---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21998'
abstract:
- lang: eng
text: Little Red Dots (LRDs), among the most enigmatic high-redshift discoveries
by JWST, are commonly believed to be powered by accreting supermassive black holes.
Here, we explore the possibility that these sources are globular clusters in formation,
with rest-frame UV arising from a very young stellar population and rest-frame
optical from a short-lived supermassive (>104 M⊙) star. The spectral profiles
of LRDs are broadly consistent with this scenario, though the observed temperatures
and bolometric luminosities favor emission reprocessed by optically thick continuum-driven
winds not fully captured by current models. The LRD z ∼ 5−7 UV luminosity function
naturally evolves, under standard evolutionary and mass-loss prescriptions, into
a present-day mass function with a turnover at log10(M*/M⊙) = 5.3 and an exponential
cutoff at high masses, consistent with local globular cluster populations. We
estimate the total present-day number density of LRDs formed across all redshifts
to be ≈0.3 Mpc−3, similar within uncertainties to local globular clusters. The
observed LRD redshift range matches the age distribution of metal-poor globular
clusters, without current LRD counterparts to the metal-rich population. If LRDs
are globular clusters in formation, we predict chemical abundance patterns characteristic
of multiple stellar populations, including enhanced He and N, and potential Na–O
and Al–Mg anticorrelations. These results offer a local perspective to explore
this surprisingly abundant population of distant sources, and a potential new
window into extreme stellar astrophysics in the early Universe.
acknowledgement: "We thank the referees for detailed and highly constructive reports
that significantly improved the scope and breadth of the manuscript. J.C. thanks
Hollis Akins, Volker Bromm, Rui Chaves-Marques, Steve Finkelstein, Karl Gebhardt,
Keith Hawkins, Harley Katz, Stellar Offner, Daniel Schaerer, Grace Telford, and
Jorick Vink for conversations that improved the Letter. A.d.G. acknowledges support
from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory. M.B.K.
acknowledges support from NSF grants AST-2108962 and AST-2408247; NASA grant 80NSSC22K0827;
HST-GO-16686, HST-AR-17028, JWST-GO-03788, and JWST-AR-06278 from the Space Telescope
Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555;
and from the Samuel T. and Fern Yanagisawa Regents Professorship in Astronomy at
UT Austin. A.A.C.S. acknowledges support by the Deutsche Forschungsgemeinschaft
(DFG, German Research Foundation) in the form of an Emmy Noether Research Group—Project-ID
445674056 (SA4064/1-1, PI Sander). A.A.C.S. further acknowledges support from the
Deutsches Zentrum für Luft und Raumfahrt (DLR) grant grants 50 OR 2509 (PI: A.A.C.
Sander) and 50 OR 2306 (PI: V. Ramachandran/A.A.C. Sander) as well as from the Federal
Ministry of Research, Technology, and Space (BMFTR) and the Baden-Württemberg Ministry
of Science as part of the Excellence Strategy of the German Federal and State Governments.
This project was cofunded by the European Union (Project 101183150—OCEANS).\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 1180, 1181, 1208, 1212, 1213,
1215, 1286, 1345, 1433, 2198, 2561, 2750, 2767, 4106, 4233, 5105, 5224, 6368, and
6585."
article_number: L4
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Danielle A.
full_name: Berg, Danielle A.
last_name: Berg
- first_name: Michael
full_name: Boylan-Kolchin, Michael
last_name: Boylan-Kolchin
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- 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: Julian B.
full_name: Muñoz, Julian B.
last_name: Muñoz
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Andreas A.C.
full_name: Sander, Andreas A.C.
last_name: Sander
citation:
ama: Chisholm J, Berg DA, Boylan-Kolchin M, et al. Little Red Dots as globular clusters
in formation. The Astrophysical Journal Letters. 2026;1004(1). doi:10.3847/2041-8213/ae6dae
apa: Chisholm, J., Berg, D. A., Boylan-Kolchin, M., De Graaff, A., Furtak, L. J.,
Kokorev, V., … Sander, A. A. C. (2026). Little Red Dots as globular clusters in
formation. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae6dae
chicago: Chisholm, John, Danielle A. Berg, Michael Boylan-Kolchin, Anna De Graaff,
Lukas J. Furtak, Vasily Kokorev, Jorryt J Matthee, Julian B. Muñoz, Rohan P. Naidu,
and Andreas A.C. Sander. “Little Red Dots as Globular Clusters in Formation.”
The Astrophysical Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae6dae.
ieee: J. Chisholm et al., “Little Red Dots as globular clusters in formation,”
The Astrophysical Journal Letters, vol. 1004, no. 1. IOP Publishing, 2026.
ista: Chisholm J, Berg DA, Boylan-Kolchin M, De Graaff A, Furtak LJ, Kokorev V,
Matthee JJ, Muñoz JB, Naidu RP, Sander AAC. 2026. Little Red Dots as globular
clusters in formation. The Astrophysical Journal Letters. 1004(1), L4.
mla: Chisholm, John, et al. “Little Red Dots as Globular Clusters in Formation.”
The Astrophysical Journal Letters, vol. 1004, no. 1, L4, IOP Publishing,
2026, doi:10.3847/2041-8213/ae6dae.
short: J. Chisholm, D.A. Berg, M. Boylan-Kolchin, A. De Graaff, L.J. Furtak, V.
Kokorev, J.J. Matthee, J.B. Muñoz, R.P. Naidu, A.A.C. Sander, The Astrophysical
Journal Letters 1004 (2026).
date_created: 2026-06-14T22:01:42Z
date_published: 2026-06-10T00:00:00Z
date_updated: 2026-06-19T09:50:33Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ae6dae
external_id:
arxiv:
- '2602.15935'
file:
- access_level: open_access
checksum: 66949af6e620c8ef37de42688829a3e3
content_type: application/pdf
creator: dernst
date_created: 2026-06-19T09:45:21Z
date_updated: 2026-06-19T09:45:21Z
file_id: '22098'
file_name: 2026_AstrophysicalJourLetters_Chisholm.pdf
file_size: 919919
relation: main_file
success: 1
file_date_updated: 2026-06-19T09:45:21Z
has_accepted_license: '1'
intvolume: ' 1004'
issue: '1'
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Little Red Dots as globular clusters in formation
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: 1004
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '21709'
abstract:
- lang: eng
text: 'JWST’s “little red dots” (LRDs) are increasingly interpreted as active galactic
nuclei (AGN) obscured by dense thermalized gas rather than dust as evidenced by
their X-ray weakness, blackbody-like continua, and Balmer line profiles. Key questions
are how LRDs connect to standard UV-luminous AGN, whether transitional phases
exist, and whether they are observable. We present the “X-ray dot” (XRD), a compact
source at z = 3.28 observed by the NIRSpec Wide Guaranteed Time Observation survey.
The XRD exhibits LRD hallmarks: a blackbody-like (Teff ≃ 6400 K) red continuum,
a faint but blue rest-UV excess, falling mid-IR emission, and broad Balmer lines
(FWHM ∼ 2700–3200 km s−1). Unlike LRDs, however, it is remarkably X-ray luminous
(L2−10 keV = 1044.18 erg s−1) and has a continuum inflection that is blueward
of the Balmer limit. We find that the red rest-optical and blue mid-IR continuum
cannot be reproduced by standard dust-attenuated AGN models without invoking extremely
steep extinction curves, nor can the weak mid-IR emission be reconciled with well-established
X-ray–torus scaling relations. We therefore consider an alternative scenario:
the XRD may be an LRD in transition, where the gas envelope dominates the optical
continuum but optically thin sight lines allow X-rays to escape. The XRD may thus
provide a physical link between LRDs and standard AGN, offering direct evidence
that LRDs are powered by supermassive black holes and providing insight into their
accretion properties.'
acknowledgement: "We would like to thank the anonymous reviewer for their constructive
comments, which improved the final manuscript.\r\n\r\nWe thank Bernd Husemann for
his critical contributions to the NIRSpec Wide GTO survey, and in particular his
help in selecting high-priority X-ray-luminous targets.\r\n\r\nR.E.H. acknowledges
support by the German Aerospace Center (DLR) and the Federal Ministry for Economic
Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.” A.d.G. acknowledges
support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.
A.J.B. acknowledges funding from the “FirstGalaxies” Advanced grant from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
program (grant agreement No. 789056). R.P.N. thanks Neil Pappalardo and Jane Pappalardo
for their generous support of the MIT Pappalardo Fellowships in Physics. Support
for this work was provided by the Brinson Foundation through a Brinson Prize Fellowship
grant. H.Ü. acknowledges funding by the European Union (ERC APEX, 101164796). 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 Executive Agency.
Neither the European Union nor the granting authority can be held responsible for
them. G.V. acknowledges support from European Union’s HE ERC Starting grant No.
101040227—WINGS. B.W. acknowledges support provided by NASA through Hubble Fellowship
grant HST-HF2-51592.001 awarded by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in Astronomy, In., for
NASA, under the contract NAS 5-26555.\r\n\r\nThe data products presented herein
were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic
Dawn Center (DAWN).\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
Nos. GTO-1213. The data described here may be obtained from the MAST archive at
DOI: 10.17909/qffz-b324.\r\n\r\nThis Letter employs a list of Chandra datasets,
obtained by the Chandra X-ray Observatory, contained in DOI: 10.25574/cdc.540.\r\n\r\nThis
work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and
12328) with the NASA/ESA HST, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555.\r\n\r\nThis work
makes use of color palettes created by Martin Krzywinski designed for colorblindness.
The color palettes and more information can be found at http://mkweb.bcgsc.ca/colorblind/.\r\n\r\nFacilities:
CXO - Chandra X-ray Observatory satellite (ACIS), HST - Hubble Space Telescope satellite
(ACS, WFC3) - , CFHT - Canada-France-Hawaii Telescope (WIRCam), JWST - James Webb
Space Telescope (NIRSpec), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS)
- , JCMT - James Clerk Maxwell Telescope (SCUBA).\r\n\r\nSoftware: Astropy (Astropy
Collaboration et al. 2013, 2018, 2022), dust_attenuation, dust_extinction (K. Gordon
2024), jax (J. Bradbury et al. 2018), LaTeX (L. Lamport 1994), Matplotlib (J. D.
Hunter 2007), NumPy (T. E. Oliphant 2006; S. van der Walt et al. 2011; C. R. Harris
et al. 2020), NumPyro (D. Phan et al. 2019), scipy (P. Virtanen et al. 2020), sedpy
(B. Johnson & J. Leja 2017), specutils (Astropy-Specutils Development Team 2019),
unite (R. E. Hviding 2025)."
article_number: L18
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Raphael E.
full_name: Hviding, Raphael E.
last_name: Hviding
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Hanpu
full_name: Liu, Hanpu
last_name: Liu
- first_name: Andy D.
full_name: Goulding, Andy D.
last_name: Goulding
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Andrew J.
full_name: Bunker, Andrew J.
last_name: Bunker
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Marijn
full_name: Franx, Marijn
last_name: Franx
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Hannah
full_name: Übler, Hannah
last_name: Übler
- first_name: Giacomo
full_name: Venturi, Giacomo
last_name: Venturi
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
citation:
ama: 'Hviding RE, De Graaff A, Liu H, et al. The X-ray dot: Exotic dust or a late-stage
Little Red Dot? The Astrophysical Journal Letters. 2026;1000(1). doi:10.3847/2041-8213/ae4c88'
apa: 'Hviding, R. E., De Graaff, A., Liu, H., Goulding, A. D., Ma, Y., Greene, J.
E., … Wang, B. (2026). The X-ray dot: Exotic dust or a late-stage Little Red Dot?
The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae4c88'
chicago: 'Hviding, Raphael E., Anna De Graaff, Hanpu Liu, Andy D. Goulding, Yilun
Ma, Jenny E. Greene, Leindert A. Boogaard, et al. “The X-Ray Dot: Exotic Dust
or a Late-Stage Little Red Dot?” The Astrophysical Journal Letters. IOP
Publishing, 2026. https://doi.org/10.3847/2041-8213/ae4c88.'
ieee: 'R. E. Hviding et al., “The X-ray dot: Exotic dust or a late-stage
Little Red Dot?,” The Astrophysical Journal Letters, vol. 1000, no. 1.
IOP Publishing, 2026.'
ista: 'Hviding RE, De Graaff A, Liu H, Goulding AD, Ma Y, Greene JE, Boogaard LA,
Bunker AJ, Cleri NJ, Franx M, Hirschmann M, Leja J, Matthee JJ, Naidu RP, Setton
DJ, Übler H, Venturi G, Wang B. 2026. The X-ray dot: Exotic dust or a late-stage
Little Red Dot? The Astrophysical Journal Letters. 1000(1), L18.'
mla: 'Hviding, Raphael E., et al. “The X-Ray Dot: Exotic Dust or a Late-Stage Little
Red Dot?” The Astrophysical Journal Letters, vol. 1000, no. 1, L18, IOP
Publishing, 2026, doi:10.3847/2041-8213/ae4c88.'
short: R.E. Hviding, A. De Graaff, H. Liu, A.D. Goulding, Y. Ma, J.E. Greene, L.A.
Boogaard, A.J. Bunker, N.J. Cleri, M. Franx, M. Hirschmann, J. Leja, J.J. Matthee,
R.P. Naidu, D.J. Setton, H. Übler, G. Venturi, B. Wang, The Astrophysical Journal
Letters 1000 (2026).
date_created: 2026-04-12T22:01:48Z
date_published: 2026-03-20T00:00:00Z
date_updated: 2026-05-04T07:13:07Z
day: '20'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ae4c88
external_id:
arxiv:
- '2601.09778'
file:
- access_level: open_access
checksum: 1be4f361bf59aa08b8c98ed4f475a463
content_type: application/pdf
creator: dernst
date_created: 2026-05-04T07:11:37Z
date_updated: 2026-05-04T07:11:37Z
file_id: '21784'
file_name: 2026_AstrophysicalJourLetters_Hviding.pdf
file_size: 2821786
relation: main_file
success: 1
file_date_updated: 2026-05-04T07:11:37Z
has_accepted_license: '1'
intvolume: ' 1000'
issue: '1'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The X-ray dot: Exotic dust or a late-stage Little Red Dot?'
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: 1000
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '21713'
abstract:
- lang: eng
text: GW231123 represents the most massive binary–black hole merger detected to
date, lying firmly within, or even above, the pair-instability mass gap. The component
spins are both exceptionally high (a1 = 0.90 +0.10/-0.19, a2 = 0.80 +0.20/-0.51),
which is difficult to explain with repeated mergers. Here we show that the black
hole spin vectors are closely aligned with each other while significantly tilted
relative to the binary’s orbital angular momentum, pointing to a common accretion-driven
origin. We examine astrophysical formation channels capable of producing near-equal,
high-mass, and mutually aligned spins consistent with GW231123—particularly binaries
embedded in AGN disks and Population III remnants, which grew via coherent misaligned
gas accretion. We further argue that other high-mass, high-spin events, e.g.,
GW190521, may share a similar evolutionary pathway. These findings underscore
the critical role of sustained, coherent accretion in shaping the most extreme
black hole binaries.
acknowledgement: The authors thank Davide Gerosa and Matthew Mould for valuable suggestions.
We are grateful for support by the National Science Foundation under grant No. PHY-2309024
(I.B.) and by NASA under grants 80NSSC22K0822 and 80NSSC24K0440 (Z.H.). We used
OpenAI’s ChatGPT (OpenAI 2025) during the preparation of this manuscript. This material
is based upon work supported by NSF’s LIGO Laboratory, which is a major facility
fully funded by the National Science Foundation.
article_number: L44
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
citation:
ama: 'Bartos I, Haiman Z. Accretion is all you need: Black Hole spin alignment in
merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters.
2026;996(2). doi:10.3847/2041-8213/ae2bff'
apa: 'Bartos, I., & Haiman, Z. (2026). Accretion is all you need: Black Hole
spin alignment in merger GW231123 indicates accretion pathway. The Astrophysical
Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae2bff'
chicago: 'Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole
Spin Alignment in Merger GW231123 Indicates Accretion Pathway.” The Astrophysical
Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae2bff.'
ieee: 'I. Bartos and Z. Haiman, “Accretion is all you need: Black Hole spin alignment
in merger GW231123 indicates accretion pathway,” The Astrophysical Journal
Letters, vol. 996, no. 2. IOP Publishing, 2026.'
ista: 'Bartos I, Haiman Z. 2026. Accretion is all you need: Black Hole spin alignment
in merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters.
996(2), L44.'
mla: 'Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole Spin
Alignment in Merger GW231123 Indicates Accretion Pathway.” The Astrophysical
Journal Letters, vol. 996, no. 2, L44, IOP Publishing, 2026, doi:10.3847/2041-8213/ae2bff.'
short: I. Bartos, Z. Haiman, The Astrophysical Journal Letters 996 (2026).
corr_author: '1'
date_created: 2026-04-12T22:01:49Z
date_published: 2026-01-10T00:00:00Z
date_updated: 2026-05-04T09:54:18Z
day: '10'
ddc:
- '520'
department:
- _id: ZoHa
doi: 10.3847/2041-8213/ae2bff
external_id:
arxiv:
- '2508.08558'
file:
- access_level: open_access
checksum: ac46ba3d13f0150ccbc42665bed3ae47
content_type: application/pdf
creator: dernst
date_created: 2026-05-04T09:49:53Z
date_updated: 2026-05-04T09:49:53Z
file_id: '21788'
file_name: 2026_AstrophysicalJourLetters_Bartos.pdf
file_size: 866725
relation: main_file
success: 1
file_date_updated: 2026-05-04T09:49:53Z
has_accepted_license: '1'
intvolume: ' 996'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates
accretion pathway'
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: 996
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '21714'
abstract:
- lang: eng
text: Be stars are rapidly rotating main-sequence stars that play a crucial role
in understanding stellar evolution and binary interactions. In this Letter, we
propose a new formation scenario for black hole (BH) + Be star binaries (hereafter
BHBe binaries), where the Be star is produced through the wind Roche lobe overflow
(WRLOF) mechanism. Our analysis is based on numerical simulations of the WRLOF
process in massive binaries, building on recent theoretical work. We demonstrate
that the WRLOF model can efficiently form BHBe binaries under reasonable assumptions
on stellar wind velocities. Using rapid binary population synthesis, we estimate
the population of such systems in the Milky Way, predicting ∼1800−3200 currently
existing BHBe binaries originating from the WRLOF channel. These systems are characterized
by high eccentricities and exceptionally wide orbits, with typical orbital periods
exceeding 1000 days and a peak distribution around ∼10,000 days. Due to their
long orbital separations, these BHBe binaries are promising targets for future
detection via astrometric and interferometric observations.
acknowledgement: We are deeply grateful to the anonymous referee for the insightful
comments, which have significantly improved the quality of this work. The authors
express their gratitude to Zhaoyu Zuo and I. El Mellah for sharing the grids of
wind accretion efficiencies. Z.L. thanks Matthias U. Kruckow for detailed discussions
about the BH formation. This work is supported by the Natural Science Foundation
of China (grant Nos. 12125303, 12525304, 12288102, 12090040/3, 12473034, 12503044,
12333008, 12433009, 12422305, 12273105, 12073070, 12173081), the Strategic Priority
Research Program of the Chinese Academy of Sciences (grant Nos. XDB1160303, XDB1160201,
XDB1160000), the National Key R&D Program of China (grant Nos. 2021YFA1600403 and
2021YFA1600400), the CAS “Light of West China,” the Yunnan Revitalization Talent
Support Program-Science & Technology Champion Project (No. 202305AB350003) and Young
Talent project, the International Centre of Supernovae (ICESUN), Yunnan Key Laboratory
of Supernova Research (Nos. 202302AN360001 and 202201BC070003), Yunnan Fundamental
Research Projects (No. 202401AT070139), and the Natural Science Foundation of Henan
Province (No. 242300420944). X.C. acknowledges the New Cornerstone Science Foundation
through the XPLORER PRIZE. The authors gratefully acknowledge the “PHOENIX Supercomputing
Platform” jointly operated by the Binary Population Synthesis Group and the Stellar
Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences.
article_number: L42
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zhenwei
full_name: Li, Zhenwei
last_name: Li
- first_name: Shi
full_name: Jia, Shi
last_name: Jia
- first_name: Dandan
full_name: Wei, Dandan
id: 5dd129bd-0601-11ef-b325-833284687b76
last_name: Wei
- first_name: Hongwei
full_name: Ge, Hongwei
last_name: Ge
- first_name: Hailiang
full_name: Chen, Hailiang
last_name: Chen
- first_name: Yangyang
full_name: Zhang, Yangyang
last_name: Zhang
- first_name: Xuefei
full_name: Chen, Xuefei
last_name: Chen
- first_name: Zhanwen
full_name: Han, Zhanwen
last_name: Han
citation:
ama: 'Li Z, Jia S, Wei D, et al. Formation of Be stars via wind accretion: Case
study on Black Hole + Be star binaries. The Astrophysical Journal Letters.
2026;996(2). doi:10.3847/2041-8213/ae3008'
apa: 'Li, Z., Jia, S., Wei, D., Ge, H., Chen, H., Zhang, Y., … Han, Z. (2026). Formation
of Be stars via wind accretion: Case study on Black Hole + Be star binaries. The
Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae3008'
chicago: 'Li, Zhenwei, Shi Jia, Dandan Wei, Hongwei Ge, Hailiang Chen, Yangyang
Zhang, Xuefei Chen, and Zhanwen Han. “Formation of Be Stars via Wind Accretion:
Case Study on Black Hole + Be Star Binaries.” The Astrophysical Journal Letters.
IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae3008.'
ieee: 'Z. Li et al., “Formation of Be stars via wind accretion: Case study
on Black Hole + Be star binaries,” The Astrophysical Journal Letters, vol.
996, no. 2. IOP Publishing, 2026.'
ista: 'Li Z, Jia S, Wei D, Ge H, Chen H, Zhang Y, Chen X, Han Z. 2026. Formation
of Be stars via wind accretion: Case study on Black Hole + Be star binaries. The
Astrophysical Journal Letters. 996(2), L42.'
mla: 'Li, Zhenwei, et al. “Formation of Be Stars via Wind Accretion: Case Study
on Black Hole + Be Star Binaries.” The Astrophysical Journal Letters, vol.
996, no. 2, L42, IOP Publishing, 2026, doi:10.3847/2041-8213/ae3008.'
short: Z. Li, S. Jia, D. Wei, H. Ge, H. Chen, Y. Zhang, X. Chen, Z. Han, The Astrophysical
Journal Letters 996 (2026).
date_created: 2026-04-12T22:01:50Z
date_published: 2026-01-10T00:00:00Z
date_updated: 2026-04-16T06:26:18Z
day: '10'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.3847/2041-8213/ae3008
external_id:
arxiv:
- '2512.18565'
file:
- access_level: open_access
checksum: 09200c1cf405101abdd298ce80c9a90d
content_type: application/pdf
creator: dernst
date_created: 2026-04-16T06:24:30Z
date_updated: 2026-04-16T06:24:30Z
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file_name: 2026_AstrophysicalJourLetters_Li.pdf
file_size: 5202345
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intvolume: ' 996'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Formation of Be stars via wind accretion: Case study on Black Hole + Be star
binaries'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 996
year: '2026'
...
---
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OA_type: gold
PlanS_conform: '1'
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abstract:
- lang: eng
text: 'We compile a sample of 83 little red dots (LRDs) with JWST imaging and find
that a substantial fraction (∼43%, rising to ≳80% for the most luminous LRDs)
host one or more spatially offset, UV-bright companions at projected separations
of 0.5 kpc ≲ d ≲ 5 kpc, with median 〈d〉 = 1.0 kpc. This fraction is even higher
when smaller spatial scales are probed at high signal-to-noise ratio: the two
most strongly lensed LRDs, A383-LRD1 and the newly discovered A68-LRD1, both have
UV-bright companions at separations of only d ∼ 0.3 kpc, below the resolution
limit of most unlensed JWST samples. We explore whether these ubiquitous red/blue
configurations may be physically linked to the formation of LRDs, in analogy with
the “synchronized pair” scenario originally proposed for direct-collapse black
hole formation. In this picture, UV radiation from the companions, with typically
modest stellar masses (M∗ ∼ 108−109 M⊙), suppresses molecular hydrogen cooling
in nearby gas, allowing nearly isothermal collapse and the formation of extremely
compact objects, such as massive black holes, supermassive stars, or quasi-stars.
Using component-resolved photometry and spectral energy distribution modeling,
we infer Lyman–Werner radiation fields of J21,LW ∼ 102.5–105 at the locations
of the red components, comparable to those required in direct-collapse models,
suggesting that the necessary photodissociation conditions are realized in many
LRD systems. This framework provides a simple and self-consistent explanation
for the extreme compactness and distinctive spectral properties of LRDs and links
long-standing theoretical models for early compact object formation directly to
a population now observed with JWST in the early Universe.'
acknowledgement: 'We thank Earl Bellinger, Fabio Pacucci, Andrea Ferrara, and Dale
Kocevski for useful discussions. This work is based on observations made with the
NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski
Archive for Space Telescopes at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-03127 for JWST. These imaging observations are associated with
programs 1345, 1180, 1181, 1243, 6882, 2561, 1324, 4111, and 1895. The compiled
dataset can be accessed at doi:10.17909/1m8f-9c47. The Cosmic Dawn Center (DAWN)
is funded by the Danish National Research Foundation under grant DNRF140. J.M. and
A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). This work
was performed in part at Aspen Center for Physics, which is supported by National
Science Foundation grant PHY-2210452. This work used the following Python packages:
Matplotlib (J. D. Hunter 2007), SciPy (P. Virtanen et al. 2020), NumPy (S. van der
Walt et al. 2011), AstroPy (Astropy Collaboration et al. 2022), colossus (B. Diemer
2018), and photutils (L. Bradley et al. 2025).'
article_number: L4
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Josephine F.W.
full_name: Baggen, Josephine F.W.
last_name: Baggen
- first_name: Matthew T.
full_name: Scoggins, Matthew T.
last_name: Scoggins
- first_name: Pieter
full_name: Van Dokkum, Pieter
last_name: Van Dokkum
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
- 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
citation:
ama: 'Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee
JJ. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner
sources enabling direct-collapse Black Hole formation. The Astrophysical Journal
Letters. 2026;1002(1). doi:10.3847/2041-8213/ae58a5'
apa: 'Baggen, J. F. W., Scoggins, M. T., Van Dokkum, P., Haiman, Z., Torralba Torregrosa,
A., & Matthee, J. J. (2026). Connecting the dots: UV-bright companions of
Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation.
The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae58a5'
chicago: 'Baggen, Josephine F.W., Matthew T. Scoggins, Pieter Van Dokkum, Zoltán
Haiman, Alberto Torralba Torregrosa, and Jorryt J Matthee. “Connecting the Dots:
UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse
Black Hole Formation.” The Astrophysical Journal Letters. IOP Publishing,
2026. https://doi.org/10.3847/2041-8213/ae58a5.'
ieee: 'J. F. W. Baggen, M. T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa,
and J. J. Matthee, “Connecting the dots: UV-bright companions of Little Red Dots
as Lyman–Werner sources enabling direct-collapse Black Hole formation,” The
Astrophysical Journal Letters, vol. 1002, no. 1. IOP Publishing, 2026.'
ista: 'Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee
JJ. 2026. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner
sources enabling direct-collapse Black Hole formation. The Astrophysical Journal
Letters. 1002(1), L4.'
mla: 'Baggen, Josephine F. W., et al. “Connecting the Dots: UV-Bright Companions
of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole
Formation.” The Astrophysical Journal Letters, vol. 1002, no. 1, L4, IOP
Publishing, 2026, doi:10.3847/2041-8213/ae58a5.'
short: J.F.W. Baggen, M.T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa,
J.J. Matthee, The Astrophysical Journal Letters 1002 (2026).
date_created: 2026-05-10T22:02:15Z
date_published: 2026-04-10T00:00:00Z
date_updated: 2026-05-11T06:48:33Z
day: '10'
ddc:
- '520'
department:
- _id: ZoHa
- _id: JoMa
doi: 10.3847/2041-8213/ae58a5
external_id:
arxiv:
- '2602.02702'
file:
- access_level: open_access
checksum: 8c31d8603cd6ad39c772a72d136dc3f8
content_type: application/pdf
creator: dernst
date_created: 2026-05-11T06:44:37Z
date_updated: 2026-05-11T06:44:37Z
file_id: '21851'
file_name: 2026_AstrophysicalJourLetters_Baggen.pdf
file_size: 13359642
relation: main_file
success: 1
file_date_updated: 2026-05-11T06:44:37Z
has_accepted_license: '1'
intvolume: ' 1002'
issue: '1'
language:
- iso: eng
month: '04'
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'
scopus_import: '1'
status: public
title: 'Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner
sources enabling direct-collapse Black Hole formation'
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: 1002
year: '2026'
...
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abstract:
- lang: eng
text: Recent studies at high redshift have revealed an enigmatic class of little
red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere.
However, it is unclear whether such objects exist at lower redshift, especially
given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from
JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed
by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral
energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with
effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably
deep absorption, stronger than previously measured in any LRD. The absorption
trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The
presence of blue- and red-shifted absorption suggests complex dynamics of the
obscuring gas along the line of sight. We speculate that the absorption trough
can be produced by a thick wind launched from a thick, rotating photospheric disk,
the latter being the source of the red optical continuum. While the source is
unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble
Space Telescope imaging shows an extended morphology with (formular displayed)
kpc, which we interpret as a host galaxy with a stellar mass of ∼10^8 M⊙, in line
with the narrow Hα emission. The discovery of this object at cosmic noon highlights
the feasibility of systematic searches for extreme LRDs with wide-area facilities
such as Euclid and Roman.
acknowledgement: "IOP Science home\r\nThe Astrophysical Journal Letters\r\nThe American
Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA
Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and
Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7\r\nAlberto Torralba,
Jorryt Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush
Desai, Anna de Graaff, Jenny E. Greene, Christian Kragh JespersenShow full author
list\r\n\r\nPublished 2026 June 30 • © 2026. The Author(s). Published by the American
Astronomical Society.\r\nThe Astrophysical Journal Letters, Volume 1005, Number
2\r\nCitation Alberto Torralba et al 2026 ApJL 1005 L37\r\nDOI 10.3847/2041-8213/ae7bfd\r\n\r\nPDFOpens
in a new tab.ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens
in a new tab.ePub\r\nArticle metrics\r\n122 Total downloads\r\n\r\nShare this article\r\nArticle
information\r\nAbstract\r\nRecent studies at high redshift have revealed an enigmatic
class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any
stellar atmosphere. However, it is unclear whether such objects exist at lower redshift,
especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery
of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam
pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter
spectroscopy. The rest-optical to near-infrared spectral energy distribution of
PAN-BH*-1 is consistent with a photospheric continuum with effective temperature
Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger
than previously measured in any LRD. The absorption trough spans from −520 to +267
km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted
absorption suggests complex dynamics of the obscuring gas along the line of sight.
We speculate that the absorption trough can be produced by a thick wind launched
from a thick, rotating photospheric disk, the latter being the source of the red
optical continuum. While the source is unresolved in the rest-optical JWST data
(reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended
morphology with \r\n kpc, which we interpret as a host galaxy with a stellar mass
of ∼108 M⊙, in line with the narrow Hα emission. The discovery of this object at
cosmic noon highlights the feasibility of systematic searches for extreme LRDs with
wide-area facilities such as Euclid and Roman.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious
article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work
may be used under the terms of the Creative Commons Attribution 4.0 licence. Any
further distribution of this work must maintain attribution to the author(s) and
the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe unprecedented
sensitivity of JWST has enabled the discovery of a new, abundant population of objects
at redshifts z ≈ 3–9 nicknamed the “little red dots” (LRDs). These are characterized
by their compact rest-frame optical morphology, broad emission lines, and a characteristic
rest-UV to optical “V-shape” in their spectral energy distributions (SED; e.g.,
D. D. Kocevski et al. 2023; V. Kokorev et al. 2024; J. Matthee et al. 2024; I. Labbe
et al. 2025).\r\n\r\nThe nature of LRDs is highly debated (see K. Inayoshi & L.
C. Ho 2025, for a recent overview) as the LRDs show systematic differences with
respect to other types of active galactic nuclei (AGN), such as faintness in X-rays
(e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024), mid-to-far-infrared dust emission
(e.g., G. C. K. Leung et al. 2025; C. C. Williams et al. 2024; I. Delvecchio et
al. 2025; D. J. Setton et al. 2025; M. Xiao et al. 2025), and radio (e.g., G. Mazzolari
et al. 2026; M. A. Latif et al. 2025; K. Perger et al. 2025, see A. J. Gloudemans
et al. 2025).\r\n\r\nA recurring spectral feature of LRDs is the presence of a strong
Balmer break (e.g., D. J. Setton et al. 2025; B. Wang et al. 2024; R. E. Hviding
et al. 2025; W. Q. Sun et al. 2026), in some cases stronger than any star or stellar
population can produce. The two most prominent examples known to date are The Cliff
at z ≈ 3.5 (A. de Graaff et al. 2025a) and MoM-BH* at z ≈ 7.8 (R. P. Naidu et al.
2025). The joint appearance of strong Balmer lines as well as strong Balmer breaks
has been modeled as being due to absorption by a dense, neutral gas with a high
column density in the line of sight to a highly ionizing source (K. Inayoshi & R.
Maiolino 2025; X. Ji et al. 2025; A. Sneppen et al. 2026; A. Torralba et al. 2026).
These observations have sparked the development of new theoretical models, ranging
from a spherical envelope analogous to stellar atmospheres (e.g., M. C. Begelman
& J. Dexter 2026; D. Kido et al. 2025; H. Liu et al. 2025; D. Nandal & A. Loeb 2026)
or a thick accretion disk (e.g., H. Liu et al. 2025, 2026; K. Inayoshi et al. 2025;
Y.-X. Chen et al. 2026).\r\n\r\nBesides their spectral features, the evolution of
the LRD number densities is also in stark contrast to other types of AGNs (e.g.,
K. Inayoshi 2025). At 4 ≲ z ≲ 7, LRDs represent a few percent of the galaxy population
(e.g., D. D. Kocevski et al. 2023, 2025; J. E. Greene et al. 2024; V. Kokorev et
al. 2024; X. Lin et al. 2024; R. Maiolino et al. 2024; J. Matthee et al. 2024),
with number densities of ≳10−5 Mpc−3. The number density does not appear to drop
quickly beyond z > 5 (e.g., J. Zhang et al. 2026), with various LRDs having been
confirmed at z > 8 (V. Kokorev et al. 2023; A. J. Taylor et al. 2025; R. Tripodi
et al. 2025), well beyond the quasar redshift record (F. Wang et al. 2021). Photometric
LRD candidates exist beyond z > 10 (T. S. Tanaka et al. 2025). In turn, the number
density of LRDs seems to decline steeply at z < 4 (e.g., Y. Ma et al. 2026), with
estimates of a number density of ∼10−6 cMpc−3 at z ∼ 2 and even ∼10−10 cMpc−3 at
z ≈ 0.3 (X. Lin et al. 2026). While it is challenging to ensure a uniform selection
function across such a large redshift baseline and dedicated spectroscopic follow-up
of such lower redshift candidates has only just started, it is challenging to attribute
five orders of magnitude to such effects.\r\n\r\nMotivated by the discovery of rare
objects with extreme Balmer breaks at z > 3 and the very small number of known
LRDs at lower redshift, we performed a dedicated search for extreme Balmer break
objects using a template-match approach on a large compilation of JWST NIRCam data
over ≈0.3 deg2 and z ≈ 1.5–7.0. This survey is presented in A. Weibel et al. (2026a).
As part of an ongoing ground-based spectroscopic campaign of LRD candidates at z
∼ 2 (Y. Ma et al. 2026), we followed up the most luminous candidate with a photometric
redshift of z ≈ 2 with the X-Shooter spectrograph on the Very Large Telescope (VLT).
In this Letter, we present the discovery and spectroscopic confirmation of PAN-BH*-1,
a luminous LRD at z = 1.73 with an extreme Balmer break comparable to the strongest
observed in any LRD (and, in general, any astrophysical source). The low redshift
of this source enables high-resolution spectroscopy from ground-based observatories
that is otherwise impossible to obtain at high redshift.\r\n\r\nThroughout this
Letter, we use a ΛCDM cosmology with Ωm = 0.31, ΩΛ = 0.69, and h = 0.677 as described
by Planck Collaboration et al. (2020). All the magnitudes are given in the AB system
(J. B. Oke & J. E. Gunn 1983).\r\n\r\n2. Observations\r\n2.1. Photometry and Source
Selection\r\nWe identified PAN-BH*-1 (ID: PAN-1115, RA, DEC: 40.015835, −1.659363
J2000) as part of a systematic search across ≈0.3 deg2 of JWST NIRCam legacy imaging
comprising at least six filters of coverage (A. Weibel et al. 2026b). Notably, this
dataset includes the Cycle 1 pure parallel survey PANORAMIC (PID: 2514, PIs: Williams
& Oesch; C. C. Williams et al. 2025) that contributes 28 of the 35 independent lines
of sight, thereby enabling the discovery of rare objects such as PAN-BH*-1 across
diverse large-scale structure environments. Specifically, this source was identified
in the footprint j024000m0142 of the PANORAMIC DR1,15 which is adjacent to the A370
field (G. O. Abell et al. 1989), where archival images by the Hubble Space Telescope
(HST) are available from the BUFFALO survey (C. L. Steinhardt et al. 2020). The
HST/ACS images were processed with grizli and also released as part of the PANORAMIC
dataset.\r\n\r\nPAN-BH*-1 is in the outskirts of the A370 lensing cluster, but the
magnification is only μ ≈ 1.05 according to the models from A. Niemiec et al. (2023).
Throughout the rest of the paper, we report the uncorrected flux measurements, since
the effect of magnification (∼5%) is negligible given the uncertainties in the observations
and the lensing model.\r\n\r\nThe search strategy and full photometric selection
are described in a companion paper (A. Weibel et al. 2026a). Briefly, that work
presents a new selection of LRDs as a combination of a “black hole star” template
(BH*; R. P. Naidu et al. 2025) embedded in a host galaxy, instead of the typically
used “V-shaped” selections (e.g., D. D. Kocevski et al. 2025; V. Kokorev et al.
2024). The host galaxies are modeled using eazy’s blue_sfhz templates. The BH*s
are modeled using a novel template set comprising empirical luminosity-based stacks
constructed in W. Q. Sun et al. (2026), the cloudy template from R. P. Naidu et
al. (2025), and by using spectra of prominent LRDs spanning the observed effective
temperature range (I. Labbe et al. 2024; A. de Graaff et al. 2025a; B. Wang et al.
2026).\r\n\r\nPAN-BH*-1 stood out as one of the few sources where the BH* template
effectively dominated all the light over the full wavelength range covered by NIRCam
(hence the name). The redshift of PAN-BH*-1 was estimated to be zphot = 1.85. Follow-up
VLT/X-Shooter spectroscopy confirmed the redshift as zspec = 1.731 (see Section
3.2).\r\n\r\nPAN-BH*-1 is also covered by archival data from the VLT with the HAWK-I
camera in the Ks band (G. B. Brammer et al. 2016) and in data from the Spitzer Space
Telescope in IRAC bands 1 and 3 (3.6 and 5.7 μm), and MIPS 24 μm (P. Capak 2019).
PAN-BH*-1 is detected in the Ks band and in the two IRAC filters. Performing Spitzer
photometry of this source is challenging due to the large point spread function
(PSF) and a neighboring source, especially in the MIPS band. However, the NIRCam
photometry of the neighboring source suggests it has a limited contribution to the
IRAC fluxes. The details of the photometry extraction are described in Appendix
A, and the measured magnitudes in Table 2.\r\n\r\n2.2. VLT/X-Shooter Spectroscopy\r\nPAN-BH*-1
was observed for 5.8 ks with the X-Shooter spectrograph (J. Vernet et al. 2011)
on the VLT as a bright backup target for program 116.294D (PI: Matthee) in visitor
mode on 2025 December 17. The main aim of this program was to confirm candidate
LRDs at cosmic noon (Y. Ma et al. 2026). These observations confirmed the redshift
through the detection of Hα at z = 1.731. A DDT program (ID 116.2AQ0; PI: Matthee)
obtained additional follow-up data of PAN-BH*-1 in service mode for 26.2 ks during
2026 January 10–26, yielding a total exposure time of 8.9 hr. X-Shooter observes
with three arms simultaneously, UVB, VIS, and near-infrared (NIR), covering rest-frame
wavelengths of ≈0.14–0.9 μm, albeit hampered by skyline emission and telluric absorption,
primarily in the rest-frame optical.\r\n\r\nThe observing conditions were clear,
with a seeing ranging from 05 to 07 (median 06). The service mode observations were
primarily conducted during dark nights, with some gray (FLI = 0.03–0.6, median 0.1),
and a typical airmass of 1.35. We used UVB, VIS, and NIR slits with widths 10, 09,
and 09, yielding a nominal resolution of R = 5400, 8900, and 5600, respectively
(FWHM ∼53 km s−1 for NIR). The target acquisition was done using blind offsets from
a reference star, due to the target being too faint for direct acquisition. We used
a standard nodding on the slit pattern, with 4″ nod throws in an ABBA pattern, and
1″ jitters in the NIR arm to improve the sky subtraction. In each observing block
of ≈1 hr, the exposure times were 700, 655, and (2×)365 s for the three arms at
each nod position.\r\n\r\nThe reduction of the X-Shooter data uses a combination
of EsoRex libraries16 and Python code based on the reduction pipeline employed in
J. Matthee et al. (2021). Each observing block was reduced separately. We used standard
stars taken during the observing night for a first-pass flux calibration. Telluric
corrections were applied using the molecfit tool (A. Smette et al. 2015) implemented
in the X-Shooter EsoRex pipeline. Telluric stars were observed during the visitor
nights, but they were not always observed during the service mode observations in
January. For those observations, we took the telluric star that was observed at
the closest observing date. Based on the variation in telluric absorption among
the reference stars taken during this period, we estimate the variation in the transmission
and propagate the uncertainty in the telluric correction. For each observing block,
we then extracted an optimally extracted 1D spectrum using the spatial profile of
the Hα line, thus accounting for seeing variations and (more importantly) minor
errors in the accuracy of the slit pointing. Before median combining these spectra,
we normalize them by the median Hα flux of all observations to account for variations
in slit losses and flux calibrations.\r\n\r\nBesides Hα (integrated S/N = 75) and
Hβ (integrated S/N = 6; Section 3.2), we also detect continuum emission in the best
regions in the H and K bands at 1.6 μm and 2.1 μm, respectively, with a low signal-to-noise
ratio (S/N) of ∼1 per resolution element. Unfortunately, the [O iii] λλ4960, 5008
doublet is undetectable because the observed wavelengths are impacted by very strong
telluric absorption. No other lines or continuum are detected in the X-Shooter spectrum.\r\n\r\n3.
Properties of PAN-BH*-1\r\n3.1. Spectral Shape: A Photospheric Continuum with Strong
Hα Emission\r\nThe photometric SED of PAN-BH*-1 has remarkable similarities with
The Cliff (Figure 1): luminous in the rest optical, with a sudden drop toward the
rest-UV around the Balmer limit, and very weak near-to-mid infrared continuum emission.
With a rough extrapolation of the two HST photometric points using a power-law fit
(fλ ∝ λβ), we obtain a UV slope of β = −0.1 ± 1.2, and MUV = −16.7 ± 0.7. For the
rest-frame optical to NIR data, we fit a Planck blackbody law to the JWST data points,
after subtracting the measured Hα flux (see Section 3.2) from the F200W photometry.
The rest-optical and NIR photometry of PAN-BH*-1 is remarkably well described by
a single temperature blackbody with T = 4204 K (with a best-fit ). We measure the
strength of the Balmer break from the fν ratio F115W/F814W = 7 ± 1, in line with
the Balmer break strengths of The Cliff (; A. de Graaff et al. 2025a)17 and MoM-BH*
(7.8 ± 1.8; R. P. Naidu et al. 2025), measured from JWST/NIRSpec PRISM spectra as
fν,4000–4100/fν,3620−3720. In Figure 2, we compare the Balmer break strength with
the spectroscopic sample of A. de Graaff et al. (2025b), showing that out of 134
sources, only two have breaks significantly above 5. This suggests that PAN-BH*-1
has among the most extreme Balmer breaks known, although we caution that our value
is derived from wide-band photometry with pivot wavelengths corresponding to 4212
and 3042 Å, respectively, rather than from spectroscopy.\r\n\r\nZoom InZoom OutReset
image size\r\nFigure 1. SED of PAN-BH*-1 Top: cutouts from all the HST and JWST
images in which PAN-BH*-1 is covered. It shows a remarkably compact morphology in
all the wavelengths, resolved only in the HST F606W and F814W bands (Section 3.3).
Bottom: photometry from JWST/NIRCam (blue squares), HST/ACS (purple pentagons),
and Spitzer/IRAC+MIPS (red hexagons, and red triangle for the 5σ upper limit). The
empty square is the F200W flux after subtracting the Hα flux measured from X-Shooter
spectroscopy. We show the spectrum of The Cliff for comparison (gray line), shifted
to z = 1.73 and normalized to the F150W flux of PAN-BH*-1. We also show the best-fitting
blackbody spectrum (blue dashed line) and the best model from the synthetic LRD
atmosphere models from H. Liu et al. (2026), shifted to z = 1.73 (green line), undersampled
by a factor of 500 for clarity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\nZoom InZoom OutReset image size\r\nFigure 2. Spectroscopic sample of LRDs
by redshift and Balmer break strength. We plot the redshift and Balmer break strength
of PAN-BH*-1, and the JWST sample from A. de Graaff et al. (2025b) (purple diamonds),
and three local LRDs in X. Lin et al. (2026), for comparison. We also highlight
three sources with a particularly strong Balmer break: The Cliff (A. de Graaff et
al. 2025a), MoM-BH* (R. P. Naidu et al. 2025), and CAPERS-LRDz9 (A. J. Taylor et
al. 2025). The Balmer break strength of the JWST spectroscopic sample is computed
as fν,4000–4100/fν,3620–3720, whereas the value for PAN-BH*-1 is directly obtained
from the F115W/F814W photometry.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\n3.2. Hα and Hβ Emission Lines\r\nThe Hα profile appears as a complex combination
of a broad line with strong absorption close to the systemic redshift. We fit the
Hα emission line with a similar model as the one used in A. Torralba et al. (2026)
and J. Matthee et al. (2026). The Hα model consists of two Gaussian emission components
(with narrow and intermediate line widths), and a broad symmetric exponential convolved
with the intermediate profile and parameterized as in F. D’Eugenio et al. (2025a).
The absorption is implemented as an opacity law defined as e−τ(λ), where τ(λ) also
follows a single Gaussian velocity distribution (F. D’Eugenio et al. 2025a, 2025b;
A. Torralba et al. 2026). For simplicity, we assume a covering factor of Cf = 1
for the absorbing gas. In previous works, the width of the narrow component is tied
to that of [O iii], assuming both components come from the same region, often interpreted
as the interstellar medium (ISM) of the host galaxy. In this case, we have no information
about [O iii] due to this doublet falling in a wavelength range heavily affected
by strong telluric absorption. We fit the Hα line after masking relevant skylines
and strong telluric absorption bands. The fitted Hα parameters are listed in Table
1 and the best-fit model is shown in Figure 3. The absorption feature is notably
strong, with an equivalent width of EWabs = −148 ± 12 Å with respect to the fitted
continuum and 12.2 ± 0.2 Å if including the broad emission component. The absorption
corresponds to a Balmer optical depth at the line center of , reaching roughly the
continuum level. The FWHM of the single Gaussian fitted to the absorber is 283 ±
\ 8 km s−1, and is offset from the systemic redshift by −94 ± 4 km s−1. We note
that this parameterization is somewhat arbitrary, and we discuss in detail the absorber
properties in Section 4.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Hα
spectrum, and the best fit to our fiducial model. We show the X-Shooter R ∼ 5600
spectrum of the Hα line of PAN-BH*-1, along with the best-fit to the model described
in Section 3.2; total model (red solid line) and individual components (discontinuous
color lines). The red wing of the line is severely affected by telluric absorption,
thus the large uncertainties.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution
image\r\nTable 1. Properties of PAN-BH*-1\r\n\r\nParameter\tValue\tUnit\r\nWidth
(FWHM; Hα)\r\nExponential\t1257 ± 27\tkm s−1\r\nIntermediate\t687 ± 43\tkm s−1\r\nNarrow\t184
± 12\tkm s−1\r\nAbsorption\t283 ± 8\tkm s−1\r\nFlux (Hα)\r\nExponential\t643 ± 7\t10−18
erg s−1 cm−2\r\nIntermediate\t19 ± 5\t10−18 erg s−1 cm−2\r\nNarrow\t38 ± 3\t10−18
erg s−1 cm−2\r\nTotal\t522 ± 7\t10−18 erg s−1 cm−2\r\nGeneral properties\r\n(LHα/erg
s−1)\t43.046 ± 0.006\t⋯\r\nEW0(Hα)\t520 ± 20\tÅ\r\nSFR(Hα, narrow)a\t2.1 ± 0.2\tM⊙
yr−1\r\nSFR(Hα, narrow)b\t3.3 ± 0.3\tM⊙ yr−1\r\nreff,UV (F606W+F814W)\t\tkpc\r\nreff,opt
(F200W)\t<0.047\tkpc\r\nHα/Hβ (total)\t>9.4\t⋯\r\nHα/Hβ (narrow)\t5 ± 1\t⋯\r\nNotes.
aCalibration from I. G. Kramarenko et al. (2026). bCalibration from R. C. Kennicutt
& N. J. Evans (2012). SFR values calculated assuming no dust attenuation.\r\n\r\nDownload
table as: \r\nASCIITypeset image\r\n\r\nThe Hβ line is marginally detected. After
undersampling the spectrum by a factor 5, a hint of a weak narrow component can
be identified (Figure 4), along with a tentative absorption at the same mean velocity
as in Hα. We fit the best Hα model to the Hβ spectrum, only rescaling it by a multiplicative
factor, and adding a flat continuum component. By doing this, we find an Hβ flux
of (47 ± 8) × 10−18 erg s−1 cm−2 (S/N ≈ 6). Conservatively, we obtain a Balmer decrement
of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with the high decrements found
for the LRD population (e.g., G. P. Nikopoulos et al. 2026; A. de Graaff et al.
2025b; J. Matthee et al. 2026). In Figure 5, we show the Hβ spectrum compared to
the rescaled Hα model. By matching the best-fit Hα profile with the data at the
expected observed wavelength for Hβ (±5000 km s−1), we obtain a better agreement
(, BIC = 1537) than fitting a flat continuum only (, BIC = 1658) with ΔBIC = 121
≫ 10, strongly favoring a detection of a broad Hβ emission line, and securing the
spectroscopic redshift. Similarly, we fit a narrow Gaussian to Hβ with the same
width and velocity as the Hα best-fit model, assuming a completely saturated absorption.
We obtain a Balmer decrement for the narrow component of Hα/Hβ = 5 ± 1, which would
imply a dust extinction of using a J. A. Cardelli et al. (1989) attenuation law,
under the assumption of case B recombination. However, due to the low S/N of Hβ
this result is only tentative, and compatible with a standard Case B value within
∼2σ.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. X-Shooter spectrum of Hα
and Hβ of PAN-BH*-1 (blue). We compare to the spectrum of The Cliff (gray; data
from JWST DDT #9433), normalized in each panel to the flux of PAN-BH*-1 in the range
v ∈ (−3000, −2000) km s−1. Due to the low S/N, the Hβ spectrum of PAN-BH*-1 is rebinned
to a coarser grid by a factor 5, after masking the most relevant skylines.\r\n\r\nDownload
figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image
size\r\nFigure 5. Hβ spectrum. The spectrum is rebinned by a factor of 10 with inverse
variance flux weighting for visual clarity, due to the low S/N. We compare to the
best-fit Hα model, scaled by a factor of 0.112. In the bottom panel, we show the
χ residuals between the spectrum and the rescaled Hα model in black, and for only
the continuum in pink (ΔBIC = 121 strongly favoring the presence of a broad Hβ line).\r\n\r\nDownload
figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.3. Spatial Morphology\r\nIn
order to assess whether PAN-BH*-1 is spatially resolved, we use the Bayesian profile
fitting software pysersic (I. Pasha & T. B. Miller 2023)18 to fit a single Sérsic
profile to the JWST and HST imaging data of PAN-BH*-1. For JWST/NIRCam, we choose
F200W as the filter with the highest S/N in the short wavelength channel, benefiting
from a high spatial resolution and probing rest-frame optical wavelengths. To model
its PSF, we use version 2.2.0 of the stpsf software (formerly webbpsf, M. D. Perrin
et al. 2014). For the two HST bands F606W and F814W, we instead construct empirical
PSFs from public imaging data in the GOODS-S field following A. Weibel et al. (2024).
In all three bands, we sample the posterior with the No U-turn sampler in two chains
with 1000 warm-up and 2000 sampling steps each. We find that PAN-BH*-1 is unresolved
with NIRCam in F200W where the effective radius converges toward the edge of the
prior at 0.25 pixels. Using the 95th percentile of the posterior chains as an upper
limit on the effective radius, we find a rest-optical size of reff < 47 pc.\r\n\r\nPAN-BH*-1
appears to be resolved in the HST images corresponding to rest-frame pivot 0.2 and
0.3 μm, respectively. Due to the low signal-to-noise of the F606W and F814W photometry,
we fit both bands simultaneously fixing all the morphological parameters in both
images. We measure physical effective radii of kpc (see Appendix B). The modest
stretching by the foreground A370 lensing cluster could imply a correction of ∼10%
to the measured radius (A. Niemiec et al. 2023), which we disregard given the uncertainties.
These measured sizes are consistent with the typical sizes for galaxies with a stellar
mass ≲ 109 M⊙ at z = 1.75 (A. van der Wel et al. 2014). These findings are consistent
with the scenario of a compact LRD “engine” dominating the rest-optical light embedded
in a host galaxy, whose contribution becomes significant blueward of the Balmer
break (see A. P. Cloonan et al. 2026, for a relevant discussion).\r\n\r\n4. Absorber
Kinematics\r\nAs described in Section 3.2, the velocity distribution of the absorber
is empirically modeled with a Gaussian, which we find has a central velocity of
−94 ± 4 km s−1 relative to the redshift of the narrow emission component (adopted
as systemic). The absorption trough extends from negative to positive velocities
with respect to the redshift of the narrow component, but also with respect to the
center of the symmetric exponential wings. However, there are several degeneracies
between the shape of the absorber and other components of the emission line, such
as the narrow central emission (see Section 3.2). Furthermore, direct interpretation
of the absorber center velocity shift is challenging in an optically thick gas with
presumably complex dynamics, and it does not necessarily trace bulk motion. A more
robust, physically motivated pair of quantities is the minimum and maximum absorber
velocities. We define them as the values where the transmission of the Balmer absorber
increases to 99%, km s−1 and km s−1. These values trace the largest velocities
in the line of sight of gas with significant Balmer absorption. The absorbing trough
extends over 787 ± 17 km s−1 under this definition. The values of and are relatively
agnostic to the choice of the shape of the absorber, since they are determined by
the wavelength where the line profile deviates from a broad, symmetric exponential
profile. In Figure 6, we illustrate three proposed configurations of the velocity
distribution of the absorbing gas that could explain the shape of the observed Balmer
absorption, and we discuss these scenarios below.\r\n\r\nZoom InZoom OutReset image
size\r\nFigure 6. Geometric configurations for the absorber. We illustrate three
scenarios that could give rise to the observed Balmer absorption in PAN-BH*-1. In
scenario (a), the obscuring agent is a thick screen of gas with a certain bulk velocity,
and turbulent motions produce the broadening of the absorption trough. In (b), there
are two (or more) absorbers with opposite velocities in the line of sight. These
first two scenarios are dynamically unstable; therefore, variability is expected
in the absorption. Lastly, in (c), we observed an extended source through a disk
wind with a rotational component (vϕ) in addition to the poloidal (nonazimuthal)
velocity (vp). In the last scenario, the redshifted absorption is produced by streamlines
that oppose the observer when projected along the line of sight, despite the fact
that the gas is outflowing from the central source.\r\n\r\nDownload figure:\r\n\r\nStandard
imageHigh-resolution image\r\n4.1. Unstable Gas Flows?\r\nThe fact that there is
significant absorption at both negative and positive velocities with respect to
the systemic redshift cannot be simply explained by an axisymmetric outflowing or
inflowing wind. In the case of observing a compact object through a spherically
symmetric, nonturbulent bulk flow, a classical P Cygni profile is expected, with
a purely blueshifted absorption (or redshifted if the wind is infalling). The fact
that we also see redshifted absorption rules out this simple scenario. In principle,
turbulent motions could also produce broadening of the absorbing medium (scenario
a in Figure 6). However, the required turbulent velocity dispersion σturb ≈ 120
km s−1 (from the Gaussian fit in Section 3.2) is comparable to the mean velocity
of the absorption trough, meaning that turbulence dominates the gas flow. In such
a case, strong variability of the absorption profile would be expected, given the
typical dynamical crossing times (see Sect. 4.1 in F. D’Eugenio et al. 2025b). For
example, for a radius of 1016 cm (e.g., A. Torralba et al. 2026) and a mass of 106
M⊙, the dynamical freefall time is yr. Moreover, the turbulent velocity would be
highly supersonic, and the dissipation timescale would be comparable to the dynamical
time (e.g., M.-M. Mac Low 1999). Alternatively, in the context of a strong Balmer
absorber at z ∼ 7, F. D’Eugenio et al. (2026) recently discussed a “breathing mode”
scenario with cyclic inflows and outflows along the same line of sight, with the
gas being in different phases at different depths (scenario b in Figure 6; see also
K. Park et al. 2017). In this case, the same arguments regarding the stability of
the absorber would apply, and absorber variability is expected on observed timescales
of ∼5 yr (for a source at z = 1.7), which is testable with future observations.\r\n\r\n4.2.
The Case for the Disk Wind Hypothesis\r\nAn alternative, dynamically stable scenario
is a disk wind configuration (scenario c in Figure 6). Here, the wind would be launched
from a thick disk near the central engine, which we speculate could be the source
of the optical continuum emission (e.g., H. Liu et al. 2025, 2026; L. Zwick et al.
2025; Y.-X. Chen et al. 2026). A rotating disk would imprint to the wind an azimuthal
velocity component (vϕ). Observations at specific lines of sight, particularly for
high inclination angles (close to edge-on) where the rotational component dominates
the poloidal velocity, can give rise to both blueshifted and redshifted absorption
features (D. Proga et al. 2000; P. B. Hall et al. 2002, 2013; D. Proga & T. R. Kallman
2004; M. Giustini & D. Proga 2012). Most observed LRDs have blueshifted P Cygni–like
absorbers (J. Matthee et al. 2026), which can be naively interpreted as a uniformly
expanding shell. The low incidence of redshifted Balmer absorbers in LRD spectra
(e.g., I. Labbe et al. 2024; A. de Graaff et al. 2025a; F. D’Eugenio et al. 2025b,
2026; Y. Ma et al. 2026) can therefore be explained by the requirement of high inclination
angles to observe such features (see also A. Sneppen et al. 2026). Such a picture
is broadly in line with disk wind models for AGN with broad absorption lines (e.g.,
P. B. Hall et al. 2002; H. Zhou et al. 2019) and around stars with circumstellar
disks (e.g., J. Erkal et al. 2022), such as accreting T Tauri stars (S. Edwards
et al. 2006) or cataclysmic variables (D. Proga 2003).\r\n\r\n4.3. Implications
of Rotating Winds for the Emission Lines of LRDs\r\nThe disk wind hypothesis would
imply that a photosphere in the shape of a rotating disk is the source of the optical
continuum emission, and drives winds that can explain the observed absorption trough.
Emission lines originating in a thin rotating disk would have a double-peaked profile
in the idealized case (for most inclination angles), but this is not necessarily
true if the disk is not sufficiently thin (e.g., N. Murray & J. Chiang 1997), for
instance, in the case of a puffed-up disk associated with super-Eddington accretion
(e.g., H. Liu et al. 2026). In addition, most line emission would not be produced
directly at the base of the disk, but slightly outside (e.g., via collisional cooling
or residual recombination; A. Torralba et al. 2026), where the rotational velocity
is lower, and the dynamics are complex (e.g., G. A. Shields 1977).\r\n\r\nThe Balmer
lines of most LRDs are dominated by broad, symmetric exponential components that
are associated with broadening by electron scattering (e.g., V. Rusakov et al. 2026;
J. Matthee et al. 2026). For PAN-BH*-1, the Hα line profile of PAN-BH*-1 is compatible
with a broad exponential profile emerging through a dense wind where the absorption
trough is produced. In dense gas with a large column density of neutral hydrogen,
and optically thick to Balmer transitions (NHI,2s ≳ 1014 cm−2), resonant scattering
effects become important. Crucially, resonant scattering impacts Hα and Hβ differently
(e.g., S.-J. Chang et al. 2026), hence the 3D radiative transfer and photon redistribution
of both lines may produce different profiles (see, e.g., Figure 2 in D. Proga 2003).
Therefore, the empirical fitting and interpretation of the absorption profiles becomes
nontrivial. Dedicated radiative transfer modeling is necessary to study such effects,
and they can be tested in other emission lines with high optical depth, such as
He i λ10830 Å, or resonant lines like C iv λ1550.\r\n\r\n5. Implications for the
Galaxy and Black Hole Masses\r\n5.1. Properties of the Host Galaxy\r\nAssuming that
the narrow component of Hα corresponds to ISM emission in the host galaxy, we compute
the associated star formation rate using the local calibration from R. C. Kennicutt
& N. J. Evans (2012) and assuming no dust attenuation. We obtain SFR(Hα) = 3.3 ±
0.3 M⊙ yr−1. A somewhat lower value of SFR(Hα) = 2.1 ± 0.2 M⊙ yr−1 is obtained using
the high-redshift (z ≳ 4) calibrations in I. G. Kramarenko et al. (2026), which
might be more appropriate for a young dwarf galaxy with a bursty star formation
history. The star formation rates are low, but in line with a main-sequence galaxy
with (extrapolating the relation from J. S. Speagle et al. 2014). Assuming zero
dust attenuation, the UV absolute magnitude (MUV = −16.7 ± 0.7; Section 3.1) would
imply SFR(UV) = 0.18 ± 0.12 M⊙ yr−1 (R. C. Kennicutt & N. J. Evans 2012). The discrepancy
between the UV and Hα inferred star formation rate suggests there is some amount
of dust attenuation in the host galaxy.\r\n\r\nWe derive a dynamical mass from the
width of the narrow component Hα line and the estimated UV size as , adopting the
empirical virial correction K(n)K(q) from A. van der Wel et al. (2022), where K(n)
and K(q) are functions of the best-fit ellipticity and Sérsic index (see Appendix
B). Adopting a Mdyn/M* factor of 40 as found by A. de Graaff et al. (2024) for dwarf
galaxies at high redshift, we infer a stellar mass of . However, the Mdyn/M* is
very uncertain in this regime, and the uncertainty can span over 1 dex (A. Saldana-Lopez
et al. 2025). We advise caution in interpreting this result, as there are large
uncertainties in the measurements of the narrow Hα component, the HST morphology,
and the empirical relations used.\r\n\r\nAs discussed in Section 4, the absorption
profile is compatible with broadening by a rotating disk wind, and numerical modeling
of such configurations often predicts a narrow component arising from increased
transmission due to purely kinematic effects in the wind geometry (D. Proga et al.
2000; D. Proga 2003; D. Proga & T. R. Kallman 2004). This would be an alternative
explanation for at least part of the narrow component flux. On the other hand, most
LRDs present narrow [O iii] emission that is often associated with the host galaxy.
Indeed, the ionized gas producing [O iii] emission should have associated emission
in the Hα and higher-order Balmer lines. However, constraining this component largely
depends on the assumptions on dust attenuation or ISM conditions, and requires very
high S/N and resolution data. Deep, space-based follow-up observations of PAN-BH*-1
would be very constraining for the wind kinematics (e.g., by the joint analysis
of Hβ) and to assess whether a narrow component comes from a host galaxy (e.g.,
by comparing to a narrow Hβ component or [O iii] λλ4960, 5008).\r\n\r\n5.2. Black
Hole Mass From Photosphere Models\r\nThe general physical setup of LRDs is an open
debate, and their masses are a major unknown. Due to the multiple differences with
respect to the classical AGN population, the validity of standard virial calibrations
has been questioned (e.g., V. Rusakov et al. 2026; J. E. Greene et al. 2026; A.
Sneppen et al. 2026; A. Torralba et al. 2026, although see, e.g., M. Brazzini et
al. 2025, 2026; J. Scholtz et al. 2026 for an alternative interpretation).\r\n\r\nOne
can obtain a mass estimate assuming a system in radiative equilibrium with Lbol/LEdd
= 1 (e.g., H. Umeda et al. 2026); this yields a total mass of ≈106 M⊙, using the
bolometric luminosity from integrating the best-fit blackbody in Section 3.1. Recently,
H. Liu et al. (2026) developed a synthetic spectral library of LRD atmosphere models.
In these models, the density of the photosphere is regulated by the net surface
gravity of an optically thick atmosphere, enabling constraints on the mass of the
system. We fit the JWST photometry of PAN-BH*-1 using the models from H. Liu et
al. (2026), assuming a negligible contribution from a host galaxy to the optical
continuum. The best-fit model has effective temperature Teff = 4800 K, surface gravity
, and metallicity (; see Figure 1). The best-fit implies a total mass of the system
(BH plus gas) of (Equation (6) in H. Liu et al. 2026, assuming hydrostatic equilibrium).
For the second and third best fits, we obtain and −2, respectively (, respectively;
with the same metallicity and effective temperature), which would imply lower limits
to the system mass between and 4. The bolometric luminosity of PAN-BH*-1 (from the
integral of the best-fit green curve in Figure 1) implies an Eddington luminosity
ratio of L/LEdd ≲ 13, assuming the best-fit mass from the H. Liu et al. (2026) models.
The elevated Eddington ratio is in line with the hypothesis of a radiation-driven
wind discussed in Section 4, and allows for somewhat larger system masses. The low
masses obtained with this model, combined with the stellar mass inferred from dynamical
arguments for the host galaxy (Section 3.3) set lower limits to the BH-to-stellar
mass ratio of MBH/M* ≳ 10−4–10−2, which are compatible with the relations observed
in the Local Universe, within the large uncertainties (A. E. Reines & M. Volonteri
2015).\r\n\r\n6. Conclusions\r\nIn this Letter, we presented the discovery and spectroscopic
confirmation of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.731. The
strength of the Balmer break (F115W/F814W = 7 ± 1) is comparable to the most extreme
LRDs known, The Cliff (A. de Graaff et al. 2025a) and MoM-BH* (R. P. Naidu et al.
2025). We summarize the observations and our main conclusions as follows.\r\n\r\n\r\n1.
\ \r\nWe obtained deep VLT/X-Shooter spectroscopy of PAN-BH*-1. The Hα emission
line is luminous and broad (LHα = 1043 erg s−1), and has an unusually strong absorption.
Hβ is detected with an S/N ≈ 6, and we conservatively estimate a lower limit for
the Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with other
LRDs in the literature (e.g., A. de Graaff et al. 2025b; G. P. Nikopoulos et al.
2026).\r\n2. \r\nThe absorption trough spans from −520 to 267 km s−1 (at a transmission
level of 99%). We interpret the presence of blue- and redshifted absorption as produced
by a disk wind, analogous to those analyzed in the context of broad absorption line
quasars or accreting stars. This hypothesis would imply that the source of the optical
continuum is likely a thick photospheric disk.\r\n3. \r\nWe detect a narrow Hα
component (FWHM = 184 ± 12 km s−1), which we interpret as probing a host galaxy
with M* ≈ 108 M⊙ and SFR = 2–3 M⊙. This interpretation is in line with the extended
rest-NUV morphology measured in the HST bands (\r\n kpc).\r\n4. \r\nBy fitting
the synthetic atmosphere models of H. Liu et al. (2026), we estimate a system mass
(BH+envelope) of 104–106 M⊙. The inferred masses, together with the stellar mass
inferred from morphology and narrow emission line dynamics, imply BH-to-stellar
mass ratios of 10−2–10−4, close to the extrapolated trend in the local Universe
(A. E. Reines & M. Volonteri 2015).\r\n5. \r\nThe confirmation of this source at
cosmic noon (magnitude of ≈22 in the K band, Hα flux ≈5 × 10−16 erg s−1 cm−2) proves
the feasibility of detecting extreme LRDs at such epochs with wide-area spectroscopic
surveys like Euclid or the forthcoming Nancy Grace Roman Space Telescope.\r\n\r\nAcknowledgments\r\nA.T.
thanks Debasish Dutta and Tamara Bogdanović for useful conversations about stellar
and AGN winds.\r\n\r\nWe thank the scientific referee for the useful and constructive
feedback, which helped improve the quality of this paper.\r\n\r\nJ.M. and A.T. acknowledge
funding by the European Union (ERC, AGENTS, 101076224). The work of CCW is supported
by NOIRLab, which is managed by the Association of Universities for Research in
Astronomy (AURA) under a cooperative agreement with the National Science Foundation.
A.P.C. warmly acknowledges the support of the National Science Foundation through
the NSF Graduate Research Fellowship Program. A.d.G. acknowledges support from a
Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.\r\n\r\nBased
on observations made with ESO Telescopes at the Paranal Observatory under program
IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is based in part on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with programs #2514 and #9433. C.C.W. gratefully acknowledges support for program
JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs
R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access
period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble
Space Telescope obtained from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., under NASA contract
NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST
and HST data presented in this article were obtained from the Mikulski Archive for
Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations
analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis work is based in
part on observations made with the Spitzer Space Telescope, which was operated by
the Jet Propulsion Laboratory, California Institute of Technology under a contract
with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis
work was supported by the International Space Science Institute (ISSI) in Bern,
through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST
cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope
(Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam,
NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space
Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration
et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al.
2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023),
stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL
Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP
(K. Barbary 2016)."
article_number: L37
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Aidan P.
full_name: Cloonan, Aidan P.
last_name: Cloonan
- first_name: Aayush A
full_name: Desai, Aayush A
id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
last_name: Desai
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Christian Kragh
full_name: Jespersen, Christian Kragh
last_name: Jespersen
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Wendy Q.
full_name: Sun, Wendy Q.
last_name: Sun
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: 'Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic
noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick
winds in a Little Red Dot at z = 1.7. 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:
- access_level: open_access
checksum: 7600db260d799ddea45cf3bd01effe41
content_type: application/pdf
creator: dernst
date_created: 2026-07-13T07:46:22Z
date_updated: 2026-07-13T07:46:22Z
file_id: '22274'
file_name: 2026_AstrophysicalJourLetters_Torralba.pdf
file_size: 5419071
relation: main_file
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file_date_updated: 2026-07-13T07:46:22Z
has_accepted_license: '1'
intvolume: ' 1005'
issue: '2'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: 'A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum,
and broad absorption by thick winds in a Little Red Dot at z = 1.7'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 1005
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21058'
abstract:
- lang: eng
text: Luminous broad Hα emission and red rest-optical spectral energy distributions
(SEDs) are the hallmark of compact little red dots (LRDs), implying highly attenuated
dusty starbursts and/or obscured active galactic nuclei (AGN). However, the lack
of observed far-infrared (FIR) emission has proved difficult to reconcile with
the implied attenuated luminosity in these models. Here, we utilize deep new Atacama
Large Millimeter/submillimeter Array imaging, new and existing JWST/MIRI imaging,
and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs
(z = 3.1 and z = 4.47) to place the strongest constraints on the IR luminosity
in LRDs to date. The detections at λrest = 1–4 μm imply flat slopes in the rest-IR,
ruling out a contribution from hot (T ≳ 500 K) dust. Similarly, FIR nondetections
rule out any appreciable cold (T ≲ 75 K) dust component. Assuming energy balance,
these observations are inconsistent with the typical FIR dust emission of dusty
starbursts and quasar tori, which usually show a mixture of cold and hot dust.
Additionally, our [C ii] nondetections rule out typical dusty starbursts. We compute
empirical maximum IR SEDs and find that both LRDs must have log(LIR/L ) 12.2 at
the 3σ level. These limits are in tension with the predictions of rest-optical
spectrophotometric fits, be they galaxy-only, AGN-only, or composite. It is unlikely
that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature
distribution that conspires to avoid current observing facilities. Rather, we
favor an intrinsically redder LRD SED model that alleviates the need for strong
dust attenuation.
acknowledgement: "Support for this work was provided by The Brinson Foundation through
a Brinson Prize Fellowship grant. D.S. acknowledges Zhengrong Li for kindly sharing
model dust SEDs, Tim Rawle for helping with accessing archival Herschel Lensing
Survey data, and Xiaohui Fan for helpful conversations that steered the direction
of this work. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2024.00826.S.
ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic
of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory
is operated by ESO, AUI/NRAO and NAOJ. 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
(DOI: 10.17909/m7ks-wg55), 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 #6761.\r\n\r\nSupport for this work was
provided by NSF/AAG #2306950. Support for this work for R.P.N. was provided by NASA
through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space
Telescope Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work has received
funding from the Swiss State Secretariat for Education, Research and Innovation
(SERI) under contract number MB22.00072, as well as from the Swiss National Science
Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center is
funded by the Danish National Research Foundation under grant DNRF140. A.Z. acknowledges
support by grant No. 2020750 from the United States–Israel Binational Science Foundation
(BSF) and grant No. 2109066 from the United States National Science Foundation (NSF)
and by the Israel Science Foundation grant No. 864/23. The work of C.C.W. is supported
by NOIRLab, which is managed by the Association of Universities for Research in
Astronomy (AURA) under a cooperative agreement with the National Science Foundation.
S.A. acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team
Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University
of Arizona."
article_number: L10
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Justin S.
full_name: Spilker, Justin S.
last_name: Spilker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- first_name: Yilun 逸伦
full_name: Ma, Yilun 逸伦
last_name: Ma
- first_name: Bingjie 冰洁
full_name: Wang, Bingjie 冰洁
last_name: Wang
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Anna
full_name: de Graaff, Anna
last_name: de Graaff
- first_name: Stacey
full_name: Alberts, Stacey
last_name: Alberts
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Sam E.
full_name: Cutler, Sam E.
last_name: Cutler
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Olivia R.
full_name: Cooper, Olivia R.
last_name: Cooper
- first_name: Pratika
full_name: Dayal, Pratika
last_name: Dayal
- first_name: Seiji
full_name: Fujimoto, Seiji
last_name: Fujimoto
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Andy D.
full_name: Goulding, Andy D.
last_name: Goulding
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Ian
full_name: McConachie, Ian
last_name: McConachie
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Tim B.
full_name: Miller, Tim B.
last_name: Miller
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Richard
full_name: Pan, Richard
last_name: Pan
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: John R.
full_name: Weaver, John R.
last_name: Weaver
- first_name: Mengyuan
full_name: Xiao, Mengyuan
last_name: Xiao
- first_name: Yunchong
full_name: Zhang, Yunchong
last_name: Zhang
- first_name: Adi
full_name: Zitrin, Adi
last_name: Zitrin
citation:
ama: Setton DJ, Greene JE, Spilker JS, et al. A confirmed deficit of hot and cold
dust emission in the most luminous Little Red Dots. The Astrophysical Journal
Letters. 2025;991. doi:10.3847/2041-8213/ade78b
apa: Setton, D. J., Greene, J. E., Spilker, J. S., Williams, C. C., Labbé, I., Ma,
Y. 逸伦, … Zitrin, A. (2025). A confirmed deficit of hot and cold dust emission
in the most luminous Little Red Dots. The Astrophysical Journal Letters.
IOP Publishing. https://doi.org/10.3847/2041-8213/ade78b
chicago: Setton, David J., Jenny E. Greene, Justin S. Spilker, Christina C. Williams,
Ivo Labbé, Yilun 逸伦 Ma, Bingjie 冰洁 Wang, et al. “A Confirmed Deficit of Hot and
Cold Dust Emission in the Most Luminous Little Red Dots.” The Astrophysical
Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ade78b.
ieee: D. J. Setton et al., “A confirmed deficit of hot and cold dust emission
in the most luminous Little Red Dots,” The Astrophysical Journal Letters,
vol. 991. IOP Publishing, 2025.
ista: Setton DJ, Greene JE, Spilker JS, Williams CC, Labbé I, Ma Y逸伦, Wang B冰洁,
Whitaker KE, Leja J, de Graaff A, Alberts S, Bezanson R, Boogaard LA, Brammer
G, Cutler SE, Cleri NJ, Cooper OR, Dayal P, Fujimoto S, Furtak LJ, Goulding AD,
Hirschmann M, Kokorev V, Maseda MV, McConachie I, Matthee JJ, Miller TB, Naidu
RP, Oesch PA, Pan R, Price SH, Suess KA, Weaver JR, Xiao M, Zhang Y, Zitrin A.
2025. A confirmed deficit of hot and cold dust emission in the most luminous Little
Red Dots. The Astrophysical Journal Letters. 991, L10.
mla: Setton, David J., et al. “A Confirmed Deficit of Hot and Cold Dust Emission
in the Most Luminous Little Red Dots.” The Astrophysical Journal Letters,
vol. 991, L10, IOP Publishing, 2025, doi:10.3847/2041-8213/ade78b.
short: D.J. Setton, J.E. Greene, J.S. Spilker, C.C. Williams, I. Labbé, Y.逸伦 Ma,
B.冰洁 Wang, K.E. Whitaker, J. Leja, A. de Graaff, S. Alberts, R. Bezanson, L.A.
Boogaard, G. Brammer, S.E. Cutler, N.J. Cleri, O.R. Cooper, P. Dayal, S. Fujimoto,
L.J. Furtak, A.D. Goulding, M. Hirschmann, V. Kokorev, M.V. Maseda, I. McConachie,
J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, R. Pan, S.H. Price, K.A. Suess,
J.R. Weaver, M. Xiao, Y. Zhang, A. Zitrin, The Astrophysical Journal Letters 991
(2025).
date_created: 2026-01-28T15:23:00Z
date_published: 2025-09-12T00:00:00Z
date_updated: 2026-02-09T07:14:08Z
day: '12'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ade78b
external_id:
arxiv:
- '2503.02059'
file:
- access_level: open_access
checksum: 799518db92ded4e166df4234195af998
content_type: application/pdf
creator: dernst
date_created: 2026-02-09T07:10:29Z
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has_accepted_license: '1'
intvolume: ' 991'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: A confirmed deficit of hot and cold dust emission in the most luminous Little
Red Dots
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: 991
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21121'
abstract:
- lang: eng
text: The relation between the masses of supermassive black holes (SMBHs) and their
host galaxies encodes information on their mode of growth, especially at the earliest
epochs. The James Webb Space Telescope (JWST) has opened such investigations by
detecting the host galaxies of active galactic nuclei (AGN) and more luminous
quasars within the first billion years of the Universe (z ≳ 6). Here, we evaluate
the relation between the mass of SMBHs and the total stellar mass of their host
galaxies using a sample of nine quasars at 6.18 ≤ z ≤ 6.4 from the Subaru High-z
Exploration of Low-luminosity Quasars survey with NIRCam and NIRSpec observations.
We find that the observed location of these quasars in the SMBH–galaxy mass plane
(logMBH/M 8–9; logM*/M 9.5–11) is consistent with a nonevolving intrinsic mass
relation with dispersion (0.80 +0.23 -0.28 dex) higher than the local value (∼0.3–0.4
dex) of their more massive descendants. Our analysis is based on a forward model
of systematics and includes a consideration of the impact of selection effects
and measurement uncertainties with an assumption on the slope of the mass relation.
While degeneracies between parameters persist, the best-fit solution has a reasonable
AGN fraction (2.3%) of galaxies at z ∼ 6 with an actively growing UV-unobscured
black hole. In particular, models with a substantially higher normalisation in
MBH would require an unrealistically low intrinsic dispersion (∼0.22 dex). Consequently,
our results predict a large population of AGN at lower black hole masses, as are
now just starting to be discovered in focused efforts with JWST.
acknowledgement: 'This work is based on observations made with the NASA/ESA/CSA James
Webb Space Telescope. The data were obtained from the Mikulski Archive for Space
Telescopes at the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127
for JWST. These observations are associated with programs GO #1967 and GO #3859.
The specific observations analyzed can be accessed via DOI: 10.17909/719q-cn32.
Support for these programs was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127. This work was supported by
World Premier International Research Center Initiative (WPI), MEXT, Japan. This
work used computing resources at Kavli IPMU. J.S. is supported by JSPS KAKENHI (JP22H01262).
M.O. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI
grant No. 24K22894. Y.M. was supported by the Japan Society for the Promotion of
Science (JSPS) KAKENHI grant No. 21H04494. M.V. gratefully acknowledges financial
support from the Independent Research Fund Denmark via grant numbers DFF 8021-00130
and 3103-00146 and from the Carlsberg Foundation via grant CF23-0417. S.E.I.B. is
supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant
number BO 5771/1-1. K.I. acknowledges support from the National Natural Science
Foundation of China (12073003, 11721303, 11991052). K.I. acknowledges support under
the grant PID2022-136827NB-C44 provided by MCIN/AEI/10.13039/501100011033 / FEDER,
UE. A.L. acknowledges support from PRIN MUR 2022— Project “2022935STW.” J.T.S. is
supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—project
number 518006966. F.W. acknowledges support from NSF award AST-2513040. M.H. acknowledges
support from the FNS under the SNSF starting grant 218032. B.T. acknowledges support
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation program (grant agreement number 950533) and from the Excellence
Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German
Research Foundation) under Germany’s Excellence Strategy—EXC 2094—390783311.'
article_number: L67
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: John David
full_name: Silverman, John David
last_name: Silverman
- first_name: Junyao
full_name: Li, Junyao
last_name: Li
- first_name: Xuheng
full_name: Ding, Xuheng
last_name: Ding
- first_name: Masafusa
full_name: Onoue, Masafusa
last_name: Onoue
- first_name: Michael A.
full_name: Strauss, Michael A.
last_name: Strauss
- first_name: Yoshiki
full_name: Matsuoka, Yoshiki
last_name: Matsuoka
- first_name: Takuma
full_name: Izumi, Takuma
last_name: Izumi
- first_name: Knud
full_name: Jahnke, Knud
last_name: Jahnke
- first_name: Tommaso
full_name: Treu, Tommaso
last_name: Treu
- first_name: Marta
full_name: Volonteri, Marta
last_name: Volonteri
- first_name: Camryn L.
full_name: Phillips, Camryn L.
last_name: Phillips
- first_name: Irham T.
full_name: Andika, Irham T.
last_name: Andika
- first_name: Kentaro
full_name: Aoki, Kentaro
last_name: Aoki
- first_name: Junya
full_name: Arita, Junya
last_name: Arita
- first_name: Shunsuke
full_name: Baba, Shunsuke
last_name: Baba
- first_name: Sarah E. I.
full_name: Bosman, Sarah E. I.
last_name: Bosman
- first_name: Anna-Christina
full_name: Eilers, Anna-Christina
last_name: Eilers
- first_name: Xiaohui
full_name: Fan, Xiaohui
last_name: Fan
- first_name: Seiji
full_name: Fujimoto, Seiji
last_name: Fujimoto
- first_name: Melanie
full_name: Habouzit, Melanie
last_name: Habouzit
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
- first_name: Masatoshi
full_name: Imanishi, Masatoshi
last_name: Imanishi
- first_name: Kohei
full_name: Inayoshi, Kohei
last_name: Inayoshi
- first_name: Kazushi
full_name: Iwasawa, Kazushi
last_name: Iwasawa
- first_name: Nobunari
full_name: Kashikawa, Nobunari
last_name: Kashikawa
- first_name: Toshihiro
full_name: Kawaguchi, Toshihiro
last_name: Kawaguchi
- first_name: Chien-Hsiu
full_name: Lee, Chien-Hsiu
last_name: Lee
- first_name: Alessandro
full_name: Lupi, Alessandro
last_name: Lupi
- first_name: Tohru
full_name: Nagao, Tohru
last_name: Nagao
- first_name: Jan-Torge
full_name: Schindler, Jan-Torge
last_name: Schindler
- first_name: Malte
full_name: Schramm, Malte
last_name: Schramm
- first_name: Kazuhiro
full_name: Shimasaku, Kazuhiro
last_name: Shimasaku
- first_name: Yoshiki
full_name: Toba, Yoshiki
last_name: Toba
- first_name: Benny
full_name: Trakhtenbrot, Benny
last_name: Trakhtenbrot
- first_name: Hideki
full_name: Umehata, Hideki
last_name: Umehata
- first_name: Marianne
full_name: Vestergaard, Marianne
last_name: Vestergaard
- first_name: Fabian
full_name: Walter, Fabian
last_name: Walter
- first_name: Feige
full_name: Wang, Feige
last_name: Wang
- first_name: Jinyi
full_name: Yang, Jinyi
last_name: Yang
citation:
ama: Silverman JD, Li J, Ding X, et al. SHELLQs–JWST perspective on the intrinsic
mass relation between supermassive black holes and their host galaxies at z >
6. The Astrophysical Journal Letters. 2025;995(2). doi:10.3847/2041-8213/ae279c
apa: Silverman, J. D., Li, J., Ding, X., Onoue, M., Strauss, M. A., Matsuoka, Y.,
… Yang, J. (2025). SHELLQs–JWST perspective on the intrinsic mass relation between
supermassive black holes and their host galaxies at z > 6. The Astrophysical
Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae279c
chicago: Silverman, John David, Junyao Li, Xuheng Ding, Masafusa Onoue, Michael
A. Strauss, Yoshiki Matsuoka, Takuma Izumi, et al. “SHELLQs–JWST Perspective on
the Intrinsic Mass Relation between Supermassive Black Holes and Their Host Galaxies
at z > 6.” The Astrophysical Journal Letters. IOP Publishing, 2025.
https://doi.org/10.3847/2041-8213/ae279c.
ieee: J. D. Silverman et al., “SHELLQs–JWST perspective on the intrinsic
mass relation between supermassive black holes and their host galaxies at z >
6,” The Astrophysical Journal Letters, vol. 995, no. 2. IOP Publishing,
2025.
ista: Silverman JD, Li J, Ding X, Onoue M, Strauss MA, Matsuoka Y, Izumi T, Jahnke
K, Treu T, Volonteri M, Phillips CL, Andika IT, Aoki K, Arita J, Baba S, Bosman
SEI, Eilers A-C, Fan X, Fujimoto S, Habouzit M, Haiman Z, Imanishi M, Inayoshi
K, Iwasawa K, Kashikawa N, Kawaguchi T, Lee C-H, Lupi A, Nagao T, Schindler J-T,
Schramm M, Shimasaku K, Toba Y, Trakhtenbrot B, Umehata H, Vestergaard M, Walter
F, Wang F, Yang J. 2025. SHELLQs–JWST perspective on the intrinsic mass relation
between supermassive black holes and their host galaxies at z > 6. The Astrophysical
Journal Letters. 995(2), L67.
mla: Silverman, John David, et al. “SHELLQs–JWST Perspective on the Intrinsic Mass
Relation between Supermassive Black Holes and Their Host Galaxies at z > 6.”
The Astrophysical Journal Letters, vol. 995, no. 2, L67, IOP Publishing,
2025, doi:10.3847/2041-8213/ae279c.
short: J.D. Silverman, J. Li, X. Ding, M. Onoue, M.A. Strauss, Y. Matsuoka, T. Izumi,
K. Jahnke, T. Treu, M. Volonteri, C.L. Phillips, I.T. Andika, K. Aoki, J. Arita,
S. Baba, S.E.I. Bosman, A.-C. Eilers, X. Fan, S. Fujimoto, M. Habouzit, Z. Haiman,
M. Imanishi, K. Inayoshi, K. Iwasawa, N. Kashikawa, T. Kawaguchi, C.-H. Lee, A.
Lupi, T. Nagao, J.-T. Schindler, M. Schramm, K. Shimasaku, Y. Toba, B. Trakhtenbrot,
H. Umehata, M. Vestergaard, F. Walter, F. Wang, J. Yang, The Astrophysical Journal
Letters 995 (2025).
date_created: 2026-01-31T09:27:53Z
date_published: 2025-12-17T00:00:00Z
date_updated: 2026-02-10T07:02:39Z
day: '17'
ddc:
- '520'
department:
- _id: ZoHa
doi: 10.3847/2041-8213/ae279c
external_id:
arxiv:
- '2507.23066'
file:
- access_level: open_access
checksum: e38c0c444be9c1507eec28c62ce04cbc
content_type: application/pdf
creator: dernst
date_created: 2026-02-10T06:56:37Z
date_updated: 2026-02-10T06:56:37Z
file_id: '21202'
file_name: 2025_AstrophysicalJounalLetters_Silvermann.pdf
file_size: 997137
relation: main_file
success: 1
file_date_updated: 2026-02-10T06:56:37Z
has_accepted_license: '1'
intvolume: ' 995'
issue: '2'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
status: public
title: SHELLQs–JWST perspective on the intrinsic mass relation between supermassive
black holes and their host galaxies at z > 6
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 995
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21317'
abstract:
- lang: eng
text: Accreting white dwarfs (WDs) in close binary systems, commonly known as cataclysmic
variables (CVs), with orbital periods below the canonical period minimum (≈80
minutes) are rare. Such short periods can only be reached if the donor star in
the CV is either significantly evolved before initiating mass transfer to the
WD or is metal-poor. We present optical photometry and spectroscopy of Gaia19bxc,
a high-amplitude variable identified as a polar CV with an exceptionally short
orbital period of 64.42 minutes—well below the canonical CV period minimum. High-speed
photometry confirms persistent double-peaked variability consistent with cyclotron
beaming, thus indicating the presence of a magnetic WD. Phase-resolved Keck/Low-Resolution
Imaging Spectrometer (LRIS) spectroscopy reveals strong hydrogen and helium emission
lines but no donor features, indicating the accretor is a magnetic WD and the
donor is hydrogen-rich, but cold and faint. The absence of a detectable donor
and the low inferred temperature (≲3500 K) disfavor an evolved donor scenario.
Instead, the short period and the system’s halo-like kinematics suggest Gaia19bxc
may be the first known metal-poor polar. Because metal-poor donors are more compact
than solar-metallicity donors of the same mass, they can reach shorter minimum
periods. Gaia19bxc is one of only a handful of known metal-poor CVs below the
canonical period minimum and has the shortest period of any such magnetic system
discovered to date.
acknowledgement: "Based on observations obtained with the Samuel Oschin Telescope
48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky
Transient Facility project. ZTF is supported by the National Science Foundation
under grants No. AST-1440341 and AST-2034437 and a collaboration including current
partners Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center
at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron
and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin
at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories,
IN2P3, University of Warwick, Ruhr University Bochum, Northwestern University and
former partners the University of Washington, Los Alamos National Laboratories,
and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC,
and UW. This work has made use of data from the European Space Agency (ESA) mission
Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and
Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium).
Funding for the DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement. Some of the data
presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit
organization operated as a scientific partnership among the California Institute
of Technology, the University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous financial support
of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Maunakea has always had within the
Native Hawaiian community. We are most fortunate to have had the opportunity to
conduct observations from this mountain. We are grateful to the staff of the Palomar
and Keck Observatories for their work in helping us carry out our observations.\r\n\r\nI.G.
acknowledges support from Kazan Federal University. A.C.R. acknowledges support
from the National Science Foundation via an NSF Graduate Research Fellowship. We
thank the anonymous referee for useful comments and suggestions, which contributed
to the improvement of this manuscript."
article_number: L57
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Ilkham
full_name: Galiullin, Ilkham
last_name: Galiullin
- first_name: Antonio C.
full_name: Rodriguez, Antonio C.
last_name: Rodriguez
- first_name: Kareem
full_name: El-Badry, Kareem
last_name: El-Badry
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Paula
full_name: Szkody, Paula
last_name: Szkody
- first_name: Pranav
full_name: Nagarajan, Pranav
last_name: Nagarajan
- first_name: Samuel
full_name: Whitebook, Samuel
last_name: Whitebook
citation:
ama: Galiullin I, Rodriguez AC, El-Badry K, et al. Optical spectroscopy of the most
compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich
donor. The Astrophysical Journal Letters. 2025;990(2). doi:10.3847/2041-8213/adff82
apa: Galiullin, I., Rodriguez, A. C., El-Badry, K., Caiazzo, I., Szkody, P., Nagarajan,
P., & Whitebook, S. (2025). Optical spectroscopy of the most compact accreting
binary harboring a magnetic White Dwarf and a hydrogen-rich donor. The Astrophysical
Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/adff82
chicago: Galiullin, Ilkham, Antonio C. Rodriguez, Kareem El-Badry, Ilaria Caiazzo,
Paula Szkody, Pranav Nagarajan, and Samuel Whitebook. “Optical Spectroscopy of
the Most Compact Accreting Binary Harboring a Magnetic White Dwarf and a Hydrogen-Rich
Donor.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/adff82.
ieee: I. Galiullin et al., “Optical spectroscopy of the most compact accreting
binary harboring a magnetic White Dwarf and a hydrogen-rich donor,” The Astrophysical
Journal Letters, vol. 990, no. 2. IOP Publishing, 2025.
ista: Galiullin I, Rodriguez AC, El-Badry K, Caiazzo I, Szkody P, Nagarajan P, Whitebook
S. 2025. Optical spectroscopy of the most compact accreting binary harboring a
magnetic White Dwarf and a hydrogen-rich donor. The Astrophysical Journal Letters.
990(2), L57.
mla: Galiullin, Ilkham, et al. “Optical Spectroscopy of the Most Compact Accreting
Binary Harboring a Magnetic White Dwarf and a Hydrogen-Rich Donor.” The Astrophysical
Journal Letters, vol. 990, no. 2, L57, IOP Publishing, 2025, doi:10.3847/2041-8213/adff82.
short: I. Galiullin, A.C. Rodriguez, K. El-Badry, I. Caiazzo, P. Szkody, P. Nagarajan,
S. Whitebook, The Astrophysical Journal Letters 990 (2025).
date_created: 2026-02-18T10:17:04Z
date_published: 2025-09-08T00:00:00Z
date_updated: 2026-02-19T07:27:01Z
day: '08'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.3847/2041-8213/adff82
external_id:
arxiv:
- '2508.20170'
file:
- access_level: open_access
checksum: f76556d129aa0e9facc85602b0b5b54d
content_type: application/pdf
creator: dernst
date_created: 2026-02-19T07:24:10Z
date_updated: 2026-02-19T07:24:10Z
file_id: '21329'
file_name: 2025_AstrophysicalJournal_Galiullin.pdf
file_size: 3772189
relation: main_file
success: 1
file_date_updated: 2026-02-19T07:24:10Z
has_accepted_license: '1'
intvolume: ' 990'
issue: '2'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Optical spectroscopy of the most compact accreting binary harboring a magnetic
White Dwarf and a hydrogen-rich donor
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: 990
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '19638'
abstract:
- lang: eng
text: The James Webb Space Telescope has revealed low-luminosity active galactic
nuclei at redshifts of z ≳ 4–7, many of which host accreting massive black holes
(BHs) with BH-to-galaxy mass (MBH/M⋆) ratios exceeding the local values by more
than an order of magnitude. The origin of these overmassive BHs remains unclear
but requires potential contributions from heavy seeds and/or episodes of super-Eddington
accretion. We present a growth model coupled with dark matter halo assembly to
explore the evolution of the MBH/M⋆ ratio under different seeding and feedback
scenarios. Given the gas inflow rates in protogalaxies, BHs grow episodically
at moderate super-Eddington rates, and the mass ratio increases early on, despite
significant mass loss through feedback. Regardless of seeding mechanisms, the
mass ratio converges to a universal value ∼0.1–0.3, set by the balance between
gas feeding and star formation efficiency in the nucleus. This behavior defines
an attractor in the MBH–M⋆ diagram, where overmassive BHs grow more slowly than
their hosts, while undermassive seeds experience rapid growth before aligning
with the attractor. We derive an analytical expression for the universal mass
ratio, linking it to feedback strength and halo growth. The convergence of evolutionary
tracks erases seeding information from the mass ratio by z ∼ 4–6. Detecting BHs
with ∼105−6 M⊙ at higher redshifts that deviate from the convergence trend would
provide key diagnostics of their birth conditions.
acknowledgement: We thank the anonymous referee for a careful reading of our manuscript
and for comments that helped improve this Letter. This work is supported by the
Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24KF0130. We
acknowledge support from the National Natural Science Foundation of China (12073003,
12003003, 11721303, 11991052, 11950410493), and the China Manned Space Project (CMS-CSST-2021-A04
and CMS-CSST-2021-A06). L.C.H. is supported by the National Science Foundation of
China (12233001), the National Key R&D Program of China (2022YFF0503401). Z.H. acknowledges
support by US NSF grant AST-2006176 and by NASA grant 80NSSC22K0822. Some of the
numerical calculation and analysis were performed with the Cray XC50 at the Center
for Computational Astrophysics (CfCA) of the National Astronomical Observatory of
Japan and with the High-performance Computing Platform of Peking University.
article_number: L37
article_processing_charge: Yes
article_type: letter_note
arxiv: 1
author:
- first_name: Haojie
full_name: Hu, Haojie
last_name: Hu
- first_name: Kohei
full_name: Inayoshi, Kohei
last_name: Inayoshi
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
- first_name: Luis C.
full_name: Ho, Luis C.
last_name: Ho
- first_name: Ken
full_name: Ohsuga, Ken
last_name: Ohsuga
citation:
ama: Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. The convergence of heavy and light
seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal
Letters. 2025;983(2). doi:10.3847/2041-8213/adc680
apa: Hu, H., Inayoshi, K., Haiman, Z., Ho, L. C., & Ohsuga, K. (2025). The convergence
of heavy and light seeds to overmassive black holes at cosmic dawn. The Astrophysical
Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/adc680
chicago: Hu, Haojie, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, and Ken Ohsuga.
“The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic
Dawn.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/adc680.
ieee: H. Hu, K. Inayoshi, Z. Haiman, L. C. Ho, and K. Ohsuga, “The convergence of
heavy and light seeds to overmassive black holes at cosmic dawn,” The Astrophysical
Journal Letters, vol. 983, no. 2. IOP Publishing, 2025.
ista: Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. 2025. The convergence of heavy
and light seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal
Letters. 983(2), L37.
mla: Hu, Haojie, et al. “The Convergence of Heavy and Light Seeds to Overmassive
Black Holes at Cosmic Dawn.” The Astrophysical Journal Letters, vol. 983,
no. 2, L37, IOP Publishing, 2025, doi:10.3847/2041-8213/adc680.
short: H. Hu, K. Inayoshi, Z. Haiman, L.C. Ho, K. Ohsuga, The Astrophysical Journal
Letters 983 (2025).
date_created: 2025-05-04T22:02:31Z
date_published: 2025-04-20T00:00:00Z
date_updated: 2026-02-16T12:44:04Z
day: '20'
ddc:
- '520'
department:
- _id: ZoHa
doi: 10.3847/2041-8213/adc680
external_id:
arxiv:
- '2503.03870'
isi:
- '001467616800001'
file:
- access_level: open_access
checksum: 1a4fbeeb12e9022873e86c72d230a5ec
content_type: application/pdf
creator: dernst
date_created: 2025-05-05T11:30:34Z
date_updated: 2025-05-05T11:30:34Z
file_id: '19655'
file_name: 2025_AstrophysicalJourLetters_Hu.pdf
file_size: 3334014
relation: main_file
success: 1
file_date_updated: 2025-05-05T11:30:34Z
has_accepted_license: '1'
intvolume: ' 983'
isi: 1
issue: '2'
language:
- iso: eng
month: '04'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: The convergence of heavy and light seeds to overmassive black holes at cosmic
dawn
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: 983
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '20030'
abstract:
- lang: eng
text: We report the discovery of a Lyα emitter (LAE) candidate in the immediate
foreground of the quasar PSO J158-14 at zQSO = 6.0685 at a projected distance
∼29 pkpc that is associated with an extremely metal-poor absorption system. This
system was found in archival observations of the quasar field with the Very Large
Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) and was previously missed
in searches of absorption systems using quasar absorption line spectroscopy, as
it imparts no detectable metal absorption lines on the background quasar spectrum.
The detected Lyα emission line at a redshift of zLAE = 6.0323 is well aligned
with the outer edge of the quasar’s proximity zone and can plausibly cause its
observed damping wing if it is associated with a proximate subdamped Lyα absorption
system with a column density of log Nhi/cm^-2 19.7. A >10 hr medium-resolution
spectrum of the quasar observed with the Magellan/Folded-port InfraRed Echellette
(FIRE) and VLT/X-Shooter spectrographs reveals a metallicity constraint of [Z/H]
< −3. Such low metallicity makes this system an extremely metal-poor galaxy candidate
and provides an exciting site to study possible signatures of Population III stars.
acknowledgement: "We thank the referee for the feedback and suggestions that greatly
improved the quality of this manuscript. We would like to thank Carlos Contreras,
Matías Díaz, Carla Fuentes, Mauricio Martínez, Alberto Pastén, Roger Leiton, Hugo
Rivera, and Gabriel Prieto for their help and support during the Magellan/FIRE observations.
We would also like to thank Rongmon Bordoloi for helpful discussions. R.A.M. acknowledges
support from the Swiss National Science Foundation (SNSF) through project grant
200020_207349. This Letter includes data gathered with the 6.5 m Magellan Telescopes
located at Las Campanas Observatory, Chile.\r\nBased on observations collected at
the European Southern Observatory under ESO programs 106.215A and 096.A-0418.\r\n\r\nThe
HST data presented in this Letter were obtained from the Mikulski Archive for Space
Telescopes (MAST) at the Space Telescope Science Institute. The observations analyzed
in this work can be accessed via doi:10.17909/gxmz-zd87."
article_number: L33
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Dominika
full_name: Ďurovčíková, Dominika
last_name: Ďurovčíková
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Louise
full_name: Welsh, Louise
last_name: Welsh
- first_name: Romain A.
full_name: Meyer, Romain A.
last_name: Meyer
- 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: Emma V.
full_name: Ryan-Weber, Emma V.
last_name: Ryan-Weber
- first_name: Minghao
full_name: Yue, Minghao
last_name: Yue
- first_name: Harley
full_name: Katz, Harley
last_name: Katz
- first_name: Sindhu
full_name: Satyavolu, Sindhu
last_name: Satyavolu
- first_name: George
full_name: Becker, George
last_name: Becker
- first_name: Frederick B.
full_name: Davies, Frederick B.
last_name: Davies
- first_name: Emanuele Paolo
full_name: Farina, Emanuele Paolo
last_name: Farina
citation:
ama: Ďurovčíková D, Eilers AC, Simcoe RA, et al. An extremely metal-poor Lyα emitter
candidate at z = 6 revealed through absorption spectroscopy. The Astrophysical
Journal Letters. 2025;987(2). doi:10.3847/2041-8213/ade71c
apa: Ďurovčíková, D., Eilers, A. C., Simcoe, R. A., Welsh, L., Meyer, R. A., Matthee,
J. J., … Farina, E. P. (2025). An extremely metal-poor Lyα emitter candidate at
z = 6 revealed through absorption spectroscopy. The Astrophysical Journal Letters.
IOP Publishing. https://doi.org/10.3847/2041-8213/ade71c
chicago: Ďurovčíková, Dominika, Anna Christina Eilers, Robert A. Simcoe, Louise
Welsh, Romain A. Meyer, Jorryt J Matthee, Emma V. Ryan-Weber, et al. “An Extremely
Metal-Poor Lyα Emitter Candidate at z = 6 Revealed through Absorption Spectroscopy.”
The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ade71c.
ieee: D. Ďurovčíková et al., “An extremely metal-poor Lyα emitter candidate
at z = 6 revealed through absorption spectroscopy,” The Astrophysical Journal
Letters, vol. 987, no. 2. IOP Publishing, 2025.
ista: Ďurovčíková D, Eilers AC, Simcoe RA, Welsh L, Meyer RA, Matthee JJ, Ryan-Weber
EV, Yue M, Katz H, Satyavolu S, Becker G, Davies FB, Farina EP. 2025. An extremely
metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy.
The Astrophysical Journal Letters. 987(2), L33.
mla: Ďurovčíková, Dominika, et al. “An Extremely Metal-Poor Lyα Emitter Candidate
at z = 6 Revealed through Absorption Spectroscopy.” The Astrophysical Journal
Letters, vol. 987, no. 2, L33, IOP Publishing, 2025, doi:10.3847/2041-8213/ade71c.
short: D. Ďurovčíková, A.C. Eilers, R.A. Simcoe, L. Welsh, R.A. Meyer, J.J. Matthee,
E.V. Ryan-Weber, M. Yue, H. Katz, S. Satyavolu, G. Becker, F.B. Davies, E.P. Farina,
The Astrophysical Journal Letters 987 (2025).
date_created: 2025-07-20T22:02:01Z
date_published: 2025-07-10T00:00:00Z
date_updated: 2026-02-16T12:44:23Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ade71c
external_id:
arxiv:
- '2505.01499'
isi:
- '001524847100001'
file:
- access_level: open_access
checksum: 75d0c08514209fc6e3078fdec8e815a2
content_type: application/pdf
creator: dernst
date_created: 2025-07-22T08:38:14Z
date_updated: 2025-07-22T08:38:14Z
file_id: '20066'
file_name: 2025_AstrophysicalJourLetters_Durovcikova.pdf
file_size: 6453728
relation: main_file
success: 1
file_date_updated: 2025-07-22T08:38:14Z
has_accepted_license: '1'
intvolume: ' 987'
isi: 1
issue: '2'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption
spectroscopy
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 987
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '20425'
abstract:
- lang: eng
text: Ultraviolet (UV) radiation from accreting black holes ionizes the intergalactic
gas around early quasars, carving out highly ionized bubbles in their surroundings.
Any changes in a quasar’s luminosity are therefore predicted to produce outward-propagating
ionization gradients, affecting the Lyα absorption opacity near the quasar’s systemic
redshift. This “proximity effect” is well-documented in rest-UV quasar spectra
but only provides a one-dimensional probe along our line of sight. Here we present
deep spectroscopic observations with the James Webb Space Telescope (JWST) of
galaxies in the background of a superluminous quasar at zQSO ≈ 6.3, which reveal
the quasar’s “light echo” with Lyα tomography in the transverse direction. This
transverse proximity effect is detected for the first time toward multiple galaxy
sightlines, allowing us to map the extent and geometry of the quasar’s ionization
cone. We obtain constraints on the orientation and inclination of the cone, as
well as an upper limit on the obscured solid angle fraction of fobsc < 91%. Additionally,
we find a timescale of the quasar’s UV radiation of tqso = 10^5.6+0.1-0.3 yr,
which is significantly shorter than would be required to build up the central
supermassive black hole (SMBH) with conventional growth models, but is consistent
with independent measurements of the quasars’ duty cycle. Our inferred obscured
fraction disfavors a scenario where short quasar lifetimes can be explained exclusively
by geometric obscuration, and instead supports the idea that radiatively inefficient
accretion or growth in initially heavily enshrouded cocoons plays a pivotal role
in early SMBH growth. Our results pave the way for novel studies of quasars’ ionizing
geometries and radiative histories at early cosmic times.
acknowledgement: "This work is based on observations made with the NASA/ESA/CSA James
Webb Space Telescope. The data were obtained from the Mikulski Archive for Space
Telescopes at the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127
for JWST. These observations are associated with programs #1243 and #4713.\r\n\r\nAll
of the data presented in this Letter 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/w7hm-qb39.\r\nJ.M. is supported by the
European Union (ERC, AGENTS, 101076224)."
article_number: L40
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Minghao
full_name: Yue, Minghao
last_name: Yue
- 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: Joseph F.
full_name: Hennawi, Joseph F.
last_name: Hennawi
- first_name: Frederick B.
full_name: Davies, Frederick B.
last_name: Davies
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Richard
full_name: Teague, Richard
last_name: Teague
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Yi
full_name: Kang, Yi
last_name: Kang
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- 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
citation:
ama: Eilers AC, Yue M, Matthee JJ, et al. The light echo of a high-redshift quasar
mapped with Lyα tomography. The Astrophysical Journal Letters. 2025;991(2).
doi:10.3847/2041-8213/ae057a
apa: Eilers, A. C., Yue, M., Matthee, J. J., Hennawi, J. F., Davies, F. B., Simcoe,
R. A., … Navarrete, B. (2025). The light echo of a high-redshift quasar mapped
with Lyα tomography. The Astrophysical Journal Letters. IOP Publishing.
https://doi.org/10.3847/2041-8213/ae057a
chicago: Eilers, Anna Christina, Minghao Yue, Jorryt J Matthee, Joseph F. Hennawi,
Frederick B. Davies, Robert A. Simcoe, Richard Teague, et al. “The Light Echo
of a High-Redshift Quasar Mapped with Lyα Tomography.” The Astrophysical Journal
Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ae057a.
ieee: A. C. Eilers et al., “The light echo of a high-redshift quasar mapped
with Lyα tomography,” The Astrophysical Journal Letters, vol. 991, no.
2. IOP Publishing, 2025.
ista: Eilers AC, Yue M, Matthee JJ, Hennawi JF, Davies FB, Simcoe RA, Teague R,
Bordoloi R, Brammer G, Kang Y, Kashino D, Mackenzie R, Naidu RP, Navarrete B.
2025. The light echo of a high-redshift quasar mapped with Lyα tomography. The
Astrophysical Journal Letters. 991(2), L40.
mla: Eilers, Anna Christina, et al. “The Light Echo of a High-Redshift Quasar Mapped
with Lyα Tomography.” The Astrophysical Journal Letters, vol. 991, no.
2, L40, IOP Publishing, 2025, doi:10.3847/2041-8213/ae057a.
short: A.C. Eilers, M. Yue, J.J. Matthee, J.F. Hennawi, F.B. Davies, R.A. Simcoe,
R. Teague, R. Bordoloi, G. Brammer, Y. Kang, D. Kashino, R. Mackenzie, R.P. Naidu,
B. Navarrete, The Astrophysical Journal Letters 991 (2025).
date_created: 2025-10-05T22:01:35Z
date_published: 2025-09-25T00:00:00Z
date_updated: 2026-02-16T12:44:42Z
day: '25'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.3847/2041-8213/ae057a
external_id:
arxiv:
- '2509.05417'
isi:
- '001581023000001'
file:
- access_level: open_access
checksum: 3cb8099b9a915755164e5675b33f8a03
content_type: application/pdf
creator: dernst
date_created: 2025-10-13T09:25:12Z
date_updated: 2025-10-13T09:25:12Z
file_id: '20461'
file_name: 2025_AstrophysicalJour_Eilers.pdf
file_size: 23585591
relation: main_file
success: 1
file_date_updated: 2025-10-13T09:25:12Z
has_accepted_license: '1'
intvolume: ' 991'
isi: 1
issue: '2'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: The light echo of a high-redshift quasar mapped with Lyα tomography
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: 991
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '20493'
abstract:
- lang: eng
text: 'We propose a formation pathway linking black holes (BHs) observed in gravitational-wave
(GW) mergers, wide BH–stellar systems uncovered by Gaia, and accreting low-mass
X-ray binaries (LMXBs). In this scenario, a stellar-mass BH binary undergoes isolated
binary evolution and merges while hosting a distant, dynamically unimportant tertiary
stellar companion. The tertiary becomes relevant only after the merger, when the
remnant BH receives a GW recoil kick. Depending on the kick velocity and system
configuration, the outcome can be: (1) a bright electromagnetic (EM) counterpart
to the GW merger; (2) an LMXB; (3) a wide BH–stellar companion system resembling
the Gaia BH population; or (4) an unbound isolated BH. Modeling the three-body
dynamics, we find that ∼0.02% of LIGO–Virgo–KAGRA (LVK) mergers may be followed
by an EM counterpart within ∼10 days, produced by tidal disruption of the star
by the BH. The flare is likely brightest in the optical–UV and lasts for days
to weeks; in some cases, partial disruption causes recurring flares with a period
of ∼2 months. We further estimate that this channel can produce ∼1%–10% of Gaia
BH systems in the Milky Way. This scenario provides the first physically motivated
link between GW sources, Gaia BHs, and some X-ray binaries, and predicts a rare
but robust pathway for EM counterparts to binary BH mergers, potentially detectable
in LVK’s O5 run.'
acknowledgement: We thank the anonymous referee for the useful and detailed report.
S.N. acknowledges the partial support of NSF-BSF grant AST-2206428 and NASA XRP
grant 80NSSC23K0262, as well as Howard and Astrid Preston for their generous support.
Z.H. acknowledges support from NASA grants 80NSSC22K0822 and 80NSSC24K0440. E.Q.
thanks the Gordon and Betty Moore Foundation for support through grant GBMF5076.
article_number: L12
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Smadar
full_name: Naoz, Smadar
last_name: Naoz
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
- first_name: Eliot
full_name: Quataert, Eliot
last_name: Quataert
- first_name: Liz
full_name: Holzknecht, Liz
last_name: Holzknecht
citation:
ama: Naoz S, Haiman Z, Quataert E, Holzknecht L. Triples as links between binary
Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes.
The Astrophysical Journal Letters. 2025;992(1). doi:10.3847/2041-8213/ae0a20
apa: Naoz, S., Haiman, Z., Quataert, E., & Holzknecht, L. (2025). Triples as
links between binary Black Hole mergers, their electromagnetic counterparts, and
galactic Black Holes. The Astrophysical Journal Letters. IOP Publishing.
https://doi.org/10.3847/2041-8213/ae0a20
chicago: Naoz, Smadar, Zoltán Haiman, Eliot Quataert, and Liz Holzknecht. “Triples
as Links between Binary Black Hole Mergers, Their Electromagnetic Counterparts,
and Galactic Black Holes.” The Astrophysical Journal Letters. IOP Publishing,
2025. https://doi.org/10.3847/2041-8213/ae0a20.
ieee: S. Naoz, Z. Haiman, E. Quataert, and L. Holzknecht, “Triples as links between
binary Black Hole mergers, their electromagnetic counterparts, and galactic Black
Holes,” The Astrophysical Journal Letters, vol. 992, no. 1. IOP Publishing,
2025.
ista: Naoz S, Haiman Z, Quataert E, Holzknecht L. 2025. Triples as links between
binary Black Hole mergers, their electromagnetic counterparts, and galactic Black
Holes. The Astrophysical Journal Letters. 992(1), L12.
mla: Naoz, Smadar, et al. “Triples as Links between Binary Black Hole Mergers, Their
Electromagnetic Counterparts, and Galactic Black Holes.” The Astrophysical
Journal Letters, vol. 992, no. 1, L12, IOP Publishing, 2025, doi:10.3847/2041-8213/ae0a20.
short: S. Naoz, Z. Haiman, E. Quataert, L. Holzknecht, The Astrophysical Journal
Letters 992 (2025).
date_created: 2025-10-19T22:01:31Z
date_published: 2025-10-10T00:00:00Z
date_updated: 2026-02-16T12:44:56Z
day: '10'
ddc:
- '520'
department:
- _id: ZoHa
doi: 10.3847/2041-8213/ae0a20
external_id:
arxiv:
- '2508.13270'
isi:
- '001589455900001'
file:
- access_level: open_access
checksum: cb81d666f6d7638a5bcf45653d25bcb3
content_type: application/pdf
creator: dernst
date_created: 2025-10-23T09:09:30Z
date_updated: 2025-10-23T09:09:30Z
file_id: '20520'
file_name: 2025_AstrophysicalJour_Naoz.pdf
file_size: 8787316
relation: main_file
success: 1
file_date_updated: 2025-10-23T09:09:30Z
has_accepted_license: '1'
intvolume: ' 992'
isi: 1
issue: '1'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Triples as links between binary Black Hole mergers, their electromagnetic counterparts,
and galactic Black Holes
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: 992
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '20649'
abstract:
- lang: eng
text: Ionized proximity zones around luminous quasars provide a unique laboratory
to characterize the Lyα emission lines from z > 6 galaxies without significant
attenuation from the intergalactic medium (IGM). However, Lyα line measurements
for galaxies within high-redshift quasars’ proximity zones have been rare so far.
Here we present deep spectroscopic observations obtained with the NIRSpec/Micro-Shutter
Assembly (MSA) instrument on the James Webb Space Telescope of galaxies in two
z > 6 quasar fields. We measure the Lyα line fluxes for 50 galaxies at 6 < z <
7 with UV absolute magnitude M UV < −19 (median M UV = −19.97), among which 15
are located near the luminous quasars, i.e., within Δv < 2500 km s−1. We find
that galaxies near the quasars show significant flux blueward of the systemic
Lyα wavelength, and have higher Lyα equivalent width compared to galaxies at similar
redshifts that are not located within the quasars’ environment. Our result indicates
little or no redshift evolution for the Lyα emitter fraction from z ∼ 6.4 to z
∼ 5. Leveraging the low IGM opacity in the quasars’ vicinity, we evaluate the
Lyα escape fraction (f esc Ly α) of high-redshift galaxies. Our analysis suggests
that galaxies at 〈z〉 ≈ 6.4 have an average f esc Ly α = 0.14 ± 0.04. This value
is consistent with reionization models where the Lyman continuum escape fraction
is low ( fescLyC ≲ 0.1 ) for luminous galaxies, and where the most luminous galaxies
have only a minor contribution to the total ionizing photon budget. © 2025. The
Author(s). Published by the American Astronomical Society.
acknowledgement: "We thank the referee for valuable comments. This work is based on
observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were
obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science
Institute, which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are
associated with program ID #3117 and #4713. Support for\r\nthis work was provided
by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by
the Space Telescope Science Institute, which is operated by the\r\nAssociation of
Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555."
article_number: L12
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Minghao
full_name: Yue, Minghao
last_name: Yue
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Frederick B.
full_name: Davies, Frederick B.
last_name: Davies
- first_name: Joseph F.
full_name: Hennawi, Joseph F.
last_name: Hennawi
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
citation:
ama: Yue M, Eilers AC, Matthee JJ, et al. Escape fractions from unattenuated Lyα
emitters around luminous z > 6 quasars. The Astrophysical Journal Letters.
2025;993(1). doi:10.3847/2041-8213/ae0e0e
apa: Yue, M., Eilers, A. C., Matthee, J. J., Naidu, R. P., Bordoloi, R., Davies,
F. B., … Simcoe, R. A. (2025). Escape fractions from unattenuated Lyα emitters
around luminous z > 6 quasars. The Astrophysical Journal Letters. IOP
Publishing. https://doi.org/10.3847/2041-8213/ae0e0e
chicago: Yue, Minghao, Anna Christina Eilers, Jorryt J Matthee, Rohan P. Naidu,
Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari
Mackenzie, and Robert A. Simcoe. “Escape Fractions from Unattenuated Lyα Emitters
around Luminous z > 6 Quasars.” The Astrophysical Journal Letters.
IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ae0e0e.
ieee: M. Yue et al., “Escape fractions from unattenuated Lyα emitters around
luminous z > 6 quasars,” The Astrophysical Journal Letters, vol. 993,
no. 1. IOP Publishing, 2025.
ista: Yue M, Eilers AC, Matthee JJ, Naidu RP, Bordoloi R, Davies FB, Hennawi JF,
Kashino D, Mackenzie R, Simcoe RA. 2025. Escape fractions from unattenuated Lyα
emitters around luminous z > 6 quasars. The Astrophysical Journal Letters.
993(1), L12.
mla: Yue, Minghao, et al. “Escape Fractions from Unattenuated Lyα Emitters around
Luminous z > 6 Quasars.” The Astrophysical Journal Letters, vol. 993,
no. 1, L12, IOP Publishing, 2025, doi:10.3847/2041-8213/ae0e0e.
short: M. Yue, A.C. Eilers, J.J. Matthee, R.P. Naidu, R. Bordoloi, F.B. Davies,
J.F. Hennawi, D. Kashino, R. Mackenzie, R.A. Simcoe, The Astrophysical Journal
Letters 993 (2025).
date_created: 2025-11-16T23:01:24Z
date_published: 2025-11-01T00:00:00Z
date_updated: 2026-02-16T12:45:16Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ae0e0e
external_id:
arxiv:
- '2507.05381'
isi:
- '001600890100001'
file:
- access_level: open_access
checksum: 11d35c1c52c000f8c14bc6de2e9f4b3f
content_type: application/pdf
creator: dernst
date_created: 2025-11-24T13:18:34Z
date_updated: 2025-11-24T13:18:34Z
file_id: '20680'
file_name: 2025_AstrophysicalJour_Yue.pdf
file_size: 39736710
relation: main_file
success: 1
file_date_updated: 2025-11-24T13:18:34Z
has_accepted_license: '1'
intvolume: ' 993'
isi: 1
issue: '1'
language:
- iso: eng
month: '11'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars
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: 993
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '18760'
abstract:
- lang: eng
text: With the remarkable sensitivity and resolution of JWST in the infrared, measuring
rest-optical kinematics of galaxies at z > 5 has become possible for the first
time. This study pilots a new method for measuring galaxy dynamics for highly
multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and
JADES medium-band imaging. Here we present one of the first JWST kinematic measurements
for a galaxy at z > 5. We find a significant velocity gradient, which, if interpreted
as rotation, yields Vrot = 305 ± 70 km s−1, and we hence refer to this galaxy
as Twister-z5. With a rest-frame optical effective radius of re = 2.25 kpc, the
high rotation velocity in this galaxy is not due to a compact size, as may be
expected in the early Universe, but rather to a high total mass, (math formula).
This is a factor of roughly 10× higher than the stellar mass within re. We also
observe that the radial Hα equivalent width profile and the specific star formation
rate map from resolved stellar population modeling are centrally depressed by
a factor of ∼1.5 from the center to re. Combined with the morphology of the line-emitting
gas in comparison to the continuum, this centrally suppressed star formation is
consistent with a star-forming disk surrounding a bulge growing inside out. While
large, rapidly rotating disks are common to z ∼ 2, the existence of one after
only 1 Gyr of cosmic time, shown for the first time in ionized gas, adds to the
growing evidence that some galaxies matured earlier than expected in the history
of the Universe.
acknowledgement: We thank the reviewer and editorial staff for their excellent feedback
and effort—the manuscript is much stronger as a result. Support for this work was
provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-26555. H.Ü. gratefully acknowledges support
by the Isaac Newton Trust and by the Kavli Foundation through a Newton-Kavli Junior
Fellowship. This work has received funding from the Swiss State Secretariat for
Education, Research and Innovation (SERI) under contract No. MB22.00072, as well
as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.
The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation
under grant No. 140. R.S. acknowledges an STFC Ernest Rutherford Fellowship (ST/S004831/1).
R.P.N. acknowledges support for this work provided by NASA through the NASA Hubble
Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. M.V.M. acknowledges support from the National
Science Foundation via AAG grant 2205519 and the Wisconsin Alumni Research Foundation
via grant MSN251397. R.M. also acknowledges funding from a research professorship
from the Royal Society. A.J.B., A.J.C., and G.C.J. acknowledge funding from the
"FirstGalaxies" Advanced Grant from the European Research Council (ERC) under the
European Union's Horizon 2020 research and innovation program (grant agreement No.
789056). I.L. acknowledges support by the Australian Research Council through Future
Fellowship FT220100798. D.J.E. is supported as a Simons Investigator and by a JWST/NIRCam
contract to the University of Arizona, NAS5-02015. R.M., J.W., L.S., and W.B. acknowledge
support by the Science and Technology Facilities Council (STFC), the ERC through
advanced grant 695671 "QUENCH," and the UKRI Frontier Research grant RISEandFALL.
B.E.R. acknowledges support from the NIRCam Science Team contract to the University
of Arizona, NAS5-02015. The research of C.C.W. is supported by NOIRLab, which is
managed by the Association of Universities for Research in Astronomy (AURA) under
a cooperative agreement with the National Science Foundation. The HST and JWST image
mosaics of the FRESCO fields are released at MAST as a High Level Science Product
(P. Oesch & D. Magee 2023).
article_number: L27
article_processing_charge: Yes
article_type: letter_note
arxiv: 1
author:
- first_name: Erica
full_name: Nelson, Erica
last_name: Nelson
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Clara
full_name: Giménez-Arteaga, Clara
last_name: Giménez-Arteaga
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Hannah
full_name: Übler, Hannah
last_name: Übler
- first_name: Jasleen
full_name: Matharu, Jasleen
last_name: Matharu
- first_name: Alice E.
full_name: Shapley, Alice E.
last_name: Shapley
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Emily
full_name: Wisnioski, Emily
last_name: Wisnioski
- first_name: Natascha M.
full_name: Förster Schreiber, Natascha M.
last_name: Förster Schreiber
- first_name: Renske
full_name: Smit, Renske
last_name: Smit
- first_name: Pieter
full_name: Van Dokkum, Pieter
last_name: Van Dokkum
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Ryan
full_name: Endsley, Ryan
last_name: Endsley
- first_name: Abigail I.
full_name: Hartley, Abigail I.
last_name: Hartley
- first_name: Justus
full_name: Gibson, Justus
last_name: Gibson
- first_name: Emma
full_name: Giovinazzo, Emma
last_name: Giovinazzo
- first_name: Garth
full_name: Illingworth, Garth
last_name: Illingworth
- first_name: Ivo
full_name: Labbe, Ivo
last_name: Labbe
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Alba
full_name: Covelo Paz, Alba
last_name: Covelo Paz
- first_name: Sedona H.
full_name: Price, Sedona H.
last_name: Price
- first_name: Naveen A.
full_name: Reddy, Naveen A.
last_name: Reddy
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
- first_name: Mengyuan
full_name: Xiao, Mengyuan
last_name: Xiao
- first_name: Stacey
full_name: Alberts, Stacey
last_name: Alberts
- first_name: William M.
full_name: Baker, William M.
last_name: Baker
- first_name: Andrew J.
full_name: Bunker, Andrew J.
last_name: Bunker
- first_name: Alex J.
full_name: Cameron, Alex J.
last_name: Cameron
- first_name: Stephane
full_name: Charlot, Stephane
last_name: Charlot
- first_name: Daniel J.
full_name: Eisenstein, Daniel J.
last_name: Eisenstein
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Zhiyuan
full_name: Ji, Zhiyuan
last_name: Ji
- first_name: Benjamin D.
full_name: Johnson, Benjamin D.
last_name: Johnson
- first_name: Gareth C.
full_name: Jones, Gareth C.
last_name: Jones
- first_name: Roberto
full_name: Maiolino, Roberto
last_name: Maiolino
- first_name: Brant
full_name: Robertson, Brant
last_name: Robertson
- first_name: Lester
full_name: Sandles, Lester
last_name: Sandles
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
- first_name: Joris
full_name: Witstok, Joris
last_name: Witstok
citation:
ama: 'Nelson E, Brammer G, Giménez-Arteaga C, et al. Ionized gas kinematics with
FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. Astrophysical
Journal Letters. 2024;976(2). doi:10.3847/2041-8213/ad7b17'
apa: 'Nelson, E., Brammer, G., Giménez-Arteaga, C., Oesch, P. A., Naidu, R. P.,
Übler, H., … Witstok, J. (2024). Ionized gas kinematics with FRESCO: An extended,
massive, rapidly rotating galaxy at z = 5.4. Astrophysical Journal Letters.
IOP Publishing. https://doi.org/10.3847/2041-8213/ad7b17'
chicago: 'Nelson, Erica, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch,
Rohan P. Naidu, Hannah Übler, Jasleen Matharu, et al. “Ionized Gas Kinematics
with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4.” Astrophysical
Journal Letters. IOP Publishing, 2024. https://doi.org/10.3847/2041-8213/ad7b17.'
ieee: 'E. Nelson et al., “Ionized gas kinematics with FRESCO: An extended,
massive, rapidly rotating galaxy at z = 5.4,” Astrophysical Journal Letters,
vol. 976, no. 2. IOP Publishing, 2024.'
ista: 'Nelson E, Brammer G, Giménez-Arteaga C, Oesch PA, Naidu RP, Übler H, Matharu
J, Shapley AE, Whitaker KE, Wisnioski E, Förster Schreiber NM, Smit R, Van Dokkum
P, Chisholm J, Endsley R, Hartley AI, Gibson J, Giovinazzo E, Illingworth G, Labbe
I, Maseda MV, Matthee JJ, Covelo Paz A, Price SH, Reddy NA, Shivaei I, Weibel
A, Wuyts S, Xiao M, Alberts S, Baker WM, Bunker AJ, Cameron AJ, Charlot S, Eisenstein
DJ, De Graaff A, Ji Z, Johnson BD, Jones GC, Maiolino R, Robertson B, Sandles
L, Suess KA, Tacchella S, Williams CC, Witstok J. 2024. Ionized gas kinematics
with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. Astrophysical
Journal Letters. 976(2), L27.'
mla: 'Nelson, Erica, et al. “Ionized Gas Kinematics with FRESCO: An Extended, Massive,
Rapidly Rotating Galaxy at z = 5.4.” Astrophysical Journal Letters, vol.
976, no. 2, L27, IOP Publishing, 2024, doi:10.3847/2041-8213/ad7b17.'
short: E. Nelson, G. Brammer, C. Giménez-Arteaga, P.A. Oesch, R.P. Naidu, H. Übler,
J. Matharu, A.E. Shapley, K.E. Whitaker, E. Wisnioski, N.M. Förster Schreiber,
R. Smit, P. Van Dokkum, J. Chisholm, R. Endsley, A.I. Hartley, J. Gibson, E. Giovinazzo,
G. Illingworth, I. Labbe, M.V. Maseda, J.J. Matthee, A. Covelo Paz, S.H. Price,
N.A. Reddy, I. Shivaei, A. Weibel, S. Wuyts, M. Xiao, S. Alberts, W.M. Baker,
A.J. Bunker, A.J. Cameron, S. Charlot, D.J. Eisenstein, A. De Graaff, Z. Ji, B.D.
Johnson, G.C. Jones, R. Maiolino, B. Robertson, L. Sandles, K.A. Suess, S. Tacchella,
C.C. Williams, J. Witstok, Astrophysical Journal Letters 976 (2024).
date_created: 2025-01-05T23:01:58Z
date_published: 2024-12-01T00:00:00Z
date_updated: 2025-09-09T11:58:02Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ad7b17
external_id:
arxiv:
- '2310.06887'
isi:
- '001364636000001'
file:
- access_level: open_access
checksum: 5c7320196586b4340e55f215d8737185
content_type: application/pdf
creator: dernst
date_created: 2025-01-08T08:18:39Z
date_updated: 2025-01-08T08:18:39Z
file_id: '18771'
file_name: 2024_AstrophysicalJour_Nelson.pdf
file_size: 1822989
relation: main_file
success: 1
file_date_updated: 2025-01-08T08:18:39Z
has_accepted_license: '1'
intvolume: ' 976'
isi: 1
issue: '2'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating
galaxy at z = 5.4'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 976
year: '2024'
...
---
DOAJ_listed: '1'
_id: '17234'
abstract:
- lang: eng
text: The identification of red, apparently massive galaxies at z > 7 in early James
Webb Space Telescope (JWST) photometry suggests a strongly accelerated time line
compared to standard models of galaxy growth. A major uncertainty in the interpretation
is whether the red colors are caused by evolved stellar populations, dust, or
other effects such as emission lines or active galactic nuclei (AGNs). Here we
show that three of the massive galaxy candidates at z = 6.7–8.4 have prominent
Balmer breaks in JWST/NIRSpec spectroscopy from the RUBIES program. The Balmer
breaks demonstrate unambiguously that stellar emission dominates at λrest = 0.4
μm and require formation histories extending hundreds of millions of years into
the past in galaxies only 600–800 Myr after the big bang. Two of the three galaxies
also show broad Balmer lines, with Hβ FWHM > 2500 km s−1, suggesting that dust-reddened
AGNs contribute to, or even dominate, the spectral energy distributions of these
galaxies at λrest ≳ 0.6 μm. All three galaxies have relatively narrow [O iii]
lines, seemingly ruling out a high-mass interpretation if the lines arise in dynamically
relaxed, inclined disks. Yet the inferred masses also remain highly uncertain.
We model the high-quality spectra using Prospector to decompose the continuum
into stellar and AGN components and explore limiting cases in stellar/AGN contribution.
This produces a wide range of possible stellar masses, spanning M⋆ ∼ 109−1011M⊙.
Nevertheless, all fits suggest a very early and rapid formation, most of which
follow with a truncation in star formation. Potential origins and evolutionary
tracks for these objects are discussed, from the cores of massive galaxies to
low-mass galaxies with overmassive black holes. Intriguingly, we find all of these
explanations to be incomplete; deeper and redder data are needed to understand
the physics of these systems.
acknowledgement: "We thank the anonymous referee for the helpful comments. B.W. and
J.L. acknowledge support from JWST-GO04233.009-A. The Cosmic Dawn Center is funded
by the Danish National Research Foundation (DNRF) under grant No. 140. This research
was supported by the International Space Science Institute (ISSI) in Bern, through
ISSI International Team project No. 562 (First Light at Cosmic Dawn: Exploiting
the James Webb Space Telescope Revolution). 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. The JWST data presented in this
Letter 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:10.17909/3a4n-9p88. Computations for this research were performed on the
Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar
supercomputer. This publication made use of the NASA Astrophysical Data System for
bibliographic information. \r\nFacilities: HST (ACS, WFC3), JWST (NIRCam, NIRSpec).
Software: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), dynesty (Speagle
2020), EAzY (Brammer et al. 2008),\r\nemcee (Foreman-Mackey et al. 2013), Matplotlib
(Hunter 2007), msaexp (Brammer 2023b), msafit (de Graaff et al. 2024a), NumPy (Harris
et al. 2020), Prospector (Johnson et al. 2021), Python-FSPS (Johnson et al. 2023)."
article_number: L13
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Pieter
full_name: Van Dokkum, Pieter
last_name: Van Dokkum
- first_name: Josephine F.W.
full_name: Baggen, Josephine F.W.
last_name: Baggen
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Ian
full_name: Mcconachie, Ian
last_name: Mcconachie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Erica
full_name: Nelson, Erica
last_name: Nelson
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: 'Wang B, Leja J, De Graaff A, et al. RUBIES: Evolved stellar populations with
extended formation histories at z ∼ 7-8 in candidate massive galaxies identified
with JWST/NIRSpec. Astrophysical Journal Letters. 2024;969(1). doi:10.3847/2041-8213/ad55f7'
apa: 'Wang, B., Leja, J., De Graaff, A., Brammer, G. B., Weibel, A., Van Dokkum,
P., … Williams, C. C. (2024). RUBIES: Evolved stellar populations with extended
formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec.
Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ad55f7'
chicago: 'Wang, Bingjie, Joel Leja, Anna De Graaff, Gabriel B. Brammer, Andrea Weibel,
Pieter Van Dokkum, Josephine F.W. Baggen, et al. “RUBIES: Evolved Stellar Populations
with Extended Formation Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified
with JWST/NIRSpec.” Astrophysical Journal Letters. IOP Publishing, 2024.
https://doi.org/10.3847/2041-8213/ad55f7.'
ieee: 'B. Wang et al., “RUBIES: Evolved stellar populations with extended
formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec,”
Astrophysical Journal Letters, vol. 969, no. 1. IOP Publishing, 2024.'
ista: 'Wang B, Leja J, De Graaff A, Brammer GB, Weibel A, Van Dokkum P, Baggen JFW,
Suess KA, Greene JE, Bezanson R, Cleri NJ, Hirschmann M, Labbé I, Matthee JJ,
Mcconachie I, Naidu RP, Nelson E, Oesch PA, Setton DJ, Williams CC. 2024. RUBIES:
Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate
massive galaxies identified with JWST/NIRSpec. Astrophysical Journal Letters.
969(1), L13.'
mla: 'Wang, Bingjie, et al. “RUBIES: Evolved Stellar Populations with Extended Formation
Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified with JWST/NIRSpec.”
Astrophysical Journal Letters, vol. 969, no. 1, L13, IOP Publishing, 2024,
doi:10.3847/2041-8213/ad55f7.'
short: B. Wang, J. Leja, A. De Graaff, G.B. Brammer, A. Weibel, P. Van Dokkum, J.F.W.
Baggen, K.A. Suess, J.E. Greene, R. Bezanson, N.J. Cleri, M. Hirschmann, I. Labbé,
J.J. Matthee, I. Mcconachie, R.P. Naidu, E. Nelson, P.A. Oesch, D.J. Setton, C.C.
Williams, Astrophysical Journal Letters 969 (2024).
date_created: 2024-07-14T22:01:11Z
date_published: 2024-07-01T00:00:00Z
date_updated: 2025-09-08T08:10:21Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/2041-8213/ad55f7
external_id:
arxiv:
- '2405.01473'
isi:
- '001257903200001'
file:
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checksum: bb1a6725586df12e745d091b5778bb2b
content_type: application/pdf
creator: dernst
date_created: 2024-07-16T06:24:29Z
date_updated: 2024-07-16T06:24:29Z
file_id: '17243'
file_name: 2024_AstrophysicalJourn_Wang.pdf
file_size: 3273303
relation: main_file
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file_date_updated: 2024-07-16T06:24:29Z
has_accepted_license: '1'
intvolume: ' 969'
isi: 1
issue: '1'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'RUBIES: Evolved stellar populations with extended formation histories at z
∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 969
year: '2024'
...
---
DOAJ_listed: '1'
_id: '18111'
abstract:
- lang: eng
text: Observations of tidal disruption events (TDEs) show signs of nitrogen enrichment
reminiscent of other astrophysical sources such as active galactic nuclei and
star-forming galaxies. Given that TDEs probe the gas from a single star, it is
possible to test whether the observed enrichment is consistent with expectations
from the CNO cycle by looking at the observed nitrogen/carbon (N/C) abundance
ratios. Given that ≈20% of solar-mass stars (and an even larger fraction of more
massive stars) live in close binaries, it is worthwhile to also consider what
TDEs from stars influenced by binary evolution would look like. We show here that
TDEs from stars stripped of their hydrogen-rich (and nitrogen-poor) envelopes
through previous binary-induced mass loss can produce much higher observable N/C
enhancements than even TDEs from massive stars. Additionally, we predict that
the time dependence of the N/C abundance ratio in the mass fallback rate of stripped
stars will follow the inverse behavior of main-sequence stars, enabling a more
accurate characterization of the disrupted star.
acknowledgement: "This work was performed in part at Aspen Center for Physics, which
is supported by National Science Foundation grant PHY-2210452. We thank the participants
and organizers of the summer Aspen 2023 workshop on “Stellar Interactions and the
Transients They Cause” for fruitful discussions. B.M. is grateful for support from
the Carnegie Theoretical Astrophysics\r\nCenter. M.G.-G. is grateful for the support
from Northwestern University’s Presidential Fellowship. E.R.-R. thanks the Heising-Simons
Foundation, NSF (AST-2150255 and AST2307710), Swift (80NSSC21K1409, 80NSSC19K1391),
and Chandra (22-0142) for support. "
article_number: L9
article_processing_charge: Yes
article_type: original
author:
- first_name: Brenna
full_name: Mockler, Brenna
last_name: Mockler
- first_name: Monica
full_name: Gallegos-Garcia, Monica
last_name: Gallegos-Garcia
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Jon M.
full_name: Miller, Jon M.
last_name: Miller
- first_name: Enrico
full_name: Ramirez-Ruiz, Enrico
last_name: Ramirez-Ruiz
citation:
ama: Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. Tidal
disruption events from stripped stars. Astrophysical Journal Letters. 2024;973(1).
doi:10.3847/2041-8213/ad6c34
apa: Mockler, B., Gallegos-Garcia, M., Götberg, Y. L. L., Miller, J. M., & Ramirez-Ruiz,
E. (2024). Tidal disruption events from stripped stars. Astrophysical Journal
Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ad6c34
chicago: Mockler, Brenna, Monica Gallegos-Garcia, Ylva Louise Linsdotter Götberg,
Jon M. Miller, and Enrico Ramirez-Ruiz. “Tidal Disruption Events from Stripped
Stars.” Astrophysical Journal Letters. IOP Publishing, 2024. https://doi.org/10.3847/2041-8213/ad6c34.
ieee: B. Mockler, M. Gallegos-Garcia, Y. L. L. Götberg, J. M. Miller, and E. Ramirez-Ruiz,
“Tidal disruption events from stripped stars,” Astrophysical Journal Letters,
vol. 973, no. 1. IOP Publishing, 2024.
ista: Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. 2024.
Tidal disruption events from stripped stars. Astrophysical Journal Letters. 973(1),
L9.
mla: Mockler, Brenna, et al. “Tidal Disruption Events from Stripped Stars.” Astrophysical
Journal Letters, vol. 973, no. 1, L9, IOP Publishing, 2024, doi:10.3847/2041-8213/ad6c34.
short: B. Mockler, M. Gallegos-Garcia, Y.L.L. Götberg, J.M. Miller, E. Ramirez-Ruiz,
Astrophysical Journal Letters 973 (2024).
date_created: 2024-09-22T22:01:42Z
date_published: 2024-09-12T00:00:00Z
date_updated: 2025-09-08T09:48:50Z
day: '12'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.3847/2041-8213/ad6c34
external_id:
isi:
- '001310592900001'
file:
- access_level: open_access
checksum: 050ddf873244839825714cca42b5d857
content_type: application/pdf
creator: dernst
date_created: 2024-09-30T08:54:26Z
date_updated: 2024-09-30T08:54:26Z
file_id: '18161'
file_name: 2024_AstrophysicalJourn_Mockler.pdf
file_size: 844227
relation: main_file
success: 1
file_date_updated: 2024-09-30T08:54:26Z
has_accepted_license: '1'
intvolume: ' 973'
isi: 1
issue: '1'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Tidal disruption events from stripped stars
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 973
year: '2024'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '18306'
abstract:
- lang: eng
text: Neutral sodium (Na i) is an alkali metal with a favorable absorption cross
section such that tenuous gases are easily illuminated at select transiting exoplanet
systems. We examine both the time-averaged and time-series alkali spectral flux
individually, over 4 nights at a hot Saturn system on a ∼2.8 day orbit about a
Sun-like star WASP-49 A. Very Large Telescope/ESPRESSO observations are analyzed,
providing new constraints. We recover the previously confirmed residual sodium
flux uniquely when averaged, whereas night-to-night Na i varies by more than an
order of magnitude. On HARPS/3.6 m Epoch II, we report a Doppler redshift at vΓ,NaD
= + 9.7 ± 1.6 km s−1 with respect to the planet's rest frame. Upon examining the
lightcurves, we confirm night-to-night variability, on the order of ∼1%–4% in
NaD, rarely coinciding with exoplanet transit, not readily explained by stellar
activity, starspots, tellurics, or the interstellar medium. Coincident with the
∼+10 km s−1 Doppler redshift, we detect a transient sodium absorption event dFNaD/F⋆
= 3.6% ± 1% at a relative difference of ΔFNaD(t) ∼ 4.4% ± 1%, lasting ΔtNaD ≳
40 minutes. Since exoplanetary alkali signatures are blueshifted due to the natural
vector of radiation pressure, estimated here at roughly ∼−5.7 km s−1, the radial
velocity is rather at +15.4 km s−1, far larger than any known exoplanet system.
Given that the redshift magnitude vΓ is in between the Roche limit and dynamically
stable satellite orbits, the transient sodium may be a putative indication of
a natural satellite orbiting WASP-49 A b.
acknowledgement: The research described in this Letter was carried out in part at
the Jet Propulsion Laboratory, California Institute of Technology, under a contract
with the National Aeronautics Space Administration, © 2024. California Institute
of Technology. Government sponsorship acknowledged. A.V.O. and J.V.S. thank M. Lendl
for constraints and discussions on the mass of WASP-49 A b. S.G.S acknowledges the
support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE
(EC).
article_number: L53
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Apurva V.
full_name: Oza, Apurva V.
last_name: Oza
- first_name: Julia V.
full_name: Seidel, Julia V.
last_name: Seidel
- first_name: H. Jens
full_name: Hoeijmakers, H. Jens
last_name: Hoeijmakers
- first_name: Athira
full_name: Unni, Athira
last_name: Unni
- first_name: Aurora Y.
full_name: Kesseli, Aurora Y.
last_name: Kesseli
- first_name: Carl A.
full_name: Schmidt, Carl A.
last_name: Schmidt
- first_name: Thirupathi
full_name: Sivarani, Thirupathi
last_name: Sivarani
- first_name: Aaron
full_name: Bello-Arufe, Aaron
last_name: Bello-Arufe
- first_name: Andrea
full_name: Gebek, Andrea
last_name: Gebek
- first_name: Moritz
full_name: Meyer Zu Westram, Moritz
last_name: Meyer Zu Westram
- first_name: Sérgio G.
full_name: Sousa, Sérgio G.
last_name: Sousa
- first_name: Rosaly M.C.
full_name: Lopes, Rosaly M.C.
last_name: Lopes
- first_name: Renyu
full_name: Hu, Renyu
last_name: Hu
- first_name: Katherine
full_name: De Kleer, Katherine
last_name: De Kleer
- first_name: Chloe
full_name: Fisher, Chloe
last_name: Fisher
- first_name: Sébastien
full_name: Charnoz, Sébastien
last_name: Charnoz
- first_name: Ashley D.
full_name: Baker, Ashley D.
last_name: Baker
- first_name: Samuel P.
full_name: Halverson, Samuel P.
last_name: Halverson
- first_name: Nick M.
full_name: Schneider, Nick M.
last_name: Schneider
- first_name: Angelica
full_name: Psaridi, Angelica
last_name: Psaridi
- first_name: Aurélien
full_name: Wyttenbach, Aurélien
last_name: Wyttenbach
- first_name: Santiago
full_name: Torres Rodriguez, Santiago
id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
last_name: Torres Rodriguez
orcid: 0000-0002-3150-8988
- first_name: Ishita
full_name: Bhatnagar, Ishita
last_name: Bhatnagar
- first_name: Robert E.
full_name: Johnson, Robert E.
last_name: Johnson
citation:
ama: Oza AV, Seidel JV, Hoeijmakers HJ, et al. Redshifted sodium transient near
exoplanet transit. Astrophysical Journal Letters. 2024;973(2). doi:10.3847/2041-8213/ad6b29
apa: Oza, A. V., Seidel, J. V., Hoeijmakers, H. J., Unni, A., Kesseli, A. Y., Schmidt,
C. A., … Johnson, R. E. (2024). Redshifted sodium transient near exoplanet transit.
Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ad6b29
chicago: Oza, Apurva V., Julia V. Seidel, H. Jens Hoeijmakers, Athira Unni, Aurora
Y. Kesseli, Carl A. Schmidt, Thirupathi Sivarani, et al. “Redshifted Sodium Transient
near Exoplanet Transit.” Astrophysical Journal Letters. IOP Publishing,
2024. https://doi.org/10.3847/2041-8213/ad6b29.
ieee: A. V. Oza et al., “Redshifted sodium transient near exoplanet transit,”
Astrophysical Journal Letters, vol. 973, no. 2. IOP Publishing, 2024.
ista: Oza AV, Seidel JV, Hoeijmakers HJ, Unni A, Kesseli AY, Schmidt CA, Sivarani
T, Bello-Arufe A, Gebek A, Meyer Zu Westram M, Sousa SG, Lopes RMC, Hu R, De Kleer
K, Fisher C, Charnoz S, Baker AD, Halverson SP, Schneider NM, Psaridi A, Wyttenbach
A, Torres Rodriguez S, Bhatnagar I, Johnson RE. 2024. Redshifted sodium transient
near exoplanet transit. Astrophysical Journal Letters. 973(2), L53.
mla: Oza, Apurva V., et al. “Redshifted Sodium Transient near Exoplanet Transit.”
Astrophysical Journal Letters, vol. 973, no. 2, L53, IOP Publishing, 2024,
doi:10.3847/2041-8213/ad6b29.
short: A.V. Oza, J.V. Seidel, H.J. Hoeijmakers, A. Unni, A.Y. Kesseli, C.A. Schmidt,
T. Sivarani, A. Bello-Arufe, A. Gebek, M. Meyer Zu Westram, S.G. Sousa, R.M.C.
Lopes, R. Hu, K. De Kleer, C. Fisher, S. Charnoz, A.D. Baker, S.P. Halverson,
N.M. Schneider, A. Psaridi, A. Wyttenbach, S. Torres Rodriguez, I. Bhatnagar,
R.E. Johnson, Astrophysical Journal Letters 973 (2024).
date_created: 2024-10-13T22:01:49Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:18:18Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/2041-8213/ad6b29
external_id:
arxiv:
- '2409.19844'
isi:
- '001322169500001'
file:
- access_level: open_access
checksum: 23eea2a6a0519694a84998957ad7b7fb
content_type: application/pdf
creator: dernst
date_created: 2024-10-21T11:05:11Z
date_updated: 2024-10-21T11:05:11Z
file_id: '18456'
file_name: 2024_AstrophysicalJourn_Oza.pdf
file_size: 1249747
relation: main_file
success: 1
file_date_updated: 2024-10-21T11:05:11Z
has_accepted_license: '1'
intvolume: ' 973'
isi: 1
issue: '2'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Redshifted sodium transient near exoplanet transit
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 973
year: '2024'
...
---
APC_amount: 3080,76 EUR
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '18564'
abstract:
- lang: eng
text: The recently discovered Pa 30 nebula, the putative type Iax supernova remnant
associated with the historical supernova of 1181 AD, shows puzzling characteristics
that make it unique among known supernova remnants. In particular, Pa 30 exhibits
a complex morphology, with a unique radial and filamentary structure, and it hosts
a hot stellar remnant at its center, which displays oxygen-dominated, ultrafast
winds. Because of the surviving stellar remnant and the lack of hydrogen and helium
in its filaments, it has been suggested that Pa 30 is the product of a failed
thermonuclear explosion in a near- or super-Chandrasekhar white dwarf, which created
a subluminous transient, a rare subtype of the Ia class of supernovae called type
Iax. We present here a detailed study of the 3D structure and velocities of a
full radial section of the remnant. The Integral Field Unit observations, obtained
with the new red channel of the Keck Cosmic Web Imager spectrograph, reveal that
the ejecta are consistent with being ballistic, with velocities close to the free-expansion
velocity. Additionally, we detect a large cavity inside the supernova remnant
and a sharp inner edge to the filamentary structure, which coincides with the
outer edge of a bright ring detected in infrared images. Finally, we detect a
strong asymmetry in the amount of ejecta along the line of sight, which might
hint at an asymmetric explosion. Our analysis provides strong confirmation that
the explosion originated from SN 1181.
acknowledgement: "We thank Rob Fesen for providing the [S ii] narrowband imaging and
providing helpful comments on the Letter. We also thank Eliot Quartert for the helpful
discussions. T.C. was supported by NASA through the NASA Hubble Fellowship grant
HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., for NASA, under
contract NAS5-26555. I.C. was also supported by NASA through grants from the Space
Telescope Science Institute, under NASA contracts NASA.22K1813, NAS5-26555, and
NAS5-03127. This research was supported in part by grant NSF PHY-1748958 to the
Kavli Institute for Theoretical Physics (KITP). O.T. was supported by FONDECYT grant
11241186.\r\n\r\nThis publication makes use of data products from the Wide-field
Infrared Survey Explorer, which is a joint project of the University of California,
Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration.\r\n\r\nThis research
made use of Montage. It is funded by the National Science Foundation under grant
No. ACI-1440620, and was previously funded by the National Aeronautics and Space
Administration's Earth Science Technology Office, Computation Technologies Project,
under Cooperative Agreement Number NCC5-626 between NASA and the California Institute
of Technology."
article_number: L7
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Tim
full_name: Cunningham, Tim
last_name: Cunningham
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Nikolaus Z.
full_name: Prusinski, Nikolaus Z.
last_name: Prusinski
- first_name: James
full_name: Fuller, James
last_name: Fuller
- first_name: John C.
full_name: Raymond, John C.
last_name: Raymond
- first_name: S. R.
full_name: Kulkarni, S. R.
last_name: Kulkarni
- first_name: James D.
full_name: Neill, James D.
last_name: Neill
- first_name: Paul
full_name: Duffell, Paul
last_name: Duffell
- first_name: Chris
full_name: Martin, Chris
last_name: Martin
- first_name: Odette
full_name: Toloza, Odette
last_name: Toloza
- first_name: David
full_name: Charbonneau, David
last_name: Charbonneau
- first_name: Scott J.
full_name: Kenyon, Scott J.
last_name: Kenyon
- first_name: Zeren
full_name: Lin, Zeren
last_name: Lin
- first_name: Mateusz
full_name: Matuszewski, Mateusz
last_name: Matuszewski
- first_name: Rosalie
full_name: McGurk, Rosalie
last_name: McGurk
- first_name: Abigail
full_name: Polin, Abigail
last_name: Polin
- first_name: Philippe Z.
full_name: Yao, Philippe Z.
last_name: Yao
citation:
ama: Cunningham T, Caiazzo I, Prusinski NZ, et al. Expansion properties of the young
supernova type Iax remnant Pa 30 revealed. The Astrophysical Journal Letters.
2024;975(1). doi:10.3847/2041-8213/ad713b
apa: Cunningham, T., Caiazzo, I., Prusinski, N. Z., Fuller, J., Raymond, J. C.,
Kulkarni, S. R., … Yao, P. Z. (2024). Expansion properties of the young supernova
type Iax remnant Pa 30 revealed. The Astrophysical Journal Letters. IOP
Publishing. https://doi.org/10.3847/2041-8213/ad713b
chicago: Cunningham, Tim, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John
C. Raymond, S. R. Kulkarni, James D. Neill, et al. “Expansion Properties of the
Young Supernova Type Iax Remnant Pa 30 Revealed.” The Astrophysical Journal
Letters. IOP Publishing, 2024. https://doi.org/10.3847/2041-8213/ad713b.
ieee: T. Cunningham et al., “Expansion properties of the young supernova
type Iax remnant Pa 30 revealed,” The Astrophysical Journal Letters, vol.
975, no. 1. IOP Publishing, 2024.
ista: Cunningham T, Caiazzo I, Prusinski NZ, Fuller J, Raymond JC, Kulkarni SR,
Neill JD, Duffell P, Martin C, Toloza O, Charbonneau D, Kenyon SJ, Lin Z, Matuszewski
M, McGurk R, Polin A, Yao PZ. 2024. Expansion properties of the young supernova
type Iax remnant Pa 30 revealed. The Astrophysical Journal Letters. 975(1), L7.
mla: Cunningham, Tim, et al. “Expansion Properties of the Young Supernova Type Iax
Remnant Pa 30 Revealed.” The Astrophysical Journal Letters, vol. 975, no.
1, L7, IOP Publishing, 2024, doi:10.3847/2041-8213/ad713b.
short: T. Cunningham, I. Caiazzo, N.Z. Prusinski, J. Fuller, J.C. Raymond, S.R.
Kulkarni, J.D. Neill, P. Duffell, C. Martin, O. Toloza, D. Charbonneau, S.J. Kenyon,
Z. Lin, M. Matuszewski, R. McGurk, A. Polin, P.Z. Yao, The Astrophysical Journal
Letters 975 (2024).
das_tickbox: '1'
date_created: 2024-11-19T08:12:59Z
date_published: 2024-10-24T00:00:00Z
date_updated: 2026-07-06T12:21:32Z
day: '24'
ddc:
- '520'
department:
- _id: IlCa
doi: 10.3847/2041-8213/ad713b
external_id:
arxiv:
- '2410.10940'
isi:
- '001340831400001'
file:
- access_level: open_access
checksum: 51e790dd3d85ca984e656734f9f611da
content_type: application/pdf
creator: dernst
date_created: 2024-11-20T12:24:52Z
date_updated: 2024-11-20T12:24:52Z
file_id: '18573'
file_name: 2024_AstrophysJourLetters_Cunningham.pdf
file_size: 90328868
relation: main_file
success: 1
file_date_updated: 2024-11-20T12:24:52Z
has_accepted_license: '1'
intvolume: ' 975'
isi: 1
issue: '1'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
project:
- _id: B67AFEDC-15C9-11EA-A837-991A96BB2854
name: IST Austria Open Access Fund
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Expansion properties of the young supernova type Iax remnant Pa 30 revealed
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: 975
year: '2024'
...
---
_id: '15192'
abstract:
- lang: eng
text: We searched the Gaia DR3 database for ultramassive white dwarfs with kinematics
consistent with having escaped the nearby Hyades open cluster, identifying three
such candidates. Two of these candidates have masses estimated from Gaia photometry
of approximately 1.1 solar masses; their status as products of single-stellar
evolution that have escaped the cluster was deemed too questionable for immediate
follow-up analysis. The remaining candidate has an expected mass >1.3 solar masses,
significantly reducing the probability of it being an interloper. Analysis of
follow-up Gemini GMOS spectroscopy for this source reveals a nonmagnetized hydrogen
atmosphere white dwarf with a mass and age consistent with having formed from
a single star. Assuming a single-stellar-evolution formation channel, we estimate
a 97.8% chance that the candidate is a true escapee from the Hyades. With a determined
mass of 1.317 solar masses, this is potentially the most massive known single-evolution
white dwarf and is by far the most massive with a strong association with an open
cluster.
article_number: L41
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David R.
full_name: Miller, David R.
last_name: Miller
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Jeremy
full_name: Heyl, Jeremy
last_name: Heyl
- first_name: Harvey B.
full_name: Richer, Harvey B.
last_name: Richer
- first_name: Kareem
full_name: El-Badry, Kareem
last_name: El-Badry
- first_name: Antonio C.
full_name: Rodriguez, Antonio C.
last_name: Rodriguez
- first_name: Zachary P.
full_name: Vanderbosch, Zachary P.
last_name: Vanderbosch
- first_name: Jan
full_name: van Roestel, Jan
last_name: van Roestel
citation:
ama: Miller DR, Caiazzo I, Heyl J, et al. An extremely massive white dwarf escaped
from the Hyades star cluster. The Astrophysical Journal Letters. 2023;956(2).
doi:10.3847/2041-8213/acffc4
apa: Miller, D. R., Caiazzo, I., Heyl, J., Richer, H. B., El-Badry, K., Rodriguez,
A. C., … van Roestel, J. (2023). An extremely massive white dwarf escaped from
the Hyades star cluster. The Astrophysical Journal Letters. American Astronomical
Society. https://doi.org/10.3847/2041-8213/acffc4
chicago: Miller, David R., Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem
El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, and Jan van Roestel. “An
Extremely Massive White Dwarf Escaped from the Hyades Star Cluster.” The Astrophysical
Journal Letters. American Astronomical Society, 2023. https://doi.org/10.3847/2041-8213/acffc4.
ieee: D. R. Miller et al., “An extremely massive white dwarf escaped from
the Hyades star cluster,” The Astrophysical Journal Letters, vol. 956,
no. 2. American Astronomical Society, 2023.
ista: Miller DR, Caiazzo I, Heyl J, Richer HB, El-Badry K, Rodriguez AC, Vanderbosch
ZP, van Roestel J. 2023. An extremely massive white dwarf escaped from the Hyades
star cluster. The Astrophysical Journal Letters. 956(2), L41.
mla: Miller, David R., et al. “An Extremely Massive White Dwarf Escaped from the
Hyades Star Cluster.” The Astrophysical Journal Letters, vol. 956, no.
2, L41, American Astronomical Society, 2023, doi:10.3847/2041-8213/acffc4.
short: D.R. Miller, I. Caiazzo, J. Heyl, H.B. Richer, K. El-Badry, A.C. Rodriguez,
Z.P. Vanderbosch, J. van Roestel, The Astrophysical Journal Letters 956 (2023).
date_created: 2024-03-26T09:45:38Z
date_published: 2023-10-19T00:00:00Z
date_updated: 2024-04-02T06:56:01Z
day: '19'
doi: 10.3847/2041-8213/acffc4
extern: '1'
external_id:
arxiv:
- '2310.03204'
intvolume: ' 956'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/2041-8213/acffc4
month: '10'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: An extremely massive white dwarf escaped from the Hyades star cluster
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: 956
year: '2023'
...