abstract:
- lang: eng
text: In single-molecule electronics, 4,4′-bipyridine is a well-characterized molecule
that serves both as a fundamental testbed for developing experimental methodologies
and showcases the complex behaviors expected from molecular electronic components.
In break junction experiments, it is generally understood to exhibit a high- and
a low-conductance state that are attributed to a tilted and stretched single-molecule
configuration. Despite this established view, we suggest a supramolecular origin
for these conductance states that has not previously been considered. Our findings
indicate that the high- and low-conductance states may arise from the presence
of two molecules and one molecule, respectively, challenging the conventional
interpretation. Using a state-of-the-art machine learning force field called the
neuroevolution potential, we find that the conventional interpretation of a tilted
and stretched configuration is inconsistent with our simulations. Instead, our
results suggest that the presence of two molecules promotes junction geometries
and gold rearrangements that stabilize a high-conductance state whose transmission
exceeds twice that of the low-conductance state. Furthermore, we compare this
interpretation to the existing literature of diverse experimental data on 4,4′-bipyridine
in break junctions and find that it is consistent with the broader body of experimental
evidence. Our results highlight the structural complexity of molecular behavior
within break junctions, suggesting even more complex dynamics than originally
anticipated. In this light, a broader examination of the dynamics of molecules
in single-molecule break junctions with machine learning-assisted molecular dynamics
is warranted.
acknowledgement: The authors thank Latha Venkataraman for fruitful discussions about
the main results of this paper. This project has received funding from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
programme (grant agreement No. 865870). Junfeng Lin thanks the Institute of Science
and Technology Austria for support.
article_processing_charge: Yes
article_type: original
author:
- first_name: William
full_name: Bro-Jørgensen, William
last_name: Bro-Jørgensen
- first_name: Junfeng
full_name: Lin, Junfeng
id: a25c6e57-a657-11ef-8665-c4906b069ffc
last_name: Lin
- first_name: Joseph M.
full_name: Hamill, Joseph M.
last_name: Hamill
- first_name: Gemma C.
full_name: Solomon, Gemma C.
last_name: Solomon
chemrxivid: 1
citation:
ama: 'Bro-Jørgensen W, Lin J, Hamill JM, Solomon GC. Machine learning-enhanced molecular
dynamics of 4,4′-bipyridinein a break junction: A supramolecular origin of the
high conductance. ACS Nanoscience Au. 2026;6(4):662-673. doi:10.1021/acsnanoscienceau.6c00052'
apa: 'Bro-Jørgensen, W., Lin, J., Hamill, J. M., & Solomon, G. C. (2026). Machine
learning-enhanced molecular dynamics of 4,4′-bipyridinein a break junction: A
supramolecular origin of the high conductance. ACS Nanoscience Au. American
Chemical Society. https://doi.org/10.1021/acsnanoscienceau.6c00052'
chicago: 'Bro-Jørgensen, William, Junfeng Lin, Joseph M. Hamill, and Gemma C. Solomon.
“Machine Learning-Enhanced Molecular Dynamics of 4,4′-Bipyridinein a Break Junction:
A Supramolecular Origin of the High Conductance.” ACS Nanoscience Au. American
Chemical Society, 2026. https://doi.org/10.1021/acsnanoscienceau.6c00052.'
ieee: 'W. Bro-Jørgensen, J. Lin, J. M. Hamill, and G. C. Solomon, “Machine learning-enhanced
molecular dynamics of 4,4′-bipyridinein a break junction: A supramolecular origin
of the high conductance,” ACS Nanoscience Au, vol. 6, no. 4. American Chemical
Society, pp. 662–673, 2026.'
ista: 'Bro-Jørgensen W, Lin J, Hamill JM, Solomon GC. 2026. Machine learning-enhanced
molecular dynamics of 4,4′-bipyridinein a break junction: A supramolecular origin
of the high conductance. ACS Nanoscience Au. 6(4), 662–673.'
mla: 'Bro-Jørgensen, William, et al. “Machine Learning-Enhanced Molecular Dynamics
of 4,4′-Bipyridinein a Break Junction: A Supramolecular Origin of the High Conductance.”
ACS Nanoscience Au, vol. 6, no. 4, American Chemical Society, 2026, pp.
662–73, doi:10.1021/acsnanoscienceau.6c00052.'
short: W. Bro-Jørgensen, J. Lin, J.M. Hamill, G.C. Solomon, ACS Nanoscience Au 6
(2026) 662–673.
das_tickbox: '1'
dataavailabilitystatement: 'Input and output files for the MD trajectories are available
in our ioChem-BD repository (85) and can be accessed here: 10.19061/iochem-bd-9-14.
Raw data for all MD trajectories are available here: 10.17894/ucph.78aa9ec7-d132-447f-aaf0-8e6e5d59d8ea'
date_created: 2026-10-12T12:01:45Z
date_published: 2026-08-19T00:00:00Z
date_updated: 2026-10-14T07:09:01Z
day: '19'
ddc:
- '540'
department:
- _id: LaVe
doi: 10.1021/acsnanoscienceau.6c00052
external_id:
chemrxivid:
- 10.26434/chemrxiv-2025-wt6rd/v2
pmid:
- '42630769'
file:
- access_level: open_access
checksum: 87cc93f52ba508a7d19d7c03e9ef55cb
content_type: application/pdf
creator: dernst
date_created: 2026-10-14T07:07:43Z
date_updated: 2026-10-14T07:07:43Z
file_id: '23135'
file_name: 2026_ACSNanoscienceAu_BroJorgensen.pdf
file_size: 6463446
relation: main_file
success: 1
file_date_updated: 2026-10-14T07:07:43Z
fulldoi: https://doi.org/10.1021/acsnanoscienceau.6c00052
has_accepted_license: '1'
intvolume: ' 6'
issue: '4'
language:
- iso: eng
month: '08'
oa: 1
oa_version: Published Version
page: 662-673
pmid: 1
publication: ACS Nanoscience Au
publication_identifier:
issn:
- 2694-2496
publication_status: published
publisher: American Chemical Society
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: 'Machine learning-enhanced molecular dynamics of 4,4′-bipyridinein a break
junction: A supramolecular origin of the high conductance'
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: 6
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23116'
abstract:
- lang: eng
text: The Legacy Survey of Space and Time (LSST) is expected to observe up to ∼100
million quasars in the next decade. In this work, we show that it is possible
to use such data to measure the characteristic frequency evolution of a “chirp”
induced by gravitational waves, which can serve as robust evidence for the presence
of a compact supermassive black hole binary. Following the LSST specifications,
we generate mock lightcurves consisting of (i) a post-Newtonian chirp produced
by orbital motion through, e.g., relativistic Doppler boosting, (ii) a damped
random walk representing intrinsic quasar variability, and (iii) Gaussian photometric
errors, while assuming nonuniform observations with extended gaps over a period
of 10 yr. Through a fully Bayesian analysis, we show that we can simultaneously
measure the chirp and noise parameters with little degeneracy between the two.
For chirp signals with an amplitude of A = 0.5 mag and a range of times to merger
(tm = 15–104 yr), we can typically measure a nonzero amplitude and positive frequency
derivative with over 5σ credibility. For binaries with tm = 50 yr, we achieve
3σ (5σ) confidence that the signal is chirping for A ≳ 0.1 (A > 0.2). The median
runtime of our analysis is 5.6 minutes, with a minimum as low as 35 s, making
it scalable to a large number of lightcurves. This implies that LSST could, on
its own, establish the presence of a compact supermassive black hole binary, and
thus discover gravitational wave sources detectable by LISA and by Pulsar Timing
Arrays.
acknowledgement: "C.X. thanks the Department of Astronomy of Columbia University,
where the majority of this work was performed. Z.H. thanks the Center for Computational
Astrophysics (CCA) at the Flatiron Institute for their hospitality during a sabbatical
stay, where this work was initiated. The Flatiron Institute is a division of the
Simons Foundation. This work was supported in part by NASA’s LISA Preparatory Science
Program (LPS) through grant 80NSSC24K0440 and by NASA Astrophysics Theory Program
(ATP) grant 80NSSC22K0822. The authors thank the anonymous referee for helpful feedback,
which improved this manuscript. We also thank Prof. Brian D. Metzger, Prof. David
Schiminovich, and Prof. Kishalay De for valuable discussions.\r\n\r\nSoftware: numpyro
(E. Bingham et al. 2019; D. Phan et al. 2019); celerite2 (D. Foreman-Mackey et al.
2017; D. Foreman-Mackey 2018); Python (G. Van Rossum & F. L. Drake 2009); The Software
Citation Station (T. Wagg & F. S. Broekgaarden 2024; T. Wagg et al. 2024)."
article_number: '149'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Chengcheng
full_name: Xin, Chengcheng
last_name: Xin
- first_name: Maximiliano
full_name: Isi, Maximiliano
last_name: Isi
- first_name: Will M.
full_name: Farr, Will M.
last_name: Farr
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
citation:
ama: Xin C, Isi M, Farr WM, Haiman Z. Identifying compact chirping SMBHBs in LSST
using Bayesian analysis. The Astrophysical Journal. 2026;999(1). doi:10.3847/1538-4357/ae40b3
apa: Xin, C., Isi, M., Farr, W. M., & Haiman, Z. (2026). Identifying compact
chirping SMBHBs in LSST using Bayesian analysis. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ae40b3
chicago: Xin, Chengcheng, Maximiliano Isi, Will M. Farr, and Zoltán Haiman. “Identifying
Compact Chirping SMBHBs in LSST Using Bayesian Analysis.” The Astrophysical
Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae40b3.
ieee: C. Xin, M. Isi, W. M. Farr, and Z. Haiman, “Identifying compact chirping SMBHBs
in LSST using Bayesian analysis,” The Astrophysical Journal, vol. 999,
no. 1. IOP Publishing, 2026.
ista: Xin C, Isi M, Farr WM, Haiman Z. 2026. Identifying compact chirping SMBHBs
in LSST using Bayesian analysis. The Astrophysical Journal. 999(1), 149.
mla: Xin, Chengcheng, et al. “Identifying Compact Chirping SMBHBs in LSST Using
Bayesian Analysis.” The Astrophysical Journal, vol. 999, no. 1, 149, IOP
Publishing, 2026, doi:10.3847/1538-4357/ae40b3.
short: C. Xin, M. Isi, W.M. Farr, Z. Haiman, The Astrophysical Journal 999 (2026).
das_tickbox: '0'
date_created: 2026-10-12T12:16:19Z
date_published: 2026-02-27T00:00:00Z
date_updated: 2026-10-14T08:05:50Z
day: '27'
ddc:
- '520'
department:
- _id: ZoHa
doi: 10.3847/1538-4357/ae40b3
external_id:
arxiv:
- '2506.10846'
file:
- access_level: open_access
checksum: 250ede2883cf2e3ec9ac8c36b1857d40
content_type: application/pdf
creator: dernst
date_created: 2026-10-14T08:02:55Z
date_updated: 2026-10-14T08:02:55Z
file_id: '23137'
file_name: 2026_AstrophysicalJour_Xin.pdf
file_size: 4415354
relation: main_file
success: 1
file_date_updated: 2026-10-14T08:02:55Z
fulldoi: https://doi.org/10.3847/1538-4357/ae40b3
has_accepted_license: '1'
intvolume: ' 999'
issue: '1'
language:
- iso: eng
month: '02'
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: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Identifying compact chirping SMBHBs in LSST using Bayesian analysis
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: 999
year: '2026'
...
---
OA_type: closed access
_id: '23096'
abstract:
- lang: eng
text: The first generation of stars, known as population III (Pop III), formed from
primordial gas consisting solely of hydrogen and helium and is believed to have
emerged only a few hundred million years after the Big Bang. Detecting the chemical
enrichment of metal-poor circumgalactic gas offers a promising way to trace the
enrichment signature of Pop III stars. Along the sight line to the quasar SDSS
J0100+2802, a metal absorber at z = 5.945, showing over-abundant carbon and silicon
compared with solar, has been reported to be consistent with the enrichment pattern
of Pop III stars. Here, using data recorded by the James Webb Space Telescope,
we report the discovery of an unusually metal-poor galaxy overdensity of 17 members
(mean metallicity ~3% of solar) near this metal absorber, which is ~0.4 dex more
metal-poor than coeval galaxies in similarly overdense environments. This less
chemically evolved system may have provided favourable conditions for preserving
the absorption signatures of Pop III enrichment. We infer a minimum dark matter
halo mass of log(Mh,min/M⊙) = 10.68+0.93 −1.72, supporting late-time Pop III formation
at the outskirts of atomic hydrogen cooling haloes. Our findings open a promising
observational pathway to identifying the chemical imprints of the first stars
and constrain the conditions for their formation.
acknowledgement: This work is based on observations made with the NASA/ESA/CSA JWST,
associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope,
associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and
096.A-0095. We acknowledge the University of Copenhagen for giving this project
access to the LUMI supercomputer owned by the EuroHPC Joint Undertaking and hosted
by CSC (Finland) and the LUMI consortium through Denmark. Z.L. thanks Y. Ren for
helpful discussions. We thank O. Zier, A. Smith, R. Kannan and E. Garaldi for helpful
discussions about the THESAN-ZOOM simulation. Z.L. acknowledges the fellowship from
the Cosmic Dawn Center, which is funded by the Danish National Research Foundation
under grant no. 140. K.K. acknowledges support from the Villum Foundation (71574).
L.C. is supported by DFF/Independent Research Fund Denmark (2032-00071). V.D. acknowledges
financial support from the Bando Ricerca Fondamentale INAF 2022 Large Grant XQR-30.
A.V. acknowledges funding from the Cosmic Frontier Center and the University of
Texas at Austin’s College of Natural Sciences. S. Zou acknowledges support from
the Chinese Academy of Sciences (E5295401).
article_processing_charge: No
article_type: original
author:
- first_name: Zihao
full_name: Li, Zihao
last_name: Li
- first_name: Koki
full_name: Kakiichi, Koki
last_name: Kakiichi
- first_name: Lise
full_name: Christensen, Lise
last_name: Christensen
- first_name: Zheng
full_name: Cai, Zheng
last_name: Cai
- first_name: Valentina
full_name: D’Odorico, Valentina
last_name: D’Odorico
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Trystyn A.M.
full_name: Berg, Trystyn A.M.
last_name: Berg
- first_name: Irene
full_name: Vanni, Irene
last_name: Vanni
- first_name: Stefania
full_name: Salvadori, Stefania
last_name: Salvadori
- first_name: Alessandra
full_name: Venditti, Alessandra
last_name: Venditti
- first_name: Shiwu
full_name: Zhang, Shiwu
last_name: Zhang
- first_name: Sarah E.I.
full_name: Bosman, Sarah E.I.
last_name: Bosman
- first_name: Eduardo
full_name: Bañados, Eduardo
last_name: Bañados
- first_name: Frederick B.
full_name: Davies, Frederick B.
last_name: Davies
- first_name: Xiaohui
full_name: Fan, Xiaohui
last_name: Fan
- first_name: Hyunsung D.
full_name: Jun, Hyunsung D.
last_name: Jun
- first_name: Xiangyu
full_name: Jin, Xiangyu
last_name: Jin
- first_name: Mingyu
full_name: Li, Mingyu
last_name: Li
- first_name: Sofía
full_name: Rojas-Ruiz, Sofía
last_name: Rojas-Ruiz
- first_name: Feige
full_name: Wang, Feige
last_name: Wang
- first_name: Jinyi
full_name: Yang, Jinyi
last_name: Yang
- first_name: Siwei
full_name: Zou, Siwei
last_name: Zou
- first_name: Huanian
full_name: Zhang, Huanian
last_name: Zhang
- first_name: Yongda
full_name: Zhu, Yongda
last_name: Zhu
citation:
ama: Li Z, Kakiichi K, Christensen L, et al. First-star imprints in a metal-poor
galaxy overdensity near the end of reionization. Nature Astronomy. 2026.
doi:10.1038/s41550-026-02993-5
apa: Li, Z., Kakiichi, K., Christensen, L., Cai, Z., D’Odorico, V., Matthee, J.
J., … Zhu, Y. (2026). First-star imprints in a metal-poor galaxy overdensity near
the end of reionization. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-026-02993-5
chicago: Li, Zihao, Koki Kakiichi, Lise Christensen, Zheng Cai, Valentina D’Odorico,
Jorryt J Matthee, Daichi Kashino, et al. “First-Star Imprints in a Metal-Poor
Galaxy Overdensity near the End of Reionization.” Nature Astronomy. Springer
Nature, 2026. https://doi.org/10.1038/s41550-026-02993-5.
ieee: Z. Li et al., “First-star imprints in a metal-poor galaxy overdensity
near the end of reionization,” Nature Astronomy. Springer Nature, 2026.
ista: Li Z, Kakiichi K, Christensen L, Cai Z, D’Odorico V, Matthee JJ, Kashino D,
Bordoloi R, Mackenzie R, Berg TAM, Vanni I, Salvadori S, Venditti A, Zhang S,
Bosman SEI, Bañados E, Davies FB, Fan X, Jun HD, Jin X, Li M, Rojas-Ruiz S, Wang
F, Yang J, Zou S, Zhang H, Zhu Y. 2026. First-star imprints in a metal-poor galaxy
overdensity near the end of reionization. Nature Astronomy.
mla: Li, Zihao, et al. “First-Star Imprints in a Metal-Poor Galaxy Overdensity near
the End of Reionization.” Nature Astronomy, Springer Nature, 2026, doi:10.1038/s41550-026-02993-5.
short: Z. Li, K. Kakiichi, L. Christensen, Z. Cai, V. D’Odorico, J.J. Matthee, D.
Kashino, R. Bordoloi, R. Mackenzie, T.A.M. Berg, I. Vanni, S. Salvadori, A. Venditti,
S. Zhang, S.E.I. Bosman, E. Bañados, F.B. Davies, X. Fan, H.D. Jun, X. Jin, M.
Li, S. Rojas-Ruiz, F. Wang, J. Yang, S. Zou, H. Zhang, Y. Zhu, Nature Astronomy
(2026).
das_tickbox: '1'
dataavailabilitystatement: This work is based on observations made with the NASA/ESA/CSA
JWST, associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope
associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and
096.A-0095. The JWST data are available via the Mikulski Archive for Space Telescopes
at http://archive.stsci.edu under JWST programmes GO-2078 (ref. 127) and GO-1243
(ref. 128). The metal absorber catalogue of XQR-30 is available via GitHub at https://github.com/XQR-30/Metal-catalogue.
The [O III] emitter catalogue from the EIGER survey is available via GitHub at https://eiger-jwst.github.io/data.html.
Other data presented in this paper are available upon request to the corresponding
author.
date_created: 2026-10-11T22:02:07Z
date_published: 2026-09-29T00:00:00Z
date_updated: 2026-10-14T06:42:17Z
day: '29'
department:
- _id: JoMa
doi: 10.1038/s41550-026-02993-5
fulldoi: https://doi.org/10.1038/s41550-026-02993-5
language:
- iso: eng
month: '09'
oa_version: None
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: First-star imprints in a metal-poor galaxy overdensity near the end of reionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '23112'
abstract:
- lang: eng
text: We study the joint spectral properties of two coupled random matrices H(1)
and H(2), which are either real symmetric or complex Hermitian. The entries of
these matrices exhibit polynomially decaying correlations, both within each matrix
and between them. Surprisingly, we find that under extremely weak decorrelation
condition, permitting H(1) and H(2) to be almost fully correlated, the fluctuations
of their individual eigenvalues in the bulk of the spectrum are still asymptotically
independent. Furthermore, we demonstrate that this decorrelation condition is
optimal.
acknowledgement: The author is grateful to László Erdős and Giorgio Cipolloni for
suggesting the project and fruitful discussions. The author was supported by the
ERC Advanced Grant “RMTBeyond” No. 101020331.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Oleksii
full_name: Kolupaiev, Oleksii
id: 149b70d4-896a-11ed-bdf8-8c63fd44ca61
last_name: Kolupaiev
orcid: 0000-0003-1491-4623
citation:
ama: Kolupaiev O. Spectral independence of almost fully correlated random matrices.
Bernoulli. 2026;32(4):2999-3023. doi:10.3150/26-bej1976
apa: Kolupaiev, O. (2026). Spectral independence of almost fully correlated random
matrices. Bernoulli. Bernoulli Society for Mathematical Statistics and
Probability. https://doi.org/10.3150/26-bej1976
chicago: Kolupaiev, Oleksii. “Spectral Independence of Almost Fully Correlated Random
Matrices.” Bernoulli. Bernoulli Society for Mathematical Statistics and
Probability, 2026. https://doi.org/10.3150/26-bej1976.
ieee: O. Kolupaiev, “Spectral independence of almost fully correlated random matrices,”
Bernoulli, vol. 32, no. 4. Bernoulli Society for Mathematical Statistics
and Probability, pp. 2999–3023, 2026.
ista: Kolupaiev O. 2026. Spectral independence of almost fully correlated random
matrices. Bernoulli. 32(4), 2999–3023.
mla: Kolupaiev, Oleksii. “Spectral Independence of Almost Fully Correlated Random
Matrices.” Bernoulli, vol. 32, no. 4, Bernoulli Society for Mathematical
Statistics and Probability, 2026, pp. 2999–3023, doi:10.3150/26-bej1976.
short: O. Kolupaiev, Bernoulli 32 (2026) 2999–3023.
corr_author: '1'
das_tickbox: '0'
date_created: 2026-10-12T12:04:45Z
date_published: 2026-11-01T00:00:00Z
date_updated: 2026-10-14T07:34:08Z
day: '01'
department:
- _id: LaEr
doi: 10.3150/26-bej1976
ec_funded: 1
external_id:
arxiv:
- '2503.21472'
fulldoi: https://doi.org/10.3150/26-bej1976
intvolume: ' 32'
issue: '4'
keyword:
- correlated random matrix
- eigenvalue perturbation theory
- Local law
- Wigner-type matrix
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2503.21472
month: '11'
oa: 1
oa_version: Preprint
page: 2999-3023
project:
- _id: 62796744-2b32-11ec-9570-940b20777f1d
call_identifier: H2020
grant_number: '101020331'
name: Random matrices beyond Wigner-Dyson-Mehta
publication: Bernoulli
publication_identifier:
issn:
- 1350-7265
publication_status: published
publisher: Bernoulli Society for Mathematical Statistics and Probability
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: no
title: Spectral independence of almost fully correlated random matrices
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 32
year: '2026'
...
---
OA_place: publisher
OA_type: free access
_id: '23060'
article_processing_charge: No
article_type: editorial
author:
- first_name: Chiara
full_name: Ziletti, Chiara
id: D865714E-FA4E-11E9-B85B-F5C5E5697425
last_name: Ziletti
citation:
ama: Ziletti C. International Council on Archives (ICA) Barcelona Congress 2025,
27-30 October 2025. Scrinium. 2026;80:181-186.
apa: 'Ziletti, C. (2026). International Council on Archives (ICA) Barcelona Congress
2025, 27-30 October 2025. Scrinium. Barcelona, Spain: Anton Pustet Verlag.'
chicago: Ziletti, Chiara. “International Council on Archives (ICA) Barcelona Congress
2025, 27-30 October 2025.” Scrinium. Anton Pustet Verlag, 2026.
ieee: C. Ziletti, “International Council on Archives (ICA) Barcelona Congress 2025,
27-30 October 2025,” Scrinium, vol. 80. Anton Pustet Verlag, pp. 181–186,
2026.
ista: Ziletti C. 2026. International Council on Archives (ICA) Barcelona Congress
2025, 27-30 October 2025. Scrinium. 80, 181–186.
mla: Ziletti, Chiara. “International Council on Archives (ICA) Barcelona Congress
2025, 27-30 October 2025.” Scrinium, vol. 80, Anton Pustet Verlag, 2026,
pp. 181–86.
short: C. Ziletti, Scrinium 80 (2026) 181–186.
conference:
end_date: 2025-10-30
location: Barcelona, Spain
name: 'ICA: International Council on Archives'
start_date: 2025-10-27
corr_author: '1'
date_created: 2026-10-05T14:18:42Z
date_published: 2026-10-01T00:00:00Z
date_updated: 2026-10-14T06:56:51Z
day: '01'
ddc:
- '020'
department:
- _id: E-Lib
file:
- access_level: open_access
checksum: e6fa3953b73e1f900a52a525e82c0685
content_type: application/pdf
creator: cziletti
date_created: 2026-10-12T09:48:09Z
date_updated: 2026-10-12T09:48:09Z
file_id: '23106'
file_name: Scrinium_Ziletti.pdf
file_size: 555357
relation: main_file
success: 1
file_date_updated: 2026-10-12T09:48:09Z
has_accepted_license: '1'
intvolume: ' 80'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
page: 181-186
publication: Scrinium
publication_identifier:
isbn:
- '9783702512187'
issn:
- 1012-0327
publication_status: published
publisher: Anton Pustet Verlag
status: public
title: International Council on Archives (ICA) Barcelona Congress 2025, 27-30 October
2025
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 80
year: '2026'
...