---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21485'
abstract:
- lang: eng
text: Insulating oxides are among the most abundant solid materials in the universe1,2,3.
Of the many ways in which they influence natural phenomena, perhaps the most consequential
is their capacity to transfer electrical charge during contact4,5,6,7,8,9,10—which
occurs even between samples of the same oxide—yet the symmetry-breaking parameter
that causes this remains unidentified11,12. Here we show that adventitious carbonaceous
molecules adsorbed from the environment are the symmetry-breaking factor in same-material
oxide contact electrification (CE). We use acoustic levitation to measure charge
exchange between a sphere and a plate composed of identical amorphous silicon
dioxide (SiO2). Although charging polarity is random for co-prepared samples,
we control it with baking or plasma treatment. Observing the charge-exchange relaxation
afterwards, we see dynamics over a timescale of hours and connect this directly
to the presence of adventitious carbon with time-of-flight mass spectrometry,
low-energy ion scattering and infrared spectroscopy. Going further, we confirm
that adventitious carbon can even determine charge exchange among different oxides.
Our results identify the symmetry-breaking parameter that causes insulating oxides
to exchange charge in settings ranging from desert sands4 to volcanic plumes5,6,
while simultaneously highlighting an overlooked factor in CE more broadly.
acknowledged_ssus:
- _id: M-Shop
- _id: NanoFab
- _id: ScienComp
- _id: LifeSc
acknowledgement: This project has received support from the European Research Council
(ERC) under the European Union’s Horizon 2020 research and innovation programme
(grant agreement no. 949120) and from the Marie Skłodowska-Curie programme (grant
agreement no. 754411). We acknowledge the state of Lower Austria and the European
Regional Development Fund under grant no. WST3-F-542638/004-2021. N.M. acknowledges
support from grant Fondecyt 1221597. G.G. is a Serra Húnter fellow. This research
was supported by the Scientific Service Units of the Institute of Science and Technology
Austria through resources provided by the Miba Machine Shop, Nanofabrication Facility,
Scientific Computing facility and Lab Support Facility. We thank the Modic group
for the use of the Laue camera, T. Zauner for the photography of the experimental
set-up and R. Möller for insightful discussions. 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: Galien M
full_name: Grosjean, Galien M
id: 0C5FDA4A-9CF6-11E9-8939-FF05E6697425
last_name: Grosjean
orcid: 0000-0001-5154-417X
- first_name: Markus
full_name: Ostermann, Markus
last_name: Ostermann
- first_name: Markus
full_name: Sauer, Markus
last_name: Sauer
- first_name: Michael
full_name: Hahn, Michael
last_name: Hahn
- first_name: Christian M.
full_name: Pichler, Christian M.
last_name: Pichler
- first_name: Florian
full_name: Fahrnberger, Florian
last_name: Fahrnberger
- first_name: Felix
full_name: Pertl, Felix
id: 6313aec0-15b2-11ec-abd3-ed67d16139af
last_name: Pertl
orcid: 0000-0003-0463-5794
- first_name: Daniel
full_name: Balazs, Daniel
id: 302BADF6-85FC-11EA-9E3B-B9493DDC885E
last_name: Balazs
orcid: 0000-0001-7597-043X
- first_name: Mason M.
full_name: Link, Mason M.
last_name: Link
- first_name: Seong H.
full_name: Kim, Seong H.
last_name: Kim
- first_name: Devin L.
full_name: Schrader, Devin L.
last_name: Schrader
- first_name: Adriana
full_name: Blanco, Adriana
last_name: Blanco
- first_name: Francisco
full_name: Gracia, Francisco
last_name: Gracia
- first_name: Nicolás
full_name: Mujica, Nicolás
last_name: Mujica
- first_name: Scott R
full_name: Waitukaitis, Scott R
id: 3A1FFC16-F248-11E8-B48F-1D18A9856A87
last_name: Waitukaitis
orcid: 0000-0002-2299-3176
citation:
ama: Grosjean GM, Ostermann M, Sauer M, et al. Adventitious carbon breaks symmetry
in oxide contact electrification. Nature. 2026;651(8106):626-631. doi:10.1038/s41586-025-10088-w
apa: Grosjean, G. M., Ostermann, M., Sauer, M., Hahn, M., Pichler, C. M., Fahrnberger,
F., … Waitukaitis, S. R. (2026). Adventitious carbon breaks symmetry in oxide
contact electrification. Nature. Springer Nature. https://doi.org/10.1038/s41586-025-10088-w
chicago: Grosjean, Galien M, Markus Ostermann, Markus Sauer, Michael Hahn, Christian
M. Pichler, Florian Fahrnberger, Felix Pertl, et al. “Adventitious Carbon Breaks
Symmetry in Oxide Contact Electrification.” Nature. Springer Nature, 2026.
https://doi.org/10.1038/s41586-025-10088-w.
ieee: G. M. Grosjean et al., “Adventitious carbon breaks symmetry in oxide
contact electrification,” Nature, vol. 651, no. 8106. Springer Nature,
pp. 626–631, 2026.
ista: Grosjean GM, Ostermann M, Sauer M, Hahn M, Pichler CM, Fahrnberger F, Pertl
F, Balazs D, Link MM, Kim SH, Schrader DL, Blanco A, Gracia F, Mujica N, Waitukaitis
SR. 2026. Adventitious carbon breaks symmetry in oxide contact electrification.
Nature. 651(8106), 626–631.
mla: Grosjean, Galien M., et al. “Adventitious Carbon Breaks Symmetry in Oxide Contact
Electrification.” Nature, vol. 651, no. 8106, Springer Nature, 2026, pp.
626–31, doi:10.1038/s41586-025-10088-w.
short: G.M. Grosjean, M. Ostermann, M. Sauer, M. Hahn, C.M. Pichler, F. Fahrnberger,
F. Pertl, D. Balazs, M.M. Link, S.H. Kim, D.L. Schrader, A. Blanco, F. Gracia,
N. Mujica, S.R. Waitukaitis, Nature 651 (2026) 626–631.
corr_author: '1'
date_created: 2026-03-23T15:04:00Z
date_published: 2026-03-18T00:00:00Z
date_updated: 2026-04-28T12:06:01Z
day: '18'
ddc:
- '540'
department:
- _id: ScWa
- _id: GradSch
- _id: LifeSc
doi: 10.1038/s41586-025-10088-w
ec_funded: 1
external_id:
pmid:
- '41851325'
file:
- access_level: open_access
checksum: dafef9ed575b44be4263e948a47ae056
content_type: application/pdf
creator: dernst
date_created: 2026-03-24T06:57:08Z
date_updated: 2026-03-24T06:57:08Z
file_id: '21494'
file_name: 2026_Nature_Grosjean.pdf
file_size: 12245694
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success: 1
file_date_updated: 2026-03-24T06:57:08Z
fulldoi: https://doi.org/10.1038/s41586-025-10088-w
has_accepted_license: '1'
intvolume: ' 651'
issue: '8106'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
page: 626-631
pmid: 1
project:
- _id: 0aa60e99-070f-11eb-9043-a6de6bdc3afa
call_identifier: H2020
grant_number: '949120'
name: 'Tribocharge: a multi-scale approach to an enduring problem in physics'
- _id: 260C2330-B435-11E9-9278-68D0E5697425
call_identifier: H2020
grant_number: '754411'
name: ISTplus - Postdoctoral Fellowships
publication: Nature
publication_identifier:
eissn:
- 1476-4687
issn:
- 0028-0836
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
related_material:
link:
- description: News on ISTA website
relation: press_release
url: https://ista.ac.at/en/news/colliding-dust-and-the-sparks-of-creation/
status: public
title: Adventitious carbon breaks symmetry in oxide contact electrification
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 651
year: '2026'
...
---
OA_place: publisher
_id: '21651'
abstract:
- lang: eng
text: "Blockchains enable distributed consensus in permissionless settings, where
participants\r\nare unknown, dynamically changing, and do not trust each other.
While Bitcoin,\r\nbased on Proof-of-Work (PoW), was the first protocol in this
model, significant\r\nresearch has focused on permissionless protocols using alternative
physical resources,\r\nspecifically Proof-of-Space (PoSpace) and Verifiable Delay
Functions (VDFs). This\r\nthesis investigates the theoretical limits and design
space of longest-chain protocols in\r\nthe fully permissionless and dynamically
available settings using these three resources.\r\nFirst, we address the feasibility
of blockchains relying solely on storage as a resource.\r\nWe prove a fundamental
impossibility result: there exists no secure longest-chain\r\nprotocol based exclusively
on Proof-of-Space in the fully permissionless or dynamically\r\navailable settings.
Further, we quantify the adversarial capabilities required to execute\r\na double-spend
attack. Our result formally justifies the necessity of coupling PoSpace\r\nwith
time-dependent primitives (such as VDFs) or to move to less permissive settings\r\n(quasi-permissionless
or permissioned) to ensure security.\r\nSecond, we generalize Nakamoto-like heaviest
chain consensus to protocols utilizing\r\ncombinations of multiple physical resources.
We analyze chain selection rules governed\r\nby a weight function Γ(S, V,W), which
assigns weight to blocks based on recorded\r\nSpace (S), VDF speed (V ), and Work
(W). We provide a complete classification\r\nof secure weight functions, proving
that a weight function is secure against private\r\ndouble-spend attacks if and
only if it is homogeneous in the timed resources (V,W)\r\nand sub-homogeneous
in S. This framework unifies existing protocols like Bitcoin and\r\nChia under
a single theoretical model and provides a powerful tool for designing new\r\nlongest-chain
blockchains from a mix of physical resources."
alternative_title:
- ISTA Thesis
article_processing_charge: No
author:
- first_name: Mirza Ahad
full_name: Baig, Mirza Ahad
id: 3EDE6DE4-AA5A-11E9-986D-341CE6697425
last_name: Baig
citation:
ama: Baig MA. On secure chain selection rules from physical resources in a permissionless
setting. 2026. doi:10.15479/AT-ISTA-21651
apa: Baig, M. A. (2026). On secure chain selection rules from physical resources
in a permissionless setting. Institute of Science and Technology Austria.
https://doi.org/10.15479/AT-ISTA-21651
chicago: Baig, Mirza Ahad. “On Secure Chain Selection Rules from Physical Resources
in a Permissionless Setting.” Institute of Science and Technology Austria, 2026.
https://doi.org/10.15479/AT-ISTA-21651.
ieee: M. A. Baig, “On secure chain selection rules from physical resources in a
permissionless setting,” Institute of Science and Technology Austria, 2026.
ista: Baig MA. 2026. On secure chain selection rules from physical resources in
a permissionless setting. Institute of Science and Technology Austria.
mla: Baig, Mirza Ahad. On Secure Chain Selection Rules from Physical Resources
in a Permissionless Setting. Institute of Science and Technology Austria,
2026, doi:10.15479/AT-ISTA-21651.
short: M.A. Baig, On Secure Chain Selection Rules from Physical Resources in a Permissionless
Setting, Institute of Science and Technology Austria, 2026.
corr_author: '1'
date_created: 2026-04-02T09:31:34Z
date_published: 2026-03-04T00:00:00Z
date_updated: 2026-04-15T08:45:19Z
day: '04'
ddc:
- '000'
degree_awarded: PhD
department:
- _id: GradSch
- _id: KrPi
doi: 10.15479/AT-ISTA-21651
file:
- access_level: closed
checksum: c3986dba90653dac97adba662ebff238
content_type: application/x-zip-compressed
creator: mbaig
date_created: 2026-04-03T17:28:48Z
date_updated: 2026-04-13T08:24:13Z
file_id: '21655'
file_name: PhD-Thesis-Mirza-Ahad-Baig - Library Submission.zip
file_size: 139353434
relation: source_file
- access_level: open_access
checksum: 292a5989262521f7c145a109d1f348cb
content_type: application/pdf
creator: mbaig
date_created: 2026-04-03T17:29:30Z
date_updated: 2026-04-15T07:37:25Z
file_id: '21656'
file_name: 2026_Baig_Mirza_Ahad_Thesis.pdf
file_size: 1942037
relation: main_file
file_date_updated: 2026-04-15T07:37:25Z
fulldoi: https://doi.org/10.15479/AT-ISTA-21651
has_accepted_license: '1'
language:
- iso: eng
license: https://creativecommons.org/licenses/by-nc-sa/4.0/
month: '03'
oa: 1
oa_version: Published Version
publication_identifier:
isbn:
- 978-3-99078-078-7
issn:
- 2663-337X
publication_status: published
publisher: Institute of Science and Technology Austria
related_material:
record:
- id: '21134'
relation: part_of_dissertation
status: public
- id: '20587'
relation: part_of_dissertation
status: public
status: public
supervisor:
- first_name: Krzysztof Z
full_name: Pietrzak, Krzysztof Z
id: 3E04A7AA-F248-11E8-B48F-1D18A9856A87
last_name: Pietrzak
orcid: 0000-0002-9139-1654
title: On secure chain selection rules from physical resources in a permissionless
setting
tmp:
image: /images/cc_by_nc_sa.png
legal_code_url: https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode
name: Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC
BY-NC-SA 4.0)
short: CC BY-NC-SA (4.0)
type: dissertation
user_id: 8b945eb4-e2f2-11eb-945a-df72226e66a9
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '21737'
abstract:
- lang: eng
text: In calculus, l'Hopital's rule provides a simple way to evaluate the limits
of quotient functions when both the numerator and denominator vanish. But what
happens when we move beyond real functions on a real interval? In this article,
we study when the quotient of two complex-valued functions in higher dimension
can be defined continuously at the points where both functions vanish. Surprisingly,
the answer is far subtler than in the real-valued setting. We provide a complete
characterization for the continuity of the quotient function. We also point out
why extending this result to smoother quotients remains an intriguing challenge.
acknowledgement: "This project was funded in part by the European Research Council
(ERC Consolidator Grant 101045083 CoDiNA) and the National Science Foundation CAREER
Award 2239062.\r\n"
article_number: '2602.09958'
article_processing_charge: No
arxiv: 1
author:
- first_name: Albert
full_name: Chern, Albert
last_name: Chern
- first_name: Sadashige
full_name: Ishida, Sadashige
id: 6F7C4B96-A8E9-11E9-A7CA-09ECE5697425
last_name: Ishida
orcid: 0000-0002-3121-3100
citation:
ama: Chern A, Ishida S. L’Hopital rules for complex-valued functions in higher dimensions.
arXiv. doi:10.48550/ARXIV.2602.09958
apa: Chern, A., & Ishida, S. (n.d.). L’Hopital rules for complex-valued functions
in higher dimensions. arXiv. https://doi.org/10.48550/ARXIV.2602.09958
chicago: Chern, Albert, and Sadashige Ishida. “L’Hopital Rules for Complex-Valued
Functions in Higher Dimensions.” ArXiv, n.d. https://doi.org/10.48550/ARXIV.2602.09958.
ieee: A. Chern and S. Ishida, “L’Hopital rules for complex-valued functions in higher
dimensions,” arXiv. .
ista: Chern A, Ishida S. L’Hopital rules for complex-valued functions in higher
dimensions. arXiv, 2602.09958.
mla: Chern, Albert, and Sadashige Ishida. “L’Hopital Rules for Complex-Valued Functions
in Higher Dimensions.” ArXiv, 2602.09958, doi:10.48550/ARXIV.2602.09958.
short: A. Chern, S. Ishida, ArXiv (n.d.).
corr_author: '1'
date_created: 2026-04-15T16:28:24Z
date_published: 2026-02-10T00:00:00Z
date_updated: 2026-04-28T10:56:30Z
day: '10'
ddc:
- '510'
department:
- _id: GradSch
- _id: ChWo
doi: 10.48550/ARXIV.2602.09958
external_id:
arxiv:
- '2602.09958'
file:
- access_level: open_access
checksum: 6a76591c723d3e949ad5afa9f7dbb2ee
content_type: application/pdf
creator: dernst
date_created: 2026-04-28T10:53:27Z
date_updated: 2026-04-28T10:53:27Z
file_id: '21771'
file_name: 2026_arXiv_2602.09958.pdf
file_size: 867109
relation: main_file
success: 1
file_date_updated: 2026-04-28T10:53:27Z
fulldoi: https://doi.org/10.48550/ARXIV.2602.09958
has_accepted_license: '1'
keyword:
- l’Hopital theorem
- complex functions
language:
- iso: eng
month: '02'
oa: 1
oa_version: Preprint
project:
- _id: 34bc2376-11ca-11ed-8bc3-9a3b3961a088
grant_number: '101045083'
name: Computational Discovery of Numerical Algorithms for Animation and Simulation
of Natural Phenomena
publication: arXiv
publication_status: submitted
status: public
title: L'Hopital rules for complex-valued functions in higher dimensions
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: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21764'
abstract:
- lang: eng
text: "Colloidal fluids can exhibit complex phase behavior and determining phase
diagrams via experiments or computer simulations can be laborious. We demonstrate
that the dispersion relation ω(k), obtained from dynamical density functional
theory for the uniform density system, is a highly versatile tool for predicting
where in the phase diagram complex crystals form. The sign of ω(k) determines
whether density modes with wave number k grow or decay over time. We demonstrate
the predictive power by investigating the complex phase behavior of particles
interacting via core-shoulder pair potentials. With complementary Monte Carlo
simulations, we show that regions of the phase diagram where ωðkÞ has one or several
unstable (growing) wave numbers are also where crystalline phases occur. Going
further, by tuning these\r\nunstable wave numbers via the interaction-potential
and state-point parameters, we design systems with quasicrystals in the phase
diagram. We identify a system with a certain shoulder range exhibiting at least
ten different phases. Our general approach accelerates considerably the mapping
of complex phase diagrams, crucial for the design of new materials."
acknowledgement: "The authors thank Ms. Katrin Muck for her guidance related to the
use of HPC. The MC\r\ncomputer simulation results presented here were enabled via
a generous share of CPU time, offered by the Vienna Scientific Cluster (VSC) under
Project No. 71263. A. J. A. gratefully acknowledges support from the EPSRC under
Grant No. EP/P015689/1. This research was funded in part by the Austrian Science
Fund (FWF) [Grant DOI: 10.55776/PIN8759524], gratefully acknowledged by G. K ."
article_number: '148203'
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: Michael
full_name: Wassermair, Michael
id: 23d132c4-4e98-11ef-b275-9e8d4cd8c917
last_name: Wassermair
orcid: 0009-0003-6339-4051
- first_name: Gerhard
full_name: Kahl, Gerhard
last_name: Kahl
- first_name: Roland
full_name: Roth, Roland
last_name: Roth
- first_name: Andrew J.
full_name: Archer, Andrew J.
last_name: Archer
citation:
ama: Wassermair M, Kahl G, Roth R, Archer AJ. Navigating complex phase diagrams
in soft matter systems. Physical Review Letters. 2026;136(14). doi:10.1103/nbvt-fgjy
apa: Wassermair, M., Kahl, G., Roth, R., & Archer, A. J. (2026). Navigating
complex phase diagrams in soft matter systems. Physical Review Letters.
American Physical Society. https://doi.org/10.1103/nbvt-fgjy
chicago: Wassermair, Michael, Gerhard Kahl, Roland Roth, and Andrew J. Archer. “Navigating
Complex Phase Diagrams in Soft Matter Systems.” Physical Review Letters.
American Physical Society, 2026. https://doi.org/10.1103/nbvt-fgjy.
ieee: M. Wassermair, G. Kahl, R. Roth, and A. J. Archer, “Navigating complex phase
diagrams in soft matter systems,” Physical Review Letters, vol. 136, no.
14. American Physical Society, 2026.
ista: Wassermair M, Kahl G, Roth R, Archer AJ. 2026. Navigating complex phase diagrams
in soft matter systems. Physical Review Letters. 136(14), 148203.
mla: Wassermair, Michael, et al. “Navigating Complex Phase Diagrams in Soft Matter
Systems.” Physical Review Letters, vol. 136, no. 14, 148203, American Physical
Society, 2026, doi:10.1103/nbvt-fgjy.
short: M. Wassermair, G. Kahl, R. Roth, A.J. Archer, Physical Review Letters 136
(2026).
date_created: 2026-04-26T22:01:47Z
date_published: 2026-04-10T00:00:00Z
date_updated: 2026-04-28T07:03:48Z
day: '10'
ddc:
- '530'
department:
- _id: AnSa
- _id: GradSch
doi: 10.1103/nbvt-fgjy
external_id:
arxiv:
- '2603.18918'
file:
- access_level: open_access
checksum: 8ffb139122a185fcddbe6a9c901a287c
content_type: application/pdf
creator: dernst
date_created: 2026-04-28T06:58:40Z
date_updated: 2026-04-28T06:58:40Z
file_id: '21769'
file_name: 2026_PhysicalReviewLetters_Wassermair.pdf
file_size: 4336488
relation: main_file
success: 1
file_date_updated: 2026-04-28T06:58:40Z
fulldoi: https://doi.org/10.1103/nbvt-fgjy
has_accepted_license: '1'
intvolume: ' 136'
issue: '14'
language:
- iso: eng
month: '04'
oa: 1
oa_version: Published Version
publication: Physical Review Letters
publication_identifier:
eissn:
- 1079-7114
issn:
- 0031-9007
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Navigating complex phase diagrams in soft matter systems
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: 136
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21776'
abstract:
- lang: eng
text: Pyridyl motifs equipped with N-substituents can be powerful ligands for catalysis,
yet their broader adoption is limited by the lack of a practical method to prepare
these scaffolds. We report a modular, robust, and versatile Buchwald–Hartwig amination
protocol that enables the rapid synthesis of bipyridine, phenanthroline, terpyridine,
and pybox ligands bearing dialkylamine, diarylamine, and heteroaromatic N-substituents.
These conditions streamline ligand library synthesis and will facilitate systematic
studies in catalysis and related applications.
acknowledged_ssus:
- _id: LifeSc
- _id: MassSpec
- _id: NMR
- _id: M-Shop
acknowledgement: We gratefully acknowledge ISTA for generous financial support. B.P.
acknowledges the Austrian Science Fund (PAT 1250924) and the ACS GCI Pharmaceutical
Roundtable for funding; T.P.Y acknowledges the NSF(CHE-2349003) for 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 Aikaterina Paraskevopoulou for
HRMS measurements and Jan Pecak for support with ICP-OES experi-ments. NMR facilities
at UW−Madison were supported by the NSF(CHE-1048642) and a generous gift from Paul
J. and Margaret M. Bender. Open Access funding provided by Institute of Science
and Technology Austria/KEMÖ. This study was supported by Austrian Science Fund (PAT
1250924), ACSGCI Pharmaceutical Roundtable, and National Science Foundation(CHE-2349003)
and (CHE-1048642).
article_number: e70417
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Adam
full_name: Petrik, Adam
id: e273d403-329f-11ee-a353-8c34c056f8ed
last_name: Petrik
- first_name: Aleksander
full_name: Bena, Aleksander
id: 4197c39e-e8ec-11ed-86cb-afed934cd664
last_name: Bena
- first_name: Haralds
full_name: Baunis, Haralds
id: 2eea55ec-e8ec-11ed-86cb-d9c76787acfe
last_name: Baunis
- first_name: Riley M.
full_name: Kelch, Riley M.
last_name: Kelch
- first_name: Tehshik P.
full_name: Yoon, Tehshik P.
last_name: Yoon
- first_name: Bartholomäus
full_name: Pieber, Bartholomäus
id: 93e5e5b2-0da6-11ed-8a41-af589a024726
last_name: Pieber
orcid: 0000-0001-8689-388X
citation:
ama: Petrik A, Bena A, Baunis H, Kelch RM, Yoon TP, Pieber B. Facile access to N-substituted
pyridyl ligands. Advanced Synthesis & Catalysis. 2026;368(9). doi:10.1002/adsc.70417
apa: Petrik, A., Bena, A., Baunis, H., Kelch, R. M., Yoon, T. P., & Pieber,
B. (2026). Facile access to N-substituted pyridyl ligands. Advanced Synthesis
& Catalysis. Wiley. https://doi.org/10.1002/adsc.70417
chicago: Petrik, Adam, Aleksander Bena, Haralds Baunis, Riley M. Kelch, Tehshik
P. Yoon, and Bartholomäus Pieber. “Facile Access to N-Substituted Pyridyl Ligands.”
Advanced Synthesis & Catalysis. Wiley, 2026. https://doi.org/10.1002/adsc.70417.
ieee: A. Petrik, A. Bena, H. Baunis, R. M. Kelch, T. P. Yoon, and B. Pieber, “Facile
access to N-substituted pyridyl ligands,” Advanced Synthesis & Catalysis,
vol. 368, no. 9. Wiley, 2026.
ista: Petrik A, Bena A, Baunis H, Kelch RM, Yoon TP, Pieber B. 2026. Facile access
to N-substituted pyridyl ligands. Advanced Synthesis & Catalysis. 368(9),
e70417.
mla: Petrik, Adam, et al. “Facile Access to N-Substituted Pyridyl Ligands.” Advanced
Synthesis & Catalysis, vol. 368, no. 9, e70417, Wiley, 2026, doi:10.1002/adsc.70417.
short: A. Petrik, A. Bena, H. Baunis, R.M. Kelch, T.P. Yoon, B. Pieber, Advanced
Synthesis & Catalysis 368 (2026).
corr_author: '1'
date_created: 2026-05-03T22:01:36Z
date_published: 2026-05-05T00:00:00Z
date_updated: 2026-05-07T07:33:33Z
day: '05'
ddc:
- '540'
department:
- _id: BaPi
- _id: GradSch
doi: 10.1002/adsc.70417
file:
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checksum: afe9752977898642c903abdc70b4a283
content_type: application/pdf
creator: dernst
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date_updated: 2026-05-07T07:29:24Z
file_id: '21833'
file_name: 2026_AdvSynthCatal_Petrik.pdf
file_size: 437184
relation: main_file
success: 1
file_date_updated: 2026-05-07T07:29:24Z
fulldoi: https://doi.org/10.1002/adsc.70417
has_accepted_license: '1'
intvolume: ' 368'
issue: '9'
language:
- iso: eng
month: '05'
oa: 1
oa_version: Published Version
project:
- _id: 8f1d607d-16d5-11f0-9cad-ab453295ba5e
grant_number: PAT 1250924
name: Photoactive ligands for transformative nickel catalysis
publication: Advanced Synthesis & Catalysis
publication_identifier:
eissn:
- 1615-4169
issn:
- 1615-4150
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
title: Facile access to N-substituted pyridyl ligands
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: 368
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21845'
abstract:
- lang: eng
text: UTe2 exhibits the remarkable phenomenon of re-entrant superconductivity, whereby
the zero-resistance state reappears above 40 tesla after being suppressed with
a field of around 10 tesla. One potential pairing mechanism, invoked in the related
re-entrant superconductors UCoGe and URhGe, involves transverse fluctuations of
a ferromagnetic order parameter. However, the requisite ferromagnetic order—present
in both UCoGe and URhGe—is absent in UTe2, and neutron scattering shows instead
that the magnetic susceptibility is peaked at an antiferromagnetic wavevector.
Here, we measure the magnetotropic susceptibility of UTe2 across two field-angle
planes. This quantity is sensitive to the magnetic susceptibility in a direction
transverse to the applied magnetic field—a quantity that is not accessed in conventional
magnetization measurements. We observe a very large decrease in the magnetotropic
susceptibility over a broad range of field orientations, indicating a large increase
in the transverse magnetic susceptibility. Because our technique probes the magnetic
susceptibility in the long wavelength (q = 0) limit, this suggests that the strong
transverse susceptibility arises from ferromagnetic spin fluctuations. These ferromagnetic
fluctuations are likely important for understanding the pairing mechanism in UTe2,
as all three superconducting phases of UTe2 surround this region of enhanced susceptibility
in the field-angle phase diagram.
acknowledged_ssus:
- _id: NanoFab
acknowledgement: We appreciate technical support from Salvatore Bagiante, Evgeniia
Volobueva, Lubuna Shafeek, Ali Bangura, and Zoltán Köllö, and scientific discussions
with Daniel Agterberg, Johnpierre Paglione, Qimiao Si, Josephine Yu and Yue Yu.
V.Z., A.N., M.N., and K.A.M. acknowledge funding received from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
(TROPIC-101078696). V.Z., A.N., M.N., and K.A.M. thank the ISTA Nanofabrication
Facility for technical support. B.J.R. acknowledges funding from the Office of Basic
Energy Sciences of the United States Department of Energy under award number DE-SC0020143
for data analysis and writing. The National High Magnetic Field Laboratory is supported
by the National Science Foundation through NSF/DMR-2128556*, the State of Florida,
and the U.S. Department of Energy. A.S. acknowledges support from the DOE/BES “Science
of 100 T” grant. A.S. thanks Downtown Subscription in Santa Fe, NM, for their patience
in hosting him. Sample preparation and characterization were supported by the NSF
through DMR-2105191.
article_number: '3742'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Valeska
full_name: Zambra, Valeska
id: 467ed36b-dc96-11ea-b7c8-b043a380b282
last_name: Zambra
orcid: 0000-0002-8806-5719
- first_name: Amit
full_name: Nathwani, Amit
id: 1a362536-4d02-11f1-8543-8351136efc50
last_name: Nathwani
- first_name: Muhammad
full_name: Nauman, Muhammad
id: 32c21954-2022-11eb-9d5f-af9f93c24e71
last_name: Nauman
orcid: 0000-0002-2111-4846
- first_name: Sylvia K.
full_name: Lewin, Sylvia K.
last_name: Lewin
- first_name: Corey E.
full_name: Frank, Corey E.
last_name: Frank
- first_name: Nicholas P.
full_name: Butch, Nicholas P.
last_name: Butch
- first_name: Arkady
full_name: Shekhter, Arkady
last_name: Shekhter
- first_name: B. J.
full_name: Ramshaw, B. J.
last_name: Ramshaw
- first_name: Kimberly A
full_name: Modic, Kimberly A
id: 13C26AC0-EB69-11E9-87C6-5F3BE6697425
last_name: Modic
orcid: 0000-0001-9760-3147
citation:
ama: Zambra V, Nathwani A, Nauman M, et al. Giant transverse magnetic fluctuations
at the edge of re-entrant superconductivity in UTe2. Nature Communications.
2026;17. doi:10.1038/s41467-026-71899-7
apa: Zambra, V., Nathwani, A., Nauman, M., Lewin, S. K., Frank, C. E., Butch, N.
P., … Modic, K. A. (2026). Giant transverse magnetic fluctuations at the edge
of re-entrant superconductivity in UTe2. Nature Communications. Springer
Nature. https://doi.org/10.1038/s41467-026-71899-7
chicago: Zambra, Valeska, Amit Nathwani, Muhammad Nauman, Sylvia K. Lewin, Corey
E. Frank, Nicholas P. Butch, Arkady Shekhter, B. J. Ramshaw, and Kimberly A Modic.
“Giant Transverse Magnetic Fluctuations at the Edge of Re-Entrant Superconductivity
in UTe2.” Nature Communications. Springer Nature, 2026. https://doi.org/10.1038/s41467-026-71899-7.
ieee: V. Zambra et al., “Giant transverse magnetic fluctuations at the edge
of re-entrant superconductivity in UTe2,” Nature Communications, vol. 17.
Springer Nature, 2026.
ista: Zambra V, Nathwani A, Nauman M, Lewin SK, Frank CE, Butch NP, Shekhter A,
Ramshaw BJ, Modic KA. 2026. Giant transverse magnetic fluctuations at the edge
of re-entrant superconductivity in UTe2. Nature Communications. 17, 3742.
mla: Zambra, Valeska, et al. “Giant Transverse Magnetic Fluctuations at the Edge
of Re-Entrant Superconductivity in UTe2.” Nature Communications, vol. 17,
3742, Springer Nature, 2026, doi:10.1038/s41467-026-71899-7.
short: V. Zambra, A. Nathwani, M. Nauman, S.K. Lewin, C.E. Frank, N.P. Butch, A.
Shekhter, B.J. Ramshaw, K.A. Modic, Nature Communications 17 (2026).
corr_author: '1'
date_created: 2026-05-10T22:02:15Z
date_published: 2026-04-29T00:00:00Z
date_updated: 2026-05-11T06:36:00Z
day: '29'
ddc:
- '530'
department:
- _id: KiMo
- _id: GradSch
doi: 10.1038/s41467-026-71899-7
external_id:
arxiv:
- '2506.08984'
file:
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checksum: 8cb95b033ad2a1a7a8181f6f078c05b5
content_type: application/pdf
creator: dernst
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date_updated: 2026-05-11T06:32:12Z
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file_size: 1784917
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language:
- iso: eng
month: '04'
oa: 1
oa_version: Published Version
project:
- _id: bd968c70-d553-11ed-ba76-cde40b0aba64
grant_number: '101078696'
name: Gaining leverage with spin liquids and superconductors
publication: Nature Communications
publication_identifier:
eissn:
- 2041-1723
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
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scopus_import: '1'
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title: Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity
in UTe2
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
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...
---
DOAJ_listed: '1'
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OA_type: gold
PlanS_conform: '1'
_id: '21917'
abstract:
- lang: eng
text: A defining feature of quantum many-body systems is the exponential scaling
of the Hilbert space with the number of degrees of freedom. This exponential complexity
naïvely renders a complete state characterization, for instance via the complete
set of bipartite Renyi entropies for all disjoint regions, a challenging task.
Recently, a compact way of storing subregions' purities by encoding them as amplitudes
of a fictitious quantum wave function, known as entanglement feature, was proposed.
Notably, the entanglement feature can be a simple object even for highly entangled
quantum states. However the complexity and practical usage of the entanglement
feature for general quantum states has not been explored. In this work, we demonstrate
that the entanglement feature can be efficiently learned using only a polynomial
amount of samples in the number of degrees of freedom through the so-called tensor
cross interpolation (TCI) algorithm, assuming it is expressible as a finite bond
dimension MPS. We benchmark this learning process on Haar and random MPS states,
confirming analytic expectations. Applying the TCI algorithm to quantum eigenstates
of various one dimensional quantum systems, we identify cases where eigenstates
have entanglement feature learnable with TCI. We conclude with possible applications
of the learned entanglement feature, such as quantifying the distance between
different entanglement patterns and finding the optimal one-dimensional ordering
of physical indices in a given state, highlighting the potential utility of the
proposed purity interpolation method.
acknowledgement: "We acknowledge useful discussions with Richard Küng\r\non the interpolation
methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular,
Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI
and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary.
We also acknowledge the comments of anonymous Referee B, that encouraged us to expand
the\r\nmanuscript with discussion of additional applications\r\nof entanglement
feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at
the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron
Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto
the TCI approach. D.K and M.S. acknowledge support by the European Research Council
(ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation
methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular,
Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI
and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary.
We also acknowledge the comments of anonymous Referee B, that encouraged us to expand
the\r\nmanuscript with discussion of additional applications\r\nof entanglement
feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at
the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron
Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto
the TCI approach. D.K and M.S. acknowledge support by the European Research Council
(ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation
methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular,
Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI
and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary.
We also acknowledge the comments of anonymous Referee B, that encouraged us to expand
the\r\nmanuscript with discussion of additional applications\r\nof entanglement
feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at
the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron
Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto
the TCI approach. D.K and M.S. acknowledge support by the European Research Council
(ERC) under the European Union’s Horizon 2020 research and innovation program (Grant
Agreement No. 850899).\r\nR.V. acknowledges partial support from the US Department
of Energy, Office of Science, Basic Energy\r\nSciences, under award No. DE-SC0023999,
and the\r\nSwiss National Science Foundation (grant 10008234).\r\nThis research
was supported in part by grant NSF\r\nPHY-2309135 to the Kavli Institute for Theoretical\r\nPhysics
(KITP)"
article_number: '2114'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Dmytro
full_name: Kolisnyk, Dmytro
id: 530a7320-5355-11ee-ae5a-82a46997aaa7
last_name: Kolisnyk
orcid: 0000-0002-8612-8202
- first_name: Raimel A
full_name: Medina Ramos, Raimel A
id: CE680B90-D85A-11E9-B684-C920E6697425
last_name: Medina Ramos
orcid: 0000-0002-5383-2869
- first_name: Romain
full_name: Vasseur, Romain
last_name: Vasseur
- first_name: Maksym
full_name: Serbyn, Maksym
id: 47809E7E-F248-11E8-B48F-1D18A9856A87
last_name: Serbyn
orcid: 0000-0002-2399-5827
citation:
ama: Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. Tensor cross interpolation
of purities in quantum many-body systems. Quantum. 2026;10. doi:10.22331/q-2026-05-22-2114
apa: Kolisnyk, D., Medina Ramos, R. A., Vasseur, R., & Serbyn, M. (2026). Tensor
cross interpolation of purities in quantum many-body systems. Quantum.
Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften.
https://doi.org/10.22331/q-2026-05-22-2114
chicago: Kolisnyk, Dmytro, Raimel A Medina Ramos, Romain Vasseur, and Maksym Serbyn.
“Tensor Cross Interpolation of Purities in Quantum Many-Body Systems.” Quantum.
Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften,
2026. https://doi.org/10.22331/q-2026-05-22-2114.
ieee: D. Kolisnyk, R. A. Medina Ramos, R. Vasseur, and M. Serbyn, “Tensor cross
interpolation of purities in quantum many-body systems,” Quantum, vol.
10. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften,
2026.
ista: Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. 2026. Tensor cross interpolation
of purities in quantum many-body systems. Quantum. 10, 2114.
mla: Kolisnyk, Dmytro, et al. “Tensor Cross Interpolation of Purities in Quantum
Many-Body Systems.” Quantum, vol. 10, 2114, Verein zur Förderung des Open
Access Publizierens in den Quantenwissenschaften, 2026, doi:10.22331/q-2026-05-22-2114.
short: D. Kolisnyk, R.A. Medina Ramos, R. Vasseur, M. Serbyn, Quantum 10 (2026).
corr_author: '1'
date_created: 2026-05-26T19:39:12Z
date_published: 2026-05-22T00:00:00Z
date_updated: 2026-06-02T09:15:13Z
day: '22'
ddc:
- '530'
department:
- _id: MaSe
- _id: GradSch
doi: 10.22331/q-2026-05-22-2114
ec_funded: 1
external_id:
arxiv:
- '2503.17230'
file:
- access_level: open_access
checksum: f8ce78607ad06120cdf894dc8cef55da
content_type: application/pdf
creator: dernst
date_created: 2026-06-02T09:12:11Z
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- iso: eng
month: '05'
oa: 1
oa_version: Published Version
project:
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call_identifier: H2020
grant_number: '850899'
name: 'Non-Ergodic Quantum Matter: Universality, Dynamics and Control'
publication: Quantum
publication_identifier:
eissn:
- 2521-327X
publication_status: published
publisher: Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften
quality_controlled: '1'
status: public
title: Tensor cross interpolation of purities in quantum many-body systems
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: 10
year: '2026'
...
---
OA_place: publisher
_id: '21918'
acknowledged_ssus:
- _id: ScienComp
acknowledgement: "At different stages of my PhD, my work was supported by several
grants: the\r\nDOC fellowship of the Austrian Academy of Sciences (26293, awarded
to me),\r\nthe FWF-SFB grant (PT1032F06504 n. F65, awarded to Jan Maas), and the
ERC\r\ngrant (PR1032ERC01 n. 716117, awarded to Jan Maas). I also appreciate the
help\r\nfrom the Scientific Computing unit for their advice on the cluster usage."
alternative_title:
- ISTA Thesis
article_processing_charge: No
author:
- first_name: Kseniia
full_name: Khudiakova, Kseniia
id: 4E6DC800-AE37-11E9-AC72-31CAE5697425
last_name: Khudiakova
orcid: 0000-0002-6246-1465
citation:
ama: Khudiakova K. How epistasis and purifying selection shape genetic diversity.
2026. doi:10.15479/AT-ISTA-21918
apa: Khudiakova, K. (2026). How epistasis and purifying selection shape genetic
diversity. Institute of Science and Technology Austria. https://doi.org/10.15479/AT-ISTA-21918
chicago: Khudiakova, Kseniia. “How Epistasis and Purifying Selection Shape Genetic
Diversity.” Institute of Science and Technology Austria, 2026. https://doi.org/10.15479/AT-ISTA-21918.
ieee: K. Khudiakova, “How epistasis and purifying selection shape genetic diversity,”
Institute of Science and Technology Austria, 2026.
ista: Khudiakova K. 2026. How epistasis and purifying selection shape genetic diversity.
Institute of Science and Technology Austria.
mla: Khudiakova, Kseniia. How Epistasis and Purifying Selection Shape Genetic
Diversity. Institute of Science and Technology Austria, 2026, doi:10.15479/AT-ISTA-21918.
short: K. Khudiakova, How Epistasis and Purifying Selection Shape Genetic Diversity,
Institute of Science and Technology Austria, 2026.
corr_author: '1'
date_created: 2026-05-27T06:26:08Z
date_published: 2026-06-07T00:00:00Z
date_updated: 2026-06-12T12:43:35Z
day: '07'
ddc:
- '576'
degree_awarded: PhD
department:
- _id: GradSch
- _id: NiBa
- _id: JaMa
doi: 10.15479/AT-ISTA-21918
ec_funded: 1
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has_accepted_license: '1'
language:
- iso: eng
license: https://creativecommons.org/licenses/by-nc-nd/4.0/
month: '06'
oa_version: Published Version
page: '89'
project:
- _id: 256E75B8-B435-11E9-9278-68D0E5697425
call_identifier: H2020
grant_number: '716117'
name: Optimal Transport and Stochastic Dynamics
- _id: 34d33d68-11ca-11ed-8bc3-ec13763c0ca8
grant_number: '26293'
name: The impact of deleterious mutations on small populations
- _id: fc31cba2-9c52-11eb-aca3-ff467d239cd2
grant_number: F6504
name: Taming Complexity in Partial Differential Systems
publication_identifier:
issn:
- 2663-337X
publication_status: published
publisher: Institute of Science and Technology Austria
related_material:
record:
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- id: '12513'
relation: part_of_dissertation
status: deleted
- id: '21967'
relation: part_of_dissertation
status: public
- id: '21968'
relation: part_of_dissertation
status: public
status: public
supervisor:
- first_name: Nicholas H
full_name: Barton, Nicholas H
id: 4880FE40-F248-11E8-B48F-1D18A9856A87
last_name: Barton
orcid: 0000-0002-8548-5240
- first_name: Jan
full_name: Maas, Jan
id: 4C5696CE-F248-11E8-B48F-1D18A9856A87
last_name: Maas
orcid: 0000-0002-0845-1338
title: How epistasis and purifying selection shape genetic diversity
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: dissertation
user_id: 8b945eb4-e2f2-11eb-945a-df72226e66a9
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21929'
abstract:
- lang: eng
text: 'The import of proteins into mitochondria poses fundamental mechanistic challenges:
aggregation-prone precursor proteins must be maintained in aqueous compartments
and threaded through narrow pores without becoming stuck or mislocalized. Recent
evidence from mitochondrial protein import studies and other chaperone systems
underscores the critical role of dynamics in balancing sufficiently tight binding,
promiscuity, specificity, and release. Dynamic binding of client precursor proteins
to import machinery components arises naturally from the avidity of their interactions.
Conformational entropy enhances their stability, while the multivalent nature
of these interactions ensures that client transfer to downstream insertases occurs
without a substantial energy barrier. Here, we discuss this emerging paradigm
of dynamic protein handling, using examples where dynamic structures have been
resolved and highlight outstanding questions.'
acknowledgement: We gratefully acknowledge research funding by the Austrian Science
Fund (FWF), projects 10.55776/PAT1647625 and 10.55776/I6223. We thank Prof. Long
Li (Peking University) for providing structural models and EM density for the TOM
and TIM23 complexes, used to generate part of Figure 3. Open Access funding provided
by Institute of Science and Technology Austria.
article_number: e70630
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Jakob
full_name: Schneider, Jakob
id: 64368429-eb97-11eb-a6c2-c980b1f44415
last_name: Schneider
- first_name: Undina
full_name: Guillerm, Undina
id: bb74f472-ae54-11eb-9835-bc9c22fb1183
last_name: Guillerm
- first_name: Caroline
full_name: Simoes Pereira, Caroline
id: 87266c4a-96d2-11ef-be2c-fe5633233ec3
last_name: Simoes Pereira
- first_name: Paul
full_name: Schanda, Paul
id: 7B541462-FAF6-11E9-A490-E8DFE5697425
last_name: Schanda
orcid: 0000-0002-9350-7606
citation:
ama: Schneider J, Guillerm U, Simoes Pereira C, Schanda P. Dynamic disorder is crucial
for mitochondrial protein import. Protein Science. 2026;35(6). doi:10.1002/pro.70630
apa: Schneider, J., Guillerm, U., Simoes Pereira, C., & Schanda, P. (2026).
Dynamic disorder is crucial for mitochondrial protein import. Protein Science.
Wiley. https://doi.org/10.1002/pro.70630
chicago: Schneider, Jakob, Undina Guillerm, Caroline Simoes Pereira, and Paul Schanda.
“Dynamic Disorder Is Crucial for Mitochondrial Protein Import.” Protein Science.
Wiley, 2026. https://doi.org/10.1002/pro.70630.
ieee: J. Schneider, U. Guillerm, C. Simoes Pereira, and P. Schanda, “Dynamic disorder
is crucial for mitochondrial protein import,” Protein Science, vol. 35,
no. 6. Wiley, 2026.
ista: Schneider J, Guillerm U, Simoes Pereira C, Schanda P. 2026. Dynamic disorder
is crucial for mitochondrial protein import. Protein Science. 35(6), e70630.
mla: Schneider, Jakob, et al. “Dynamic Disorder Is Crucial for Mitochondrial Protein
Import.” Protein Science, vol. 35, no. 6, e70630, Wiley, 2026, doi:10.1002/pro.70630.
short: J. Schneider, U. Guillerm, C. Simoes Pereira, P. Schanda, Protein Science
35 (2026).
corr_author: '1'
date_created: 2026-05-31T22:02:12Z
date_published: 2026-06-01T00:00:00Z
date_updated: 2026-06-02T07:26:34Z
day: '01'
ddc:
- '572'
department:
- _id: GradSch
- _id: PaSc
doi: 10.1002/pro.70630
external_id:
pmid:
- '42159315'
file:
- access_level: open_access
checksum: e0163459a7238fdcc3fc5e17bedcce9a
content_type: application/pdf
creator: dernst
date_created: 2026-06-02T07:23:12Z
date_updated: 2026-06-02T07:23:12Z
file_id: '21937'
file_name: 2026_ProteinScience_Schneider.pdf
file_size: 3897305
relation: main_file
success: 1
file_date_updated: 2026-06-02T07:23:12Z
fulldoi: https://doi.org/10.1002/pro.70630
has_accepted_license: '1'
intvolume: ' 35'
issue: '6'
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
pmid: 1
project:
- _id: bdb9578d-d553-11ed-ba76-ed5d39fce6f0
grant_number: I06223
name: Structure and mechanism of the mitochondrial MIM insertase
publication: Protein Science
publication_identifier:
eissn:
- 1469-896X
issn:
- 0961-8368
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
title: Dynamic disorder is crucial for mitochondrial protein import
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: 35
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '21963'
abstract:
- lang: eng
text: The cerebral cortex consists of immense numbers of neuronal and glial cell-types
derived from radial glial progenitor (RGP) cells. How RGPs generate appropriate
quantities of distinct cortical cell-types to safeguard a brain of correct size,
is not well understood. However, genetic aberration in human, including mutations
in PTEN, lead to cortical malformation such as macrocephaly, albeit with unknown
etiology. Here we utilized Mosaic Analysis with Double Markers (MADM)-based clonal
analysis and single cell phenotyping to decipher the role of Pten in neurogenic
and gliogenic RGP lineage progression during cortical ontogeny. While neurogenic
RGP lineage progression and projection neuron production was moderately altered
in the absence of Pten, cortical astrocyte production was drastically increased.
Through genetic epistasis experiments we show that the loss of Pten uncouples
astrocyte generation from essential growth factor signaling hubs, funneling into
MAPK. Collectively, our results suggest that Pten regulates RGP lineage progression
with distinct sequential functions in cortical projection neurogenesis and astrocyte
production to ensure the emergence of a correctly-sized cerebral cortex.
acknowledged_ssus:
- _id: Bio
- _id: LifeSc
- _id: PreCl
acknowledgement: "We thank Kay-Uwe Wagner (Wayne State University) for generously
sharing Jak1/2–flox mouse lines; A.\r\nSommer (VBCF GmbH, NGS Unit) for technical
support; N. Kim, V. Mick, S. Schnabl, S. Gobeil, and L.\r\nAndersen for technical
assistance; all members of the Hippenmeyer lab for discussion and B. Novitch for\r\ncomments
on earlier versions of the manuscript. This research was supported by the Scientific
Service Units\r\n(SSU) of IST Austria through resources provided by the Imaging
and Optics Facility (IOF), Lab Support-\r\n(LSF) and Preclinical Facilities (PCF).
O.A.M received support from the Austrian Academy of Sciences\r\nÖAW (DOC 186584),
and N.A. from FWF Elise Richter Program (Grant V1041T). This work was also\r\nsupported
by IST Austria institutional funds; FWF SFB F78 (Neuro Stem Modulation) to S.H.,
and the\r\nEuropean Research Council (ERC) under the European Union’s Horizon 2020
research and innovation\r\nprogramme (grant agreement No 725780 LinPro) to S.H."
article_processing_charge: No
author:
- first_name: Osvaldo
full_name: Miranda, Osvaldo
id: 862A3C56-A8BF-11E9-B4FA-D9E3E5697425
last_name: Miranda
orcid: 0000-0001-6618-6889
- first_name: Ximena
full_name: Contreras, Ximena
id: 475990FE-F248-11E8-B48F-1D18A9856A87
last_name: Contreras
- first_name: Florian
full_name: Pauler, Florian
id: 48EA0138-F248-11E8-B48F-1D18A9856A87
last_name: Pauler
orcid: 0000-0002-7462-0048
- first_name: Amarbayasgalan
full_name: Davaatseren, Amarbayasgalan
id: 70ADC922-B424-11E9-99E3-BA18E6697425
last_name: Davaatseren
- first_name: Nicole
full_name: Amberg, Nicole
id: 4CD6AAC6-F248-11E8-B48F-1D18A9856A87
last_name: Amberg
orcid: 0000-0002-3183-8207
- first_name: Carmen
full_name: Streicher, Carmen
id: 36BCB99C-F248-11E8-B48F-1D18A9856A87
last_name: Streicher
- first_name: Ana
full_name: Villalba Requena, Ana
id: 68cb85a0-39f7-11eb-9559-9aaab4f6a247
last_name: Villalba Requena
orcid: 0000-0002-5615-5277
- first_name: Anna-Magdalena
full_name: Heger, Anna-Magdalena
id: 4B76FFD2-F248-11E8-B48F-1D18A9856A87
last_name: Heger
- first_name: Corentine
full_name: Marie, Corentine
last_name: Marie
- first_name: Bassem A.
full_name: Hassan, Bassem A.
last_name: Hassan
- first_name: Thomas
full_name: Rülicke, Thomas
last_name: Rülicke
- first_name: Simon
full_name: Hippenmeyer, Simon
id: 37B36620-F248-11E8-B48F-1D18A9856A87
last_name: Hippenmeyer
orcid: 0000-0003-2279-1061
citation:
ama: Miranda O, Contreras X, Pauler F, et al. Pten orchestrates neurogenic radial
glia lineage progression and tunes neocortical astrocyte production. bioRxiv.
doi:10.64898/2026.05.01.722191
apa: Miranda, O., Contreras, X., Pauler, F., Davaatseren, A., Amberg, N., Streicher,
C., … Hippenmeyer, S. (n.d.). Pten orchestrates neurogenic radial glia lineage
progression and tunes neocortical astrocyte production. bioRxiv. https://doi.org/10.64898/2026.05.01.722191
chicago: Miranda, Osvaldo, Ximena Contreras, Florian Pauler, Amarbayasgalan Davaatseren,
Nicole Amberg, Carmen Streicher, Ana Villalba Requena, et al. “Pten Orchestrates
Neurogenic Radial Glia Lineage Progression and Tunes Neocortical Astrocyte Production.”
BioRxiv, n.d. https://doi.org/10.64898/2026.05.01.722191.
ieee: O. Miranda et al., “Pten orchestrates neurogenic radial glia lineage
progression and tunes neocortical astrocyte production,” bioRxiv. .
ista: Miranda O, Contreras X, Pauler F, Davaatseren A, Amberg N, Streicher C, Villalba
Requena A, Heger A-M, Marie C, Hassan BA, Rülicke T, Hippenmeyer S. Pten orchestrates
neurogenic radial glia lineage progression and tunes neocortical astrocyte production.
bioRxiv, 10.64898/2026.05.01.722191.
mla: Miranda, Osvaldo, et al. “Pten Orchestrates Neurogenic Radial Glia Lineage
Progression and Tunes Neocortical Astrocyte Production.” BioRxiv, doi:10.64898/2026.05.01.722191.
short: O. Miranda, X. Contreras, F. Pauler, A. Davaatseren, N. Amberg, C. Streicher,
A. Villalba Requena, A.-M. Heger, C. Marie, B.A. Hassan, T. Rülicke, S. Hippenmeyer,
BioRxiv (n.d.).
corr_author: '1'
date_created: 2026-06-09T08:08:53Z
date_published: 2026-05-05T00:00:00Z
date_updated: 2026-06-16T08:57:20Z
day: '05'
ddc:
- '570'
department:
- _id: SiHi
- _id: PreCl
- _id: GradSch
doi: 10.64898/2026.05.01.722191
ec_funded: 1
fulldoi: https://doi.org/10.64898/2026.05.01.722191
has_accepted_license: '1'
language:
- iso: eng
license: https://creativecommons.org/licenses/by-nc/4.0/
main_file_link:
- open_access: '1'
url: https://doi.org/10.64898/2026.05.01.722191
month: '05'
oa: 1
oa_version: Preprint
project:
- _id: 059F6AB4-7A3F-11EA-A408-12923DDC885E
grant_number: F7805
name: Stem Cell Modulation in Neural Development and Regeneration/ P05-Molecular
Mechanisms of Neural Stem Cell Lineage Progression
- _id: 260018B0-B435-11E9-9278-68D0E5697425
call_identifier: H2020
grant_number: '725780'
name: Principles of Neural Stem Cell Lineage Progression in Cerebral Cortex Development
publication: bioRxiv
publication_status: submitted
status: public
title: Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical
astrocyte production
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: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '21981'
abstract:
- lang: eng
text: For Hamiltonian actions of semidirect products G = FxH, we study 2-cocycles
arising from residual Hamiltonian actions of F on Hamiltonian reductions for H.
The motivation comes from the study of Teichmüller spaces for surfaces with boundary,
which carry Hamiltonian actions of the Virasoro algebra. In this paper, we give
a general setup for the problem, and we suggest an easier way to obtain the Gelfand-Fuchs
2-cocycles for Hamiltonian actions on Teichmüller spaces.
article_number: '105878'
article_processing_charge: Yes (via OA deal)
article_type: original
arxiv: 1
author:
- first_name: Viacheslav
full_name: Goncharov, Viacheslav
id: 8a0e2993-7114-11f0-b60e-f50e633649d8
last_name: Goncharov
citation:
ama: Goncharov V. An easier way to compute 2-cocycles coming from a reduction for
semidirect products. Journal of Geometry and Physics. 2026;227. doi:10.1016/j.geomphys.2026.105878
apa: Goncharov, V. (2026). An easier way to compute 2-cocycles coming from a reduction
for semidirect products. Journal of Geometry and Physics. Elsevier. https://doi.org/10.1016/j.geomphys.2026.105878
chicago: Goncharov, Viacheslav. “An Easier Way to Compute 2-Cocycles Coming from
a Reduction for Semidirect Products.” Journal of Geometry and Physics.
Elsevier, 2026. https://doi.org/10.1016/j.geomphys.2026.105878.
ieee: V. Goncharov, “An easier way to compute 2-cocycles coming from a reduction
for semidirect products,” Journal of Geometry and Physics, vol. 227. Elsevier,
2026.
ista: Goncharov V. 2026. An easier way to compute 2-cocycles coming from a reduction
for semidirect products. Journal of Geometry and Physics. 227, 105878.
mla: Goncharov, Viacheslav. “An Easier Way to Compute 2-Cocycles Coming from a Reduction
for Semidirect Products.” Journal of Geometry and Physics, vol. 227, 105878,
Elsevier, 2026, doi:10.1016/j.geomphys.2026.105878.
short: V. Goncharov, Journal of Geometry and Physics 227 (2026).
corr_author: '1'
date_created: 2026-06-10T07:29:13Z
date_published: 2026-05-21T00:00:00Z
date_updated: 2026-06-16T09:23:39Z
day: '21'
ddc:
- '000'
department:
- _id: GradSch
doi: 10.1016/j.geomphys.2026.105878
external_id:
arxiv:
- '2509.16169'
fulldoi: https://doi.org/10.1016/j.geomphys.2026.105878
has_accepted_license: '1'
intvolume: ' 227'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1016/j.geomphys.2026.105878
month: '05'
oa: 1
oa_version: Published Version
publication: Journal of Geometry and Physics
publication_identifier:
eissn:
- 1879-1662
issn:
- 0393-0440
publication_status: epub_ahead
publisher: Elsevier
quality_controlled: '1'
scopus_import: '1'
status: public
title: An easier way to compute 2-cocycles coming from a reduction for semidirect
products
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: 227
year: '2026'
...
---
OA_place: publisher
OA_type: gold
_id: '22119'
article_number: EGU26-19367
article_processing_charge: No
author:
- first_name: José M
full_name: Muñoz Hermosilla, José M
id: e1037a6d-646e-11ef-b402-e0ed9ab0901e
last_name: Muñoz Hermosilla
orcid: 0000-0002-1990-8508
- first_name: Evan
full_name: Miles, Evan
last_name: Miles
- first_name: Michael
full_name: McCarthy, Michael
id: 22a2674a-61ce-11ee-94b5-d18813baf16f
last_name: McCarthy
- first_name: Juan Vicente
full_name: Melo Velasco, Juan Vicente
id: 2611dec0-b9c6-11ed-9bea-a81c2b17a549
last_name: Melo Velasco
- first_name: Florian
full_name: Hardmeier, Florian
last_name: Hardmeier
- first_name: PRATEEK
full_name: GANTAYAT, PRATEEK
id: 02734268-3e8d-11ef-80a1-cec4a088d004
last_name: GANTAYAT
- first_name: Adrià
full_name: Fontrodona-Bach, Adrià
id: f06891fd-9f42-11ee-8632-a20971c43046
last_name: Fontrodona-Bach
- first_name: Guillaume
full_name: Jouvet, Guillaume
last_name: Jouvet
- first_name: Francesca
full_name: Pellicciotti, Francesca
id: b28f055a-81ea-11ed-b70c-a9fe7f7b0e70
last_name: Pellicciotti
orcid: 0000-0002-5554-8087
citation:
ama: 'Muñoz Hermosilla JM, Miles E, McCarthy M, et al. Constraining debris input
to Oberaletsch Glacier using ensemble-based Lagrangian modelling. In: EGU General
Assembly 2026. European Geosciences Union; 2026. doi:10.5194/egusphere-egu26-19367'
apa: 'Muñoz Hermosilla, J. M., Miles, E., McCarthy, M., Melo Velasco, J. V., Hardmeier,
F., GANTAYAT, P., … Pellicciotti, F. (2026). Constraining debris input to Oberaletsch
Glacier using ensemble-based Lagrangian modelling. In EGU General Assembly
2026. Vienna, Austria & Virtual: European Geosciences Union. https://doi.org/10.5194/egusphere-egu26-19367'
chicago: Muñoz Hermosilla, José M, Evan Miles, Michael McCarthy, Juan Vicente Melo
Velasco, Florian Hardmeier, PRATEEK GANTAYAT, Adrià Fontrodona-Bach, Guillaume
Jouvet, and Francesca Pellicciotti. “Constraining Debris Input to Oberaletsch
Glacier Using Ensemble-Based Lagrangian Modelling.” In EGU General Assembly
2026. European Geosciences Union, 2026. https://doi.org/10.5194/egusphere-egu26-19367.
ieee: J. M. Muñoz Hermosilla et al., “Constraining debris input to Oberaletsch
Glacier using ensemble-based Lagrangian modelling,” in EGU General Assembly
2026, Vienna, Austria & Virtual, 2026.
ista: Muñoz Hermosilla JM, Miles E, McCarthy M, Melo Velasco JV, Hardmeier F, GANTAYAT
P, Fontrodona-Bach A, Jouvet G, Pellicciotti F. 2026. Constraining debris input
to Oberaletsch Glacier using ensemble-based Lagrangian modelling. EGU General
Assembly 2026. EGU General Assembly, EGU26-19367.
mla: Muñoz Hermosilla, José M., et al. “Constraining Debris Input to Oberaletsch
Glacier Using Ensemble-Based Lagrangian Modelling.” EGU General Assembly 2026,
EGU26-19367, European Geosciences Union, 2026, doi:10.5194/egusphere-egu26-19367.
short: J.M. Muñoz Hermosilla, E. Miles, M. McCarthy, J.V. Melo Velasco, F. Hardmeier,
P. GANTAYAT, A. Fontrodona-Bach, G. Jouvet, F. Pellicciotti, in:, EGU General
Assembly 2026, European Geosciences Union, 2026.
conference:
end_date: 2026-05-08
location: Vienna, Austria & Virtual
name: EGU General Assembly
start_date: 2026-05-03
corr_author: '1'
date_created: 2026-06-22T12:16:50Z
date_published: 2026-07-02T00:00:00Z
date_updated: 2026-07-02T06:42:37Z
day: '02'
ddc:
- '550'
department:
- _id: FrPe
- _id: GradSch
doi: 10.5194/egusphere-egu26-19367
file:
- access_level: open_access
checksum: 2ea3e691cfa53176d0e801b9172842d6
content_type: application/pdf
creator: dernst
date_created: 2026-07-02T06:22:50Z
date_updated: 2026-07-02T06:22:50Z
file_id: '22233'
file_name: 2026_EGU26_MunozHermosilla.pdf
file_size: 284023
relation: main_file
success: 1
file_date_updated: 2026-07-02T06:22:50Z
fulldoi: https://doi.org/10.5194/egusphere-egu26-19367
has_accepted_license: '1'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
publication: EGU General Assembly 2026
publication_status: published
publisher: European Geosciences Union
status: public
title: Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian
modelling
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: conference_abstract
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '22241'
abstract:
- lang: eng
text: We revisit the computation of 3D generalized winding numbers, a useful measure
for inside-outside classification on triangle meshes with gaps, self-intersections,
and open boundaries. At the core of our new method is an analytical reduction
of the surface integral that defines the winding number, resulting in a single
ray-mesh intersection test and an elementary sum over boundary edges per evaluation.
This construction is orders of magnitude more efficient than the state of the
art in practice, which we show in an extensive performance benchmark. Conveniently,
the method also reduces to the best-available asymptotic complexity in the worst
case, and it introduces no approximations apart from floating-point errors. Our
algorithm is conceptually simple to understand, straightforward to implement and
debug, and it works reliably even on extremely noisy and corrupt input geometry.
acknowledgement: "We thank Sadashige Ishida and Ryusuke Sugimoto for their insightful
discussions and proofreading and other members of the ISTA\r\nVisual Computing Group
for their general feedback. This project was\r\nfunded in part by the European Research
Council (ERC Consolidator\r\nGrant 101045083 CoDiNA)."
article_number: '41'
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Peiyuan
full_name: Xie, Peiyuan
id: 488e236c-6bad-11f0-9831-859175c78e8a
last_name: Xie
- first_name: Christian
full_name: Hafner, Christian
id: 400429CC-F248-11E8-B48F-1D18A9856A87
last_name: Hafner
- first_name: Christopher J
full_name: Wojtan, Christopher J
id: 3C61F1D2-F248-11E8-B48F-1D18A9856A87
last_name: Wojtan
orcid: 0000-0001-6646-5546
citation:
ama: Xie P, Hafner C, Wojtan C. Fast and exact winding numbers for triangle meshes.
ACM Transactions on Graphics. 2026;45(4). doi:10.1145/3811339
apa: Xie, P., Hafner, C., & Wojtan, C. (2026). Fast and exact winding numbers
for triangle meshes. ACM Transactions on Graphics. Association for Computing
Machinery. https://doi.org/10.1145/3811339
chicago: Xie, Peiyuan, Christian Hafner, and Chris Wojtan. “Fast and Exact Winding
Numbers for Triangle Meshes.” ACM Transactions on Graphics. Association
for Computing Machinery, 2026. https://doi.org/10.1145/3811339.
ieee: P. Xie, C. Hafner, and C. Wojtan, “Fast and exact winding numbers for triangle
meshes,” ACM Transactions on Graphics, vol. 45, no. 4. Association for
Computing Machinery, 2026.
ista: Xie P, Hafner C, Wojtan C. 2026. Fast and exact winding numbers for triangle
meshes. ACM Transactions on Graphics. 45(4), 41.
mla: Xie, Peiyuan, et al. “Fast and Exact Winding Numbers for Triangle Meshes.”
ACM Transactions on Graphics, vol. 45, no. 4, 41, Association for Computing
Machinery, 2026, doi:10.1145/3811339.
short: P. Xie, C. Hafner, C. Wojtan, ACM Transactions on Graphics 45 (2026).
corr_author: '1'
das_tickbox: '0'
date_created: 2026-07-03T21:03:48Z
date_published: 2026-07-03T00:00:00Z
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title: Fast and exact winding numbers for triangle meshes
tmp:
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abstract:
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text: 'The abundant population of little red dots (LRDs), compact objects with red
UV to optical colors and broad Balmer lines at high redshift, is revealing new
insights into the properties of early active galactic nuclei (AGN). Perhaps the
most surprising features of this population are the presence of Balmer absorption
and ubiquitous strong Balmer breaks. Recent models link these features to an active
supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We
present a stringent test of such models using VLT/MUSE observations of A2744-45924,
the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744
lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula
(h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc.
The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα)
compared to Lyα nebulae typically observed around quasars of similar luminosity.
We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial
shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and
Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered
by star formation. In the environment of A2744-45924, we identified four extended
Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations
based on Hα emission, and show no evidence for radiation from A2744-45924 affecting
its surroundings. The lack of strong, compact, and broad Lyα and the absence of
a luminous extended halo, suggest that the UV AGN light is obscured by dense gas
cloaking the SMBH with a covering factor close to unity.'
acknowledgement: 'We thank the anonymous referee for constructive and useful comments.
We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected
at the European Organisation for Astronomical Research in the Southern Hemisphere
under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224).
Views and opinions expressed are however those of the author(s) only and do not
necessarily reflect those of the European Union or the European Research Council.
Neither the European Union nor the granting authority can be held responsible for
them. We acknowledge funding from JWST program GO-3516. This work is based in part
on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data
were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations
are associated with program #3516. MG thanks the Max Planck Society for support
through the MPRG. FDE acknowledges support by the Science and Technology Facilities
Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI
Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant
SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.'
article_number: A147
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for
an extremely bright little red dot. Indications of enshrouded supermassive black
hole growth. Astronomy & Astrophysics. 2026;705. doi:10.1051/0004-6361/202555596
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke,
M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555596
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya
Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo
for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive
Black Hole Growth.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202555596.
ieee: A. Torralba Torregrosa et al., “A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth,” Astronomy
& Astrophysics, vol. 705. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia
S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie
R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely
bright little red dot. Indications of enshrouded supermassive black hole growth.
Astronomy & Astrophysics. 705, A147.
mla: Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright
Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” Astronomy
& Astrophysics, vol. 705, A147, EDP Sciences, 2026, doi:10.1051/0004-6361/202555596.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke,
S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa,
R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy & Astrophysics
705 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-01-25T23:01:41Z
date_published: 2026-01-14T00:00:00Z
date_updated: 2026-07-08T06:38:23Z
day: '14'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202555596
external_id:
arxiv:
- '2505.09542'
file:
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language:
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month: '01'
oa: 1
oa_version: Published Version
project:
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grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
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publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
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title: A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded
supermassive black hole growth
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_id: '21658'
abstract:
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text: Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential
rotation between the core and the envelope of evolved solar-like stars. Quadrupolar
(ℓ = 2) mixed modes also contain information regarding internal dynamics but are
very rarely characterised due to their low amplitude and the challenging identification
of adjacent or overlapping rotationally split multiplets affected by near-degeneracy
effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond
ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed
modes while explicitly accounting for near-degeneracy effects that distort their
rotational multiplets. We have derived a new asymptotic formulation of near-degenerate
mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction
between modes of adjacent radial orders. This formalism, expressed directly in
the mixed-mode basis, provides analytical expressions for the near-degeneracy
effects. We implemented the formalism within a global Bayesian mode-fitting framework
for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were
able to asymptotically model the asymmetric rotational splitting present in various
radial orders of ℓ = 2 modes observed in young red giant stars without the need
for any numerical stellar modelling. We applied our formalism to the Kepler target
KIC 7341231, and it yielded core and envelope rotation rates consistent with previous
numerical modelling while providing improved constraints from the global and model-independent
approach. We also characterised the new target, KIC 8179973, measuring its rotation
rate and mixed-mode parameters for the first time. As our framework relies on
a direct global fit, it allows for much better precision on the asteroseismic
parameters and rotation rate estimates than standard methods, yielding better
constraints for rotation inversions. We have placed the first observational constraints
on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving
the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.
acknowledgement: 'We thank the referee for their careful and constructive report,
which has substantially enhanced both the quality and clarity of the manuscript.
L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research
Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement
N°101165631). While partially funded by the European Union, views and opinions expressed
are, however, those of the authors only and do not necessarily reflect those of
the European Union or the European Research Council. Neither the European Union
nor the granting authority can be held responsible for them. The authors acknowledge
the great support and feedback provided during the redaction of this article by
Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt
for her insights on uncertainty estimates. The authors also thank the members of
the Asteroseismology and Stellar Dynamics group of the Institute of Science and
Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K.
Smith. This paper includes data collected by the Kepler mission and obtained from
the MAST data archive at the Space Telescope Science Institute (STScI). Funding
for the Kepler mission is provided by the NASA Science Mission Directorate. STScI
is operated by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013,
2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et
al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017),
slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011),
sloscillations (Kuszlewicz et al. 2019, 2023).'
article_number: A321
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Bastien Raymond Bernard
full_name: Liagre, Bastien Raymond Bernard
id: 662f1873-cab4-11f0-a719-8087d302868d
last_name: Liagre
- first_name: Aayush A
full_name: Desai, Aayush A
id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
last_name: Desai
- first_name: Lukas
full_name: Einramhof, Lukas
id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c
last_name: Einramhof
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar
mixed modes: From an asymptotic description to data fitting. Astronomy &
Astrophysics. 2026;707. doi:10.1051/0004-6361/202558023'
apa: 'Liagre, B. R. B., Desai, A. A., Einramhof, L., & Bugnet, L. A. (2026).
Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
to data fitting. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558023'
chicago: 'Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and
Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From
an Asymptotic Description to Data Fitting.” Astronomy & Astrophysics.
EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558023.'
ieee: 'B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy
effects in quadrupolar mixed modes: From an asymptotic description to data fitting,”
Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.'
ista: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects
in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy
& Astrophysics. 707, A321.'
mla: 'Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar
Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy &
Astrophysics, vol. 707, A321, EDP Sciences, 2026, doi:10.1051/0004-6361/202558023.'
short: B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy & Astrophysics
707 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-07-08T06:39:05Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
- _id: IlCa
- _id: GradSch
doi: 10.1051/0004-6361/202558023
external_id:
arxiv:
- '2511.05314 '
file:
- access_level: open_access
checksum: 560cac19dc70184626b85e71a26ee22e
content_type: application/pdf
creator: dernst
date_created: 2026-04-07T09:00:50Z
date_updated: 2026-04-07T09:00:50Z
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file_name: 2026_AstronomyAstrophysics_Liagre.pdf
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has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
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issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
to data fitting'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
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short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
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abstract:
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text: Recent studies at high redshift have revealed an enigmatic class of little
red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere.
However, it is unclear whether such objects exist at lower redshift, especially
given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from
JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed
by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral
energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with
effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably
deep absorption, stronger than previously measured in any LRD. The absorption
trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The
presence of blue- and red-shifted absorption suggests complex dynamics of the
obscuring gas along the line of sight. We speculate that the absorption trough
can be produced by a thick wind launched from a thick, rotating photospheric disk,
the latter being the source of the red optical continuum. While the source is
unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble
Space Telescope imaging shows an extended morphology with (formular displayed)
kpc, which we interpret as a host galaxy with a stellar mass of ∼10^8 M⊙, in line
with the narrow Hα emission. The discovery of this object at cosmic noon highlights
the feasibility of systematic searches for extreme LRDs with wide-area facilities
such as Euclid and Roman.
acknowledgement: "IOP Science home\r\nThe Astrophysical Journal Letters\r\nThe American
Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA
Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and
Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7\r\nAlberto Torralba,
Jorryt Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush
Desai, Anna de Graaff, Jenny E. Greene, Christian Kragh JespersenShow full author
list\r\n\r\nPublished 2026 June 30 • © 2026. The Author(s). Published by the American
Astronomical Society.\r\nThe Astrophysical Journal Letters, Volume 1005, Number
2\r\nCitation Alberto Torralba et al 2026 ApJL 1005 L37\r\nDOI 10.3847/2041-8213/ae7bfd\r\n\r\nPDFOpens
in a new tab.ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens
in a new tab.ePub\r\nArticle metrics\r\n122 Total downloads\r\n\r\nShare this article\r\nArticle
information\r\nAbstract\r\nRecent studies at high redshift have revealed an enigmatic
class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any
stellar atmosphere. However, it is unclear whether such objects exist at lower redshift,
especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam
pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter
spectroscopy. The rest-optical to near-infrared spectral energy distribution of
PAN-BH*-1 is consistent with a photospheric continuum with effective temperature
Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger
than previously measured in any LRD. The absorption trough spans from −520 to +267
km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted
absorption suggests complex dynamics of the obscuring gas along the line of sight.
We speculate that the absorption trough can be produced by a thick wind launched
from a thick, rotating photospheric disk, the latter being the source of the red
optical continuum. While the source is unresolved in the rest-optical JWST data
(reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended
morphology with \r\n kpc, which we interpret as a host galaxy with a stellar mass
of ∼108 M⊙, in line with the narrow Hα emission. The discovery of this object at
cosmic noon highlights the feasibility of systematic searches for extreme LRDs with
wide-area facilities such as Euclid and Roman.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious
article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work
may be used under the terms of the Creative Commons Attribution 4.0 licence. Any
further distribution of this work must maintain attribution to the author(s) and
the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe unprecedented
sensitivity of JWST has enabled the discovery of a new, abundant population of objects
at redshifts z ≈ 3–9 nicknamed the “little red dots” (LRDs). These are characterized
by their compact rest-frame optical morphology, broad emission lines, and a characteristic
rest-UV to optical “V-shape” in their spectral energy distributions (SED; e.g.,
D. D. Kocevski et al. 2023; V. Kokorev et al. 2024; J. Matthee et al. 2024; I. Labbe
et al. 2025).\r\n\r\nThe nature of LRDs is highly debated (see K. Inayoshi & L.
C. Ho 2025, for a recent overview) as the LRDs show systematic differences with
respect to other types of active galactic nuclei (AGN), such as faintness in X-rays
(e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024), mid-to-far-infrared dust emission
(e.g., G. C. K. Leung et al. 2025; C. C. Williams et al. 2024; I. Delvecchio et
al. 2025; D. J. Setton et al. 2025; M. Xiao et al. 2025), and radio (e.g., G. Mazzolari
et al. 2026; M. A. Latif et al. 2025; K. Perger et al. 2025, see A. J. Gloudemans
et al. 2025).\r\n\r\nA recurring spectral feature of LRDs is the presence of a strong
Balmer break (e.g., D. J. Setton et al. 2025; B. Wang et al. 2024; R. E. Hviding
et al. 2025; W. Q. Sun et al. 2026), in some cases stronger than any star or stellar
population can produce. The two most prominent examples known to date are The Cliff
at z ≈ 3.5 (A. de Graaff et al. 2025a) and MoM-BH* at z ≈ 7.8 (R. P. Naidu et al.
2025). The joint appearance of strong Balmer lines as well as strong Balmer breaks
has been modeled as being due to absorption by a dense, neutral gas with a high
column density in the line of sight to a highly ionizing source (K. Inayoshi & R.
Maiolino 2025; X. Ji et al. 2025; A. Sneppen et al. 2026; A. Torralba et al. 2026).
These observations have sparked the development of new theoretical models, ranging
from a spherical envelope analogous to stellar atmospheres (e.g., M. C. Begelman
& J. Dexter 2026; D. Kido et al. 2025; H. Liu et al. 2025; D. Nandal & A. Loeb 2026)
or a thick accretion disk (e.g., H. Liu et al. 2025, 2026; K. Inayoshi et al. 2025;
Y.-X. Chen et al. 2026).\r\n\r\nBesides their spectral features, the evolution of
the LRD number densities is also in stark contrast to other types of AGNs (e.g.,
K. Inayoshi 2025). At 4 ≲ z ≲ 7, LRDs represent a few percent of the galaxy population
(e.g., D. D. Kocevski et al. 2023, 2025; J. E. Greene et al. 2024; V. Kokorev et
al. 2024; X. Lin et al. 2024; R. Maiolino et al. 2024; J. Matthee et al. 2024),
with number densities of ≳10−5 Mpc−3. The number density does not appear to drop
quickly beyond z > 5 (e.g., J. Zhang et al. 2026), with various LRDs having been
confirmed at z > 8 (V. Kokorev et al. 2023; A. J. Taylor et al. 2025; R. Tripodi
et al. 2025), well beyond the quasar redshift record (F. Wang et al. 2021). Photometric
LRD candidates exist beyond z > 10 (T. S. Tanaka et al. 2025). In turn, the number
density of LRDs seems to decline steeply at z < 4 (e.g., Y. Ma et al. 2026), with
estimates of a number density of ∼10−6 cMpc−3 at z ∼ 2 and even ∼10−10 cMpc−3 at
z ≈ 0.3 (X. Lin et al. 2026). While it is challenging to ensure a uniform selection
function across such a large redshift baseline and dedicated spectroscopic follow-up
of such lower redshift candidates has only just started, it is challenging to attribute
five orders of magnitude to such effects.\r\n\r\nMotivated by the discovery of rare
objects with extreme Balmer breaks at z > 3 and the very small number of known
LRDs at lower redshift, we performed a dedicated search for extreme Balmer break
objects using a template-match approach on a large compilation of JWST NIRCam data
over ≈0.3 deg2 and z ≈ 1.5–7.0. This survey is presented in A. Weibel et al. (2026a).
As part of an ongoing ground-based spectroscopic campaign of LRD candidates at z
∼ 2 (Y. Ma et al. 2026), we followed up the most luminous candidate with a photometric
redshift of z ≈ 2 with the X-Shooter spectrograph on the Very Large Telescope (VLT).
In this Letter, we present the discovery and spectroscopic confirmation of PAN-BH*-1,
a luminous LRD at z = 1.73 with an extreme Balmer break comparable to the strongest
observed in any LRD (and, in general, any astrophysical source). The low redshift
of this source enables high-resolution spectroscopy from ground-based observatories
that is otherwise impossible to obtain at high redshift.\r\n\r\nThroughout this
Letter, we use a ΛCDM cosmology with Ωm = 0.31, ΩΛ = 0.69, and h = 0.677 as described
by Planck Collaboration et al. (2020). All the magnitudes are given in the AB system
(J. B. Oke & J. E. Gunn 1983).\r\n\r\n2. Observations\r\n2.1. Photometry and Source
Selection\r\nWe identified PAN-BH*-1 (ID: PAN-1115, RA, DEC: 40.015835, −1.659363
J2000) as part of a systematic search across ≈0.3 deg2 of JWST NIRCam legacy imaging
comprising at least six filters of coverage (A. Weibel et al. 2026b). Notably, this
dataset includes the Cycle 1 pure parallel survey PANORAMIC (PID: 2514, PIs: Williams
& Oesch; C. C. Williams et al. 2025) that contributes 28 of the 35 independent lines
of sight, thereby enabling the discovery of rare objects such as PAN-BH*-1 across
diverse large-scale structure environments. Specifically, this source was identified
in the footprint j024000m0142 of the PANORAMIC DR1,15 which is adjacent to the A370
field (G. O. Abell et al. 1989), where archival images by the Hubble Space Telescope
(HST) are available from the BUFFALO survey (C. L. Steinhardt et al. 2020). The
HST/ACS images were processed with grizli and also released as part of the PANORAMIC
dataset.\r\n\r\nPAN-BH*-1 is in the outskirts of the A370 lensing cluster, but the
magnification is only μ ≈ 1.05 according to the models from A. Niemiec et al. (2023).
Throughout the rest of the paper, we report the uncorrected flux measurements, since
the effect of magnification (∼5%) is negligible given the uncertainties in the observations
and the lensing model.\r\n\r\nThe search strategy and full photometric selection
are described in a companion paper (A. Weibel et al. 2026a). Briefly, that work
presents a new selection of LRDs as a combination of a “black hole star” template
(BH*; R. P. Naidu et al. 2025) embedded in a host galaxy, instead of the typically
used “V-shaped” selections (e.g., D. D. Kocevski et al. 2025; V. Kokorev et al.
2024). The host galaxies are modeled using eazy’s blue_sfhz templates. The BH*s
are modeled using a novel template set comprising empirical luminosity-based stacks
constructed in W. Q. Sun et al. (2026), the cloudy template from R. P. Naidu et
al. (2025), and by using spectra of prominent LRDs spanning the observed effective
temperature range (I. Labbe et al. 2024; A. de Graaff et al. 2025a; B. Wang et al.
2026).\r\n\r\nPAN-BH*-1 stood out as one of the few sources where the BH* template
effectively dominated all the light over the full wavelength range covered by NIRCam
(hence the name). The redshift of PAN-BH*-1 was estimated to be zphot = 1.85. Follow-up
VLT/X-Shooter spectroscopy confirmed the redshift as zspec = 1.731 (see Section
3.2).\r\n\r\nPAN-BH*-1 is also covered by archival data from the VLT with the HAWK-I
camera in the Ks band (G. B. Brammer et al. 2016) and in data from the Spitzer Space
Telescope in IRAC bands 1 and 3 (3.6 and 5.7 μm), and MIPS 24 μm (P. Capak 2019).
PAN-BH*-1 is detected in the Ks band and in the two IRAC filters. Performing Spitzer
photometry of this source is challenging due to the large point spread function
(PSF) and a neighboring source, especially in the MIPS band. However, the NIRCam
photometry of the neighboring source suggests it has a limited contribution to the
IRAC fluxes. The details of the photometry extraction are described in Appendix
A, and the measured magnitudes in Table 2.\r\n\r\n2.2. VLT/X-Shooter Spectroscopy\r\nPAN-BH*-1
was observed for 5.8 ks with the X-Shooter spectrograph (J. Vernet et al. 2011)
on the VLT as a bright backup target for program 116.294D (PI: Matthee) in visitor
mode on 2025 December 17. The main aim of this program was to confirm candidate
LRDs at cosmic noon (Y. Ma et al. 2026). These observations confirmed the redshift
through the detection of Hα at z = 1.731. A DDT program (ID 116.2AQ0; PI: Matthee)
obtained additional follow-up data of PAN-BH*-1 in service mode for 26.2 ks during
2026 January 10–26, yielding a total exposure time of 8.9 hr. X-Shooter observes
with three arms simultaneously, UVB, VIS, and near-infrared (NIR), covering rest-frame
wavelengths of ≈0.14–0.9 μm, albeit hampered by skyline emission and telluric absorption,
primarily in the rest-frame optical.\r\n\r\nThe observing conditions were clear,
with a seeing ranging from 05 to 07 (median 06). The service mode observations were
primarily conducted during dark nights, with some gray (FLI = 0.03–0.6, median 0.1),
and a typical airmass of 1.35. We used UVB, VIS, and NIR slits with widths 10, 09,
and 09, yielding a nominal resolution of R = 5400, 8900, and 5600, respectively
(FWHM ∼53 km s−1 for NIR). The target acquisition was done using blind offsets from
a reference star, due to the target being too faint for direct acquisition. We used
a standard nodding on the slit pattern, with 4″ nod throws in an ABBA pattern, and
1″ jitters in the NIR arm to improve the sky subtraction. In each observing block
of ≈1 hr, the exposure times were 700, 655, and (2×)365 s for the three arms at
each nod position.\r\n\r\nThe reduction of the X-Shooter data uses a combination
of EsoRex libraries16 and Python code based on the reduction pipeline employed in
J. Matthee et al. (2021). Each observing block was reduced separately. We used standard
stars taken during the observing night for a first-pass flux calibration. Telluric
corrections were applied using the molecfit tool (A. Smette et al. 2015) implemented
in the X-Shooter EsoRex pipeline. Telluric stars were observed during the visitor
nights, but they were not always observed during the service mode observations in
January. For those observations, we took the telluric star that was observed at
the closest observing date. Based on the variation in telluric absorption among
the reference stars taken during this period, we estimate the variation in the transmission
and propagate the uncertainty in the telluric correction. For each observing block,
we then extracted an optimally extracted 1D spectrum using the spatial profile of
the Hα line, thus accounting for seeing variations and (more importantly) minor
errors in the accuracy of the slit pointing. Before median combining these spectra,
we normalize them by the median Hα flux of all observations to account for variations
in slit losses and flux calibrations.\r\n\r\nBesides Hα (integrated S/N = 75) and
Hβ (integrated S/N = 6; Section 3.2), we also detect continuum emission in the best
regions in the H and K bands at 1.6 μm and 2.1 μm, respectively, with a low signal-to-noise
ratio (S/N) of ∼1 per resolution element. Unfortunately, the [O iii] λλ4960, 5008
doublet is undetectable because the observed wavelengths are impacted by very strong
telluric absorption. No other lines or continuum are detected in the X-Shooter spectrum.\r\n\r\n3.
Properties of PAN-BH*-1\r\n3.1. Spectral Shape: A Photospheric Continuum with Strong
Hα Emission\r\nThe photometric SED of PAN-BH*-1 has remarkable similarities with
The Cliff (Figure 1): luminous in the rest optical, with a sudden drop toward the
rest-UV around the Balmer limit, and very weak near-to-mid infrared continuum emission.
With a rough extrapolation of the two HST photometric points using a power-law fit
(fλ ∝ λβ), we obtain a UV slope of β = −0.1 ± 1.2, and MUV = −16.7 ± 0.7. For the
rest-frame optical to NIR data, we fit a Planck blackbody law to the JWST data points,
after subtracting the measured Hα flux (see Section 3.2) from the F200W photometry.
The rest-optical and NIR photometry of PAN-BH*-1 is remarkably well described by
a single temperature blackbody with T = 4204 K (with a best-fit ). We measure the
strength of the Balmer break from the fν ratio F115W/F814W = 7 ± 1, in line with
the Balmer break strengths of The Cliff (; A. de Graaff et al. 2025a)17 and MoM-BH*
(7.8 ± 1.8; R. P. Naidu et al. 2025), measured from JWST/NIRSpec PRISM spectra as
fν,4000–4100/fν,3620−3720. In Figure 2, we compare the Balmer break strength with
the spectroscopic sample of A. de Graaff et al. (2025b), showing that out of 134
sources, only two have breaks significantly above 5. This suggests that PAN-BH*-1
has among the most extreme Balmer breaks known, although we caution that our value
is derived from wide-band photometry with pivot wavelengths corresponding to 4212
and 3042 Å, respectively, rather than from spectroscopy.\r\n\r\nZoom InZoom OutReset
image size\r\nFigure 1. SED of PAN-BH*-1 Top: cutouts from all the HST and JWST
images in which PAN-BH*-1 is covered. It shows a remarkably compact morphology in
all the wavelengths, resolved only in the HST F606W and F814W bands (Section 3.3).
Bottom: photometry from JWST/NIRCam (blue squares), HST/ACS (purple pentagons),
and Spitzer/IRAC+MIPS (red hexagons, and red triangle for the 5σ upper limit). The
empty square is the F200W flux after subtracting the Hα flux measured from X-Shooter
spectroscopy. We show the spectrum of The Cliff for comparison (gray line), shifted
to z = 1.73 and normalized to the F150W flux of PAN-BH*-1. We also show the best-fitting
blackbody spectrum (blue dashed line) and the best model from the synthetic LRD
atmosphere models from H. Liu et al. (2026), shifted to z = 1.73 (green line), undersampled
by a factor of 500 for clarity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\nZoom InZoom OutReset image size\r\nFigure 2. Spectroscopic sample of LRDs
by redshift and Balmer break strength. We plot the redshift and Balmer break strength
of PAN-BH*-1, and the JWST sample from A. de Graaff et al. (2025b) (purple diamonds),
and three local LRDs in X. Lin et al. (2026), for comparison. We also highlight
three sources with a particularly strong Balmer break: The Cliff (A. de Graaff et
al. 2025a), MoM-BH* (R. P. Naidu et al. 2025), and CAPERS-LRDz9 (A. J. Taylor et
al. 2025). The Balmer break strength of the JWST spectroscopic sample is computed
as fν,4000–4100/fν,3620–3720, whereas the value for PAN-BH*-1 is directly obtained
from the F115W/F814W photometry.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\n3.2. Hα and Hβ Emission Lines\r\nThe Hα profile appears as a complex combination
of a broad line with strong absorption close to the systemic redshift. We fit the
Hα emission line with a similar model as the one used in A. Torralba et al. (2026)
and J. Matthee et al. (2026). The Hα model consists of two Gaussian emission components
(with narrow and intermediate line widths), and a broad symmetric exponential convolved
with the intermediate profile and parameterized as in F. D’Eugenio et al. (2025a).
The absorption is implemented as an opacity law defined as e−τ(λ), where τ(λ) also
follows a single Gaussian velocity distribution (F. D’Eugenio et al. 2025a, 2025b;
A. Torralba et al. 2026). For simplicity, we assume a covering factor of Cf = 1
for the absorbing gas. In previous works, the width of the narrow component is tied
to that of [O iii], assuming both components come from the same region, often interpreted
as the interstellar medium (ISM) of the host galaxy. In this case, we have no information
about [O iii] due to this doublet falling in a wavelength range heavily affected
by strong telluric absorption. We fit the Hα line after masking relevant skylines
and strong telluric absorption bands. The fitted Hα parameters are listed in Table
1 and the best-fit model is shown in Figure 3. The absorption feature is notably
strong, with an equivalent width of EWabs = −148 ± 12 Å with respect to the fitted
continuum and 12.2 ± 0.2 Å if including the broad emission component. The absorption
corresponds to a Balmer optical depth at the line center of , reaching roughly the
continuum level. The FWHM of the single Gaussian fitted to the absorber is 283 ±
\ 8 km s−1, and is offset from the systemic redshift by −94 ± 4 km s−1. We note
that this parameterization is somewhat arbitrary, and we discuss in detail the absorber
properties in Section 4.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Hα
spectrum, and the best fit to our fiducial model. We show the X-Shooter R ∼ 5600
spectrum of the Hα line of PAN-BH*-1, along with the best-fit to the model described
in Section 3.2; total model (red solid line) and individual components (discontinuous
color lines). The red wing of the line is severely affected by telluric absorption,
thus the large uncertainties.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\nTable 1. Properties of PAN-BH*-1\r\n\r\nParameter\tValue\tUnit\r\nWidth
(FWHM; Hα)\r\nExponential\t1257 ± 27\tkm s−1\r\nIntermediate\t687 ± 43\tkm s−1\r\nNarrow\t184
± 12\tkm s−1\r\nAbsorption\t283 ± 8\tkm s−1\r\nFlux (Hα)\r\nExponential\t643 ± 7\t10−18
erg s−1 cm−2\r\nIntermediate\t19 ± 5\t10−18 erg s−1 cm−2\r\nNarrow\t38 ± 3\t10−18
erg s−1 cm−2\r\nTotal\t522 ± 7\t10−18 erg s−1 cm−2\r\nGeneral properties\r\n(LHα/erg
s−1)\t43.046 ± 0.006\t⋯\r\nEW0(Hα)\t520 ± 20\tÅ\r\nSFR(Hα, narrow)a\t2.1 ± 0.2\tM⊙
yr−1\r\nSFR(Hα, narrow)b\t3.3 ± 0.3\tM⊙ yr−1\r\nreff,UV (F606W+F814W)\t\tkpc\r\nreff,opt
(F200W)\t<0.047\tkpc\r\nHα/Hβ (total)\t>9.4\t⋯\r\nHα/Hβ (narrow)\t5 ± 1\t⋯\r\nNotes.
aCalibration from I. G. Kramarenko et al. (2026). bCalibration from R. C. Kennicutt
& N. J. Evans (2012). SFR values calculated assuming no dust attenuation.\r\n\r\nDownload
table as: \r\nASCIITypeset image\r\n\r\nThe Hβ line is marginally detected. After
undersampling the spectrum by a factor 5, a hint of a weak narrow component can
be identified (Figure 4), along with a tentative absorption at the same mean velocity
as in Hα. We fit the best Hα model to the Hβ spectrum, only rescaling it by a multiplicative
factor, and adding a flat continuum component. By doing this, we find an Hβ flux
of (47 ± 8) × 10−18 erg s−1 cm−2 (S/N ≈ 6). Conservatively, we obtain a Balmer decrement
of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with the high decrements found
for the LRD population (e.g., G. P. Nikopoulos et al. 2026; A. de Graaff et al.
2025b; J. Matthee et al. 2026). In Figure 5, we show the Hβ spectrum compared to
the rescaled Hα model. By matching the best-fit Hα profile with the data at the
expected observed wavelength for Hβ (±5000 km s−1), we obtain a better agreement
(, BIC = 1537) than fitting a flat continuum only (, BIC = 1658) with ΔBIC = 121
≫ 10, strongly favoring a detection of a broad Hβ emission line, and securing the
spectroscopic redshift. Similarly, we fit a narrow Gaussian to Hβ with the same
width and velocity as the Hα best-fit model, assuming a completely saturated absorption.
We obtain a Balmer decrement for the narrow component of Hα/Hβ = 5 ± 1, which would
imply a dust extinction of using a J. A. Cardelli et al. (1989) attenuation law,
under the assumption of case B recombination. However, due to the low S/N of Hβ
this result is only tentative, and compatible with a standard Case B value within
∼2σ.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. X-Shooter spectrum of Hα
and Hβ of PAN-BH*-1 (blue). We compare to the spectrum of The Cliff (gray; data
from JWST DDT #9433), normalized in each panel to the flux of PAN-BH*-1 in the range
v ∈ (−3000, −2000) km s−1. Due to the low S/N, the Hβ spectrum of PAN-BH*-1 is rebinned
to a coarser grid by a factor 5, after masking the most relevant skylines.\r\n\r\nDownload
figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image
size\r\nFigure 5. Hβ spectrum. The spectrum is rebinned by a factor of 10 with inverse
variance flux weighting for visual clarity, due to the low S/N. We compare to the
best-fit Hα model, scaled by a factor of 0.112. In the bottom panel, we show the
χ residuals between the spectrum and the rescaled Hα model in black, and for only
the continuum in pink (ΔBIC = 121 strongly favoring the presence of a broad Hβ line).\r\n\r\nDownload
figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.3. Spatial Morphology\r\nIn
order to assess whether PAN-BH*-1 is spatially resolved, we use the Bayesian profile
fitting software pysersic (I. Pasha & T. B. Miller 2023)18 to fit a single Sérsic
profile to the JWST and HST imaging data of PAN-BH*-1. For JWST/NIRCam, we choose
F200W as the filter with the highest S/N in the short wavelength channel, benefiting
from a high spatial resolution and probing rest-frame optical wavelengths. To model
its PSF, we use version 2.2.0 of the stpsf software (formerly webbpsf, M. D. Perrin
et al. 2014). For the two HST bands F606W and F814W, we instead construct empirical
PSFs from public imaging data in the GOODS-S field following A. Weibel et al. (2024).
In all three bands, we sample the posterior with the No U-turn sampler in two chains
with 1000 warm-up and 2000 sampling steps each. We find that PAN-BH*-1 is unresolved
with NIRCam in F200W where the effective radius converges toward the edge of the
prior at 0.25 pixels. Using the 95th percentile of the posterior chains as an upper
limit on the effective radius, we find a rest-optical size of reff < 47 pc.\r\n\r\nPAN-BH*-1
appears to be resolved in the HST images corresponding to rest-frame pivot 0.2 and
0.3 μm, respectively. Due to the low signal-to-noise of the F606W and F814W photometry,
we fit both bands simultaneously fixing all the morphological parameters in both
images. We measure physical effective radii of kpc (see Appendix B). The modest
stretching by the foreground A370 lensing cluster could imply a correction of ∼10%
to the measured radius (A. Niemiec et al. 2023), which we disregard given the uncertainties.
These measured sizes are consistent with the typical sizes for galaxies with a stellar
mass ≲ 109 M⊙ at z = 1.75 (A. van der Wel et al. 2014). These findings are consistent
with the scenario of a compact LRD “engine” dominating the rest-optical light embedded
in a host galaxy, whose contribution becomes significant blueward of the Balmer
break (see A. P. Cloonan et al. 2026, for a relevant discussion).\r\n\r\n4. Absorber
Kinematics\r\nAs described in Section 3.2, the velocity distribution of the absorber
is empirically modeled with a Gaussian, which we find has a central velocity of
−94 ± 4 km s−1 relative to the redshift of the narrow emission component (adopted
as systemic). The absorption trough extends from negative to positive velocities
with respect to the redshift of the narrow component, but also with respect to the
center of the symmetric exponential wings. However, there are several degeneracies
between the shape of the absorber and other components of the emission line, such
as the narrow central emission (see Section 3.2). Furthermore, direct interpretation
of the absorber center velocity shift is challenging in an optically thick gas with
presumably complex dynamics, and it does not necessarily trace bulk motion. A more
robust, physically motivated pair of quantities is the minimum and maximum absorber
velocities. We define them as the values where the transmission of the Balmer absorber
increases to 99%, km s−1 and km s−1. These values trace the largest velocities
in the line of sight of gas with significant Balmer absorption. The absorbing trough
extends over 787 ± 17 km s−1 under this definition. The values of and are relatively
agnostic to the choice of the shape of the absorber, since they are determined by
the wavelength where the line profile deviates from a broad, symmetric exponential
profile. In Figure 6, we illustrate three proposed configurations of the velocity
distribution of the absorbing gas that could explain the shape of the observed Balmer
absorption, and we discuss these scenarios below.\r\n\r\nZoom InZoom OutReset image
size\r\nFigure 6. Geometric configurations for the absorber. We illustrate three
scenarios that could give rise to the observed Balmer absorption in PAN-BH*-1. In
scenario (a), the obscuring agent is a thick screen of gas with a certain bulk velocity,
and turbulent motions produce the broadening of the absorption trough. In (b), there
are two (or more) absorbers with opposite velocities in the line of sight. These
first two scenarios are dynamically unstable; therefore, variability is expected
in the absorption. Lastly, in (c), we observed an extended source through a disk
wind with a rotational component (vϕ) in addition to the poloidal (nonazimuthal)
velocity (vp). In the last scenario, the redshifted absorption is produced by streamlines
that oppose the observer when projected along the line of sight, despite the fact
that the gas is outflowing from the central source.\r\n\r\nDownload figure:\r\n\r\nStandard
imageHigh-resolution image\r\n4.1. Unstable Gas Flows?\r\nThe fact that there is
significant absorption at both negative and positive velocities with respect to
the systemic redshift cannot be simply explained by an axisymmetric outflowing or
inflowing wind. In the case of observing a compact object through a spherically
symmetric, nonturbulent bulk flow, a classical P Cygni profile is expected, with
a purely blueshifted absorption (or redshifted if the wind is infalling). The fact
that we also see redshifted absorption rules out this simple scenario. In principle,
turbulent motions could also produce broadening of the absorbing medium (scenario
a in Figure 6). However, the required turbulent velocity dispersion σturb ≈ 120
km s−1 (from the Gaussian fit in Section 3.2) is comparable to the mean velocity
of the absorption trough, meaning that turbulence dominates the gas flow. In such
a case, strong variability of the absorption profile would be expected, given the
typical dynamical crossing times (see Sect. 4.1 in F. D’Eugenio et al. 2025b). For
example, for a radius of 1016 cm (e.g., A. Torralba et al. 2026) and a mass of 106
M⊙, the dynamical freefall time is yr. Moreover, the turbulent velocity would be
highly supersonic, and the dissipation timescale would be comparable to the dynamical
time (e.g., M.-M. Mac Low 1999). Alternatively, in the context of a strong Balmer
absorber at z ∼ 7, F. D’Eugenio et al. (2026) recently discussed a “breathing mode”
scenario with cyclic inflows and outflows along the same line of sight, with the
gas being in different phases at different depths (scenario b in Figure 6; see also
K. Park et al. 2017). In this case, the same arguments regarding the stability of
the absorber would apply, and absorber variability is expected on observed timescales
of ∼5 yr (for a source at z = 1.7), which is testable with future observations.\r\n\r\n4.2.
The Case for the Disk Wind Hypothesis\r\nAn alternative, dynamically stable scenario
is a disk wind configuration (scenario c in Figure 6). Here, the wind would be launched
from a thick disk near the central engine, which we speculate could be the source
of the optical continuum emission (e.g., H. Liu et al. 2025, 2026; L. Zwick et al.
2025; Y.-X. Chen et al. 2026). A rotating disk would imprint to the wind an azimuthal
velocity component (vϕ). Observations at specific lines of sight, particularly for
high inclination angles (close to edge-on) where the rotational component dominates
the poloidal velocity, can give rise to both blueshifted and redshifted absorption
features (D. Proga et al. 2000; P. B. Hall et al. 2002, 2013; D. Proga & T. R. Kallman
2004; M. Giustini & D. Proga 2012). Most observed LRDs have blueshifted P Cygni–like
absorbers (J. Matthee et al. 2026), which can be naively interpreted as a uniformly
expanding shell. The low incidence of redshifted Balmer absorbers in LRD spectra
(e.g., I. Labbe et al. 2024; A. de Graaff et al. 2025a; F. D’Eugenio et al. 2025b,
2026; Y. Ma et al. 2026) can therefore be explained by the requirement of high inclination
angles to observe such features (see also A. Sneppen et al. 2026). Such a picture
is broadly in line with disk wind models for AGN with broad absorption lines (e.g.,
P. B. Hall et al. 2002; H. Zhou et al. 2019) and around stars with circumstellar
disks (e.g., J. Erkal et al. 2022), such as accreting T Tauri stars (S. Edwards
et al. 2006) or cataclysmic variables (D. Proga 2003).\r\n\r\n4.3. Implications
of Rotating Winds for the Emission Lines of LRDs\r\nThe disk wind hypothesis would
imply that a photosphere in the shape of a rotating disk is the source of the optical
continuum emission, and drives winds that can explain the observed absorption trough.
Emission lines originating in a thin rotating disk would have a double-peaked profile
in the idealized case (for most inclination angles), but this is not necessarily
true if the disk is not sufficiently thin (e.g., N. Murray & J. Chiang 1997), for
instance, in the case of a puffed-up disk associated with super-Eddington accretion
(e.g., H. Liu et al. 2026). In addition, most line emission would not be produced
directly at the base of the disk, but slightly outside (e.g., via collisional cooling
or residual recombination; A. Torralba et al. 2026), where the rotational velocity
is lower, and the dynamics are complex (e.g., G. A. Shields 1977).\r\n\r\nThe Balmer
lines of most LRDs are dominated by broad, symmetric exponential components that
are associated with broadening by electron scattering (e.g., V. Rusakov et al. 2026;
J. Matthee et al. 2026). For PAN-BH*-1, the Hα line profile of PAN-BH*-1 is compatible
with a broad exponential profile emerging through a dense wind where the absorption
trough is produced. In dense gas with a large column density of neutral hydrogen,
and optically thick to Balmer transitions (NHI,2s ≳ 1014 cm−2), resonant scattering
effects become important. Crucially, resonant scattering impacts Hα and Hβ differently
(e.g., S.-J. Chang et al. 2026), hence the 3D radiative transfer and photon redistribution
of both lines may produce different profiles (see, e.g., Figure 2 in D. Proga 2003).
Therefore, the empirical fitting and interpretation of the absorption profiles becomes
nontrivial. Dedicated radiative transfer modeling is necessary to study such effects,
and they can be tested in other emission lines with high optical depth, such as
He i λ10830 Å, or resonant lines like C iv λ1550.\r\n\r\n5. Implications for the
Galaxy and Black Hole Masses\r\n5.1. Properties of the Host Galaxy\r\nAssuming that
the narrow component of Hα corresponds to ISM emission in the host galaxy, we compute
the associated star formation rate using the local calibration from R. C. Kennicutt
& N. J. Evans (2012) and assuming no dust attenuation. We obtain SFR(Hα) = 3.3 ±
0.3 M⊙ yr−1. A somewhat lower value of SFR(Hα) = 2.1 ± 0.2 M⊙ yr−1 is obtained using
the high-redshift (z ≳ 4) calibrations in I. G. Kramarenko et al. (2026), which
might be more appropriate for a young dwarf galaxy with a bursty star formation
history. The star formation rates are low, but in line with a main-sequence galaxy
with (extrapolating the relation from J. S. Speagle et al. 2014). Assuming zero
dust attenuation, the UV absolute magnitude (MUV = −16.7 ± 0.7; Section 3.1) would
imply SFR(UV) = 0.18 ± 0.12 M⊙ yr−1 (R. C. Kennicutt & N. J. Evans 2012). The discrepancy
between the UV and Hα inferred star formation rate suggests there is some amount
of dust attenuation in the host galaxy.\r\n\r\nWe derive a dynamical mass from the
width of the narrow component Hα line and the estimated UV size as , adopting the
empirical virial correction K(n)K(q) from A. van der Wel et al. (2022), where K(n)
and K(q) are functions of the best-fit ellipticity and Sérsic index (see Appendix
B). Adopting a Mdyn/M* factor of 40 as found by A. de Graaff et al. (2024) for dwarf
galaxies at high redshift, we infer a stellar mass of . However, the Mdyn/M* is
very uncertain in this regime, and the uncertainty can span over 1 dex (A. Saldana-Lopez
et al. 2025). We advise caution in interpreting this result, as there are large
uncertainties in the measurements of the narrow Hα component, the HST morphology,
and the empirical relations used.\r\n\r\nAs discussed in Section 4, the absorption
profile is compatible with broadening by a rotating disk wind, and numerical modeling
of such configurations often predicts a narrow component arising from increased
transmission due to purely kinematic effects in the wind geometry (D. Proga et al.
2000; D. Proga 2003; D. Proga & T. R. Kallman 2004). This would be an alternative
explanation for at least part of the narrow component flux. On the other hand, most
LRDs present narrow [O iii] emission that is often associated with the host galaxy.
Indeed, the ionized gas producing [O iii] emission should have associated emission
in the Hα and higher-order Balmer lines. However, constraining this component largely
depends on the assumptions on dust attenuation or ISM conditions, and requires very
high S/N and resolution data. Deep, space-based follow-up observations of PAN-BH*-1
would be very constraining for the wind kinematics (e.g., by the joint analysis
of Hβ) and to assess whether a narrow component comes from a host galaxy (e.g.,
by comparing to a narrow Hβ component or [O iii] λλ4960, 5008).\r\n\r\n5.2. Black
Hole Mass From Photosphere Models\r\nThe general physical setup of LRDs is an open
debate, and their masses are a major unknown. Due to the multiple differences with
respect to the classical AGN population, the validity of standard virial calibrations
has been questioned (e.g., V. Rusakov et al. 2026; J. E. Greene et al. 2026; A.
Sneppen et al. 2026; A. Torralba et al. 2026, although see, e.g., M. Brazzini et
al. 2025, 2026; J. Scholtz et al. 2026 for an alternative interpretation).\r\n\r\nOne
can obtain a mass estimate assuming a system in radiative equilibrium with Lbol/LEdd
= 1 (e.g., H. Umeda et al. 2026); this yields a total mass of ≈106 M⊙, using the
bolometric luminosity from integrating the best-fit blackbody in Section 3.1. Recently,
H. Liu et al. (2026) developed a synthetic spectral library of LRD atmosphere models.
In these models, the density of the photosphere is regulated by the net surface
gravity of an optically thick atmosphere, enabling constraints on the mass of the
system. We fit the JWST photometry of PAN-BH*-1 using the models from H. Liu et
al. (2026), assuming a negligible contribution from a host galaxy to the optical
continuum. The best-fit model has effective temperature Teff = 4800 K, surface gravity
, and metallicity (; see Figure 1). The best-fit implies a total mass of the system
(BH plus gas) of (Equation (6) in H. Liu et al. 2026, assuming hydrostatic equilibrium).
For the second and third best fits, we obtain and −2, respectively (, respectively;
with the same metallicity and effective temperature), which would imply lower limits
to the system mass between and 4. The bolometric luminosity of PAN-BH*-1 (from the
integral of the best-fit green curve in Figure 1) implies an Eddington luminosity
ratio of L/LEdd ≲ 13, assuming the best-fit mass from the H. Liu et al. (2026) models.
The elevated Eddington ratio is in line with the hypothesis of a radiation-driven
wind discussed in Section 4, and allows for somewhat larger system masses. The low
masses obtained with this model, combined with the stellar mass inferred from dynamical
arguments for the host galaxy (Section 3.3) set lower limits to the BH-to-stellar
mass ratio of MBH/M* ≳ 10−4–10−2, which are compatible with the relations observed
in the Local Universe, within the large uncertainties (A. E. Reines & M. Volonteri
2015).\r\n\r\n6. Conclusions\r\nIn this Letter, we presented the discovery and spectroscopic
confirmation of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.731. The
strength of the Balmer break (F115W/F814W = 7 ± 1) is comparable to the most extreme
LRDs known, The Cliff (A. de Graaff et al. 2025a) and MoM-BH* (R. P. Naidu et al.
2025). We summarize the observations and our main conclusions as follows.\r\n\r\n\r\n1.
\ \r\nWe obtained deep VLT/X-Shooter spectroscopy of PAN-BH*-1. The Hα emission
line is luminous and broad (LHα = 1043 erg s−1), and has an unusually strong absorption.
Hβ is detected with an S/N ≈ 6, and we conservatively estimate a lower limit for
the Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with other
LRDs in the literature (e.g., A. de Graaff et al. 2025b; G. P. Nikopoulos et al.
2026).\r\n2. \r\nThe absorption trough spans from −520 to 267 km s−1 (at a transmission
level of 99%). We interpret the presence of blue- and redshifted absorption as produced
by a disk wind, analogous to those analyzed in the context of broad absorption line
quasars or accreting stars. This hypothesis would imply that the source of the optical
continuum is likely a thick photospheric disk.\r\n3. \r\nWe detect a narrow Hα
component (FWHM = 184 ± 12 km s−1), which we interpret as probing a host galaxy
with M* ≈ 108 M⊙ and SFR = 2–3 M⊙. This interpretation is in line with the extended
rest-NUV morphology measured in the HST bands (\r\n kpc).\r\n4. \r\nBy fitting
the synthetic atmosphere models of H. Liu et al. (2026), we estimate a system mass
(BH+envelope) of 104–106 M⊙. The inferred masses, together with the stellar mass
inferred from morphology and narrow emission line dynamics, imply BH-to-stellar
mass ratios of 10−2–10−4, close to the extrapolated trend in the local Universe
(A. E. Reines & M. Volonteri 2015).\r\n5. \r\nThe confirmation of this source at
cosmic noon (magnitude of ≈22 in the K band, Hα flux ≈5 × 10−16 erg s−1 cm−2) proves
the feasibility of detecting extreme LRDs at such epochs with wide-area spectroscopic
surveys like Euclid or the forthcoming Nancy Grace Roman Space Telescope.\r\n\r\nAcknowledgments\r\nA.T.
thanks Debasish Dutta and Tamara Bogdanović for useful conversations about stellar
and AGN winds.\r\n\r\nWe thank the scientific referee for the useful and constructive
feedback, which helped improve the quality of this paper.\r\n\r\nJ.M. and A.T. acknowledge
funding by the European Union (ERC, AGENTS, 101076224). The work of CCW is supported
by NOIRLab, which is managed by the Association of Universities for Research in
Astronomy (AURA) under a cooperative agreement with the National Science Foundation.
A.P.C. warmly acknowledges the support of the National Science Foundation through
the NSF Graduate Research Fellowship Program. A.d.G. acknowledges support from a
Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.\r\n\r\nBased
on observations made with ESO Telescopes at the Paranal Observatory under program
IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is based in part on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with programs #2514 and #9433. C.C.W. gratefully acknowledges support for program
JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs
R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access
period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble
Space Telescope obtained from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., under NASA contract
NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST
and HST data presented in this article were obtained from the Mikulski Archive for
Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations
analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis work is based in
part on observations made with the Spitzer Space Telescope, which was operated by
the Jet Propulsion Laboratory, California Institute of Technology under a contract
with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis
work was supported by the International Space Science Institute (ISSI) in Bern,
through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST
cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope
(Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam,
NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space
Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration
et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al.
2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023),
stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL
Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP
(K. Barbary 2016)."
article_number: L37
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Aidan P.
full_name: Cloonan, Aidan P.
last_name: Cloonan
- first_name: Aayush A
full_name: Desai, Aayush A
id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
last_name: Desai
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Christian Kragh
full_name: Jespersen, Christian Kragh
last_name: Jespersen
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Wendy Q.
full_name: Sun, Wendy Q.
last_name: Sun
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: 'Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic
noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick
winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters.
2026;1005(2). doi:10.3847/2041-8213/ae7bfd'
apa: 'Torralba Torregrosa, A., Matthee, J. J., Weibel, A., Naidu, R. P., Ma, Y.,
Cloonan, A. P., … Williams, C. C. (2026). A black hole star at cosmic noon: Extreme
Balmer break, photospheric continuum, and broad absorption by thick winds in a
Little Red Dot at z = 1.7. The Astrophysical Journal Letters. IOP Publishing.
https://doi.org/10.3847/2041-8213/ae7bfd'
chicago: 'Torralba Torregrosa, Alberto, Jorryt J Matthee, Andrea Weibel, Rohan P.
Naidu, Yilun Ma, Aidan P. Cloonan, Aayush A Desai, et al. “A Black Hole Star at
Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption
by Thick Winds in a Little Red Dot at z = 1.7.” The Astrophysical Journal Letters.
IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae7bfd.'
ieee: 'A. Torralba Torregrosa et al., “A black hole star at cosmic noon:
Extreme Balmer break, photospheric continuum, and broad absorption by thick winds
in a Little Red Dot at z = 1.7,” The Astrophysical Journal Letters, vol.
1005, no. 2. IOP Publishing, 2026.'
ista: 'Torralba Torregrosa A, Matthee JJ, Weibel A, Naidu RP, Ma Y, Cloonan AP,
Desai AA, De Graaff A, Greene JE, Jespersen CK, Kramarenko I, Mascia S, Oesch
PA, Sun WQ, Williams CC. 2026. A black hole star at cosmic noon: Extreme Balmer
break, photospheric continuum, and broad absorption by thick winds in a Little
Red Dot at z = 1.7. The Astrophysical Journal Letters. 1005(2), L37.'
mla: 'Torralba Torregrosa, Alberto, et al. “A Black Hole Star at Cosmic Noon: Extreme
Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a
Little Red Dot at z = 1.7.” The Astrophysical Journal Letters, vol. 1005,
no. 2, L37, IOP Publishing, 2026, doi:10.3847/2041-8213/ae7bfd.'
short: A. Torralba Torregrosa, J.J. Matthee, A. Weibel, R.P. Naidu, Y. Ma, A.P.
Cloonan, A.A. Desai, A. De Graaff, J.E. Greene, C.K. Jespersen, I. Kramarenko,
S. Mascia, P.A. Oesch, W.Q. Sun, C.C. Williams, The Astrophysical Journal Letters
1005 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: "Based on observations made with ESO Telescopes at the
Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is
based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope.
The data were obtained from the Mikulski Archive for Space Telescopes at the Space
Telescope Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These
observations are associated with programs #2514 and #9433. C.C.W. gratefully acknowledges
support for program JWST-GO-2514 provided by NASA through a grant from the Space
Telescope Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge
the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing
program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations
made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated
with program #15117.\r\n\r\nThe JWST and HST data presented in this article were
obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope
Science Institute. The specific observations analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis
work is based in part on observations made with the Spitzer Space Telescope, which
was operated by the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis
work was supported by the International Space Science Institute (ISSI) in Bern,
through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST
cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope
(Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam,
NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space
Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration
et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al.
2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023),
stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL
Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP
(K. Barbary 2016)."
date_created: 2026-07-12T22:02:17Z
date_published: 2026-07-10T00:00:00Z
date_updated: 2026-07-13T08:08:41Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
- _id: IlCa
- _id: GradSch
doi: 10.3847/2041-8213/ae7bfd
external_id:
arxiv:
- '2603.28335'
file:
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checksum: 7600db260d799ddea45cf3bd01effe41
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creator: dernst
date_created: 2026-07-13T07:46:22Z
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file_name: 2026_AstrophysicalJourLetters_Torralba.pdf
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fulldoi: https://doi.org/10.3847/2041-8213/ae7bfd
has_accepted_license: '1'
intvolume: ' 1005'
issue: '2'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: 'A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum,
and broad absorption by thick winds in a Little Red Dot at z = 1.7'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 1005
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
_id: '22269'
abstract:
- lang: eng
text: The divisome apparatus synthesizes septal peptidoglycan (PG) during bacterial
division. In Escherichia coli, the class A penicillin-binding protein (aPBP) called
PBP1b has been implicated in division, but its role in the process has remained
unclear. Here we show using in situ cryo-electron tomography, genetics and other
imaging methods that PBP1b is required to produce a wedge-like density of PG at
the division site and that loss of this structure weakens the division site, making
it hypersusceptible to osmotic lysis. Surprisingly, the activator LpoB needed
for general PBP1b function was not required for its role in division. Of the two
PBP1b isoforms produced in cells, we show that the one with an extended cytoplasmic
N terminus localizes to and functions at the division site, probably via recruitment
by the FtsA component of the divisome. The conservation of aPBPs with extended
cytoplasmic N termini suggests that other Gram-negative bacteria may use similar
mechanisms for division site reinforcement.
acknowledgement: We thank all members of the Bernhardt, Rudner, Navarro and Vettiger
Laboratories for support and helpful conversations. We thank C. Genoud, J. Daraspe,
A. Mucciolo and D. de Bellis at the Electron Microscopy Facility of the University
of Lausanne and E. Jeanvoine for providing access to workstations for cryo-ET image
processing; S. Sterling, C. Borsa, J. Podgorski, P. Vinh Dip, E. Brignole and A.
Osherov at the MIT.nano cryo-EM facility, K. Song and C. Xu at the University of
Massachusetts cryo-EM facility, and R. Walsh and Z. Li at the cryo-EM at Harvard
Medical School facility for providing access to the cryo-EM microscopes and for
all their help, advice and maintenance of cryo-EM equipment. AFM was performed at
the Harvard University Center for Nanoscale Systems (CNS), a member of the National
Nanotechnology Coordinated Infrastructure Network (NNCI), which is supported by
the National Science Foundation under NSF award no. ECCS-2025158. We thank N. S.
Colella for excellent advice on AFM data acquisition and analysis; the MicRoN imaging
core at Harvard Medical School for excellent advice on live cell imaging and maintenance
of fluorescence microscopes; B. Krautz for creating the cartoon illustrations (www.sciencecommunicated.com);
and L. Miles and R. Aeschimann for assistance with strain construction. A.V. was
supported by an EMBO long-term postdoctoral fellowship ALTF_89-2019, the Swiss National
Science Foundation (SNSF) Postdoc.Mobility fellowship P500PB_203143. P.P.N. was
a recipient of early postdoc.mobility and postdoc.mobility fellowships (P2BSP3_188112
and P400PB_199252). This work was also supported by funding from the National Institutes
of Health (R35GM142553 to L.H.C. and R01AI083365 to T.G.B.), investigator funds
from the Howard Hughes Medical Institute (T.G.B.), an SNSF project grant (320030-236243
to A.V.), an SNSF Starting Grant (TMSGI3_218251 to P.P.N.), an SNSF Project grant
(320030-236069 to P.P.N), an SNSF SPARK grant (CRSK-3_237167 to P.P.N.), cryo-EM
funds from the Faculty of Biology and Medicine at University of Lausanne to P.P.N.
and the Foundation Pierre Mercier pour la Science (to P.P.N.).
article_processing_charge: Yes (in subscription journal)
article_type: original
author:
- first_name: Paula P.
full_name: Navarro, Paula P.
last_name: Navarro
- first_name: Andrea
full_name: Vettiger, Andrea
last_name: Vettiger
- first_name: Roman
full_name: Hajdu, Roman
id: ffab949d-133f-11ed-8f02-94de21ace503
last_name: Hajdu
- first_name: Virly Y.
full_name: Ananda, Virly Y.
last_name: Ananda
- first_name: Alejandro
full_name: López-Tavares, Alejandro
last_name: López-Tavares
- first_name: Ernst W.
full_name: Schmid, Ernst W.
last_name: Schmid
- first_name: Johannes C.
full_name: Walter, Johannes C.
last_name: Walter
- first_name: Martin
full_name: Loose, Martin
id: 462D4284-F248-11E8-B48F-1D18A9856A87
last_name: Loose
orcid: 0000-0001-7309-9724
- first_name: Luke H.
full_name: Chao, Luke H.
last_name: Chao
- first_name: Thomas G.
full_name: Bernhardt, Thomas G.
last_name: Bernhardt
citation:
ama: Navarro PP, Vettiger A, Hajdu R, et al. The penicillin-binding protein PBP1b
fortifies the Escherichia coli division site against osmotic rupture. Nature
Microbiology. 2026. doi:10.1038/s41564-026-02403-6
apa: Navarro, P. P., Vettiger, A., Hajdu, R., Ananda, V. Y., López-Tavares, A.,
Schmid, E. W., … Bernhardt, T. G. (2026). The penicillin-binding protein PBP1b
fortifies the Escherichia coli division site against osmotic rupture. Nature
Microbiology. Springer Nature. https://doi.org/10.1038/s41564-026-02403-6
chicago: Navarro, Paula P., Andrea Vettiger, Roman Hajdu, Virly Y. Ananda, Alejandro
López-Tavares, Ernst W. Schmid, Johannes C. Walter, Martin Loose, Luke H. Chao,
and Thomas G. Bernhardt. “The Penicillin-Binding Protein PBP1b Fortifies the Escherichia
Coli Division Site against Osmotic Rupture.” Nature Microbiology. Springer
Nature, 2026. https://doi.org/10.1038/s41564-026-02403-6.
ieee: P. P. Navarro et al., “The penicillin-binding protein PBP1b fortifies
the Escherichia coli division site against osmotic rupture,” Nature Microbiology.
Springer Nature, 2026.
ista: Navarro PP, Vettiger A, Hajdu R, Ananda VY, López-Tavares A, Schmid EW, Walter
JC, Loose M, Chao LH, Bernhardt TG. 2026. The penicillin-binding protein PBP1b
fortifies the Escherichia coli division site against osmotic rupture. Nature Microbiology.
mla: Navarro, Paula P., et al. “The Penicillin-Binding Protein PBP1b Fortifies the
Escherichia Coli Division Site against Osmotic Rupture.” Nature Microbiology,
Springer Nature, 2026, doi:10.1038/s41564-026-02403-6.
short: P.P. Navarro, A. Vettiger, R. Hajdu, V.Y. Ananda, A. López-Tavares, E.W.
Schmid, J.C. Walter, M. Loose, L.H. Chao, T.G. Bernhardt, Nature Microbiology
(2026).
das_tickbox: '1'
dataavailabilitystatement: 'The data, plasmids and strains that support the findings
of this study are available from the corresponding authors by request. Representative
tomograms are deposited in EMDB: EMD-27479 (wild-type), EMD-53351 (∆ponB), EMD-53357(∆lpoB)
and EMD-53363 (∆ponA). Corresponding raw movie frames and stacks of tilt series
are deposited as EMPIAR-11090 (wild type), EMPIAR-13502 (∆ponB), EMPIAR-13513 (∆lpoB)
and EMPIAR-13512 (∆ponA), and will be released upon publication. Other data related
to this manuscript (for example, AFM, light microscopy, growth curves and so on)
can be found on Zenodo at https://doi.org/10.5281/zenodo.20841819 (ref. 101). Source
data are provided with this paper. Scripts used in this study were deposited on
GitHub at https://github.com/NavarroVettiger/Navarro-et-al_2022 and https://github.com/virlyananda/EM-ImageProcessing.'
date_created: 2026-07-12T22:02:19Z
date_published: 2026-07-03T00:00:00Z
date_updated: 2026-07-13T09:22:49Z
day: '03'
ddc:
- '570'
department:
- _id: MaLo
- _id: GradSch
doi: 10.1038/s41564-026-02403-6
external_id:
pmid:
- '42399561'
fulldoi: https://doi.org/10.1038/s41564-026-02403-6
has_accepted_license: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1038/s41564-026-02403-6
month: '07'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Microbiology
publication_identifier:
eissn:
- 2058-5276
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: The penicillin-binding protein PBP1b fortifies the Escherichia coli division
site against osmotic rupture
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '22292'
abstract:
- lang: eng
text: We show that a suitable choice of boundary conditions for the Laplacian allows
for the appearance of an arbitrary number of condensates, described by arbitrary
harmonic functions, in the thermodynamic limit of an ideal Bose gas.
acknowledgement: We are grateful to Rupert Frank and Jakob Yngvason for helpful discussions
and suggestions.
article_number: '061901'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Michiel
full_name: De Wilde, Michiel
id: bebf1407-6635-11f0-9fef-9b7e2dd151d0
last_name: De Wilde
- first_name: Robert
full_name: Seiringer, Robert
id: 4AFD0470-F248-11E8-B48F-1D18A9856A87
last_name: Seiringer
orcid: 0000-0002-6781-0521
citation:
ama: De Wilde M, Seiringer R. Arbitrary harmonic functions as Bose–Einstein condensates.
Journal of Mathematical Physics. 2026;67(6). doi:10.1063/5.0325354
apa: De Wilde, M., & Seiringer, R. (2026). Arbitrary harmonic functions as Bose–Einstein
condensates. Journal of Mathematical Physics. AIP Publishing. https://doi.org/10.1063/5.0325354
chicago: De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions
as Bose–Einstein Condensates.” Journal of Mathematical Physics. AIP Publishing,
2026. https://doi.org/10.1063/5.0325354.
ieee: M. De Wilde and R. Seiringer, “Arbitrary harmonic functions as Bose–Einstein
condensates,” Journal of Mathematical Physics, vol. 67, no. 6. AIP Publishing,
2026.
ista: De Wilde M, Seiringer R. 2026. Arbitrary harmonic functions as Bose–Einstein
condensates. Journal of Mathematical Physics. 67(6), 061901.
mla: De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions as Bose–Einstein
Condensates.” Journal of Mathematical Physics, vol. 67, no. 6, 061901,
AIP Publishing, 2026, doi:10.1063/5.0325354.
short: M. De Wilde, R. Seiringer, Journal of Mathematical Physics 67 (2026).
corr_author: '1'
das_tickbox: '1'
dataavailabilitystatement: Data sharing is not applicable to this article as no new
data were created or analyzed in this study.
date_created: 2026-07-13T09:45:09Z
date_published: 2026-06-01T00:00:00Z
date_updated: 2026-07-13T12:20:59Z
day: '01'
department:
- _id: RoSe
- _id: GradSch
doi: 10.1063/5.0325354
external_id:
arxiv:
- '2601.22883'
fulldoi: https://doi.org/10.1063/5.0325354
intvolume: ' 67'
issue: '6'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2601.22883
month: '06'
oa: 1
oa_version: Preprint
publication: Journal of Mathematical Physics
publication_identifier:
eissn:
- 1089-7658
issn:
- 0022-2488
publication_status: published
publisher: AIP Publishing
quality_controlled: '1'
researchdata_availability: not applicable
scopus_import: '1'
status: public
supplementarymaterial: not applicable
title: Arbitrary harmonic functions as Bose–Einstein condensates
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 67
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
PlanS_conform: '1'
_id: '22301'
abstract:
- lang: eng
text: Auxin, primarily indole-3-acetic acid (IAA), is a central regulator of growth
and development in land plants, but its physiological role in chlorophyte algae
remains unclear. Here, we show that exogenous IAA modulates growth in Chlorella
sorokiniana, Chlorella variabilis, and Chlamydomonas reinhardtii in a concentration-dependent
manner. Low IAA concentrations promoted growth by accelerating the onset of cell
division without affecting cell size, whereas higher concentrations inhibited
proliferation. Radiotracer assays showed that all three species take up and release
IAA across the plasma membrane through a combination of passive diffusion and
energy-dependent, saturable processes. Competition by excess unlabeled natural
and synthetic auxins further supported the presence of carrier-mediated transport
with broad substrate recognition. Phylogenetic analyses identified potential PIN-like
auxin exporters in chlorophytes and other non-plant eukaryotes, and structural
modeling supported conservation of the overall PIN fold and predicted auxin-binding
residues. However, functional assays in Xenopus laevis oocytes, tobacco BY-2 cultured
cells, and Arabidopsis thaliana did not support a role for these proteins in directional
auxin export. Instead, non-plant PIN homologs localized predominantly to the endoplasmic
reticulum and showed limited or no transport activity in heterologous systems.
Together, these findings indicate that auxin responsiveness and basic cellular
auxin transport predate canonical PIN-mediated directional auxin export, which
appears to be a later innovation of the streptophyte lineage.
acknowledged_ssus:
- _id: Bio
- _id: NanoFab
acknowledgement: Research in the Friml group was supported by the European Research
Council (ERC) under grant agreement No. 101142681 (CYNIPS), and by the Austrian
Science Fund (FWF) through projects I 6123-B and P 37051-B. A DOC Fellowship from
the Austrian Academy of Sciences (ÖAW; PR.C0102.1.F.1023.A.2) provided additional
support. Work was partly supported by the Deutsche Forschungsgemeinschaft (DFG,
German Research Foundation) under grant HA 3468/8-1. We thank the Imaging and Optics
Facility (IOF) at the Institute of Science and Technology Austria (ISTA) for support
with confocal imaging, and the Nanofabrication Facility at ISTA for assistance with
microfluidic device fabrication. We also acknowledge the microscopy service of IFIEB
CAS, supported by MEYS CR (LM2023050 Czech-BioImaging). Open Access funding provided
by Institute of Science and Technology Austria.
article_number: jipb.70309
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Adrijana
full_name: Smoljan, Adrijana
id: cced8a85-223e-11ed-af04-b0596c55053b
last_name: Smoljan
- first_name: Sarah
full_name: Koutnik‐Abele, Sarah
last_name: Koutnik‐Abele
- first_name: Dmitrii
full_name: Vladimirtsev, Dmitrii
id: 60466724-5355-11ee-ae5a-fa55e8f99c3d
last_name: Vladimirtsev
- first_name: Petr
full_name: Klíma, Petr
last_name: Klíma
- first_name: Anita
full_name: Bírošíková, Anita
last_name: Bírošíková
- first_name: Yuzhou
full_name: Zhang, Yuzhou
id: 3B6137F2-F248-11E8-B48F-1D18A9856A87
last_name: Zhang
orcid: 0000-0003-2627-6956
- first_name: Jack
full_name: Merrin, Jack
id: 4515C308-F248-11E8-B48F-1D18A9856A87
last_name: Merrin
orcid: 0000-0001-5145-4609
- first_name: Maximilian
full_name: Schuster, Maximilian
id: 37e65def-d415-11eb-ae59-a7b67be103db
last_name: Schuster
- first_name: Katarina
full_name: Kurtović, Katarina
last_name: Kurtović
- first_name: Ulrich Z.
full_name: Hammes, Ulrich Z.
last_name: Hammes
- first_name: Jan
full_name: Petrášek, Jan
last_name: Petrášek
- first_name: Jiří
full_name: Friml, Jiří
id: 4159519E-F248-11E8-B48F-1D18A9856A87
last_name: Friml
orcid: 0000-0002-8302-7596
citation:
ama: Smoljan A, Koutnik‐Abele S, Vladimirtsev D, et al. Auxin response and PIN‐mediated
transport in chlorophyte algae. Journal of Integrative Plant Biology. 2026.
doi:10.1111/jipb.70309
apa: Smoljan, A., Koutnik‐Abele, S., Vladimirtsev, D., Klíma, P., Bírošíková, A.,
Zhang, Y., … Friml, J. (2026). Auxin response and PIN‐mediated transport in chlorophyte
algae. Journal of Integrative Plant Biology. Wiley. https://doi.org/10.1111/jipb.70309
chicago: Smoljan, Adrijana, Sarah Koutnik‐Abele, Dmitrii Vladimirtsev, Petr Klíma,
Anita Bírošíková, Yuzhou Zhang, Jack Merrin, et al. “Auxin Response and PIN‐mediated
Transport in Chlorophyte Algae.” Journal of Integrative Plant Biology.
Wiley, 2026. https://doi.org/10.1111/jipb.70309.
ieee: A. Smoljan et al., “Auxin response and PIN‐mediated transport in chlorophyte
algae,” Journal of Integrative Plant Biology. Wiley, 2026.
ista: Smoljan A, Koutnik‐Abele S, Vladimirtsev D, Klíma P, Bírošíková A, Zhang Y,
Merrin J, Schuster M, Kurtović K, Hammes UZ, Petrášek J, Friml J. 2026. Auxin
response and PIN‐mediated transport in chlorophyte algae. Journal of Integrative
Plant Biology., jipb. 70309.
mla: Smoljan, Adrijana, et al. “Auxin Response and PIN‐mediated Transport in Chlorophyte
Algae.” Journal of Integrative Plant Biology, jipb. 70309, Wiley, 2026,
doi:10.1111/jipb.70309.
short: A. Smoljan, S. Koutnik‐Abele, D. Vladimirtsev, P. Klíma, A. Bírošíková, Y.
Zhang, J. Merrin, M. Schuster, K. Kurtović, U.Z. Hammes, J. Petrášek, J. Friml,
Journal of Integrative Plant Biology (2026).
corr_author: '1'
das_tickbox: '0'
date_created: 2026-07-13T10:44:55Z
date_published: 2026-06-10T00:00:00Z
date_updated: 2026-07-13T14:26:31Z
day: '10'
ddc:
- '580'
department:
- _id: JiFr
- _id: GradSch
- _id: NanoFab
- _id: Bio
doi: 10.1111/jipb.70309
external_id:
pmid:
- '42271607'
fulldoi: https://doi.org/10.1111/jipb.70309
has_accepted_license: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/jipb.70309
month: '06'
oa: 1
oa_version: Published Version
pmid: 1
project:
- _id: 8f347782-16d5-11f0-9cad-8c19706ee739
grant_number: '101142681'
name: Cyclic nucleotides as second messengers in plants
- _id: bd76d395-d553-11ed-ba76-f678c14f9033
grant_number: I06123
name: Peptide receptors for auxin canalization in Arabidopsis
- _id: 7bcece63-9f16-11ee-852c-ae94e099eeb6
grant_number: P37051
name: Guanylate cyclase activity of TIR1/AFBs auxin receptors
publication: Journal of Integrative Plant Biology
publication_identifier:
eissn:
- 1744-7909
issn:
- 1672-9072
publication_status: epub_ahead
publisher: Wiley
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: Auxin response and PIN‐mediated transport in chlorophyte algae
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: publisher
OA_type: hybrid
_id: '22129'
abstract:
- lang: eng
text: "Inside–outside classification is widely used for geometry processing tasks
such as surface reconstruction, geometry completion,\r\nand calculating signed
distance fields. We introduce a new integral formulation of this problem, which
assigns confidence\r\nscores that points are inside or outside, given incomplete
boundary geometry. Even though our geometric construction does\r\nnot appear in
previous work, we show that it is unexpectedly linked to both the well-established
generalized winding number\r\n(GWN) and pseudonormal methods for geometry completion,
and it provably reduces to either one of them for specific values\r\nof a control
parameter. The results obtained with our method frequently outperform screened
Poisson surface reconstruction\r\n(PSR), GWN, and the pseudonormal method in terms
of quality, and are at least on par with them on all of our examples. Unlike\r\nthese
methods, our algorithm naturally extends to the multi-label setting, in which
regions with an arbitrary number of colors\r\nor physical materials can be reconstructed,
and non-manifold features such as T-junctions may appear in the interface and\r\nboundary
geometry"
article_processing_charge: Yes (via OA deal)
author:
- first_name: 'Ziyu '
full_name: 'Wei, Ziyu '
last_name: Wei
- first_name: Christian
full_name: Hafner, Christian
id: 400429CC-F248-11E8-B48F-1D18A9856A87
last_name: Hafner
- first_name: Aleksei
full_name: Kalinov, Aleksei
id: 44b7120e-eb97-11eb-a6c2-e1557aa81d02
last_name: Kalinov
orcid: 0000-0003-2189-3904
- first_name: Peter
full_name: Synak, Peter
id: 331776E2-F248-11E8-B48F-1D18A9856A87
last_name: Synak
- first_name: Christopher J
full_name: Wojtan, Christopher J
id: 3C61F1D2-F248-11E8-B48F-1D18A9856A87
last_name: Wojtan
orcid: 0000-0001-6646-5546
citation:
ama: 'Wei Z, Hafner C, Kalinov A, Synak P, Wojtan C. Circles of confidence for multi-label
geometry completion. In: Computer Graphics Forum. Vol 45. Wiley. doi:10.1111/cgf.70516'
apa: 'Wei, Z., Hafner, C., Kalinov, A., Synak, P., & Wojtan, C. (n.d.). Circles
of confidence for multi-label geometry completion. In Computer Graphics Forum
(Vol. 45). Bern, Switzerland: Wiley. https://doi.org/10.1111/cgf.70516'
chicago: Wei, Ziyu , Christian Hafner, Aleksei Kalinov, Peter Synak, and Chris Wojtan.
“Circles of Confidence for Multi-Label Geometry Completion.” In Computer Graphics
Forum, Vol. 45. Wiley, n.d. https://doi.org/10.1111/cgf.70516.
ieee: Z. Wei, C. Hafner, A. Kalinov, P. Synak, and C. Wojtan, “Circles of confidence
for multi-label geometry completion,” in Computer Graphics Forum, Bern,
Switzerland, vol. 45, no. 5.
ista: 'Wei Z, Hafner C, Kalinov A, Synak P, Wojtan C. Circles of confidence for
multi-label geometry completion. Computer Graphics Forum. Eurographics: Symposium
on Geometry Processing vol. 45.'
mla: Wei, Ziyu, et al. “Circles of Confidence for Multi-Label Geometry Completion.”
Computer Graphics Forum, vol. 45, no. 5, Wiley, doi:10.1111/cgf.70516.
short: Z. Wei, C. Hafner, A. Kalinov, P. Synak, C. Wojtan, in:, Computer Graphics
Forum, Wiley, n.d.
conference:
end_date: 2026-07-03
location: Bern, Switzerland
name: 'Eurographics: Symposium on Geometry Processing'
start_date: 2026-07-01
corr_author: '1'
das_tickbox: '1'
date_created: 2026-06-23T09:08:41Z
date_published: 2026-06-24T00:00:00Z
date_updated: 2026-07-13T14:58:48Z
day: '24'
ddc:
- '005'
department:
- _id: ChWo
- _id: GradSch
doi: 10.1111/cgf.70516
file:
- access_level: open_access
checksum: 365f986db34e3fbce74089207599253b
content_type: application/pdf
creator: mly
date_created: 2026-06-23T09:07:22Z
date_updated: 2026-06-23T09:07:22Z
file_id: '22132'
file_name: document(3).pdf
file_size: 14536575
relation: main_file
success: 1
file_date_updated: 2026-06-23T09:07:22Z
fulldoi: https://doi.org/10.1111/cgf.70516
has_accepted_license: '1'
intvolume: ' 45'
issue: '5'
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
project:
- _id: 34bc2376-11ca-11ed-8bc3-9a3b3961a088
grant_number: '101045083'
name: Computational Discovery of Numerical Algorithms for Animation and Simulation
of Natural Phenomena
publication: Computer Graphics Forum
publication_status: accepted
publisher: Wiley
quality_controlled: '1'
status: public
title: Circles of confidence for multi-label geometry completion
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: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 45
year: '2026'
...