---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '23048'
abstract:
- lang: eng
  text: The previously inaccessible star formation tracer Paschen-Alpha (Paα) can
    now be spatially resolved by JWST NIRCam slitless spectroscopy in distant galaxies
    up to cosmic noon. In the first study of its kind, we combine JWST NGDEEP NIRISS
    and FRESCO NIRCam slitless spectroscopy to provide the first direct comparison
    of spatially resolved dust-obscured (traced by Paα) versus unobscured (traced
    by Hα) star formation across the main sequence. We stacked Paα and Hα emission-line
    maps, along with stellar continuum images at both wavelengths of 31 galaxies at
    1 < z < 1.8 in three bins of stellar mass spanning 7.7 ≤ log(M*/M⊙) < 11. Surface
    brightness profiles were measured and equivalent width (EW) profiles computed.
    Increasing Paα and Hα EW profiles with galactocentric radius across all stellar
    masses probed provides direct evidence for the inside-out growth of galaxies both
    via dust-obscured and unobscured star formation for the first time. For galaxies
    predominantly on the main sequence (log(M*/M⊙)≥8.8), a weakly positive (0.1 ± 0.1)
    Paα/Hα line profile gradient as a function of radius is found at 8.8 ≤ log(M*/M⊙)
    < 9.9, with a negative (−0.4 ± 0.1) Paα/Hα line profile gradient as a function
    of radius found at the highest stellar masses of 9.9 ≤ log(M*/M⊙) < 11.0. Low-mass
    galaxies (7.7 ≤ log(M*/M⊙) < 8.8) with predominantly high specific star formation
    rates relative to the main sequence are also found to have a negative (−0.5 ± 0.1)
    Paα/Hα line profile gradient as a function of radius. Our results demonstrate
    that while inside-out growth via star formation is ubiquitous across the main
    sequence just after cosmic noon, centrally concentrated dust attenuation is not.
    Along with other recent work in the literature, our findings now motivate future
    studies of resolved SFR and dust attenuation profiles in large samples of individual
    cosmic noon galaxies across the main sequence, aimed at understanding the intrinsic
    scatter in spatially resolved star formation.
acknowledgement: 'JM is grateful to the Max Planck Society for the MPIA Prize Fellowship
  and to the Cosmic Dawn Center for the DAWN Fellowship. This work is based on observations
  made with the NASA/ESA/CSA James Webb Space Telescope. The raw 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 JWST Cycle 1 GO programs #1895 and #2079. Support for both programs was provided
  by NASA through a grant from the Space Telescope Science Institute, which is operated
  by the Associations of Universities for Research in Astronomy, Incorporated, under
  NASA contract NAS5-26555. The Cosmic Dawn Center (DAWN) is funded by the Danish
  National Research Foundation under grant DNRF140. 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. This work benefited from support from
  the George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy
  at Texas A&M University. CP thanks Marsha and Ralph Schilling for generous support
  of this research.'
article_number: A33
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jasleen
  full_name: Matharu, Jasleen
  last_name: Matharu
- first_name: Lu
  full_name: Shen, Lu
  last_name: Shen
- first_name: Irene
  full_name: Shivaei, Irene
  last_name: Shivaei
- first_name: Pascal A.
  full_name: Oesch, Pascal A.
  last_name: Oesch
- first_name: Casey
  full_name: Papovich, Casey
  last_name: Papovich
- first_name: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Naveen A.
  full_name: Reddy, Naveen A.
  last_name: Reddy
- first_name: Yingjie
  full_name: Cheng, Yingjie
  last_name: Cheng
- first_name: Pieter
  full_name: Van Dokkum, Pieter
  last_name: Van Dokkum
- first_name: Steven L.
  full_name: Finkelstein, Steven L.
  last_name: Finkelstein
- first_name: Nimish P.
  full_name: Hathi, Nimish P.
  last_name: Hathi
- first_name: Jeyhan S.
  full_name: Kartaltepe, Jeyhan S.
  last_name: Kartaltepe
- first_name: Anton M.
  full_name: Koekemoer, Anton M.
  last_name: Koekemoer
- 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: Nor
  full_name: Pirzkal, Nor
  last_name: Pirzkal
- first_name: Stephen M.
  full_name: Wilkins, Stephen M.
  last_name: Wilkins
- first_name: Michael A.
  full_name: Wozniak, Michael A.
  last_name: Wozniak
- first_name: Mengyuan
  full_name: Xiao, Mengyuan
  last_name: Xiao
citation:
  ama: Matharu J, Shen L, Shivaei I, et al. A first look at a complete view of spatially
    resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless
    spectroscopy. <i>Astronomy and Astrophysics</i>. 2026;708. doi:<a href="https://doi.org/10.1051/0004-6361/202558205">10.1051/0004-6361/202558205</a>
  apa: Matharu, J., Shen, L., Shivaei, I., Oesch, P. A., Papovich, C., Brammer, G.,
    … Xiao, M. (2026). A first look at a complete view of spatially resolved star
    formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy.
    <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202558205">https://doi.org/10.1051/0004-6361/202558205</a>
  chicago: Matharu, Jasleen, Lu Shen, Irene Shivaei, Pascal A. Oesch, Casey Papovich,
    Gabriel Brammer, Naveen A. Reddy, et al. “A First Look at a Complete View of Spatially
    Resolved Star Formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO Slitless
    Spectroscopy.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href="https://doi.org/10.1051/0004-6361/202558205">https://doi.org/10.1051/0004-6361/202558205</a>.
  ieee: J. Matharu <i>et al.</i>, “A first look at a complete view of spatially resolved
    star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy,”
    <i>Astronomy and Astrophysics</i>, vol. 708. EDP Sciences, 2026.
  ista: Matharu J, Shen L, Shivaei I, Oesch PA, Papovich C, Brammer G, Reddy NA, Cheng
    Y, Van Dokkum P, Finkelstein SL, Hathi NP, Kartaltepe JS, Koekemoer AM, Matthee
    JJ, Pirzkal N, Wilkins SM, Wozniak MA, Xiao M. 2026. A first look at a complete
    view of spatially resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST
    NGDEEP+FRESCO slitless spectroscopy. Astronomy and Astrophysics. 708, A33.
  mla: Matharu, Jasleen, et al. “A First Look at a Complete View of Spatially Resolved
    Star Formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO Slitless Spectroscopy.”
    <i>Astronomy and Astrophysics</i>, vol. 708, A33, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202558205">10.1051/0004-6361/202558205</a>.
  short: J. Matharu, L. Shen, I. Shivaei, P.A. Oesch, C. Papovich, G. Brammer, N.A.
    Reddy, Y. Cheng, P. Van Dokkum, S.L. Finkelstein, N.P. Hathi, J.S. Kartaltepe,
    A.M. Koekemoer, J.J. Matthee, N. Pirzkal, S.M. Wilkins, M.A. Wozniak, M. Xiao,
    Astronomy and Astrophysics 708 (2026).
das_tickbox: '0'
date_created: 2026-10-04T22:01:55Z
date_published: 2026-04-01T00:00:00Z
date_updated: 2026-10-12T07:44:07Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202558205
external_id:
  arxiv:
  - '2511.15792'
file:
- access_level: open_access
  checksum: 875d217ea15192fa1208f3db34a7fad6
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  creator: dernst
  date_created: 2026-10-12T07:31:23Z
  date_updated: 2026-10-12T07:31:23Z
  file_id: '23101'
  file_name: 2026_AstronomyAstrophysics_Matharu.pdf
  file_size: 587642
  relation: main_file
  success: 1
file_date_updated: 2026-10-12T07:31:23Z
fulldoi: https://doi.org/10.1051/0004-6361/202558205
has_accepted_license: '1'
intvolume: '       708'
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy and Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: no
title: A first look at a complete view of spatially resolved star formation at 1  <  z  <  1.8
  with JWST NGDEEP+FRESCO slitless 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: 708
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23092'
abstract:
- lang: eng
  text: We present the number density of massive (log(M*/Mo)> 10.3) quiescent galaxies
    at 2 < z < 5 using JWST NIRSpec PRISM spectra. This work relies on spectra from
    RUBIES, which provides excellent data quality and an unparalleled, well-defined
    targeting strategy to robustly infer physical properties and number densities.
    We identify quiescent galaxy candidates within RUBIES through principal component
    analysis and construct a final sample using star formation histories derived from
    spectrophotometric fitting of the NIRSpec PRISM spectra and NIRCam photometry.
    By inverting the RUBIES selection function, we correct for survey incompleteness
    and calculate the number density of massive quiescent galaxies at these redshifts,
    providing the most complete spectroscopic estimates prior to cosmic noon to date.
    We find that early massive quiescent galaxies are surprisingly common (≳10−5 Mpc−3
    by 4 < z < 5), which is consistent with previous studies based on JWST photometry
    alone and/or in smaller survey areas. We compare our number densities with predictions
    from six state-of-the-art cosmological galaxy formation simulations. At z > 3,
    most simulations fail to produce enough massive quiescent galaxies, suggesting
    the treatment of feedback and/or the channels for early efficient formation are
    incomplete in most galaxy evolution models.
acknowledgement: "We thank Alan Pearl for his contribution to estimating the cosmic
  variance contribution to the number density uncertainties in this work. We thank
  Hans-Walter Rix for the valuable discussion on the selection function and correcting
  the spectroscopic incompleteness of massive quiescent galaxies in RUBIES.\r\n\r\nSome
  of the data products presented herein were retrieved from the Dawn JWST Archive
  (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by
  the Danish National Research Foundation under grant DNRF140.\r\n\r\nThe Cosmic Dawn
  Center is funded by the Danish National Research Foundation (DNRF) under grant #140.\r\n\r\nSupport
  for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship
  grant.\r\n\r\nR.B. gratefully acknowledges support from the Research Corporation
  for Scientific Advancement (RCSA) Cottrell Scholar Award ID No: 27587.\r\n\r\nThe
  work of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities
  for Research in Astronomy (AURA) under a cooperative agreement with the National
  Science Foundation.\r\n\r\nT.B.M. was supported by a CIERA Postdoctoral Fellowship.\r\n\r\nThis
  work is based in part on observations made with the NASA/ESA/CSA James Webb Space
  Telescope. The data were obtained from the Mikulski Archive for Space Telescopes
  at the Space Telescope Science Institute, which is operated by the Association of
  Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for
  JWST. These observations are associated with program numbers 1180, 1181, 1210, 1211,
  1213, 1214, 1215, 1286, 1345, 1433, 1747, 2028, 2073, 2198, 2282, 2561, 2565, 2750,
  2756, 2767, 3073, 3215, 4233, 4446, 4557, 6368, 6541, and 6585. The specific observations
  analyzed can be accessed via DOI: 10.17909/sjsj-8p46.\r\n\r\nSupport for program
  No. 4233 was provided by NASA through a grant from the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-03127.\r\n\r\nThe authors acknowledge the CEERS
  and PRIMER teams for developing their observing program with a zero-exclusive access
  period.\r\n\r\nFacility: JWST - James Webb Space Telescope.\r\n\r\nSoftware: Astropy
  (Astropy Collaboration et al. 2013, 2018, 2022), Scipy (P. Virtanen et al. 2020),
  Photutils (L. Bradley 2023), SpectRes (A. C. Carnall 2017), Scikit-learn (F. Pedregosa
  et al. 2011), Prospector (B. Johnson & J. Leja 2017; J. Leja et al. 2017; B. Johnson
  et al. 2021)."
article_number: '252'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Yunchong
  full_name: Zhang, Yunchong
  last_name: Zhang
- first_name: Anna
  full_name: De Graaff, Anna
  last_name: De Graaff
- first_name: David J.
  full_name: Setton, David J.
  last_name: Setton
- first_name: Sedona H.
  full_name: Price, Sedona H.
  last_name: Price
- first_name: Rachel
  full_name: Bezanson, Rachel
  last_name: Bezanson
- first_name: Claudia
  full_name: Del P. Lagos, Claudia
  last_name: Del P. Lagos
- first_name: Sam E.
  full_name: Cutler, Sam E.
  last_name: Cutler
- first_name: Ian
  full_name: Mcconachie, Ian
  last_name: Mcconachie
- first_name: Nikko J.
  full_name: Cleri, Nikko J.
  last_name: Cleri
- first_name: Olivia R.
  full_name: Cooper, Olivia R.
  last_name: Cooper
- first_name: Rashmi
  full_name: Gottumukkala, Rashmi
  last_name: Gottumukkala
- first_name: Jenny E.
  full_name: Greene, Jenny E.
  last_name: Greene
- first_name: Michaela
  full_name: Hirschmann, Michaela
  last_name: Hirschmann
- first_name: Gourav
  full_name: Khullar, Gourav
  last_name: Khullar
- first_name: Ivo
  full_name: Labbe, Ivo
  last_name: Labbe
- first_name: Joel
  full_name: Leja, Joel
  last_name: Leja
- first_name: Michael V.
  full_name: Maseda, Michael V.
  last_name: Maseda
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Tim B.
  full_name: Miller, Tim B.
  last_name: Miller
- first_name: Themiya
  full_name: Nanayakkara, Themiya
  last_name: Nanayakkara
- first_name: Katherine A.
  full_name: Suess, Katherine A.
  last_name: Suess
- first_name: Bingjie
  full_name: Wang, Bingjie
  last_name: Wang
- first_name: Katherine E.
  full_name: Whitaker, Katherine E.
  last_name: Whitaker
- first_name: Christina C.
  full_name: Williams, Christina C.
  last_name: Williams
citation:
  ama: Zhang Y, De Graaff A, Setton DJ, et al. RUBIES spectroscopically confirms the
    high number density of quiescent galaxies from2&#60;z&#60;5. <i>The Astrophysical
    Journal</i>. 2026;997(2). doi:<a href="https://doi.org/10.3847/1538-4357/ae24e1">10.3847/1538-4357/ae24e1</a>
  apa: Zhang, Y., De Graaff, A., Setton, D. J., Price, S. H., Bezanson, R., Del P.
    Lagos, C., … Williams, C. C. (2026). RUBIES spectroscopically confirms the high
    number density of quiescent galaxies from2&#60;z&#60;5. <i>The Astrophysical Journal</i>.
    IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae24e1">https://doi.org/10.3847/1538-4357/ae24e1</a>
  chicago: Zhang, Yunchong, Anna De Graaff, David J. Setton, Sedona H. Price, Rachel
    Bezanson, Claudia Del P. Lagos, Sam E. Cutler, et al. “RUBIES Spectroscopically
    Confirms the High Number Density of Quiescent Galaxies From2&#60;z&#60;5.” <i>The
    Astrophysical Journal</i>. IOP Publishing, 2026. <a href="https://doi.org/10.3847/1538-4357/ae24e1">https://doi.org/10.3847/1538-4357/ae24e1</a>.
  ieee: Y. Zhang <i>et al.</i>, “RUBIES spectroscopically confirms the high number
    density of quiescent galaxies from2&#60;z&#60;5,” <i>The Astrophysical Journal</i>,
    vol. 997, no. 2. IOP Publishing, 2026.
  ista: Zhang Y, De Graaff A, Setton DJ, Price SH, Bezanson R, Del P. Lagos C, Cutler
    SE, Mcconachie I, Cleri NJ, Cooper OR, Gottumukkala R, Greene JE, Hirschmann M,
    Khullar G, Labbe I, Leja J, Maseda MV, Matthee JJ, Miller TB, Nanayakkara T, Suess
    KA, Wang B, Whitaker KE, Williams CC. 2026. RUBIES spectroscopically confirms
    the high number density of quiescent galaxies from2&#60;z&#60;5. The Astrophysical
    Journal. 997(2), 252.
  mla: Zhang, Yunchong, et al. “RUBIES Spectroscopically Confirms the High Number
    Density of Quiescent Galaxies From2&#60;z&#60;5.” <i>The Astrophysical Journal</i>,
    vol. 997, no. 2, 252, IOP Publishing, 2026, doi:<a href="https://doi.org/10.3847/1538-4357/ae24e1">10.3847/1538-4357/ae24e1</a>.
  short: Y. Zhang, A. De Graaff, D.J. Setton, S.H. Price, R. Bezanson, C. Del P. Lagos,
    S.E. Cutler, I. Mcconachie, N.J. Cleri, O.R. Cooper, R. Gottumukkala, J.E. Greene,
    M. Hirschmann, G. Khullar, I. Labbe, J. Leja, M.V. Maseda, J.J. Matthee, T.B.
    Miller, T. Nanayakkara, K.A. Suess, B. Wang, K.E. Whitaker, C.C. Williams, The
    Astrophysical Journal 997 (2026).
date_created: 2026-10-11T22:02:05Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-10-12T11:55:05Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae24e1
external_id:
  arxiv:
  - '2508.08577'
file:
- access_level: open_access
  checksum: 547c63f9265be5d41efdc555a25423cc
  content_type: application/pdf
  creator: dernst
  date_created: 2026-10-12T11:51:24Z
  date_updated: 2026-10-12T11:51:24Z
  file_id: '23110'
  file_name: 2026_AstrophysicalJour_Zhang.pdf
  file_size: 5995619
  relation: main_file
  success: 1
file_date_updated: 2026-10-12T11:51:24Z
fulldoi: https://doi.org/10.3847/1538-4357/ae24e1
has_accepted_license: '1'
intvolume: '       997'
issue: '2'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: RUBIES spectroscopically confirms the high number density of quiescent galaxies
  from2<z<5
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 997
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23115'
abstract:
- lang: eng
  text: "We investigate the association between galaxies and neutral O I absorption
    systems at z ∼ 6, which trace metalenriched gas during the epoch of reionization.
    We identify 40 galaxies across six quasar fields, residing in 15\r\noverdensities
    within 300 kpc of the background sight lines. Five O I absorption systems are
    associated with five of\r\nthese overdensities, yielding a covering fraction of\r\n0.27
    0.10\r\n+0.13\r\nwithin 300 kpc. The absorption occurs beyond typical\r\nvirial
    radii, indicating that the gas traces extended overdensity environments rather
    than individual galaxy halos,\r\nunlike the z ∼ 0 circumgalactic medium (CGM),
    which is largely bound to halos. These galaxy-associated\r\nabsorbers account
    for ∼35% of all O I systems seen in blind quasar surveys, implying the remainder
    arise in\r\nlower-mass galaxies below our detection threshold or in dense neutral
    intergalactic medium pockets. The CGM\r\naround these galaxies contains ≳ 2 ×
    106 M⊙ of oxygen, comparable to the interstellar medium oxygen mass of\r\nthe
    galaxies themselves, suggesting that the surrounding environment holds as much
    metal mass as the galaxies.\r\nAll five galaxy-associated systems show significantly
    higher\r\nlog NCII NOI ( / )\r\nratios than absorbers lacking galaxy\r\nassociations.
    Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal that four of the
    five exhibit\r\nenrichment patterns consistent with Population III nucleosynthesis
    at the outskirts of galaxy overdensities. These\r\nrare systems offer a unique
    window into the role of first-generation stars in shaping the early metal enrichment
    of\r\ngalaxies and their environments."
acknowledgement: "IOP Science home\r\nAccessibility Help\r\n\r\nJournals\r\nBooks\r\nPublishing
  Support\r\nLogin\r\nThe Astrophysical Journal\r\nThe American Astronomical Society,
  find out more.\r\n\r\nThe following article isOpen access\r\nEIGER. VIII. First
  Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch
  of Reionization\r\nJack Higginson, Rongmon Bordoloi, Robert A. Simcoe, Jorryt Matthee,
  Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, Simon J. Lilly, Anna-Christina
  Eilers, Rohan P. NaiduShow full author list\r\n\r\nPublished 2026 February 24 •
  © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical
  Journal, Volume 999, Number 1\r\nCitation Jack Higginson et al 2026 ApJ 999 49\r\nDOI
  10.3847/1538-4357/ae3e81\r\n\r\nPDFOpens in a new tab.\r\nePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle
  data\r\nPDFOpens in a new tab.\r\nePub\r\nArticle metrics\r\n626 Total downloads\r\n\r\n22
  total citations on Dimensions.\r\nShare this article\r\nArticle information\r\nAbstract\r\nWe
  investigate the association between galaxies and neutral O i absorption systems
  at z ∼ 6, which trace metal-enriched gas during the epoch of reionization. We identify
  40 galaxies across six quasar fields, residing in 15 overdensities within 300 kpc
  of the background sight lines. Five O i absorption systems are associated with five
  of these overdensities, yielding a covering fraction of \r\n within 300 kpc. The
  absorption occurs beyond typical virial radii, indicating that the gas traces extended
  overdensity environments rather than individual galaxy halos, unlike the z ∼ 0 circumgalactic
  medium (CGM), which is largely bound to halos. These galaxy-associated absorbers
  account for ∼35% of all O i systems seen in blind quasar surveys, implying the remainder
  arise in lower-mass galaxies below our detection threshold or in dense neutral intergalactic
  medium pockets. The CGM around these galaxies contains  ≳  2 × 106 M⊙ of oxygen,
  comparable to the interstellar medium oxygen mass of the galaxies themselves, suggesting
  that the surrounding environment holds as much metal mass as the galaxies. All five
  galaxy-associated systems show significantly higher \r\n ratios than absorbers lacking
  galaxy associations. Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal
  that four of the five exhibit enrichment patterns consistent with Population III
  nucleosynthesis at the outskirts of galaxy overdensities. These rare systems offer
  a unique window into the role of first-generation stars in shaping the early metal
  enrichment of galaxies and their environments.\r\n\r\nExport citation and abstract\r\nBibTeX\r\nRIS\r\n\r\nPrevious
  article in issue\r\nNext article in issue\r\nRelated links\r\n\r\nOriginal content
  from this work may be used under the terms of the Creative Commons Attribution 4.0
  licence. Any further distribution of this work must maintain attribution to the
  author(s) and the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe
  first generations of stars formed shortly after the Epoch of Recombination within
  dark matter overdensities, producing the first significant quantities of metals
  and enriching the intergalactic medium (IGM) while reionizing hydrogen and helium
  (e.g., R. S. Klessen & S. C. O. Glover 2023). These metals and gas eventually coalesced
  into the first galaxies, which over cosmic time evolved into Milky Way–like systems
  today. Studying these young galaxies and their environments provides critical insight
  into galaxy formation and evolution, constraining models of stellar feedback, gas
  accretion, and chemical enrichment (C.-A. Faucher-Giguère & S. P. Oh 2023; C. Peroux
  & D. Nelson 2024).\r\n\r\nAt low redshift, decades of observations using deep ground-based
  spectroscopy and Hubble Space Telescope (HST) data of background quasars and foreground
  galaxies have built a rich understanding of the circumgalactic medium (CGM) and
  its interplay with galaxies (e.g., J. Tumlinson et al. 2017). The CGM plays a crucial
  role in gas recycling, star formation regulation, and quenching; understanding its
  structure and composition informs galaxy growth models (Y. Peng et al. 2015; E.
  Zinger et al. 2020).\r\n\r\nHigh-redshift studies, leveraging ground- and space-based
  near-infrared (NIR) spectroscopy of quasars, reveal that the early Universe was
  already chemically enriched by the epoch of reionization (e.g., T. J. Cooper et
  al. 2019; L. Christensen et al. 2023; R. L. Davies et al. 2023a). Among tracers
  of neutral and low-ionization gas, O i has emerged as a key probe: surveys report
  an increase in O i number density at z  ≳  5–6 (G. D. Becker et al. 2019; L. Christensen
  et al. 2023; A. M. Sebastian et al. 2024; A. Sodini et al. 2024), while higher-ionization
  species like C iv and Si iv decline, consistent with a softer and evolving UV background
  at the end of reionization (T. J. Cooper et al. 2019; V. D’Odorico et al. 2022;
  R. L. Davies et al. 2023a, 2023b).\r\n\r\nHistorically, connecting absorption systems
  with their host galaxies was challenging due to the difficulty of obtaining deep,
  high-redshift galaxy spectroscopy. This has changed with the advent of JWST, providing
  unprecedented views of early galaxies and their impact on surrounding gas through
  surveys such as EIGER (D. Kashino et al. 2023) and ASPIRE (F. Wang et al. 2023).
  First systematic studies of cool, low-ionization CGM traced by Mg ii around z ∼
  6 galaxies suggest that high-redshift CGM differs significantly from its low-redshift
  counterpart: these galaxies typically have low masses, and strong stellar feedback
  can eject metals far beyond the halo’s gravitational potential (R. Bordoloi et al.
  2024). Such pioneering studies now allow systematic investigations of the CGM in
  the early Universe.\r\n\r\nThe UV background during reionization was inhomogeneous
  and rapidly evolving (e.g., S. R. Furlanetto & S. P. Oh 2005; B. D. Oppenheimer
  et al. 2009; K. Finlator et al. 2013; G. D. Becker et al. 2015; S. E. I. Bosman
  et al. 2022), initially dominated by Population III stars (K. Nakajima & R. Maiolino
  2022; K. Nakajima et al. 2025), then by early star-forming galaxies (L. Jiang et
  al. 2022; J. Matthee et al. 2022), with active galactic nuclei (AGN) contributing
  significantly by z ∼ 5 (A. D’Aloisio et al. 2017; G. Kulkarni et al. 2019; C.-A.
  Faucher-Giguère 2020). Modeling indicates that pockets of Population III star formation
  may persist throughout the Epoch of Reionization (L. Tornatore et al. 2007; R. H.
  Mebane et al. 2018; J. L. Johnson & A. Aykutalp 2019; A. Venditti et al. 2023; O.
  Zier et al. 2025).\r\n\r\nThe large reservoir of neutral O i observed in quasar
  absorption lines at high redshift is typically self-shielded, providing robust estimates
  of chemical abundances. Studying the association of these absorbers with galaxies
  offers unique insight into the CGM of early galaxies, and into potential contributions
  from Population III stars to early chemical enrichment.\r\n\r\nIn this work, we
  study the cool, neutral CGM around galaxies at z ∼ 6, traced by O i absorption from
  the EIGER survey (D. Kashino et al. 2023). We focus on O i absorbers associated
  with [O iii]5008-emitting galaxies at 5.875 <z < 6.378 within 300 kpc of six background
  quasars. We quantify absorber incidence, column densities, and mass estimates, and
  analyze ionic abundances to probe chemical enrichment, including potential contributions
  from Population III stars.\r\n\r\nThis paper is organized as follows. Section 2
  describes the observations; Section 3 details our methods for galaxy selection,
  redshift estimation, galaxy properties, defining galaxy overdensities, absorber
  measurements, and completeness; Section 4 presents the results, including the association
  of O i absorption with galaxies, the incidence of galaxy-associated O i absorbers,
  their chemical abundances, and physical interpretations; Section 5 summarizes our
  conclusions. Throughout, we adopt a ΛCDM cosmology with H0 = 67.66 km s−1 Mpc−1
  (Planck Collaboration et al. 2020).\r\n\r\n2. Observations\r\nEIGER (Program ID
  1243; PI: S. J. Lilly) is a large JWST Wide Field Slitless Spectroscopy (WFSS) program
  totaling 126.5 hr, conducting deep WFSS observations in six extragalactic fields,
  each centered on an ultraluminous quasar at z ≥ 6. These quasars have also been
  observed with deep optical and NIR medium- and high-resolution spectroscopy with
  Magellan/FIRE, Very Large Telescope/X-shooter, and Keck High Resolution Echelle
  Spectrometer (HIRES)/MOSFIRE, providing over 100 hr of complementary NIR spectroscopy
  across the six sight lines. We refer the reader to A.-C. Eilers et al. (2023) and
  A.-C. Ďurovčíková et al. (2025) for data reduction and details of the ground-based
  quasar spectroscopy. In addition, all fields are covered by deep JWST/NIRCam and
  HST imaging. A detailed description of the survey design, methodology, and spectroscopic
  and photometric observation details is provided in D. Kashino et al. (2023), J.
  Matthee et al. (2023), and R. Bordoloi et al. (2024). In this work, we make use
  of the complete EIGER survey of z ≥ 5.9 galaxies spanning all six extragalactic
  fields (D. Kashino et al. 2026).\r\n\r\nWe note that all six quasars were chosen
  with prior knowledge of metal absorption systems along their lines of sight, which
  could in principle bias any attempt to associate galaxies with those absorbers.
  In contrast, a galaxy-centric approach starts with quasar–galaxy pairs without prior
  knowledge of absorption and then builds statistics systematically (see e.g., R.
  Bordoloi et al. 2011; J. K. Werk et al. 2013; R. Bordoloi et al. 2014). However,
  once a blind, well-characterized galaxy survey is in place, the two approaches converge.
  This is conceptually similar to a program that combines quasar spectroscopy performed
  without prior absorber selection with a complete galaxy survey. This work employs
  deep blind galaxy searches in each of the EIGER fields, yielding an emission-line
  complete sample of spectroscopic galaxies (J. Matthee et al. 2022; R. Bordoloi et
  al. 2024) and a complete census of absorption lines along these sight lines (Section
  3.5). By combining these two elements—a galaxy survey with quantified completeness
  and an absorption survey with well-defined sensitivity—we establish a robust framework
  for conducting a census of CGM absorption around galaxies. This combined approach
  has been successfully demonstrated at low redshifts (J. N. Burchett et al. 2019).\r\n\r\n3.
  Methods\r\nIn this section, we describe how galaxy redshifts and properties are
  measured and how absorption lines are identified and measured.\r\n\r\n3.1. Galaxy
  Redshifts\r\nSince our focus is on galaxies at z ∼ 6 near the quasar sight lines,
  we begin with the full EIGER catalog of [O iii] emitters (D. Kashino et al. 2026),
  which contains 948 galaxies detected via [O iii] emission within 5.33 ≤ z ≤ 6.97.
  From this catalog, we select galaxies that (1) lie at least 10,000 km s−1 in the
  foreground of each quasar , (2) are within a projected impact parameter of 300 pkpc,
  and (3) have O i λ1302 coverage in the quasar NIR spectra outside of the Gunn–Peterson
  trough. This yields a sample of 40 galaxies. Of these, 33 fall within the central
  of the EIGER spectroscopic footprint (R. Bordoloi et al. 2024), observed with both
  JWST/NIRCam reverse grism modules (A and B). Because the two modules disperse light
  in opposite directions, they provide independent moderate-resolution (R ∼ 1500)
  spectra of the same target, enabling us to assess redshift measurement uncertainties.\r\n\r\nFollowing
  the procedure in R. Bordoloi et al. (2024), we visually inspect each NIRCam 2D spectrum
  using the custom Python application programming interface (API) zgui(R. Bordoloi
  et al. 2025), extract 1D spectra from each module, and fit Gaussians to the emission
  line to determine redshifts. Redshifts from the two modules are consistent with
  a mean velocity offset of Δv = 9.3 km s−1 with a standard deviation of 24 km s−1
  (Figure 1). We therefore adopt an average redshift uncertainty of ≈24 km s−1 for
  the [O iii] emitters, sufficient for associating metal absorption systems with their
  host galaxies. Hereafter, we focus on this sample of 40 galaxies.\r\n\r\nZoom InZoom
  OutReset image size\r\nFigure 1. Redshift uncertainty distribution of the [O iii]
  emitter EIGER galaxies. The histogram shows the difference in redshift between emission-line
  measurements from NIRCam Grism Module A and Module B spectra, expressed in km s−1.
  Individual redshifts were derived from Gaussian fits to the [O iii] and Hβ lines.
  The two modules yield consistent results with a mean offset and standard deviation
  of Δz = 0.0028 ± 0.0073 (Δv = 9.3 ± 24 km s−1).\r\n\r\nDownload figure:\r\n\r\nStandard
  image\r\nHigh-resolution image\r\n3.2. Galaxy Stellar Mass, Star formation Rate,
  Halo Mass\r\nTo estimate galaxy stellar masses and star formation rates (SFRs),
  we follow the procedure of J. Matthee et al. (2022). We first measure the [O iii]
  and Hβ emission-line fluxes of each galaxy, and combine these with JWST/NIRCam broadband
  photometry (F115W, F200W, and F356W) to perform spectral energy distribution fitting
  at the galaxy redshift using the Prospector code (B. D. Johnson et al. 2021). We
  assume a G. Chabrier (2003) initial mass function (IMF), adopt MIST isochrones (J.
  Choi et al. 2016; A. Dotter 2016), a nonparametric star formation history model
  (R. P. Naidu et al. 2024), and the dust attenuation curve of D. Calzetti et al.
  (2000). Galaxy SFRs are derived by averaging over the most recent 50 Myr of star
  formation history from the Prospector posteriors.\r\n\r\nFigure 2 (left) shows the
  impact parameter distribution of the 40 EIGER galaxies relative to the background
  quasars (black star symbols). The galaxies are randomly distributed with respect
  to the quasar sight lines. The right panel shows their stellar masses and SFRs,
  with symbols color coded by galaxy redshift. Following R. Bordoloi et al. (2024),
  we estimate halo masses and virial radii (Rvir) using abundance matching from P.
  Behroozi et al. (2019). Uncertainties in Rvir are propagated from the 16th and 84th
  percentile stellar mass errors, giving a mean uncertainty of ΔRvir = 1.8 kpc. The
  galaxies span stellar masses of and SFRs of , with all systems being star-forming
  by selection.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 2. Properties of
  40 spectroscopically confirmed galaxies at 5.9 ≤ z ≤ 6.4 within 300 kpc of background
  quasars in the EIGER survey. Each square denotes a galaxy and is color coded by
  redshift. Left: angular positions and impact parameters relative to the background
  quasar (black star), with dashed concentric rings marking 100, 200, and 300 kpc
  at z = 6. Right: stellar mass vs. SFR, averaged over the last 50 Myr. Error bars
  show the 16th–84th percentile uncertainties in stellar mass and SFR.\r\n\r\nDownload
  figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nOne galaxy (z = 5.910384,
  galaxyID = 15362, qsoID = J159) has an exceptionally high stellar mass of , beyond
  the calibrated range of the P. Behroozi et al. (2019) relation. This object exhibits
  a compact, pointlike morphology and likely hosts an obscured AGN, placing it among
  the recently identified population of little red dots (LRDs; e.g., J. Matthee et
  al. 2024). We do not detect broad Hβ for this object. However, this is not unexpected,
  as LRDs can have Hα/Hβ values as high as ∼10 (M. Brooks et al. (2025; A. Torralba
  et al. 2026, in preparation). As robust AGN modeling at these redshifts is not yet
  established, we estimated its halo mass by linearly extrapolating the P. Behroozi
  et al. (2019) relation from the stable stellar mass regime. We explicitly note where
  this assumption may affect our results in the following sections. Additionally,
  this galaxy has not been plotted in the right panel of 2.\r\n\r\n3.3. Galaxy Overdensities\r\nA
  significant fraction of z ≥ 6 galaxies in the EIGER survey are not isolated but
  are found in overdense environments, either as mergers or members of “protogroups”
  (see, e.g., D. Kashino et al. 2026). The EIGER [O iii] galaxy catalog already merges
  individual [O iii] emission clumps within 2″ into a single system, even when they
  exhibit complex morphologies or merger signatures. To identify larger-scale overdensities,
  we therefore search for galaxies that lie at similar redshifts but are widely separated
  on the sky.\r\n\r\nWithin 300 kpc from the QSO sight lines, we identify overdensities
  around the 40 selected EIGER galaxies using a friends-of-friends algorithm (R. Bordoloi
  et al. 2025). Galaxies are grouped as an overdensity if they lie within 1 pMpc in
  projected separation and within ±1000 km s−1 in redshift space. A galaxy is considered
  part of an overdensity only if all members are “fully” connected, i.e., each galaxy
  in the overdensity satisfies these conditions with all other members. Around each
  detected O i absorption system, we further search for overdensities within ±1500
  km s−1 of the absorber redshift, and merge these associations to ensure all clustered
  galaxies are treated as a single overdensity. This conservative approach ensures
  that we capture the full galaxy environment of O i absorbers. The 40 galaxies studied
  in this work are part of 15 distinct overdensities, with each grouping containing
  1–5 members. The number of galaxies in each grouping is reported in Table 1. The
  typical velocity dispersion of these overdensities is 449.2 km s−1.\r\n\r\nTable
  1. O i Absorption Lines and Associated Galaxy Properties\r\n\r\nLabel\tQuasar\tzgala\tR\t〈v〉b\t#c\tzO
  I\t\t\t\t\t\r\n \t \t \t(kpc)\t(km s−1)\tGalaxies\t \t(cm−2)\t(cm−2)\t(cm−2)\t(cm−2)\t(cm−2)\r\n(1)\t(2)\t(3)\t(4)\t(5)\t(6)\t(7)\t(8)\t(9)\t(10)\t(11)\t(12)\r\na\tJ0100\t5.941\t119.6\t157\t5\t5.945\t\t\t\t\t\r\nb\tJ1148\t6.008\t157.5\t130\t3\t6.011\t\td\t\t\t\r\nc\tJ159\t5.934\t25.2\t−920\t5\t5.913\t\t\t\t⋯\t⋯\r\nd\tJ159\t6.049\t40.8\t230\t2\t6.054\t\t<13.12\t\t⋯\t⋯\r\ne\tJ1030\t6.075\t147.9\t−131\t2\t6.076\te\t\t\t⋯\t⋯\r\nNotes.
  The galaxies listed are the primary members of groups with detections at the lowest
  impact parameter from the host quasar. aRedshift of the primary member of the overdensity.
  bVelocity offset of O i relative to the primary member galaxy of the overdensity.
  cNumber of galaxy members in the overdensity. dFor this system, Si II λ1304 was
  not present, so the value given here is derived from fitting Si II λ1526. eThis
  system is blended; see discussion in Section 3.4.\r\n\r\nDownload table as: \r\nASCII\r\nTypeset
  image\r\n\r\nThroughout this work, we define the galaxy with the smallest impact
  parameter to the background quasar sight line within each galaxy overdensity as
  the primary member. This convention is adopted solely to simplify the presentation
  and does not imply a unique physical association between the intervening absorption
  system and this galaxy. In fact, the concept of a unique absorber–galaxy association
  at high redshift is significantly less robust than in the low-redshift Universe
  (e.g., R. Bordoloi et al. 2024). As discussed in Section 4.1, none of the O i absorption
  systems lie within the virial radius of any individual halo. Even at low redshift,
  the galaxy with the smallest impact parameter is not necessarily the one with the
  smallest velocity offset from the absorber, and therefore does not constitute evidence
  for a unique absorber–galaxy pair (A. Hamanowicz et al. 2020). This behavior is
  also observed for galaxies residing in groups (R. Bordoloi et al. 2011). Our analysis,
  therefore, focuses on the broader environment, which we argue is most appropriately
  characterized by galaxy overdensities, and our choice of a primary galaxy does not
  affect our main conclusions.\r\n\r\n3.4. Absorption-line Detection and Measurements\r\nWe
  follow the procedures outlined in R. Bordoloi et al. (2024) to identify and measure
  the strength of O i absorption systems around EIGER galaxies, and provide a brief
  summary here. We first use a custom Python-based 1D spectrum viewer to identify
  and tabulate all intervening absorption lines in the EIGER quasar spectra. A semiautomated
  CGM absorption-line analysis pipeline is then used to perform the measurements.
  For each galaxy, we extract a ±1500 km s−1 spectral window centered on its systemic
  redshift, for all transitions of interest. In this work, we analyze slices around
  O i λ1302, Si ii λ1260, Si ii λ1304, Si ii λ1527, C ii λ1334, Si iv λ1393, Si iv
  λ1402, C iv λ1548, and C iv λ1550. Each slice is locally continuum-normalized using
  an automated Legendre polynomial fit, with the polynomial order chosen via the Bayesian
  Information Criterion. The continuum fits and absorption features are visually inspected,
  and both rest-frame equivalent widths (Wr) and apparent optical depth (AOD) column
  densities are measured. We define a detection as any absorption system with Wr ≥
  3σw, where σw is the 1σ uncertainty in Wr. We note that this uncertainty contains
  both the statistical uncertainty due to the signal-to-noise ratio of the data and
  the continuum-fitting uncertainty. Nondetections are reported as 2σw upper limits
  measured within ±100 km s−1 of the systemic redshift of the galaxy. For column density,
  we report the 2σ uncertainty on AOD column density as an upper limit on nondetections.
  When a transition is detected in multiple instruments, each spectrum is analyzed
  independently, and the inverse-variance-weighted mean is adopted as the final Wr.
  The details of this automated approach and full documentation of the APIs used can
  be found in R. Bordoloi et al. (2025).\r\n\r\nFor all detections, we perform Voigt
  profile fitting using the rbvfit package, which employs Markov Chain Monte Carlo
  (MCMC) sampling to simultaneously fit multiple absorption systems across different
  instruments (R. Bordoloi & J. Higginson 2025). This approach yields robust column
  densities, resolves the kinematic structure, and enables accurate modeling of blended
  lines. Additionally, since we obtain a marginalized posterior distribution for the
  fitted parameters, the results yield accurate column density estimates even if the
  Doppler b parameter or velocity centroids are not well constrained in moderate-resolution
  spectra (see discussion in R. Bordoloi et al. 2024). In our case, most of the O
  i Si ii C ii transitions are all covered by higher-resolution HIRES spectroscopy
  and thus their properties are well constrained. rbvfit supports two MCMC samplers,
  emcee (D. Foreman-Mackey et al. 2013) and zeus (M. Karamanis et al. 2021; M. Karamanis
  & F. Beutler 2020), both of which are used in this work depending on the complexity
  of the fit. We typically adopt 50 walkers with initial perturbations of either 10−3
  or 10−6, and default chain lengths of 8000–20,000 steps, ensuring the total number
  of steps exceeds 50 times the autocorrelation time. Additional steps are run as
  needed to achieve convergence. In each case, a flat prior is assumed with reasonable
  physical bounds.\r\n\r\nFigure 3 shows an example of Voigt profile fits to O i λ1302
  and Si ii λ1304 lines simultaneously modeled across FIRE, X-shooter, and HIRES.
  We fit a two-component Voigt profile with a mean velocity offset from the host galaxy
  of voffset =  157 km s−1 . This joint fitting maximizes information from all instruments
  while preserving the kinematic detail provided by higher-resolution data. Galaxy
  overdensities associated with this system are marked with green vertical ticks.
  This system has a total O i column density 13.46. All other O i fits are presented
  in Figure 8. All absorption-line measurements are presented in Table 1.\r\n\r\nZoom
  InZoom OutReset image size\r\nFigure 3. Voigt profile fits to O i and Si ii absorption
  profiles at z = 5.945 toward the quasar SDSS J0100+2802. Shown are the flux (black),
  error spectrum (red), best-fit Voigt model (orange/black), and individual Voigt
  components (thin blue), using data from FIRE, X-shooter, and HIRES. Vertical green
  lines mark galaxy members of the associated overdensity. Spectra from all instruments
  and all transitions are simultaneously fit using the rbvfit Bayesian absorption-line
  fitter.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nWe
  note that an O i and Si ii absorption system is detected along the J1030 quasar
  sight line at z ∼ 6.075, blended with an intervening C iv absorber at z ∼ 4.948
  (Figure 8, top left panels; see also C. G. Díaz et al. 2021). The z ∼ 6.076 system
  is confirmed by the independent detection of Si ii, Mg ii, C ii, and Fe ii absorption
  in FIRE and X-shooter data, and we simultaneously fit the C iv, O i, and Si ii systems
  across three instruments. Although the proximity of the C iv doublet in wavelength
  space introduces an inherent degeneracy with the O i and Si ii pair, high-resolution
  HIRES data reveal sufficient kinematic substructure to warrant an additional component
  at a mean velocity offset of voffset = –85.4 km s−1. We interpret this component
  as O i, supported by the aforementioned coincident detections. To constrain the
  system, we use the secondary lines to fix the velocity centroid of the O i component
  and perform simultaneous Voigt profile fitting across all three instruments, including
  both C iv transitions and single-component O i and Si ii models. The column density
  reported in this work corresponds to this singular O i component, and the system
  is marked with an asterisk in Table 1.\r\n\r\n3.5. O i Absorption Detection Completeness\r\nWe
  quantify the completeness of O i absorption detection around each galaxy as follows.
  For each galaxy overdensity, we compute the detection sensitivity on a pixel-by-pixel
  basis following the general framework of, e.g., K. M. Lanzetta et al. (1987), M.
  L. Bernet et al. (2010), and N. L. Mathes et al. (2017). In particular, we use a
  continuum-normalized spectral slice of ±1500 km s−1 centered on the expected O i
  absorption at the redshift of each galaxy overdensity.\r\n\r\nWe define the completeness
  in O i absorption detection in a single instrument as\r\n\r\nwhere H is the Heaviside
  step function, and is the equivalent-width cutoff at which completeness is defined.
  We adopt Å to facilitate comparison with the literature (see Section 4.2). Nσ is
  the detection threshold, which we set to Nσ = 3 by convention. The equivalent-width
  error, σEW(z), is given by\r\n\r\nwhere Δλj is the wavelength spacing between adjacent
  pixels (set by the spectrograph), and npix is the number of pixels over which the
  equivalent width is computed. We adopt the typical width of an O i absorber as npix
  for our analysis, yielding npix, X-shooter = 10, npix, HIRES = 50, and npix, FIRE
  = 11, respectively. This is a conservative approach to calculating completeness,
  as the typical width of the absorbers is larger than the resolving power of the
  instruments. We neglect continuum-fitting errors, so σEW(z) reflects only statistical
  uncertainties from the spectra. Any chip gaps or sky lines are masked. σI and Ic
  are the flux uncertainty and continuum levels of the spectrum.\r\n\r\nFor galaxy
  overdensities observed with multiple spectrographs, we define the combined completeness
  as requiring detection in at least one instrument across the relevant wavelength
  range. For example, with three or more instruments available,\r\n\r\nwhere the logical
  OR (∨) runs over all instruments i ∈ X-shooter, FIRE, HIRES. We then compute the
  mean completeness for each overdensity, and obtain the overall mean completeness,
  , by averaging over all overdensities weighted by their wavelength coverage. This
  yields a mean completeness of 91.4% for O i absorption around galaxy overdensities
  in the EIGER survey for 0.05 Å.\r\n\r\n4. Results\r\nIn this section, we present
  the variation of O i absorption around z ∼ 6 galaxies, the incidence of O i absorption
  per comoving path length that is due to O i absorption around galaxies, and the
  chemical abundance of these systems.\r\n\r\n4.1. Variation of O i Absorption around
  Galaxies\r\nSince all 40 galaxies in our sample reside within 15 identified overdensities
  (Section 3.3), we investigate whether O i absorption is preferentially detected
  in these environments. For clarity, we show the primary galaxy in each overdensity
  (as defined in Section 3.3) when presenting the radial distribution of O i absorption.
  Out of the 15 overdensities, 5 show associated O i absorption.\r\n\r\nFigure 4 shows
  the 2D spatial distribution of galaxies around these five detected systems, with
  the size depicting the virial radii of the galaxies. The galaxies are randomly distributed
  around the absorbers, and we do not find correlations with stellar mass, star formation,
  or other galaxy properties. In all five cases where we have O i detection, the galaxy
  member with the minimum impact parameter is also the member with the lowest R/Rvir.\r\n\r\nZoom
  InZoom OutReset image size\r\nFigure 4. Galaxy overdensities around z ∼ 6 O i absorbers
  in the EIGER survey. Each panel shows the background quasar (red star) at the center,
  with foreground galaxies associated with O i absorption marked as circles. Circles
  are color coded by the velocity offset between the galaxy and the O i absorber,
  and circle sizes are scaled to their virial radii. Only galaxies within 300 kpc
  of the quasar are shown, highlighting the overdensities nearest the absorbers. Dashed
  circles denote projected impact parameters of 50, 100, 200, and 300 pkpc from the
  quasar.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nFigure
  5 presents 1D the radial profiles around the primary galaxies in these systems.
  The marker size indicates the number of member galaxies in each overdensity, while
  the color encodes the velocity offset from the corresponding O i absorption. Panels
  (a) and (c) show impact parameter (R), and panels (b) and (d) show the same distribution
  normalized by the halo virial radius (R/Rvir).\r\n\r\nZoom InZoom OutReset image
  size\r\nFigure 5. Radial absorption profiles of O i absorption at z ∼ 6. Each point
  marks the impact parameter to the nearest galaxy in a galaxy overdensity, with all
  detected O i absorption arising in such environments. Overdensities with O i absorption
  are shown as circles, while nondetections (2σ limits) are indicated by downward
  arrows. Points are color coded by the velocity offset between the galaxy redshift
  and the O i absorber, and their size scales with the number of members in the overdensity.
  The mean uncertainty on the virial radius is ΔRvir = 1.81 kpc. Top panels: rest-frame
  equivalent width vs. impact parameter (R, left) and normalized impact parameter
  (R/Rvir, right). Bottom panels: same as above, but for O i column densities.\r\n\r\nDownload
  figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nMost of the O i detections
  occur within R ≲ 175 kpc of the primary galaxy, corresponding to an incidence rate
  of , estimated using 68% Wilson score confidence intervals. Within 100 kpc, the
  incidence is , increasing to for R ≤ 50 kpc. Conversely, at R  >  150 kpc, an incidence
  of is measured. Within 300 kpc of the primary galaxy, the overall incidence is ,
  with values of for 50 ≤ R ≤ 300 kpc and for 100 ≤ R ≤ 300 kpc. These rates are substantially
  weaker than the incidence of strong Mg ii absorption at z ∼ 6 (R. Bordoloi et al.
  2024), indicating that neutral oxygen preferentially traces a different phase of
  the circumgalactic environment.\r\n\r\nPanels (b) and (d) reveal that O i absorbers
  are typically located at much larger R/Rvir than strong low-ionization tracers such
  as Mg ii. This distinction suggests that O i absorption at z ∼ 6 is not confined
  to the CGM of an individual galaxy but instead reflects the larger-scale gaseous
  environment of galaxy overdensities—what might be described as “cosmic ecosystems”
  rather than isolated halos.\r\n\r\nComparing the stellar mass distributions of overdensities
  with and without O i absorption, we find no statistically significant differences.
  The mean stellar mass of galaxies in overdensities with absorption is , compared
  to for those without.\r\n\r\nWe emphasize that at z ∼ 6, the large R/Rvir values
  of these halos imply that O i absorption typically arises at scales well beyond
  the typical CGM [R/Rvir ≲ 1] (J. Tumlinson et al. 2017) probed by low-ionization
  lines at lower redshift. Unlike the low-z CGM, where metal absorbers are closely
  tied to the halo of a single massive galaxy, the O i absorbers studied here appear
  to be linked to extended networks of low-mass, young galaxies embedded in shared
  overdensities. Over cosmic time, these small systems and their diffuse gaseous environments
  are expected to merge and evolve into more massive systems, eventually forming Milky
  Way–like galaxies by z = 0. Thus, neutral O i at reionization is best understood
  not as a tracer of isolated galactic halos, but as a probe of the extended environments
  that connect galaxies, gas, and structure growth in the early Universe.\r\n\r\nBecause
  O i absorption traces dense, neutral gas and requires only minimal ionization corrections,
  we can place a conservative lower limit on the total oxygen mass associated with
  the EIGER galaxies. These estimates are intended as simple, order-of-magnitude calculations
  to provide intuition about the amount of neutral oxygen relative to the observed
  galaxy properties. Following the formalism of R. Bordoloi et al. (2014), the oxygen
  mass contained in an annulus bounded by Rin and Rout is\r\n\r\nwhere Rin and Rout
  are the inner and outer radii of the annulus, fc is the covering fraction (the incidence
  of O i detections in that bin), 〈NOI〉 is the mean O i column density in the annulus,
  and mO = 16 mp is the mass of an oxygen atom, with mp being the mass of a proton.
  For a conservative lower limit, we adopt fion = 1, where fion is the ionization
  fraction (i.e., we assume that all of the oxygen mass is in the neutral phase).
  We justify this assumption as follows: O i is tightly coupled to H i through charge
  exchange, and in dense gas, the required ionization correction is minor, even under
  strong radiation fields such as the Fermi Bubbles (R. Bordoloi et al. 2017; T. Ashley
  et al. 2022). Under a typical metagalactic UV background, it is generally less than
  10% and does not significantly alter the inferred oxygen abundance. In addition,
  oxygen does not deplete onto dust grains, unlike Si or C. For these reasons, we
  consider the approximation NO,total ≈ NOI to be valid for our analysis.\r\n\r\nWe
  compute masses in two radial bins: 0–100 kpc and 100–300 kpc, respectively. The
  total oxygen mass within radius is obtained by summing the masses of the constituent
  annuli. This yields a strict lower limit of  ≳  2 ×106M⊙ on the total oxygen mass
  within = 300 kpc.\r\n\r\nWe compare the inferred oxygen mass in the extended environment
  of our sample with the total oxygen content in the interstellar medium (ISM) of
  a typical z ∼ 6 galaxy. In computing this quantity, we make the following assumptions.
  First, we assume that all galaxies in this work lie on the typical z ∼ 6 mass–metallicity
  relation, derived by stacking [O iii] emitter galaxies (J. Matthee et al. 2022),
  and we adopt the gas-phase metallicity from this relation for each galaxy.\r\n\r\nBecause
  direct measurements of the total H2 and H i gas content are not available at these
  redshifts, we extrapolate the molecular gas fraction from L. J. Tacconi et al. (2018)
  to z ∼ 6 and adopt a conservative H i gas fraction based on local observations (S.
  Huang et al. 2012). We note that high-z galaxies are likely more gas-rich than their
  local counterparts; therefore, the inferred ISM gas masses should be considered
  lower limits.\r\n\r\nWith these caveats in mind, we estimate the total ISM oxygen
  mass as\r\n\r\nwhere we define . Here, XO is the gas-phase oxygen abundance derived
  from the mass–metallicity relation, and and MHI are the molecular and atomic gas
  masses derived as described above. For our galaxy sample, the mean stellar mass
  is , corresponding to an ISM oxygen mass of MO,ISM  ≳  6.8 × 105 M⊙. Remarkably,
  this indicates that the typical ISM oxygen content is comparable to the oxygen mass
  in the extended environment around these galaxies, implying that the circumgalactic
  or intergalactic medium at z ∼ 6 contains a substantial reservoir of oxygen. While
  these estimates depend on several specific assumptions, the inferred ISM and CGM
  oxygen masses appear to be of similar magnitude.\r\n\r\nAt low redshift, both L*
  and sub-L* galaxies similarly exhibit substantial metal content in their circumgalactic
  medium (CGM), with the CGM containing at least as much metal as the ISM of their
  host galaxies (J. Tumlinson et al. 2011; R. Bordoloi et al. 2014). A key difference
  is that, whereas the low-z CGM is typically gravitationally bound to its host galaxy,
  at high redshift much of the gas exists in the extended environment of galaxy overdensities
  rather than being bound to individual galaxies (see also R. Bordoloi et al. 2024).\r\n\r\n4.2.
  Expected Incidence of O i Absorbers\r\nIn this section, we report the expected redshift-path
  incidence of O i absorbers around [O iii] emitting galaxies detected in the EIGER
  survey. We define the number of O i absorbers associated with each galaxy overdensity
  per unit absorption distance above a detection threshold (WOI ≥ 0.05Å ) as\r\n\r\n\r\nHere,
  Rmax = 300 kpc is the survey radius adopted in this work, and is the mean O i absorber
  detection completeness (see Section 3.5; 91.4% for WOI ≥ 0.05 Å). nOD is defined
  as\r\n\r\n\r\nngal is the number density of [O iii] emitting galaxies per unit comoving
  volume, estimated from the [O iii] luminosity function at z ∼ 6. And 〈overdensity
  size〉 is simply the mean number of galaxies in each galaxy overdensity empirically
  measured to be 〈overdensity size〉 = 2.67. fc is the O i absorption covering fraction
  within 300 kpc for WOI ≥ 0.05 Å (). (The covering fraction within 300 kpc is independent
  of the definition of the primary member.)\r\n\r\nTo estimate the number density
  of galaxies per unit comoving volume (ngal), we integrate the z ∼ 6 [O iii] luminosity
  function derived from the EIGER survey, with a minimum luminosity of Lmin = 1042.2
  ergs−1 (J. Matthee et al. 2022):\r\n\r\n\r\nwhere Φ(L) is the [O iii] luminosity
  function defined as\r\n\r\n\r\nHere, Φ* is the characteristic number density, L*
  is the characteristic luminosity, and α is the faint-end slope. We adopt Φ* = 10−4.02
  Mpc−3, L* = 1043.33 ergs−1, and α = −1.92, values derived from detailed completeness
  calculations of the EIGER [O iii]-emitting galaxies (R. Mackenzie et al. 2026, in
  preparation). This results in ngal = 8.586 × 10−04 Mpc−3. Using these values in
  Equation (6) yields , for O i absorption around galaxies at a mean galaxy redshift
  of 6.001.\r\n\r\nAll calculations in this section are performed with a detection
  threshold of WOI > 0.05Å, since the survey is highly complete down to this equivalent-width
  limit and because most of the literature surveys we compare against adopt the same
  threshold.\r\n\r\nWe emphasize that this approach differs from blind QSO absorption-line
  surveys (e.g., G. D. Becker et al. 2006; L. Christensen et al. 2023; A. M. Sebastian
  et al. 2024; A. Sodini et al. 2024), where all O i absorption-line systems along
  the full quasar redshift path are counted to compute dN/dX directly, under the assumption
  that the absorber cross section is contributed by all galaxies. In contrast, our
  method begins by defining the absorber cross section around galaxy overdensities
  and then estimating the corresponding contribution to dN/dX from the galaxy overdensities
  under study. Comparing these two approaches constrains the fraction of O i (or other
  metal) absorption systems that arise in the extended halos of these galaxies. Figure
  6 shows these literature measurements as colored circles, while the contribution
  to dN/dX around z ∼ 6 galaxy overdensities is indicated by an orange square. To
  quantify the relative contribution of galaxy overdensities, we fit a single power
  law to all literature values at z  >  4 (blue dashed line with shaded region). Comparing
  the dN/dX inferred from quasar absorption-line surveys at z ∼ 6 to our measured
  value, we find that O i dN/dX around z ∼ 6 EIGER galaxy environments account for
  35% ± 16% of all O i absorption-line systems detected in blind quasar surveys. This
  implies that [O iii] emitting galaxy environments at z ∼ 6 contribute roughly one-third
  of the O i absorption systems at that epoch. Although the EIGER QSOs were selected
  to have known absorption systems along their sight lines, the EIGER galaxy survey
  around these sight lines is highly complete and independent of this selection. Therefore,
  we can create an unbiased measurement of the absorption cross section (dN/dX) around
  these galaxy overdensities. We justify this comparison to blind absorption surveys
  in Section 2.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Incidence of O
  i absorbers per comoving path length, dN/dX. Values are derived from all O i absorption
  lines along high-z quasar sight lines. Literature measurements are shown from G.
  D. Becker et al. (2019; blue circles), L. Christensen et al. (2023; purple circles),
  and A. M. Sebastian et al. (2024; red circles). The blue dashed line shows a power-law
  fit to the z  > 4 literature data, with the shaded region marking the 1σ uncertainty.
  The orange square gives the inferred dN/dX when including only O i absorption associated
  with host galaxies (see Section 4.2), indicating that only ∼35% of O i absorbers
  at z ∼ 6 arise in galaxy environments.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution
  image\r\nThis in turn suggests that ∼65% of the O i absorption systems detected
  along quasar sight lines at the epoch of reionization are not associated with [O
  iii] emitter galaxy overdensities. Either the bulk of O i absorption resides in
  isolated pockets of neutral IGM gas outside extended galaxy halos, or it is contributed
  by even lower-luminosity, less massive galaxies () that fall below the EIGER detection
  limits. Such systems may also be detected in galaxy halos that are oxygen-poor or
  lack strong [O iii] emission features, since our galaxy identifications primarily
  rely on [O iii] and Hβ emission lines.\r\n\r\nSimulations suggest that O i absorption
  should primarily arise in galactic halos rather than in the diffuse IGM, since metals
  are not widely distributed and ionization fronts propagate more quickly than metals
  (B. D. Oppenheimer et al. 2009; K. Finlator et al. 2013). Very low-mass protogalaxies
  forming their first stars may blur the boundary between IGM and CGM, enriching their
  surroundings with metals, especially if their star formation is bursty and prolific.
  If sufficiently numerous, such systems could contribute a nonnegligible fraction
  of oxygen in the early Universe.\r\n\r\nRecent observations support this possibility.
  K. Nakajima et al. (2025) reported a strongly lensed (μ = 98) galaxy at z ≈ 6.6
  with a stellar mass upper limit of only ∼2700 M⊙ and a dynamical mass ∼100 times
  larger. The source shows emission and may be dominated by Population III stars.
  This provides direct evidence of oxygen production in extremely low-mass systems.
  A population of such ultralow-mass dwarf galaxies could plausibly account for the
  ∼65% of O i absorbers detected along quasar sight lines that are not associated
  with galaxies in our survey. Our sensitivity limit of (J. Matthee et al. 2022) means
  such dwarfs remain undetected. However, these galaxies may lack a dense enough CGM
  to shield neutral O i from the UV background; thus, even if they produce oxygen,
  neutral O i may not survive (K. Finlator et al. 2013). Interestingly, simulations
  by S. Kušmić et al. (2024) showed that the contribution of metal ions, including
  O i, is only weakly correlated with the stellar mass of the galaxy, and the contribution
  is indistinguishable when comparing across galaxy luminosities. Additionally, they
  argue that due to the steep slope of the stellar mass function, lower-mass, lower-luminosity
  galaxies contribute the majority of absorbing metal ions in the CGM and IGM.\r\n\r\nLater
  simulation works by C. Doughty et al. (2018); C. Doughty & K. Finlator (2019) suggest
  that as the Epoch of Reionization continues, O i will reduce overall but be preferentially
  found in higher column density regions close to halos, as they have a better ability
  to self-shield from ionizing photons. In fact, C. Doughty & K. Finlator (2019) found
  that at z = 6 the majority of O i mass was located in the ISM of galaxies and only
  ∼30% of O i mass was found in the CGM and IGM. In contrast, in this work, we find
  that a substantial (comparable to ISM mass) oxygen mass exists outside galaxies;
  however, we stress that our mass measurements are order-of-magnitude estimates.
  A more direct comparison between these simulations and this work is the covering
  fraction. They report ∼5%–25% covering fraction at z = 6 for O i with out to 102
  pkpc. In the EIGER survey, we report a covering fraction using a minimum threshold
  of WOI ≥ 0.05 Å (or approximately logNOI > 13.7 cm−2) out to 300 kpc. Given the
  large measurement uncertainties and different definitions of associated galaxies,
  the covering fractions are qualitatively consistent between the two works.\r\n\r\nThe
  simulations of K. Finlator et al. (2013) suggest that O i absorbers with are most
  likely associated with halos of mass ∼109 M⊙, where self-shielding is efficient.
  They further predict that only ∼13% of all O i absorption systems should reside
  in halos of 1010–1011.5 M⊙, the mass range of galaxies probed in this work. By contrast,
  we measure a higher dN/dX of ∼35%, but qualitatively our results remain consistent
  with the idea that roughly two-thirds of O i absorbers are associated with undetected
  ∼109 M⊙ halos. Future observations targeting lower-luminosity galaxies and higher
  redshifts will be essential to test these predictions.\r\n\r\nAfter the initial
  posting of this manuscript, G. Pruto et al. (2026) presented a simulation-based
  study that adopts the observational compilation shown in Figure 6 as a reference
  and explores the corresponding behavior in numerical models. Our minimum Wr threshold
  corresponds to ; therefore, the most appropriate comparison is with their sample.
  Qualitatively, the two sets of results are in agreement. A key distinction lies
  in the definition of galactic environment. We characterize environments in terms
  of galaxy overdensities, which we argue is the most appropriate description of where
  O i absorbers reside at z ≈ 6, whereas G. Pruto et al. (2026) define the CGM based
  on the virial radii of halos with . As a result, a direct quantitative comparison
  is not straightforward. Nevertheless, their inferred dN/dX corresponds to an incidence
  rate of O i absorbers of ∼58% ± 11%, which is consistent with our measurements within
  the uncertainties. This agreement may depend on their tighter constraints on absorber
  location and on the adopted minimum Wr or threshold. G. Pruto et al. (2026) further
  report that ∼80% of O i absorbers with are predicted to lie outside the CGM, also
  in qualitative agreement with our findings.\r\n\r\n4.3. Metal Abundances in O i
  absorber population\r\nIn this section, we examine the relative abundances and metal
  column density ratios of O i absorbers associated with galaxy overdensities, and
  compare them to O i absorbers without any associated galaxies. To enable a fair
  comparison, we restrict our analysis to the six quasar sight lines from the EIGER
  survey and identify all O i absorption systems in the redshift range where an [O
  iii]-emitting galaxy could be detected (5.9 ≤ zOI ≤ zQSO). We detect 10 O i absorption
  systems in total, 5 of which have associated galaxy overdensities (Table 1) and
  5 are without any identified galaxy association.\r\n\r\nWe first compare the ionic
  column density ratios in these two populations. Figure 7 (top panels) shows the
  ratios of NSiII/NOI and NCII/NOI as functions of NOI. Systems located near galaxy
  overdensities (blue squares) systematically show higher Si ii/O i and C ii/O i ratios
  compared to systems without associated overdensities (green crosses). This offset
  could reflect differences in metallicity, or alternatively, the effects of ionization.
  However, since the majority of these O i systems lack detectable high-ionization
  transitions, it is reasonable to assume that neutral oxygen and singly ionized silicon
  and carbon dominate the elemental reservoirs (see also L. Christensen et al. 2023).
  In those cases, the observed ionic ratios provide direct tracers of relative abundances.
  Two exceptions are found along the J0100 and J1148 sight lines, which do exhibit
  Si iv and C iv absorption; for these systems, the degeneracy between chemical composition
  and ionization corrections cannot be resolved. It is plausible that, on average,
  O i absorption found near galaxy overdensities has higher elemental abundance ratios
  as the non-galaxy-associated absorbers either have significantly lower-luminosity
  and less massive galaxies, which would be expected to produce less metal, or there
  are truly no galaxies associated with this population.\r\n\r\nZoom InZoom OutReset
  image size\r\nFigure 7. Top panels: ion column density ratios of Si ii to O i (left)
  and C ii to O i (right) as a function of the detected O i column densities, shown
  in logarithmic units. Absorbers associated with galaxy overdensities (blue squares)
  and those not associated with galaxy overdensities (green crosses) exhibit clear
  variations in their column density ratios. One sight line with no detected Si ii
  absorption is indicated with a downward arrow, where a 2σ upper limit on the column
  density is assumed. Bottom panel: relative abundance ratios [Si/O] vs. [C/O] with
  respect to solar abundance. The background contours show the IMF-weighted abundance
  distributions from Population II and Population III SN models. Orange and pink circles
  indicate abundance ratios predicted by low-metallicity Population II SN models.
  The abundance ratios of several O i absorbers associated with galaxy overdensities
  are consistent with a significant contribution from Population III SNe.\r\n\r\nDownload
  figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nWe next compute the relative
  abundances [Si/O] and [C/O], presented in the bottom panel of Figure 7. These abundances
  are defined as\r\n\r\n\r\nwhere NSi,tot and NC,tot represent the summed ionic column
  densities. For systems with detected high-ionization absorption (C iv or Si iv),
  we include both low- and high-ionization states (NSiII + NSiIV and NCII + NCIV),
  marking these measurements as lower limits (blue upward arrows in the figure) since
  additional undetected ionization states may be present. We note that in the two
  systems (a and b) exhibiting high-ionization absorption (see Table 1), the low-
  and high-ionization absorption components are offset in velocity by Δv = –66 km
  s−1 and –69 km s−1, respectively. These offsets are within ≲1.5 resolution elements
  of the instrument, and therefore we cannot statistically distinguish whether the
  low- and high-ionization components are kinematically distinct. This is suggestive
  of a complex, potentially multiphase gaseous environment in the outskirts of these
  galaxies. For systems without detected high-ionization transitions, we adopt NSiII
  and NCII as the dominant contributions. We assume NO,tot ≈ NOI, as ionization corrections
  for O i are typically very small at high O i column densities (see Section 4.1 for
  discussion). We adopt solar reference abundances of = −1.18 ± 0.05 and (M. Asplund
  et al. 2021).\r\n\r\nFigure 7 (bottom panel) reveals a striking separation between
  O i absorbers associated with galaxy overdensities (blue squares) and those without
  galaxy associations (green crosses). Systems near galaxies are found in the upper
  left of the [Si/O]–[C/O] diagram, with two cases exhibiting high-ionization absorption
  (lower abundance limits, blue arrows), which will offset them even farther from
  the locus of nongalaxy absorbers.\r\n\r\nWe place these abundance patterns in the
  context of chemical enrichment models from different stellar populations (see also
  L. Christensen et al. 2023). The contours and colored circles in Figure 7 highlight
  predicted [C/O] and [Si/O] yields from representative Population II and Population
  III supernova (SN) models, weighted by a Salpeter IMF. The weighting by number of
  stars predicted by an IMF is done to represent the typical observational relative
  abundance distribution in these models. These are not exhaustive but span the dominant
  theoretical expectations.\r\n\r\nPopulation III pair-instability SNe (PISNe; 140–260M⊙;
  light green contours) predict narrow [C/O] ≃ –0.7 and high [Si/O] values, inconsistent
  with any of our observed systems. Such PISNe are also expected to produce substantial
  amounts of iron-peak elements, leading to elevated Fe/O ratios (J. Tumlinson et
  al. 2004). We will investigate Mg ii and Fe ii absorption associated with z ∼ 6
  galaxies in an upcoming work (J. Higginson et al. 2026, in preparation). Models
  of massive Population III stars (10–100 M⊙) produce both hypernovae (gray contours;
  E > 1052 erg) and standard core-collapse SNe (light blue contours; A. Heger & S.
  E. Woosley 2010), spanning a broader region overlapping some of our measurements.
  We also consider Population II models: low-metallicity core-collapse SNe from M.
  Limongi & A. Chieffi (2018; orange contours, Population II SNe (L18)) occupy −0.25
  ≲ [C/O] ≲ 0.5 and −0.4 ≲ [Si/O] ≲ 0.4, overlapping parts of the Population III range,
  while the C. Kobayashi et al. (2006) yields (pink and orange circles for hypernovae
  and SNe, respectively) tend toward lower [Si/O] and [C/O].\r\n\r\nAgainst these
  predictions, the contrast between the two absorber populations is clear. All nongalaxy
  O i systems (green crosses) fall at the lower left of the diagram, consistent with
  enrichment from both Population II and/or Population III SNe models. This regime
  also overlaps with ultra-metal-poor damped Lyman-α absorbers (DLAs) at z ∼ 3 (−0.5
  ≲ [Si/O] ≲ 0, −0.5 ≲ [C/O] ≲ 0; R. Cooke et al. 2011; R. J. Cooke et al. 2017).
  By contrast, three of the five galaxy-associated absorbers lie well outside both
  the locus of Population II predictions and the locus of ultra-metal-poor DLA relative
  abundances. These systems are best explained if Population III enrichment played
  a major role, suggesting that they may represent a distinct population from ultra-metal-poor
  DLA host galaxies (see also A. Sodini et al. 2024).\r\n\r\nSimilarly, A. Sodini
  et al. (2024) found that the [C/O] and [Si/O] abundance ratios for high-redshift
  O i absorber systems are consistent with significant enrichment from Population
  III, with the majority explained by ≥ 30% contributions. They also find a large
  spread in the implied Population III contribution; several systems require ≥ 60%
  contributions, while others fall significantly below the average. This is a strong
  indication of heterogeneous chemical enrichment by Population III stars during the
  epoch of reionization.\r\n\r\nThe absorber toward J159 at z = 5.91 shows [C/O] =
  0.20, [Si/O] = 0.55 (labeled c), and no evidence of high-ionization absorption.
  These abundance ratios are best explained by contributions from Population III SNe
  or hypernovae. The absorber toward J1030 at z = 6.07 ([C/O] = −0.38, [Si/O] = 0.65,
  labeled e) also shows no high-ionization absorption. The relative abundances in
  these two predominantly neutral systems are therefore quite robust. Interestingly,
  the J1030 system is not reproduced by any single Population II or Population III
  model, suggesting that it may have experienced multiple enrichment episodes, producing
  unusually high [Si/O] coupled with low [C/O].\r\n\r\nTwo cases require special mention.
  The absorber toward J0100 at z = 5.94 shows [C/O] ≥ 0.42 and [Si/O] ≥ 0.67 (labeled
  a), with strong C iv and Si iv absorption. Since these are lower limits, ionization
  corrections (for carbon and silicon) would push this system further upward, strengthening
  the case for Population III contributions. This observation is best explained by
  contributions from Population III hypernovae models. The J1148 absorber at z = 6.01
  shows [C/O] ≥ 0.02 and [Si/O] ≥ 0.20 (labeled b), again with high-ionization lines;
  correcting for ionization would shift it diagonally upward in the diagram. Taken
  together, four of the five galaxy-associated absorbers show relative abundances
  that cannot be explained by Population II models alone, pointing instead to significant
  enrichment from Population III SNe or hypernovae.\r\n\r\nThus, most galaxy-associated
  O i systems carry signatures of Population III enrichment. These results suggest
  that O i systems tracing galaxy overdensities at z ∼ 6 carry chemical signatures
  of Population III enrichment, likely from multiple SNe events rather than a single
  explosion. The elevated [Si/O] and [C/O] ratios in these environments imply that
  [O iii]—emitting galaxies at this epoch may retain significant Population III contributions,
  and that metal-line absorbers around such overdensities provide a powerful probe
  of the first generations of stars.\r\n\r\n4.4. Comparison to the z ≈ 0 Universe\r\nAt
  z ∼ 6, we cannot directly detect the local environments where O i absorption systems
  arise. However, at z ∼ 0, there are instances where the environments giving rise
  to O i absorption are well understood. Here, we discuss several such instances and
  compare them with z ∼ 6 observations. Such comparisons can provide useful insights
  regarding the nature of local environments within which O i systems exist at high
  z. We focus on O i absorption associated with local blue compact dwarf (BCD) galaxies
  and the Magellanic Stream (MS), owing to their low metallicities and well-characterized
  local environments.\r\n\r\nThere is evidence that O i is found preferentially in
  the H ii regions of local BCDs, with their H i regions being pristine or showing
  very low levels of enrichment (D. Kunth et al. 1994; M. Pettini & K. Lipman 1995;
  T. X. Thuan & Y. I. Izotov 1997). In particular, T. X. Thuan & Y. I. Izotov (1997)
  report that, to varying degrees, low-ionization metal lines (e.g., O i and Si ii)
  reside in the ionized hydrogen regions of BCDs rather than the neutral hydrogen
  regions. They report . Compared to the z ∼ 6 measurements in panel (b) of Figure
  7, the O i column density of the BCD is comparable, but the Si ii-to-O i ratio is
  inconsistent with the z ∼ 6 values. On the other hand, V. Lebouteiller et al. (2004)
  find that the H ii region of the BCD I Zw 36 has significantly higher metallicity
  than its H i region. However, inferred from velocity offsets, O i in that system
  is associated with the H i region. The reported O i column density of that BCD ()
  is approximately 2 orders of magnitude higher than the z ∼ 6 sample. Given the available
  evidence, we conclude that the observed z ∼ 6 O i absorption systems are not similar
  to local BCD systems and are unlikely to originate in H ii regions.\r\n\r\nThe MS
  is a filamentary trail of gas in the Local Group. Multiphase absorption-line observations
  from A. J. Fox et al. (2013) and P. Richter et al. (2013) support the argument that
  the MS was tidally stripped from the Magellanic Clouds approximately 2 Gyr ago.
  Inferences from the abundance ratios of alpha elements in the MS are best explained
  by contributions from massive stars via Type II SNe when the MS was still part of
  the Magellanic Clouds, although the presence of significant dust depletion makes
  further inferences into enrichment history difficult. An additional study of the
  MS (N. Kumari et al. 2015) reports abundance ratios in a compact high-velocity cloud
  (CHVC) that is believed to be associated with the MS. They find [Si/O] = −0.04 ±
  0.25 and [C/O] = −0.09 ± 0.23. When comparing these with the z ∼ 6 observations
  presented in panel (c) of Figure 7, we see that the CHVC abundance ratios occupy
  a different region of parameter space than the z ≈ 6 O i absorbers within identified
  galactic overdensities showing Population III enrichment signatures (points a, c,
  e). This discrepancy provides evidence that these z ∼ 6 O i absorbers with Population
  III enrichment signatures are unlikely to arise in environments similar to the MS.
  However, the ionic ratios of O i absorption systems not associated with galaxy overdensities
  (green crosses) are consistent with this measurement. With the caveat that MS measurements
  do contain dust depletion effects, it is plausible that such O i systems may trace
  IGM structures with densities comparable to those of the MS at high z.\r\n\r\n5.
  Conclusion\r\nWe have conducted a survey of neutral O i absorption systems associated
  with galaxies during the Epoch of Reionization in the EIGER survey, using six high-redshift
  quasars as background sight lines. Our study focuses on the distribution of neutral
  oxygen around -emitting galaxies within 300 kpc and their connection to galaxy overdensities.
  The main results are as follows:\r\n\r\n1.  \r\nFive O i absorbers are detected
  among 15 galaxy overdensities, spanning z = 5.91–6.16 with a mean redshift 〈z〉 =
  6.001.\r\n2.  \r\nThe O i covering fraction within 300 kpc of the closest galaxy
  is , with for R ≤ 50 kpc and for 50 ≤ R ≤ 300 kpc, where the covering fraction is
  calculated using the galaxy in an overdensity with the lowest impact parameter.\r\n3.
  \ \r\nWe find  ≳ 2 × 106 M⊙ of oxygen within 300 kpc, a mass comparable to the ISM
  oxygen content of z ∼ 6 galaxies—assuming minimal ionization correction (see Section
  4.1 for justification)—suggesting that the circumgalactic environment already holds
  metal reservoirs rivaling those inside galaxies.\r\n4.  \r\nO i absorbers are detected
  as far as ∼8 R/Rvir from galaxies, in sharp contrast to low-ionization tracers such
  as Mg ii, which are typically confined within ≲R/Rvir.\r\n5.  \r\nThe incidence
  of galaxy-associated O i absorbers is \r\n \r\n. Comparison with blind quasar absorption-line
  surveys indicates that these systems represent only ∼35% of all O i absorbers at
  z ∼ 6, implying that the majority likely arise in lower-mass galaxies below current
  detection limits or in dense neutral IGM pockets that survived reionization.\r\n6.
  \ \r\nRelative abundance and ionization ratios ([Si/O], [C/O]) show that galaxy-associated
  O i systems are chemically enriched, with signatures in several systems consistent
  with contributions from Population III stars. In particular, we identify four galaxy
  overdensities whose outskirts exhibit absorption-line abundance ratios consistent
  with contributions from Population III nucleosynthesis.\r\n\r\nOverall, these results
  indicate that neutral O i at z ∼ 6 primarily traces extended overdensity environments
  rather than the CGM of individual halos. Moreover, the chemical abundance patterns
  of galaxy-associated O i systems suggest contributions from Population III stars,
  likely arising from multiple SNe events rather than a single explosion. The elevated
  [Si/O] and [C/O] ratios imply that [O iii]-emitting galaxies at this epoch may retain
  significant Population III enrichment. Consequently, metal-line absorbers around
  such overdensities offer a powerful probe of the first generations of stars, providing
  insight into early chemical enrichment and the role of primordial stellar populations
  in shaping galaxy evolution during the Epoch of Reionization.\r\n\r\nAcknowledgments\r\nThis
  work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope.
  The data were obtained from the Mikulski Archive for Space Telescopes at the Space
  Telescope Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These
  observations are associated with program #1243. This paper includes data gathered
  with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This
  work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet
  Science Institute. Data presented herein were obtained at the W. M. Keck Observatory
  from telescope time allocated to the National Aeronautics and Space Administration
  (NASA) through the agency’s scientific partnership with the California Institute
  of Technology and the University of California. The Observatory was made possible
  by the generous financial support of the W. M. Keck Foundation. The JWST data presented
  in this article were obtained from the Mikulski Archive for Space Telescopes (MAST)
  at the Space Telescope Science Institute. The specific observations analyzed can
  be accessed via DOI: 10.17909/y94q-h212. This work was partially supported by the
  National Science Foundation under grant No. AST-2108931. Jorryt Matthee and Ivan
  Kramarenko acknowledge funding from the European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities:
  JWST - James Webb Space Telescope (NIRCam), Magellan: Baade - (FIRE), VLT: Kueyen
  - (X-shooter), and Keck: I - (HIRES, MOSFIRE).\r\n\r\nSoftware: astropy (Astropy
  Collaboration et al. 2013, 2018, 2022), rbcodes (R. Bordoloi et al. 2025), rbvfit
  (R. Bordoloi & J. Higginson 2025)."
article_number: '49'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Jack
  full_name: Higginson, Jack
  last_name: Higginson
- first_name: Rongmon
  full_name: Bordoloi, Rongmon
  last_name: Bordoloi
- first_name: Robert A.
  full_name: Simcoe, Robert A.
  last_name: Simcoe
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Daichi
  full_name: Kashino, Daichi
  last_name: Kashino
- first_name: Ruari
  full_name: Mackenzie, Ruari
  last_name: Mackenzie
- first_name: Ivan
  full_name: Kramarenko, Ivan
  id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
  last_name: Kramarenko
  orcid: 0000-0001-5346-6048
- first_name: Simon J.
  full_name: Lilly, Simon J.
  last_name: Lilly
- first_name: Anna-Christina
  full_name: Eilers, Anna-Christina
  last_name: Eilers
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: Minghao
  full_name: Yue, Minghao
  last_name: Yue
citation:
  ama: Higginson J, Bordoloi R, Simcoe RA, et al. EIGER. VIII. First stars signatures
    in the connection between O I absorption and galaxies in the epoch of reionization.
    <i>The Astrophysical Journal</i>. 2026;999(1). doi:<a href="https://doi.org/10.3847/1538-4357/ae3e81">10.3847/1538-4357/ae3e81</a>
  apa: Higginson, J., Bordoloi, R., Simcoe, R. A., Matthee, J. J., Kashino, D., Mackenzie,
    R., … Yue, M. (2026). EIGER. VIII. First stars signatures in the connection between
    O I absorption and galaxies in the epoch of reionization. <i>The Astrophysical
    Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae3e81">https://doi.org/10.3847/1538-4357/ae3e81</a>
  chicago: Higginson, Jack, Rongmon Bordoloi, Robert A. Simcoe, Jorryt J Matthee,
    Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, et al. “EIGER. VIII. First Stars
    Signatures in the Connection between O I Absorption and Galaxies in the Epoch
    of Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href="https://doi.org/10.3847/1538-4357/ae3e81">https://doi.org/10.3847/1538-4357/ae3e81</a>.
  ieee: J. Higginson <i>et al.</i>, “EIGER. VIII. First stars signatures in the connection
    between O I absorption and galaxies in the epoch of reionization,” <i>The Astrophysical
    Journal</i>, vol. 999, no. 1. IOP Publishing, 2026.
  ista: Higginson J, Bordoloi R, Simcoe RA, Matthee JJ, Kashino D, Mackenzie R, Kramarenko
    I, Lilly SJ, Eilers A-C, Naidu RP, Yue M. 2026. EIGER. VIII. First stars signatures
    in the connection between O I absorption and galaxies in the epoch of reionization.
    The Astrophysical Journal. 999(1), 49.
  mla: Higginson, Jack, et al. “EIGER. VIII. First Stars Signatures in the Connection
    between O I Absorption and Galaxies in the Epoch of Reionization.” <i>The Astrophysical
    Journal</i>, vol. 999, no. 1, 49, IOP Publishing, 2026, doi:<a href="https://doi.org/10.3847/1538-4357/ae3e81">10.3847/1538-4357/ae3e81</a>.
  short: J. Higginson, R. Bordoloi, R.A. Simcoe, J.J. Matthee, D. Kashino, R. Mackenzie,
    I. Kramarenko, S.J. Lilly, A.-C. Eilers, R.P. Naidu, M. Yue, The Astrophysical
    Journal 999 (2026).
date_created: 2026-10-12T12:15:27Z
date_published: 2026-02-24T00:00:00Z
date_updated: 2026-10-14T07:58:57Z
day: '24'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.3847/1538-4357/ae3e81
external_id:
  arxiv:
  - '2510.05220'
file:
- access_level: open_access
  checksum: 1b8caf640c32d0d27a078bfb27ffcf8a
  content_type: application/pdf
  creator: dernst
  date_created: 2026-10-14T07:50:51Z
  date_updated: 2026-10-14T07:50:51Z
  file_id: '23136'
  file_name: 2026_AstrophysicalJour_Higginson.pdf
  file_size: 2808503
  relation: main_file
  success: 1
file_date_updated: 2026-10-14T07:50:51Z
fulldoi: https://doi.org/10.3847/1538-4357/ae3e81
has_accepted_license: '1'
intvolume: '       999'
issue: '1'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: EIGER. VIII. First stars signatures in the connection between O I absorption
  and galaxies in the epoch of reionization
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 999
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '23117'
abstract:
- lang: eng
  text: 'We present a comprehensive analysis of the relationship between galaxies
    and the intergalactic medium (IGM) during the late stages of cosmic reionization,
    based on the complete JWST EIGER dataset. Using deep NIRCam 3.5 μm slitless spectroscopy,
    we construct a sample of 948 [O iii]λ5008-emitting galaxies with −21.4 ≲ MUV ≲
    −17.2 spanning 5.33 < z < 6.97 along six quasar sight lines. We correlate these
    galaxies with Lyα and Lyβ transmission measured from high-resolution quasar spectra
    across multiple redshift intervals. We find clear redshift evolution in the correlation
    between galaxy density and transmission: it is suppressed in overdense regions
    at z < 5.50, while enhanced at 5.70 < z < 6.15. The intermediate range exhibits
    a transitional behavior. Cross-correlation measurements further reveal excess
    absorption within ∼8 cMpc of galaxies at low redshifts, and enhanced transmission
    at intermediate scales (∼5–20 cMpc) at z > 5.70. Statistical tests using mock
    catalogs with realistic galaxy clustering but no correlation with the transmission
    field confirm that the observed correlations are unlikely to arise by chance.
    The evolving signals can be explained by stronger absorption in overdense regions,
    combined with the competing influences of local radiation fields and the rising
    background radiation. While local radiation dominates ionization of the surrounding
    IGM at earlier times, the background becomes increasingly important, eventually
    surpassing the impact of nearby galaxies. These results support an inside-out
    progression of reionization, with ionized regions originating around clustered,
    star-forming galaxies and gradually extending into underdense regions.'
acknowledgement: "We thank Enrico Garaldi, Rahul Kannan, Aaron Smith, and the THESAN
  team for providing us with their simulation data, and Norbert Pirzkal for helpful
  advice on our NIRCam observing program.\r\n\r\nThis work is based on observations
  made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from
  the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-03127 for JWST. These observations were taken under
  GTO program No. 1243. The specific observations analyzed can be accessed via doi:10.17909/6grb-j154.\r\n\r\nThe
  participation of S.J.L. as an Interdisciplinary Scientist in the JWST Flight Science
  Working Group 2002-2022 has been supported by the European Space Agency. His earlier
  involvement in the development of the JWST 1996–2001 was supported by the Canadian
  Space Agency.\r\n\r\nThis work is partially based on observations collected at the
  European Organisation for Astronomical Research in the Southern Hemisphere under
  ESO programmes 084.A-0360(A), 084.A-0390(A), 086.A-0162(A), 086.A-0574(A), 087.A-0607(A),
  089.A-0814(A), 093.A-0707(A), 098.B-0537(A), and 286.A-5025(A). Some of the data
  presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit
  organization operated as a scientific partnership among the California Institute
  of Technology, the University of California, and the National Aeronautics and Space
  Administration. The Observatory was made possible by the generous financial support
  of the W. M. Keck Foundation. This paper includes data gathered with the 6.5 m Magellan
  Telescopes located at Las Campanas Observatory, Chile.\r\n\r\nThis work has been
  supported by JSPS KAKENHI grant No. JP21K13956 (D.K.). J.M. is supported by the
  European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities: JWST - James Webb Space
  Telescope (NIRCam), VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), Magellan:Baade
  - Magellan I Walter Baade Telescope (FIRE), Keck:I - KECK I Telescope (MOSFIRE),
  Keck:II - KECK II Telescope (ESI).\r\n\r\nSoftware: Python, numpy (C. R. Harris
  et al. 2020), scipy (P. Virtanen et al. 2020), Astropy (Astropy Collaboration et
  al. 2013), Matplotlib (J. D. Hunter 2007), PypeIt (J. X. Prochaska et al. 2019)."
article_number: '280'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Daichi
  full_name: Kashino, Daichi
  last_name: Kashino
- first_name: Simon J.
  full_name: Lilly, Simon J.
  last_name: Lilly
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Ruari
  full_name: Mackenzie, Ruari
  last_name: Mackenzie
- first_name: Anna-Christina
  full_name: Eilers, Anna-Christina
  last_name: Eilers
- first_name: Rongmon
  full_name: Bordoloi, Rongmon
  last_name: Bordoloi
- first_name: Robert A.
  full_name: Simcoe, Robert A.
  last_name: Simcoe
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: Minghao
  full_name: Yue, Minghao
  last_name: Yue
- first_name: Bin
  full_name: Liu, Bin
  last_name: Liu
citation:
  ama: Kashino D, Lilly SJ, Matthee JJ, et al. EIGER. VII. The evolving relationship
    between galaxies and the intergalactic medium in the final stages of reionization.
    <i>The Astrophysical Journal</i>. 2026;997(2). doi:<a href="https://doi.org/10.3847/1538-4357/ae2799">10.3847/1538-4357/ae2799</a>
  apa: Kashino, D., Lilly, S. J., Matthee, J. J., Mackenzie, R., Eilers, A.-C., Bordoloi,
    R., … Liu, B. (2026). EIGER. VII. The evolving relationship between galaxies and
    the intergalactic medium in the final stages of reionization. <i>The Astrophysical
    Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae2799">https://doi.org/10.3847/1538-4357/ae2799</a>
  chicago: Kashino, Daichi, Simon J. Lilly, Jorryt J Matthee, Ruari Mackenzie, Anna-Christina
    Eilers, Rongmon Bordoloi, Robert A. Simcoe, Rohan P. Naidu, Minghao Yue, and Bin
    Liu. “EIGER. VII. The Evolving Relationship between Galaxies and the Intergalactic
    Medium in the Final Stages of Reionization.” <i>The Astrophysical Journal</i>.
    IOP Publishing, 2026. <a href="https://doi.org/10.3847/1538-4357/ae2799">https://doi.org/10.3847/1538-4357/ae2799</a>.
  ieee: D. Kashino <i>et al.</i>, “EIGER. VII. The evolving relationship between galaxies
    and the intergalactic medium in the final stages of reionization,” <i>The Astrophysical
    Journal</i>, vol. 997, no. 2. IOP Publishing, 2026.
  ista: Kashino D, Lilly SJ, Matthee JJ, Mackenzie R, Eilers A-C, Bordoloi R, Simcoe
    RA, Naidu RP, Yue M, Liu B. 2026. EIGER. VII. The evolving relationship between
    galaxies and the intergalactic medium in the final stages of reionization. The
    Astrophysical Journal. 997(2), 280.
  mla: Kashino, Daichi, et al. “EIGER. VII. The Evolving Relationship between Galaxies
    and the Intergalactic Medium in the Final Stages of Reionization.” <i>The Astrophysical
    Journal</i>, vol. 997, no. 2, 280, IOP Publishing, 2026, doi:<a href="https://doi.org/10.3847/1538-4357/ae2799">10.3847/1538-4357/ae2799</a>.
  short: D. Kashino, S.J. Lilly, J.J. Matthee, R. Mackenzie, A.-C. Eilers, R. Bordoloi,
    R.A. Simcoe, R.P. Naidu, M. Yue, B. Liu, The Astrophysical Journal 997 (2026).
das_tickbox: '0'
date_created: 2026-10-12T12:17:25Z
date_published: 2026-01-28T00:00:00Z
date_updated: 2026-10-14T08:12:05Z
day: '28'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae2799
external_id:
  arxiv:
  - '2506.03121'
file:
- access_level: open_access
  checksum: c33405da323cac352c0d751f0fe6f021
  content_type: application/pdf
  creator: dernst
  date_created: 2026-10-14T08:09:31Z
  date_updated: 2026-10-14T08:09:31Z
  file_id: '23138'
  file_name: 2026_AstrophysicalJour_Kashino.pdf
  file_size: 11393255
  relation: main_file
  success: 1
file_date_updated: 2026-10-14T08:09:31Z
fulldoi: https://doi.org/10.3847/1538-4357/ae2799
has_accepted_license: '1'
intvolume: '       997'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
researchdata_availability: no
scopus_import: '1'
status: public
supplementarymaterial: yes
title: EIGER. VII. The evolving relationship between galaxies and the intergalactic
  medium in the final stages of reionization
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 997
year: '2026'
...
---
OA_type: closed access
_id: '23096'
abstract:
- lang: eng
  text: The first generation of stars, known as population III (Pop III), formed from
    primordial gas consisting solely of hydrogen and helium and is believed to have
    emerged only a few hundred million years after the Big Bang. Detecting the chemical
    enrichment of metal-poor circumgalactic gas offers a promising way to trace the
    enrichment signature of Pop III stars. Along the sight line to the quasar SDSS
    J0100+2802, a metal absorber at z = 5.945, showing over-abundant carbon and silicon
    compared with solar, has been reported to be consistent with the enrichment pattern
    of Pop III stars. Here, using data recorded by the James Webb Space Telescope,
    we report the discovery of an unusually metal-poor galaxy overdensity of 17 members
    (mean metallicity ~3% of solar) near this metal absorber, which is ~0.4 dex more
    metal-poor than coeval galaxies in similarly overdense environments. This less
    chemically evolved system may have provided favourable conditions for preserving
    the absorption signatures of Pop III enrichment. We infer a minimum dark matter
    halo mass of log(Mh,min/M⊙) = 10.68+0.93 −1.72, supporting late-time Pop III formation
    at the outskirts of atomic hydrogen cooling haloes. Our findings open a promising
    observational pathway to identifying the chemical imprints of the first stars
    and constrain the conditions for their formation.
acknowledgement: This work is based on observations made with the NASA/ESA/CSA JWST,
  associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope,
  associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and
  096.A-0095. We acknowledge the University of Copenhagen for giving this project
  access to the LUMI supercomputer owned by the EuroHPC Joint Undertaking and hosted
  by CSC (Finland) and the LUMI consortium through Denmark. Z.L. thanks Y. Ren for
  helpful discussions. We thank O. Zier, A. Smith, R. Kannan and E. Garaldi for helpful
  discussions about the THESAN-ZOOM simulation. Z.L. acknowledges the fellowship from
  the Cosmic Dawn Center, which is funded by the Danish National Research Foundation
  under grant no. 140. K.K. acknowledges support from the Villum Foundation (71574).
  L.C. is supported by DFF/Independent Research Fund Denmark (2032-00071). V.D. acknowledges
  financial support from the Bando Ricerca Fondamentale INAF 2022 Large Grant XQR-30.
  A.V. acknowledges funding from the Cosmic Frontier Center and the University of
  Texas at Austin’s College of Natural Sciences. S. Zou acknowledges support from
  the Chinese Academy of Sciences (E5295401).
article_processing_charge: No
article_type: original
author:
- first_name: Zihao
  full_name: Li, Zihao
  last_name: Li
- first_name: Koki
  full_name: Kakiichi, Koki
  last_name: Kakiichi
- first_name: Lise
  full_name: Christensen, Lise
  last_name: Christensen
- first_name: Zheng
  full_name: Cai, Zheng
  last_name: Cai
- first_name: Valentina
  full_name: D’Odorico, Valentina
  last_name: D’Odorico
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Daichi
  full_name: Kashino, Daichi
  last_name: Kashino
- first_name: Rongmon
  full_name: Bordoloi, Rongmon
  last_name: Bordoloi
- first_name: Ruari
  full_name: Mackenzie, Ruari
  last_name: Mackenzie
- first_name: Trystyn A.M.
  full_name: Berg, Trystyn A.M.
  last_name: Berg
- first_name: Irene
  full_name: Vanni, Irene
  last_name: Vanni
- first_name: Stefania
  full_name: Salvadori, Stefania
  last_name: Salvadori
- first_name: Alessandra
  full_name: Venditti, Alessandra
  last_name: Venditti
- first_name: Shiwu
  full_name: Zhang, Shiwu
  last_name: Zhang
- first_name: Sarah E.I.
  full_name: Bosman, Sarah E.I.
  last_name: Bosman
- first_name: Eduardo
  full_name: Bañados, Eduardo
  last_name: Bañados
- first_name: Frederick B.
  full_name: Davies, Frederick B.
  last_name: Davies
- first_name: Xiaohui
  full_name: Fan, Xiaohui
  last_name: Fan
- first_name: Hyunsung D.
  full_name: Jun, Hyunsung D.
  last_name: Jun
- first_name: Xiangyu
  full_name: Jin, Xiangyu
  last_name: Jin
- first_name: Mingyu
  full_name: Li, Mingyu
  last_name: Li
- first_name: Sofía
  full_name: Rojas-Ruiz, Sofía
  last_name: Rojas-Ruiz
- first_name: Feige
  full_name: Wang, Feige
  last_name: Wang
- first_name: Jinyi
  full_name: Yang, Jinyi
  last_name: Yang
- first_name: Siwei
  full_name: Zou, Siwei
  last_name: Zou
- first_name: Huanian
  full_name: Zhang, Huanian
  last_name: Zhang
- first_name: Yongda
  full_name: Zhu, Yongda
  last_name: Zhu
citation:
  ama: Li Z, Kakiichi K, Christensen L, et al. First-star imprints in a metal-poor
    galaxy overdensity near the end of reionization. <i>Nature Astronomy</i>. 2026.
    doi:<a href="https://doi.org/10.1038/s41550-026-02993-5">10.1038/s41550-026-02993-5</a>
  apa: Li, Z., Kakiichi, K., Christensen, L., Cai, Z., D’Odorico, V., Matthee, J.
    J., … Zhu, Y. (2026). First-star imprints in a metal-poor galaxy overdensity near
    the end of reionization. <i>Nature Astronomy</i>. Springer Nature. <a href="https://doi.org/10.1038/s41550-026-02993-5">https://doi.org/10.1038/s41550-026-02993-5</a>
  chicago: Li, Zihao, Koki Kakiichi, Lise Christensen, Zheng Cai, Valentina D’Odorico,
    Jorryt J Matthee, Daichi Kashino, et al. “First-Star Imprints in a Metal-Poor
    Galaxy Overdensity near the End of Reionization.” <i>Nature Astronomy</i>. Springer
    Nature, 2026. <a href="https://doi.org/10.1038/s41550-026-02993-5">https://doi.org/10.1038/s41550-026-02993-5</a>.
  ieee: Z. Li <i>et al.</i>, “First-star imprints in a metal-poor galaxy overdensity
    near the end of reionization,” <i>Nature Astronomy</i>. Springer Nature, 2026.
  ista: Li Z, Kakiichi K, Christensen L, Cai Z, D’Odorico V, Matthee JJ, Kashino D,
    Bordoloi R, Mackenzie R, Berg TAM, Vanni I, Salvadori S, Venditti A, Zhang S,
    Bosman SEI, Bañados E, Davies FB, Fan X, Jun HD, Jin X, Li M, Rojas-Ruiz S, Wang
    F, Yang J, Zou S, Zhang H, Zhu Y. 2026. First-star imprints in a metal-poor galaxy
    overdensity near the end of reionization. Nature Astronomy.
  mla: Li, Zihao, et al. “First-Star Imprints in a Metal-Poor Galaxy Overdensity near
    the End of Reionization.” <i>Nature Astronomy</i>, Springer Nature, 2026, doi:<a
    href="https://doi.org/10.1038/s41550-026-02993-5">10.1038/s41550-026-02993-5</a>.
  short: Z. Li, K. Kakiichi, L. Christensen, Z. Cai, V. D’Odorico, J.J. Matthee, D.
    Kashino, R. Bordoloi, R. Mackenzie, T.A.M. Berg, I. Vanni, S. Salvadori, A. Venditti,
    S. Zhang, S.E.I. Bosman, E. Bañados, F.B. Davies, X. Fan, H.D. Jun, X. Jin, M.
    Li, S. Rojas-Ruiz, F. Wang, J. Yang, S. Zou, H. Zhang, Y. Zhu, Nature Astronomy
    (2026).
das_tickbox: '1'
dataavailabilitystatement: This work is based on observations made with the NASA/ESA/CSA
  JWST, associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope
  associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and
  096.A-0095. The JWST data are available via the Mikulski Archive for Space Telescopes
  at http://archive.stsci.edu under JWST programmes GO-2078 (ref. 127) and GO-1243
  (ref. 128). The metal absorber catalogue of XQR-30 is available via GitHub at https://github.com/XQR-30/Metal-catalogue.
  The [O III] emitter catalogue from the EIGER survey is available via GitHub at https://eiger-jwst.github.io/data.html.
  Other data presented in this paper are available upon request to the corresponding
  author.
date_created: 2026-10-11T22:02:07Z
date_published: 2026-09-29T00:00:00Z
date_updated: 2026-10-14T06:42:17Z
day: '29'
department:
- _id: JoMa
doi: 10.1038/s41550-026-02993-5
fulldoi: https://doi.org/10.1038/s41550-026-02993-5
language:
- iso: eng
month: '09'
oa_version: None
publication: Nature Astronomy
publication_identifier:
  eissn:
  - 2397-3366
publication_status: epub_ahead
publisher: Springer Nature
quality_controlled: '1'
researchdata_availability: yes
scopus_import: '1'
status: public
supplementarymaterial: yes
title: First-star imprints in a metal-poor galaxy overdensity near the end of reionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2026'
...
---
OA_place: repository
OA_type: green
_id: '20864'
abstract:
- lang: eng
  text: Studies of the distant Universe are providing key insights into our understanding
    of the formation of galaxies. The advent of the James Webb Space Telescope (JWST)
    has significantly enhanced our observational capabilities, leading to an expanded
    redshift frontier, providing unprecedented detail in the characterisation of early
    galaxies and enabling the discovery of new populations of accreting black holes.
    This review aims to provide an introduction to the basic processes and components
    that shape the observed spectra of galaxies, with a focus on their relevance to
    techniques with which high-redshift galaxies are selected. The review further
    introduces specific topics that have attracted significant attention in recent
    literature, including the discovery of highly efficient galaxy formation in the
    early Universe, the relation between galaxies and the process of reionization,
    new insights into the formation of the first stars and the enrichment of interstellar
    gas with heavy elements, and breakthroughs in our understanding of the origins
    of supermassive black holes.
acknowledgement: I thank Claudia Di Cesare, Edoardo Iani, Gauri Kotiwale and Wendy
  Sun for proofreading, Daichi Kashino, Gauri Kotiwale, Sara Mascia, Benjamín Navarette
  and Joris Witstok for their assistance in preparing some of the Figures, and Richard
  Ellis and Stephen Blundell for constructive comments. Funded by the European Union
  (ERC, AGENTS, 101076224).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: 'Matthee JJ. JWST provides a new view of cosmic dawn: Latest developments in
    studies of early galaxies. <i>Contemporary Physics</i>. 2025;66(1-4):116-151.
    doi:<a href="https://doi.org/10.1080/00107514.2025.2586370">10.1080/00107514.2025.2586370</a>'
  apa: 'Matthee, J. J. (2025). JWST provides a new view of cosmic dawn: Latest developments
    in studies of early galaxies. <i>Contemporary Physics</i>. Taylor &#38; Francis.
    <a href="https://doi.org/10.1080/00107514.2025.2586370">https://doi.org/10.1080/00107514.2025.2586370</a>'
  chicago: 'Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments
    in Studies of Early Galaxies.” <i>Contemporary Physics</i>. Taylor &#38; Francis,
    2025. <a href="https://doi.org/10.1080/00107514.2025.2586370">https://doi.org/10.1080/00107514.2025.2586370</a>.'
  ieee: 'J. J. Matthee, “JWST provides a new view of cosmic dawn: Latest developments
    in studies of early galaxies,” <i>Contemporary Physics</i>, vol. 66, no. 1–4.
    Taylor &#38; Francis, pp. 116–151, 2025.'
  ista: 'Matthee JJ. 2025. JWST provides a new view of cosmic dawn: Latest developments
    in studies of early galaxies. Contemporary Physics. 66(1–4), 116–151.'
  mla: 'Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments
    in Studies of Early Galaxies.” <i>Contemporary Physics</i>, vol. 66, no. 1–4,
    Taylor &#38; Francis, 2025, pp. 116–51, doi:<a href="https://doi.org/10.1080/00107514.2025.2586370">10.1080/00107514.2025.2586370</a>.'
  short: J.J. Matthee, Contemporary Physics 66 (2025) 116–151.
corr_author: '1'
date_created: 2025-12-29T12:05:25Z
date_published: 2025-12-04T00:00:00Z
date_updated: 2026-04-07T08:44:00Z
day: '04'
department:
- _id: JoMa
doi: 10.1080/00107514.2025.2586370
external_id:
  arxiv:
  - '2511.04843'
fulldoi: https://doi.org/10.1080/00107514.2025.2586370
intvolume: '        66'
issue: 1-4
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.2511.04843
month: '12'
oa: 1
oa_version: Preprint
page: 116-151
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: Contemporary Physics
publication_identifier:
  eissn:
  - 1366-5812
  issn:
  - 0010-7514
publication_status: published
publisher: Taylor & Francis
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'JWST provides a new view of cosmic dawn: Latest developments in studies of
  early galaxies'
type: journal_article
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 66
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20932'
abstract:
- lang: eng
  text: Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial
    for understanding the properties of cosmic reionizers because the opacity of the
    intergalactic medium (IGM) prevents the direct detection of LyC emission from
    sources during the Epoch of Reionization (EoR). In this study, we confirm two
    new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute
    escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The
    LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate
    leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue
    UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03
    and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively.
    These two LyC candidate leakers were detected in a catalog of 91 spectroscopically
    confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed
    properties that were proposed as indirect indicators of LyC emission, such as
    Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according
    to these properties, stacked the LyC observations of this subsample, and assessed
    the limits of the escape fractions in the stacks. We aim to enhance our understanding
    of LyC escape mechanisms and improve our predictions of the LyC fesc during the
    EoR by analyzing the individual candidates and the stacks in the context of the
    currently limited sample of known LyC leakers at z ∼ 3.
acknowledgement: 'We acknowledge support from the National Science Foundation of China
  – 12225301, INAF Large grant “Spectroscopic survey with JWST” jand from PRIN 2022
  MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European
  Union – Next Generation EU, and Postgraduate Scholarship Program under the grant
  of China Scholarship Council. P.W. and B.V. acknowledge support from the INAF Mini
  Grant ‘1.05.24.07.01 RSN1: Spatially Resolved Near-IR Emission of Intermediate-Redshift
  Jellyfish Galaxies’ (PI Watson). We acknowledge A. Acebron, C. Grillo, and P. Rosati
  for their fundamental contribution to the strong lensing analysis and results. We
  also extend our gratitude to the JWST and HST teams for their efforts in designing,
  building, and operating these transformative missions.'
article_number: A328
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Y.
  full_name: Liu, Y.
  last_name: Liu
- first_name: Sara
  full_name: Mascia, Sara
  id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
  last_name: Mascia
- first_name: L.
  full_name: Pentericci, L.
  last_name: Pentericci
- first_name: P.
  full_name: Watson, P.
  last_name: Watson
- first_name: A.
  full_name: Alavi, A.
  last_name: Alavi
- first_name: P.
  full_name: Bergamini, P.
  last_name: Bergamini
- first_name: M.
  full_name: Bradač, M.
  last_name: Bradač
- first_name: A.
  full_name: Calabrò, A.
  last_name: Calabrò
- first_name: K.
  full_name: Glazebrook, K.
  last_name: Glazebrook
- first_name: A.
  full_name: Henry, A.
  last_name: Henry
- first_name: M.
  full_name: Llerena, M.
  last_name: Llerena
- first_name: E.
  full_name: Merlin, E.
  last_name: Merlin
- first_name: B.
  full_name: Metha, B.
  last_name: Metha
- first_name: T.
  full_name: Nanayakkara, T.
  last_name: Nanayakkara
- first_name: L.
  full_name: Napolitano, L.
  last_name: Napolitano
- first_name: N.
  full_name: Roy, N.
  last_name: Roy
- first_name: B.
  full_name: Siana, B.
  last_name: Siana
- first_name: E.
  full_name: Vanzella, E.
  last_name: Vanzella
- first_name: B.
  full_name: Vulcani, B.
  last_name: Vulcani
- first_name: X.
  full_name: Wang, X.
  last_name: Wang
citation:
  ama: Liu Y, Mascia S, Pentericci L, et al. A Lyman continuum analysis of ∼100 galaxies
    at z spec∼ 3 in the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>.
    2025;704. doi:<a href="https://doi.org/10.1051/0004-6361/202556410">10.1051/0004-6361/202556410</a>
  apa: Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P.,
    … Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in
    the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences.
    <a href="https://doi.org/10.1051/0004-6361/202556410">https://doi.org/10.1051/0004-6361/202556410</a>
  chicago: Liu, Y., Sara Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini,
    M. Bradač, et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in
    the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences,
    2025. <a href="https://doi.org/10.1051/0004-6361/202556410">https://doi.org/10.1051/0004-6361/202556410</a>.
  ieee: Y. Liu <i>et al.</i>, “A Lyman continuum analysis of ∼100 galaxies at z spec∼
    3 in the Abell 2744 cluster field,” <i>Astronomy &#38; Astrophysics</i>, vol.
    704. EDP Sciences, 2025.
  ista: Liu Y, Mascia S, Pentericci L, Watson P, Alavi A, Bergamini P, Bradač M, Calabrò
    A, Glazebrook K, Henry A, Llerena M, Merlin E, Metha B, Nanayakkara T, Napolitano
    L, Roy N, Siana B, Vanzella E, Vulcani B, Wang X. 2025. A Lyman continuum analysis
    of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy &#38;
    Astrophysics. 704, A328.
  mla: Liu, Y., et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in
    the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 704,
    A328, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202556410">10.1051/0004-6361/202556410</a>.
  short: Y. Liu, S. Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač,
    A. Calabrò, K. Glazebrook, A. Henry, M. Llerena, E. Merlin, B. Metha, T. Nanayakkara,
    L. Napolitano, N. Roy, B. Siana, E. Vanzella, B. Vulcani, X. Wang, Astronomy &#38;
    Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:35Z
date_published: 2025-12-01T00:00:00Z
date_updated: 2026-02-16T12:14:52Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202556410
external_id:
  arxiv:
  - '2507.11045'
file:
- access_level: open_access
  checksum: 3e6061f3c4bfb521b3333ea4913c241a
  content_type: application/pdf
  creator: dernst
  date_created: 2026-01-05T09:26:17Z
  date_updated: 2026-01-05T09:26:17Z
  file_id: '20938'
  file_name: 2025_AstronomyAstrophysics_Liu.pdf
  file_size: 4642530
  relation: main_file
  success: 1
file_date_updated: 2026-01-05T09:26:17Z
fulldoi: https://doi.org/10.1051/0004-6361/202556410
has_accepted_license: '1'
intvolume: '       704'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744
  cluster field
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 704
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21057'
abstract:
- lang: eng
  text: Among the most puzzling early discoveries of JWST are “little red dots” (LRDs),
    compact red sources that host broad Balmer emission lines, and in many cases exhibit
    a “V-shaped” change in slope in the rest-optical. The physical properties of LRDs
    currently have order-of-magnitude uncertainties, because models to explain the
    continuum of these sources differ immensely. Here, we leverage the complete selection
    of red sources in the RUBIES program, supplemented with public PRISM spectra,
    to study the origin of this V shape. By fitting a broken power law with a flexible
    inflection point, we find that a large fraction of red Hα emitters at 2 < z <
    6 exhibit a strong change in slope, and that all strong inflections appear associated
    with the Balmer limit (0.3645 μm). Using a simple model of a reddened active galactic
    nucleus (AGN) with an unobscured scattered-light component, we demonstrate that
    the observed V shape in LRDs is unlikely to occur at any specific wavelength if
    the entire continuum is dominated by light from a power-law AGN continuum. In
    contrast, models with an intrinsic feature at the Balmer limit, such as those
    that are dominated by an evolved stellar population, can produce the observed
    spectral shapes, provided that a reddened component picks up sufficiently redward
    of the break. While no model can comfortably explain the full LRD spectral energy
    distribution, the common inflection location suggests that a single component
    consistently dominates the rest-frame UV optical in LRDs, and that this component
    is associated with T ∼ 10^4 K hydrogen.
acknowledgement: "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 specific observations analyzed can be accessed via DOI:
  10.17909/0esg-h949. All of the data products presented herein were retrieved from
  the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center, which
  is funded by the Danish National Research Foundation under grant No. 140. We express
  gratitude toward the members of the GTO, GO, and DDT teams, whose public data we
  utilized in this work.\r\n\r\nSupport for this work was provided by The Brinson
  Foundation through a Brinson Prize Fellowship grant. Support for program No. 4233
  was provided by NASA through a grant from the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-03127. This research was supported by the International
  Space Science Institute (ISSI) in Bern, through ISSI International Team project
  No. 562. D.S. acknowledges helpful conversations with Xiaohui Fan and Jared Siegel
  that contributed to the quality of this work, in addition to aesthetic sign-off
  from Stephanie Permut on the colors of figures. T.B.M. was supported by a CIERA
  fellowship. 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."
article_number: '118'
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: Anna
  full_name: de Graaff, Anna
  last_name: de Graaff
- first_name: Yilun 逸伦
  full_name: Ma, Yilun 逸伦
  last_name: Ma
- 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: Rachel
  full_name: Bezanson, Rachel
  last_name: Bezanson
- first_name: Leindert A.
  full_name: Boogaard, Leindert A.
  last_name: Boogaard
- first_name: Nikko J.
  full_name: Cleri, Nikko J.
  last_name: Cleri
- first_name: Harley
  full_name: Katz, Harley
  last_name: Katz
- first_name: Ivo
  full_name: Labbe, Ivo
  last_name: Labbe
- first_name: Michael V.
  full_name: Maseda, Michael V.
  last_name: Maseda
- first_name: Ian
  full_name: McConachie, Ian
  last_name: McConachie
- first_name: Tim B.
  full_name: Miller, Tim B.
  last_name: Miller
- 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: Pieter
  full_name: van Dokkum, Pieter
  last_name: van Dokkum
- first_name: Bingjie 冰洁
  full_name: Wang 王, Bingjie 冰洁
  last_name: Wang 王
- first_name: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Katherine E.
  full_name: Whitaker, Katherine E.
  last_name: Whitaker
- first_name: Christina C.
  full_name: Williams, Christina C.
  last_name: Williams
citation:
  ama: 'Setton DJ, Greene JE, de Graaff A, et al. Little Red Dots at an inflection
    point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit. <i>The
    Astrophysical Journal</i>. 2025;995(1). doi:<a href="https://doi.org/10.3847/1538-4357/ae1500">10.3847/1538-4357/ae1500</a>'
  apa: 'Setton, D. J., Greene, J. E., de Graaff, A., Ma, Y. 逸伦, Leja, J., Matthee,
    J. J., … Williams, C. C. (2025). Little Red Dots at an inflection point: Ubiquitous
    v-shaped turnover consistently occurs at the Balmer limit. <i>The Astrophysical
    Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae1500">https://doi.org/10.3847/1538-4357/ae1500</a>'
  chicago: 'Setton, David J., Jenny E. Greene, Anna de Graaff, Yilun 逸伦 Ma, Joel Leja,
    Jorryt J Matthee, Rachel Bezanson, et al. “Little Red Dots at an Inflection Point:
    Ubiquitous v-Shaped Turnover Consistently Occurs at the Balmer Limit.” <i>The
    Astrophysical Journal</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4357/ae1500">https://doi.org/10.3847/1538-4357/ae1500</a>.'
  ieee: 'D. J. Setton <i>et al.</i>, “Little Red Dots at an inflection point: Ubiquitous
    v-shaped turnover consistently occurs at the Balmer limit,” <i>The Astrophysical
    Journal</i>, vol. 995, no. 1. IOP Publishing, 2025.'
  ista: 'Setton DJ, Greene JE, de Graaff A, Ma Y逸伦, Leja J, Matthee JJ, Bezanson R,
    Boogaard LA, Cleri NJ, Katz H, Labbe I, Maseda MV, McConachie I, Miller TB, Price
    SH, Suess KA, van Dokkum P, Wang 王 B冰洁, Weibel A, Whitaker KE, Williams CC. 2025.
    Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently
    occurs at the Balmer limit. The Astrophysical Journal. 995(1), 118.'
  mla: 'Setton, David J., et al. “Little Red Dots at an Inflection Point: Ubiquitous
    v-Shaped Turnover Consistently Occurs at the Balmer Limit.” <i>The Astrophysical
    Journal</i>, vol. 995, no. 1, 118, IOP Publishing, 2025, doi:<a href="https://doi.org/10.3847/1538-4357/ae1500">10.3847/1538-4357/ae1500</a>.'
  short: D.J. Setton, J.E. Greene, A. de Graaff, Y.逸伦 Ma, J. Leja, J.J. Matthee, R.
    Bezanson, L.A. Boogaard, N.J. Cleri, H. Katz, I. Labbe, M.V. Maseda, I. McConachie,
    T.B. Miller, S.H. Price, K.A. Suess, P. van Dokkum, B.冰洁 Wang 王, A. Weibel, K.E.
    Whitaker, C.C. Williams, The Astrophysical Journal 995 (2025).
date_created: 2026-01-28T15:21:47Z
date_published: 2025-12-09T00:00:00Z
date_updated: 2026-02-09T06:41:48Z
day: '09'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae1500
external_id:
  arxiv:
  - '2411.03424'
file:
- access_level: open_access
  checksum: 2a424eb43748a6370ff058c98adb15c6
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-09T06:39:23Z
  date_updated: 2026-02-09T06:39:23Z
  file_id: '21163'
  file_name: 2025_AstrophysicalJournal_Setton.pdf
  file_size: 1989640
  relation: main_file
  success: 1
file_date_updated: 2026-02-09T06:39:23Z
fulldoi: https://doi.org/10.3847/1538-4357/ae1500
has_accepted_license: '1'
intvolume: '       995'
issue: '1'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently
  occurs at the Balmer limit'
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: '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. <i>The Astrophysical Journal
    Letters</i>. 2025;991. doi:<a href="https://doi.org/10.3847/2041-8213/ade78b">10.3847/2041-8213/ade78b</a>
  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. <i>The Astrophysical Journal Letters</i>.
    IOP Publishing. <a href="https://doi.org/10.3847/2041-8213/ade78b">https://doi.org/10.3847/2041-8213/ade78b</a>
  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.” <i>The Astrophysical
    Journal Letters</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/2041-8213/ade78b">https://doi.org/10.3847/2041-8213/ade78b</a>.
  ieee: D. J. Setton <i>et al.</i>, “A confirmed deficit of hot and cold dust emission
    in the most luminous Little Red Dots,” <i>The Astrophysical Journal Letters</i>,
    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.” <i>The Astrophysical Journal Letters</i>,
    vol. 991, L10, IOP Publishing, 2025, doi:<a href="https://doi.org/10.3847/2041-8213/ade78b">10.3847/2041-8213/ade78b</a>.
  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
  date_updated: 2026-02-09T07:10:29Z
  file_id: '21165'
  file_name: 2025_AstrophysicalJournalLetters_Setton.pdf
  file_size: 1394204
  relation: main_file
  success: 1
file_date_updated: 2026-02-09T07:10:29Z
fulldoi: https://doi.org/10.3847/2041-8213/ade78b
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: diamond
PlanS_conform: '1'
_id: '21060'
abstract:
- lang: eng
  text: "Compact, star-forming galaxies with high star formation rate surface densities
    (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because
    intense stellar feedback creates low-density channels that allow photons to escape.
    Irregular or disturbed morphologies, such as those resulting from mergers, can
    also facilitate LyC escape by creating anisotropic gas distributions. We investigated
    the influence of galaxy morphology on LyC production and escape at redshifts 5
    ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys.
    Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15
    M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent
    with canonical expectations. Since direct measurements of fesc are not possible
    during the Epoch of  Reionization (EoR), we predicted fesc for high-redshift galaxies
    by applying survival analysis to a subsample of LyC emitters from the Low-Redshift
    Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era
    galaxies. We find that these galaxies exhibit, on average, modest predicted escape
    fractions (∼0.04). In addition, we evaluated the correlation between morphological
    features and LyC emission. Our findings indicate that neither ξion nor the predicted
    fesc values show a significant correlation with the presence of merger signatures.
    This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances
    are not the primary mechanism driving LyC emission and leakage. Instead, compactness
    and star formation activity likely play a more pivotal role in regulating LyC
    escape. "
acknowledgement: This work is based on observations made with the NASA/ESA/CSA James
  Webb Space Telescope. The data were obtained from the Mikulski Archive for Space
  Telescopes at the Space Telescope Science Institute, which is operated by the Association
  of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127
  for JWST. These observations are associated with programs GTO 1243, ERS 1345, DDT
  2750, and GTO 1180, 1181, 3215, 1210, 1286. Funded by the European Union (ERC, AGENTS,
  101076224). Views and opinions expressed are however those of the author(s) only
  and do not necessarily reflect those of the European Union or the European Research
  Council. Neither the European Union nor the granting authority can be held responsible
  for them. We acknowledge support from the INAF Large Grant 2022 “Extragalactic Surveys
  with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization
  and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project
  2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union
  – Next Generation EU. RA acknowledges support of Grant PID2023-147386NB-I00 funded
  by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S
  funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results
  received the support of a fellowship from the “la Caixa” Foundation (ID 100010434).
  The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants
  PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of
  Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and
  by “ERDF A way of making Europe”.
article_number: A122
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sara
  full_name: Mascia, Sara
  id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
  last_name: Mascia
- first_name: L.
  full_name: Pentericci, L.
  last_name: Pentericci
- first_name: M.
  full_name: Llerena, M.
  last_name: Llerena
- first_name: A.
  full_name: Calabrò, A.
  last_name: Calabrò
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: S.
  full_name: Flury, S.
  last_name: Flury
- first_name: F.
  full_name: Pacucci, F.
  last_name: Pacucci
- first_name: A.
  full_name: Jaskot, A.
  last_name: Jaskot
- first_name: R. O.
  full_name: Amorín, R. O.
  last_name: Amorín
- first_name: R.
  full_name: Bhatawdekar, R.
  last_name: Bhatawdekar
- first_name: M.
  full_name: Castellano, M.
  last_name: Castellano
- first_name: N.
  full_name: Cleri, N.
  last_name: Cleri
- first_name: L.
  full_name: Costantin, L.
  last_name: Costantin
- first_name: K.
  full_name: Davis, K.
  last_name: Davis
- first_name: Claudia
  full_name: Di Cesare, Claudia
  id: 2d002343-372f-11ef-98ec-a164d20427cb
  last_name: Di Cesare
- first_name: M.
  full_name: Dickinson, M.
  last_name: Dickinson
- first_name: A.
  full_name: Fontana, A.
  last_name: Fontana
- first_name: Y.
  full_name: Guo, Y.
  last_name: Guo
- first_name: M.
  full_name: Giavalisco, M.
  last_name: Giavalisco
- first_name: B. W.
  full_name: Holwerda, B. W.
  last_name: Holwerda
- first_name: W.
  full_name: Hu, W.
  last_name: Hu
- first_name: M.
  full_name: Huertas-Company, M.
  last_name: Huertas-Company
- first_name: Intae
  full_name: Jung, Intae
  last_name: Jung
- first_name: J.
  full_name: Kartaltepe, J.
  last_name: Kartaltepe
- first_name: D.
  full_name: Kashino, D.
  last_name: Kashino
- first_name: A. M.
  full_name: Koekemoer, A. M.
  last_name: Koekemoer
- first_name: R. A.
  full_name: Lucas, R. A.
  last_name: Lucas
- first_name: J.
  full_name: Lotz, J.
  last_name: Lotz
- first_name: L.
  full_name: Napolitano, L.
  last_name: Napolitano
- first_name: S.
  full_name: Jogee, S.
  last_name: Jogee
- first_name: S.
  full_name: Wilkins, S.
  last_name: Wilkins
citation:
  ama: Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy
    morphology on the production and escape of ionizing photons in the early Universe.
    <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href="https://doi.org/10.1051/0004-6361/202553760">10.1051/0004-6361/202553760</a>
  apa: Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury,
    S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the
    production and escape of ionizing photons in the early Universe. <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202553760">https://doi.org/10.1051/0004-6361/202553760</a>
  chicago: Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee,
    S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on
    the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202553760">https://doi.org/10.1051/0004-6361/202553760</a>.
  ieee: S. Mascia <i>et al.</i>, “Little impact of mergers and galaxy morphology on
    the production and escape of ionizing photons in the early Universe,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.
  ista: Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci
    F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis
    K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W,
    Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz
    J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy
    morphology on the production and escape of ionizing photons in the early Universe.
    Astronomy &#38; Astrophysics. 701, A122.
  mla: Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the
    Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy
    &#38; Astrophysics</i>, vol. 701, A122, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202553760">10.1051/0004-6361/202553760</a>.
  short: S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury,
    F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L.
    Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco,
    B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino,
    A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy
    &#38; Astrophysics 701 (2025).
corr_author: '1'
date_created: 2026-01-28T15:24:24Z
date_published: 2025-09-01T00:00:00Z
date_updated: 2026-02-09T07:33:46Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202553760
external_id:
  arxiv:
  - '2501.08268'
file:
- access_level: open_access
  checksum: 990e384ca19e14b35296712d3b9e2919
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-09T07:28:08Z
  date_updated: 2026-02-09T07:28:08Z
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  file_name: 2025_AstronomyAstrophysics_Mascia.pdf
  file_size: 9994234
  relation: main_file
  success: 1
file_date_updated: 2026-02-09T07:28:08Z
fulldoi: https://doi.org/10.1051/0004-6361/202553760
has_accepted_license: '1'
intvolume: '       701'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Little impact of mergers and galaxy morphology on the production and escape
  of ionizing photons in the early Universe
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 701
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21061'
abstract:
- lang: eng
  text: 'Detecting the first generation of stars, Population III (Pop III), has been
    a long-standing goal in astrophysics, yet they remain elusive even in the JWST
    era. Here we present a novel NIRCam-based selection method for Pop III galaxies,
    and carefully validate it through completeness and contamination simulations.
    We systematically search ≃ 500 arcmin2 across JWST legacy fields for Pop III candidates,
    including GLIMPSE, which, assisted by gravitational lensing, has produced JWST’s
    deepest NIRCam imaging thus far. We discover one promising Pop III galaxy candidate
    (GLIMPSE-16043) at z=6.50 -0.24 +0.03, a moderately lensed galaxy (µ = + 2.9 -0.2
    +0.1) with an intrinsic UV magnitude of MUV= -15.89 -0.14 +0.12. It exhibits key
    Pop III features: strong Hα emission (rest-frame EW 2810 ± 550 Å); a Balmer jump;
    no dust (UV slope β = −2.34 ± 0.36); and undetectable metal lines (e.g., [O III];
    [O III]/Hβ < 0.44), implying a gas-phase metallicity of Zgas/Z⊙ < 0.5%. These
    properties indicate the presence of a nascent, metal-deficient young stellar population
    (<5 Myr) with a stellar mass of ≃105 M⊙. Intriguingly, this source deviates significantly
    from the extrapolated UV–metallicity relation derived from recent JWST observations
    at z = 4–10, consistent with UV enhancement by a top-heavy Pop III initial mass
    function or the presence of an extremely metal-poor active galactic nucleus. We
    also  derive the first observational constraints on the Pop III UV luminosity
    function at z ≃ 6–7. The volume density of GLIMPSE-16043 (≈10^−4 cMpc−3) is in
    excellent agreement with theoretical predictions, independently reinforcing its
    plausibility. This study demonstrates the power of our novel NIRCam method to
    finally reveal distant galaxies even more pristine than the Milky Way’s most metal-poor
    satellites, thereby promising to bring us closer to the first generation of stars
    than we have ever been before.'
acknowledgement: "We are grateful to the CEERS, PRIMER, JOF, UNCOVER, and GLIMPSE
  teams for developing their NIRCam surveys, and to the various JWST and HST surveys
  acknowledged in Section 3 that enabled our search. We thank Kimihiko Nakajima and
  Kohei Inayoshi for sharing Pop III and/or AGN templates, Steven Finkelstein for
  comments on the completeness and contamination rate simulation, Aaron Yung for SEDs
  of simulated galaxies, Joel Leja, Ben Johnson, and Sandro Tacchella for advise on
  SED fitting, and Takashi Kojima and Hiroto Yanagisawa for discussions.\r\n\r\nWe
  made extensive use of the DAWN JWST Archive for various comparisons presented in
  this paper. Some of the data products presented herein were retrieved from the Dawn
  JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which
  is funded by the Danish National Research Foundation under grant DNRF140. The prism
  spectra used in this paper were observed as part of the following programs, and
  we are grateful to these teams for helping build the rich spectroscopic legacy of
  JWST: 1180, 1181, 1210, 1286, 3215 (A. J. Bunker et al. 2024; F. D’Eugenio et al.
  2024); 1211–1215 (M. V. Maseda et al. 2024); 1345 (S. L. Finkelstein et al. 2024);
  1433 (T. Y.-Y. Hsiao et al. 2024); 1747 (G. Roberts-Borsani et al. 2025); 2028 (X.
  Wang et al. 2024); 2073 (PI: J. Hennawi); 2198 (L. Barrufet et al. 2025); 2282 (L.
  D. Bradley et al. 2023); 2561 (R. Bezanson et al. 2024; S. H. Price et al. 2024);
  2565 (T. Nanayakkara et al. 2023); 2750 (P. Arrabal Haro et al. 2023b); 2756 (PI:
  W. Chen); 2767 (C. C. Williams et al. 2023); 3073 (M. Castellano et al. 2024); 4106
  (PI: E. Nelson); 4233 (A. de Graaff et al. 2025); 4446 (B. L. Frye et al. 2024);
  4557 (PI: H. Yan); 6541 (PI: E. Egami); 6585 (PI: D. Coulter).\r\n\r\nThis work
  is based on observations made with the NASA/ESA/CSA James Webb Space Telescope.
  The data were obtained from the Mikulski Archive for Space Telescopes at the Space
  Telescope Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. The specific
  observations can be accessed via doi: 10.17909/xpxt-a441. These observations include
  data associated with program No. 03293. Support for program No. 03293 was provided
  by NASA through a grant from the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc., under NASA contract
  NAS 5-03127.\r\n\r\nThis project has received funding from NASA through the NASA
  Hubble Fellowship grant HST-HF2-51505.001-A awarded by the Space Telescope Science
  Institute, which is operated by the Association of Universities for Research in
  Astronomy, Incorporated, under NASA contract NAS5-26555. 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 DNRF140. H.A. and
  I.C. acknowledge support from CNES, focused on the JWST mission, and the Programme
  National Cosmology and Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded
  by CEA and CNES. I.C. acknowledges funding support from the Initiative Physique
  des Infinis (IPI), a research training program of the Idex SUPER at Sorbonne Université.
  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. P.N. acknowledges
  support from the Gordon and Betty Moore Foundation and the John Templeton Foundation
  that fund the black hole Initiative (BHI) at Harvard University, where she serves
  as one of the PIs. B.L. acknowledges support from the Deutsche Forschungsgemeinschaft
  (DFG, German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1—390900948
  (the Heidelberg STRUCTURES Excellence Cluster). Y.S. and G.M. have received funding
  from the European Research Council (ERC) under the European Union’s Horizon 2020
  research and innovation program (grant agreement No. 833925, project STAREX)."
article_number: '46'
article_processing_charge: Yes
article_type: original
author:
- first_name: Seiji
  full_name: Fujimoto, Seiji
  last_name: Fujimoto
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: John
  full_name: Chisholm, John
  last_name: Chisholm
- first_name: Hakim
  full_name: Atek, Hakim
  last_name: Atek
- first_name: Ryan
  full_name: Endsley, Ryan
  last_name: Endsley
- first_name: Vasily
  full_name: Kokorev, Vasily
  last_name: Kokorev
- first_name: Lukas J.
  full_name: Furtak, Lukas J.
  last_name: Furtak
- first_name: Richard
  full_name: Pan, Richard
  last_name: Pan
- first_name: Boyuan
  full_name: Liu, Boyuan
  last_name: Liu
- first_name: Volker
  full_name: Bromm, Volker
  last_name: Bromm
- first_name: Alessandra
  full_name: Venditti, Alessandra
  last_name: Venditti
- first_name: Eli
  full_name: Visbal, Eli
  last_name: Visbal
- first_name: Richard
  full_name: Sarmento, Richard
  last_name: Sarmento
- first_name: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Pascal A.
  full_name: Oesch, Pascal A.
  last_name: Oesch
- first_name: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Daniel
  full_name: Schaerer, Daniel
  last_name: Schaerer
- first_name: Angela
  full_name: Adamo, Angela
  last_name: Adamo
- first_name: Danielle A.
  full_name: Berg, Danielle A.
  last_name: Berg
- first_name: Rachel
  full_name: Bezanson, Rachel
  last_name: Bezanson
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Iryna
  full_name: Chemerynska, Iryna
  last_name: Chemerynska
- first_name: Adélaïde
  full_name: Claeyssens, Adélaïde
  last_name: Claeyssens
- first_name: Miroslava
  full_name: Dessauges-Zavadsky, Miroslava
  last_name: Dessauges-Zavadsky
- first_name: Anna
  full_name: Frebel, Anna
  last_name: Frebel
- first_name: Damien
  full_name: Korber, Damien
  last_name: Korber
- first_name: Ivo
  full_name: Labbe, Ivo
  last_name: Labbe
- first_name: Rui
  full_name: Marques-Chaves, Rui
  last_name: Marques-Chaves
- 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: Kristen B. W.
  full_name: McQuinn, Kristen B. W.
  last_name: McQuinn
- first_name: Julian B.
  full_name: Muñoz, Julian B.
  last_name: Muñoz
- first_name: Priyamvada
  full_name: Natarajan, Priyamvada
  last_name: Natarajan
- first_name: Alberto
  full_name: Saldana-Lopez, Alberto
  last_name: Saldana-Lopez
- first_name: Katherine A.
  full_name: Suess, Katherine A.
  last_name: Suess
- first_name: Marta
  full_name: Volonteri, Marta
  last_name: Volonteri
- first_name: Adi
  full_name: Zitrin, Adi
  last_name: Zitrin
citation:
  ama: 'Fujimoto S, Naidu RP, Chisholm J, et al. GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop
    III galaxy candidate and first constraints on the Pop III UV luminosity function
    at z ≃  6–7. <i>The Astrophysical Journal</i>. 2025;989. doi:<a href="https://doi.org/10.3847/1538-4357/ade9a1">10.3847/1538-4357/ade9a1</a>'
  apa: 'Fujimoto, S., Naidu, R. P., Chisholm, J., Atek, H., Endsley, R., Kokorev,
    V., … Zitrin, A. (2025). GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate
    and first constraints on the Pop III UV luminosity function at z ≃  6–7. <i>The
    Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ade9a1">https://doi.org/10.3847/1538-4357/ade9a1</a>'
  chicago: 'Fujimoto, Seiji, Rohan P. Naidu, John Chisholm, Hakim Atek, Ryan Endsley,
    Vasily Kokorev, Lukas J. Furtak, et al. “GLIMPSE: An Ultrafaint ≃10^5 M⊙ Pop III
    Galaxy Candidate and First Constraints on the Pop III UV Luminosity Function at
    z ≃  6–7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4357/ade9a1">https://doi.org/10.3847/1538-4357/ade9a1</a>.'
  ieee: 'S. Fujimoto <i>et al.</i>, “GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy
    candidate and first constraints on the Pop III UV luminosity function at z ≃ 
    6–7,” <i>The Astrophysical Journal</i>, vol. 989. IOP Publishing, 2025.'
  ista: 'Fujimoto S, Naidu RP, Chisholm J, Atek H, Endsley R, Kokorev V, Furtak LJ,
    Pan R, Liu B, Bromm V, Venditti A, Visbal E, Sarmento R, Weibel A, Oesch PA, Brammer
    G, Schaerer D, Adamo A, Berg DA, Bezanson R, Bouwens R, Chemerynska I, Claeyssens
    A, Dessauges-Zavadsky M, Frebel A, Korber D, Labbe I, Marques-Chaves R, Matthee
    JJ, McQuinn KBW, Muñoz JB, Natarajan P, Saldana-Lopez A, Suess KA, Volonteri M,
    Zitrin A. 2025. GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first
    constraints on the Pop III UV luminosity function at z ≃  6–7. The Astrophysical
    Journal. 989, 46.'
  mla: 'Fujimoto, Seiji, et al. “GLIMPSE: An Ultrafaint ≃10^5 M⊙ Pop III Galaxy Candidate
    and First Constraints on the Pop III UV Luminosity Function at z ≃  6–7.” <i>The
    Astrophysical Journal</i>, vol. 989, 46, IOP Publishing, 2025, doi:<a href="https://doi.org/10.3847/1538-4357/ade9a1">10.3847/1538-4357/ade9a1</a>.'
  short: S. Fujimoto, R.P. Naidu, J. Chisholm, H. Atek, R. Endsley, V. Kokorev, L.J.
    Furtak, R. Pan, B. Liu, V. Bromm, A. Venditti, E. Visbal, R. Sarmento, A. Weibel,
    P.A. Oesch, G. Brammer, D. Schaerer, A. Adamo, D.A. Berg, R. Bezanson, R. Bouwens,
    I. Chemerynska, A. Claeyssens, M. Dessauges-Zavadsky, A. Frebel, D. Korber, I.
    Labbe, R. Marques-Chaves, J.J. Matthee, K.B.W. McQuinn, J.B. Muñoz, P. Natarajan,
    A. Saldana-Lopez, K.A. Suess, M. Volonteri, A. Zitrin, The Astrophysical Journal
    989 (2025).
date_created: 2026-01-28T15:25:17Z
date_published: 2025-08-04T00:00:00Z
date_updated: 2026-02-09T08:11:01Z
day: '04'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ade9a1
file:
- access_level: open_access
  checksum: 9e08e77ce6d818fafd074e2b6c30bc43
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-09T07:57:01Z
  date_updated: 2026-02-09T07:57:01Z
  file_id: '21167'
  file_name: 2025_AstrophysicalJournal_Fujimoto.pdf
  file_size: 14405059
  relation: main_file
  success: 1
file_date_updated: 2026-02-09T07:57:01Z
fulldoi: https://doi.org/10.3847/1538-4357/ade9a1
has_accepted_license: '1'
intvolume: '       989'
language:
- iso: eng
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints
  on the Pop III UV luminosity function at z ≃  6–7'
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: 989
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21062'
abstract:
- lang: eng
  text: JWST observations have unveiled faint active galactic nuclei (AGNs) at high
    redshift that provide insights into the formation of supermassive black holes
    (SMBHs). However, disentangling their stellar from AGN light is challenging. Here,
    we use an empirical approach to infer the average stellar mass of five faint broad-line
    (BL) Hα emitters at z = 4–5 with BH masses ≈6 × 10^6 M⊙, with a method independent
    of their spectral energy distribution (SED). We use the deep JWST/NIRcam grism
    survey “All the Little Things” to measure the overdensities around BL-Hα emitters
    and around a spectroscopic reference sample of ∼300 galaxies. In our reference
    sample, we find that megaparsec-scale overdensity correlates with stellar mass.
    Their large-scale environments suggest that BL-Hα emitters are hosted by galaxies
    with stellar masses ≈5 × 10^7 M⊙, ≈40 times lower than those inferred from galaxy-only
    SED fits. Adding measurements around more luminous z ≈ 6 AGNs, we find tentative
    correlations between line width, BH mass, and the overdensity, suggestive of a
    steep BH to halo mass relation. The main implications are (1) when BH masses are
    taken at face value, we confirm extremely high BH to stellar mass ratios of ≈10%,
    (2) the galaxies of low stellar mass that host growing SMBHs are in tension with
    typical hydrodynamical simulations, except those without feedback, (3) a 1% duty
    cycle implied by the host mass hints at super-Eddington accretion, (4) the masses
    are at odds with an interpretation of the line broadening in terms of high stellar
    density, (5) our results imply a luminosity-dependent diversity of galaxy masses,
    environments, and SEDs among AGN samples.
acknowledgement: 'We thank the referee for their constructive comments that helped
  to improve the paper. We thank Junyao Li for sharing model output shown in Figure
  13, Rob Crain for sharing results from the ONLYAGN EAGLE model shown in Figure 15,
  and Adi Zitrin for 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 programs # 3516. Funded
  by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are
  however those of the author(s) only and do not necessarily reflect those of the
  European Union or the European Research Council. Neither the European Union nor
  the granting authority can be held responsible for them. We acknowledge funding
  from JWST program GO-3516. Support for this work was provided by NASA through the
  NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope
  Science Institute, which is operated by the Association of Universities for Research
  in Astronomy, Incorporated, under NASA contract NAS 5-26555. A.A. acknowledges support
  by the Swedish research council Vetenskapsrådet (2021-05559).'
article_number: '246'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- 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: Gauri
  full_name: Kotiwale, Gauri
  id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
  last_name: Kotiwale
- first_name: Lukas J.
  full_name: Furtak, Lukas J.
  last_name: Furtak
- first_name: Ivan
  full_name: Kramarenko, Ivan
  id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
  last_name: Kramarenko
  orcid: 0000-0001-5346-6048
- first_name: Ruari
  full_name: Mackenzie, Ruari
  last_name: Mackenzie
- first_name: Jenny
  full_name: Greene, Jenny
  last_name: Greene
- first_name: Angela
  full_name: Adamo, Angela
  last_name: Adamo
- first_name: Rychard J.
  full_name: Bouwens, Rychard J.
  last_name: Bouwens
- first_name: Claudia
  full_name: Di Cesare, Claudia
  id: 2d002343-372f-11ef-98ec-a164d20427cb
  last_name: Di Cesare
- first_name: Anna-Christina
  full_name: Eilers, Anna-Christina
  last_name: Eilers
- first_name: Anna
  full_name: de Graaff, Anna
  last_name: de Graaff
- first_name: Kasper E.
  full_name: Heintz, Kasper E.
  last_name: Heintz
- first_name: Daichi
  full_name: Kashino, Daichi
  last_name: Kashino
- first_name: Michael V.
  full_name: Maseda, Michael V.
  last_name: Maseda
- first_name: Sandro
  full_name: Tacchella, Sandro
  last_name: Tacchella
- first_name: Alberto
  full_name: Torralba Torregrosa, Alberto
  id: 018f0249-0e87-11f0-b167-cbce08fbd541
  last_name: Torralba Torregrosa
  orcid: 0000-0001-5586-6950
citation:
  ama: Matthee JJ, Naidu RP, Kotiwale G, et al. Environmental evidence for overly
    massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at
    z ∼ 5. <i>The Astrophysical Journal</i>. 2025;988(2). doi:<a href="https://doi.org/10.3847/1538-4357/ade886">10.3847/1538-4357/ade886</a>
  apa: Matthee, J. J., Naidu, R. P., Kotiwale, G., Furtak, L. J., Kramarenko, I.,
    Mackenzie, R., … Torralba Torregrosa, A. (2025). Environmental evidence for overly
    massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at
    z ∼ 5. <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ade886">https://doi.org/10.3847/1538-4357/ade886</a>
  chicago: Matthee, Jorryt J, Rohan P. Naidu, Gauri Kotiwale, Lukas J. Furtak, Ivan
    Kramarenko, Ruari Mackenzie, Jenny Greene, et al. “Environmental Evidence for
    Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation
    at z ∼ 5.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4357/ade886">https://doi.org/10.3847/1538-4357/ade886</a>.
  ieee: J. J. Matthee <i>et al.</i>, “Environmental evidence for overly massive Black
    Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” <i>The
    Astrophysical Journal</i>, vol. 988, no. 2. IOP Publishing, 2025.
  ista: Matthee JJ, Naidu RP, Kotiwale G, Furtak LJ, Kramarenko I, Mackenzie R, Greene
    J, Adamo A, Bouwens RJ, Di Cesare C, Eilers A-C, de Graaff A, Heintz KE, Kashino
    D, Maseda MV, Tacchella S, Torralba Torregrosa A. 2025. Environmental evidence
    for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass
    relation at z ∼ 5. The Astrophysical Journal. 988(2), 246.
  mla: Matthee, Jorryt J., et al. “Environmental Evidence for Overly Massive Black
    Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The
    Astrophysical Journal</i>, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:<a
    href="https://doi.org/10.3847/1538-4357/ade886">10.3847/1538-4357/ade886</a>.
  short: J.J. Matthee, R.P. Naidu, G. Kotiwale, L.J. Furtak, I. Kramarenko, R. Mackenzie,
    J. Greene, A. Adamo, R.J. Bouwens, C. Di Cesare, A.-C. Eilers, A. de Graaff, K.E.
    Heintz, D. Kashino, M.V. Maseda, S. Tacchella, A. Torralba Torregrosa, The Astrophysical
    Journal 988 (2025).
corr_author: '1'
date_created: 2026-01-28T15:25:42Z
date_published: 2025-07-29T00:00:00Z
date_updated: 2026-02-09T08:22:01Z
day: '29'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ade886
external_id:
  arxiv:
  - '2412.02846'
file:
- access_level: open_access
  checksum: a49fbed72f2ff9c0b13129acb6f44f9d
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  creator: dernst
  date_created: 2026-02-09T08:20:14Z
  date_updated: 2026-02-09T08:20:14Z
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  file_name: 2025_AstrophysicalJournal_Matthee.pdf
  file_size: 6237415
  relation: main_file
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file_date_updated: 2026-02-09T08:20:14Z
fulldoi: https://doi.org/10.3847/1538-4357/ade886
has_accepted_license: '1'
intvolume: '       988'
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
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Environmental evidence for overly massive Black Holes in low-mass galaxies
  and a Black Hole–Halo mass relation at z ∼ 5
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: 988
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21063'
abstract:
- lang: eng
  text: "We report the detection of a 13σ Hα emission line from HDF850.1 at z = 5.188
    ± 0.001 using the FRESCO (First Reionization Era SpectroscopicallyComplete Observations)
    NIRCam F444W grism observations. Detection of Hα in HDF850.1 is noteworthy, given
    its high far-infrared (IR) luminosity, substantial dust obscuration, and the historical
    challenges in deriving its redshift.\r\nHDF850.1 shows a clear detection in the
    F444W imaging data, distributed between a northern and southern component, mirroring
    that seen in [C II] from the Plateau de Bure Interferometer. Modelling the spectral
    energy distribution of each component separately, we find that the northern component
    has a higher mass, star formation rate (SFR), and dust extinction than the southern
    component. The observed Hα emission appears to arise entirely from the less-obscured
    southern component and shows a similar \x04v∼ + 130 km s −1 velocity offset to
    that seen for [C II] relative to the source systemic redshift. Leveraging Hα-derived
    redshiftsfrom FRESCO observations, we find that HDF850.1 isforming in one of the
    richest environments identified to date at z > 5, with 100 z = 5.17–5.20 galaxies
    distributed across 13 smaller structures and a ∼(15 cMpc)3 volume. Based on the
    evolution of analogous structures in cosmological simulations, the z = 5.17–5.20
    structures seem likely to collapse into\r\na single > 1014M cluster by z ∼ 0.
    Comparing galaxy properties forming within this overdensity with those outside,
    we find the masses, SFRs, and UV luminosities inside the overdensity to be clearly
    higher. The prominence of Hα line emission from HDF850.1 and other known highly
    obscured z > 5 galaxies illustrates the potential of NIRCam-grism programs to
    map both\r\nthe early build-up of IR-luminous galaxies and overdense structures."
acknowledgement: "We are grateful to Roberto Neri and collaborators for providing
  us with spatially resolved information on both the dust-continuum and [C ii] line
  emission from their high spatial resolution PdBI observations. This project was
  made possible in part by the Leiden University Fund/Bouwens Astrophysics Fund. RJB
  acknowledges support from NWO grants 600.065.140.11N211 (vrij competitie) and TOP
  grant TOP1.16.057. The Cosmic Dawn Center (DAWN) is funded by the Danish National
  Research Foundation under grant no. 140. Cloud-based data processing and file storage
  for this work is provided by the AWS Cloud Credits for Research program. 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. RPN acknowledges
  funding from JWST programs GO-1933 and GO-2279. Support for this work was provided
  by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by
  the Space Telescope Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges
  support from the CIDEGENT/2021/059 grant, from project PID2019-109592GB-I00/AEI/10.13039/501100011033
  from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación.
  This study forms part of the Astrophysics and High Energy Physics programme and
  was supported by MCIN with funding from European Union NextGenerationEU (PRTR-C17.I1)
  and by Generalitat Valenciana under the project n. ASFAE/2022/025. RAM acknowledges
  support from the ERC Advanced Grant 740246 (Cosmic_Gas) and the Swiss National Science
  Foundation through project grant 200020_207349.\r\n\r\nThis work is based on observations
  made with the NASA/ESA/CSA JWST. 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 no. 1895.\r\n\r\nThis
  paper made use of several publicly available software packages. We are indebted
  to the respective authors for their work: ipython (Pérez & Granger 2007), matplotlib
  (Hunter 2007), numpy (Oliphant 2006), scipy (Virtanen et al. 2020), jupyter (Kluyver
  et al. 2016), astropy (Astropy Collaboration 2013, 2018), grizli (v1.7.11; Brammer
  2018; Brammer et al. 2022), eazy (Brammer, van Dokkum & Coppi 2008), and SExtractor
  (Bertin & Arnouts 1996)."
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Thomas
  full_name: Herard-Demanche, Thomas
  last_name: Herard-Demanche
- first_name: Rychard J
  full_name: Bouwens, Rychard J
  last_name: Bouwens
- 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: Roberto
  full_name: Decarli, Roberto
  last_name: Decarli
- first_name: Erica J
  full_name: Nelson, Erica J
  last_name: Nelson
- first_name: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Mengyuan
  full_name: Xiao, Mengyuan
  last_name: Xiao
- first_name: Mauro
  full_name: Stefanon, Mauro
  last_name: Stefanon
- first_name: Fabian
  full_name: Walter, Fabian
  last_name: Walter
- 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: Romain A
  full_name: Meyer, Romain A
  last_name: Meyer
- first_name: Stijn
  full_name: Wuyts, Stijn
  last_name: Wuyts
- first_name: Naveen
  full_name: Reddy, Naveen
  last_name: Reddy
- first_name: Lucie
  full_name: Rowland, Lucie
  last_name: Rowland
- first_name: Ivana
  full_name: van Leeuwen, Ivana
  last_name: van Leeuwen
- first_name: Pablo Arrabal
  full_name: Haro, Pablo Arrabal
  last_name: Haro
- first_name: Helmut
  full_name: Dannerbauer, Helmut
  last_name: Dannerbauer
- first_name: Alice E
  full_name: Shapley, Alice E
  last_name: Shapley
- first_name: John
  full_name: Chisholm, John
  last_name: Chisholm
- first_name: Pieter
  full_name: van Dokkum, Pieter
  last_name: van Dokkum
- first_name: Ivo
  full_name: Labbe, Ivo
  last_name: Labbe
- first_name: Garth
  full_name: Illingworth, Garth
  last_name: Illingworth
- first_name: Daniel
  full_name: Schaerer, Daniel
  last_name: Schaerer
- first_name: Irene
  full_name: Shivaei, Irene
  last_name: Shivaei
citation:
  ama: 'Herard-Demanche T, Bouwens RJ, Oesch PA, et al. Mapping dusty galaxy growth
    at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding
    overdense structures. <i>Monthly Notices of the Royal Astronomical Society</i>.
    2025;537(2):788-808. doi:<a href="https://doi.org/10.1093/mnras/staf030">10.1093/mnras/staf030</a>'
  apa: 'Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., Naidu, R. P., Decarli,
    R., Nelson, E. J., … Shivaei, I. (2025). Mapping dusty galaxy growth at z &#62;
    5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense
    structures. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnras/staf030">https://doi.org/10.1093/mnras/staf030</a>'
  chicago: 'Herard-Demanche, Thomas, Rychard J Bouwens, Pascal A Oesch, Rohan P Naidu,
    Roberto Decarli, Erica J Nelson, Gabriel Brammer, et al. “Mapping Dusty Galaxy
    Growth at z &#62; 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and
    the Surrounding Overdense Structures.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2025. <a href="https://doi.org/10.1093/mnras/staf030">https://doi.org/10.1093/mnras/staf030</a>.'
  ieee: 'T. Herard-Demanche <i>et al.</i>, “Mapping dusty galaxy growth at z &#62;
    5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense
    structures,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537,
    no. 2. Oxford University Press, pp. 788–808, 2025.'
  ista: 'Herard-Demanche T, Bouwens RJ, Oesch PA, Naidu RP, Decarli R, Nelson EJ,
    Brammer G, Weibel A, Xiao M, Stefanon M, Walter F, Matthee JJ, Meyer RA, Wuyts
    S, Reddy N, Rowland L, van Leeuwen I, Haro PA, Dannerbauer H, Shapley AE, Chisholm
    J, van Dokkum P, Labbe I, Illingworth G, Schaerer D, Shivaei I. 2025. Mapping
    dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy
    HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal
    Astronomical Society. 537(2), 788–808.'
  mla: 'Herard-Demanche, Thomas, et al. “Mapping Dusty Galaxy Growth at z &#62; 5
    with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense
    Structures.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537,
    no. 2, Oxford University Press, 2025, pp. 788–808, doi:<a href="https://doi.org/10.1093/mnras/staf030">10.1093/mnras/staf030</a>.'
  short: T. Herard-Demanche, R.J. Bouwens, P.A. Oesch, R.P. Naidu, R. Decarli, E.J.
    Nelson, G. Brammer, A. Weibel, M. Xiao, M. Stefanon, F. Walter, J.J. Matthee,
    R.A. Meyer, S. Wuyts, N. Reddy, L. Rowland, I. van Leeuwen, P.A. Haro, H. Dannerbauer,
    A.E. Shapley, J. Chisholm, P. van Dokkum, I. Labbe, G. Illingworth, D. Schaerer,
    I. Shivaei, Monthly Notices of the Royal Astronomical Society 537 (2025) 788–808.
date_created: 2026-01-28T15:25:53Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2026-02-09T08:50:55Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1093/mnras/staf030
external_id:
  arxiv:
  - '2309.04525'
file:
- access_level: open_access
  checksum: 4cbade43244eaa8b60bb05a90ae613da
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-09T08:39:19Z
  date_updated: 2026-02-09T08:39:19Z
  file_id: '21169'
  file_name: 2025_MonthlyNoticesRAS_HerardDemanche.pdf
  file_size: 2787493
  relation: main_file
  success: 1
file_date_updated: 2026-02-09T08:39:19Z
fulldoi: https://doi.org/10.1093/mnras/staf030
has_accepted_license: '1'
intvolume: '       537'
issue: '2'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
page: 788-808
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
status: public
title: 'Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm
  galaxy HDF850.1 and the surrounding overdense structures'
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: 537
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21727'
abstract:
- lang: eng
  text: We present a comprehensive analysis of the MIRI Extremely Red Object Virgil,
    a Lyα emitter at zspec = 6.6379 ± 0.0035 with the photometric properties of a
    Little Red Dot. Leveraging new JWST/MIRI imaging from the MIDIS and PAHSPECS programs,
    we confirm Virgil’s extraordinary nature among galaxies in JADES/GOODS-South,
    exhibiting a strikingly red NIRCam-to-MIRI color (F444W–F1500W = 2.84 ± 0.04 mag).
    Deep NIRSpec/PRISM spectroscopy from the OASIS program offers key insights into
    the host galaxy, revealing properties of an average star-forming galaxy during
    Cosmic Reionization, such as a subsolar metallicity, low-to-moderate dust content,
    and a relatively high ionization parameter and electron temperature. By estimating
    the star formation rate of Virgil from UV and Hα, we find evidence that the galaxy
    is either entering or fading out of a bursty episode. Although line-ratio diagnostics
    employed at high z would classify Virgil as an active galactic nucleus (AGN),
    this classification becomes ambiguous once redshift evolution is considered. Nonetheless,
    Virgil occupies the same parameter space as recently confirmed AGNs at similar
    redshifts. The new deep MIRI data at 15 μm reinforce the AGN nature of Virgil,
    as inferred from multiple spectral energy distribution (SED) fitting codes. Virgil’s
    rising infrared SED and UV excess resemble those of Dust-Obscured Galaxies (DOGs)
    studied with Spitzer at Cosmic Noon, particularly blue-excess HotDOGs. Our results
    highlight the need for a multiwavelength approach incorporating MIRI to uncover
    such extreme sources at z ≳ 6 and to shed light on the interplay between galaxy
    evolution and early black hole growth during Cosmic Reionization.
acknowledgement: "The authors are deeply grateful to Antonello Calabrò for valuable
  insights on CLOUDY and pyCloudy, and for publicly sharing their SFG and AGN models,
  which were used as a reference to verify the consistency of our photoionization
  models. The authors also thank Adam Carnall for insightful input on bagpipes and
  for assistance with the implementation of the two-population model adopted in this
  work. Finally, they also thank Camilla Pacifici, Vasily Kokorev, and Cristian Vignali
  for their insightful discussions.\r\n\r\nThis work is based on observations made
  with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for
  Space Telescopes (MAST) at the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc., under NASA contract
  NAS 5-03127 for JWST. These observations are associated with JWST programs GTO #1180,
  GO #1210, GTO#1283, GO #1963, GO #1895, GO# 3215, and GO#6511.\r\n\r\nThe authors
  acknowledge the FRESCO, JEMS, and #3215 teams led by co-PIs P. Oesch, C. C. Williams,
  M. Maseda, D. Eisenstein, and R. Maiolino for developing their observing program
  with a zero-exclusive-access period. Processing for the JADES NIRCam data release
  was performed on the lux cluster at the University of California, Santa Cruz, funded
  by NSF MRI grant AST 1828315. Also 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 526555. The data presented in this article were obtained
  from MAST at the Space Telescope Science Institute. The specific observations analyzed
  can be accessed via doi: 10.17909/1rq3-8048 P. Oesch & D. Magee (2023), C. Williams
  et al. (2023), G. Illingworth (2015), and M. Rieke et al. (2023).\r\n\r\nA.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\n\r\nP.G.P.-G. acknowledges support from grant PID2022-139567NB-I00
  funded by the Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033,
  FEDER, UE.\r\n\r\nB.E.R. acknowledges support from the NIRCam Science Team contract
  to the University of Arizona, NAS5-02015, and JWST Program 3215.\r\n\r\nS.T. acknowledges
  support by the Royal Society Research Grant G125142.\r\n\r\nThe 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.\r\n\r\nJ.W. gratefully acknowledges support from the Cosmic Dawn Center
  through the DAWN Fellowship. The Cosmic Dawn Center (DAWN) is funded by the Danish
  National Research Foundation under grant No. 140.\r\n\r\nY.Z., Z.J., and P.L. gratefully
  acknowledge the JWST/NIRCam contract to the University of Arizona NAS5-02015.\r\n\r\nThe
  work of G.H.R. and P.L. was also supported by grant 80NSSC18K0555, from the NASA
  Goddard Space Flight Center to the University of Arizona.\r\n\r\nH.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.\r\n\r\nG.C.J.
  acknowledges support by the Science and Technology Facilities Council (STFC), ERC
  Advanced grant 695671 “QUENCH.”\r\n\r\nA.C.G. acknowledges support by JWST contract
  B0215/JWST-GO-02926.\r\n\r\nG.O. acknowledges support from the Swedish National
  Space Agency (SNSA).\r\n\r\nH.I. acknowledges support from JSPS KAKENHI grant No.
  JP21H01129.\r\n\r\nM.A. gratefully acknowledges support from ANID Basal Project
  FB210003 and ANID MILENIO NCN2024_112.\r\n\r\nT.D.S. acknowledges the research project
  was supported by the Hellenic Foundation for Research and Innovation (HFRI) under
  the “2nd Call for HFRI Research Projects to Support Faculty Members and Researchers”
  (project No.: 03382).\r\n\r\nR.M. acknowledges support by the Science and Technology
  Facilities Council (STFC), by the ERC through Advanced grant 695671 “QUENCH,” and
  by the UKRI Frontier Research grant RISEandFALL. R.M. also acknowledges funding
  from a research professorship from the Royal Society.\r\n\r\nI.S. acknowledges funding
  from the Atraccíon de Talento grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid,
  Spain, and the European Research Council (ERC) under the European Union’s Horizon
  2020 research and innovation program (grant No. 101117541, DistantDust).\r\n\r\nK.I.C.
  acknowledges funding from the Dutch Research Council (NWO) through the award of
  the Vici grant VI.C.212.036.\r\n\r\nFacilities: HST - Hubble Space Telescope satellite,
  JWST. -\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2022), Bagpipes (A.
  C. Carnall et al. 2019), MSAEXP (G. Brammer 2023) NumPy (C. R. Harris et al. 2020),
  pandas (The pandas development team 2024) Photutils (L. Bradley et al. 2016), TOPCAT
  (M. Taylor 2022)."
article_number: '86'
article_processing_charge: Yes
article_type: original
author:
- first_name: Pierluigi
  full_name: Rinaldi, Pierluigi
  last_name: Rinaldi
- first_name: Pablo G.
  full_name: Pérez-González, Pablo G.
  last_name: Pérez-González
- first_name: George H.
  full_name: Rieke, George H.
  last_name: Rieke
- first_name: Jianwei
  full_name: Lyu, Jianwei
  last_name: Lyu
- first_name: Francesco
  full_name: D’Eugenio, Francesco
  last_name: D’Eugenio
- first_name: Zihao
  full_name: Wu, Zihao
  last_name: Wu
- first_name: Stefano
  full_name: Carniani, Stefano
  last_name: Carniani
- first_name: Tobias J.
  full_name: Looser, Tobias J.
  last_name: Looser
- first_name: Irene
  full_name: Shivaei, Irene
  last_name: Shivaei
- first_name: Leindert A.
  full_name: Boogaard, Leindert A.
  last_name: Boogaard
- first_name: Tanio
  full_name: Diaz-Santos, Tanio
  last_name: Diaz-Santos
- first_name: Luis
  full_name: Colina, Luis
  last_name: Colina
- first_name: Göran
  full_name: Östlin, Göran
  last_name: Östlin
- first_name: Stacey
  full_name: Alberts, Stacey
  last_name: Alberts
- first_name: Javier
  full_name: Álvarez-Márquez, Javier
  last_name: Álvarez-Márquez
- first_name: Marianna
  full_name: Annuziatella, Marianna
  last_name: Annuziatella
- first_name: Manuel
  full_name: Aravena, Manuel
  last_name: Aravena
- first_name: Rachana
  full_name: Bhatawdekar, Rachana
  last_name: Bhatawdekar
- first_name: Andrew J.
  full_name: Bunker, Andrew J.
  last_name: Bunker
- first_name: Karina I.
  full_name: Caputi, Karina I.
  last_name: Caputi
- first_name: Stéphane
  full_name: Charlot, Stéphane
  last_name: Charlot
- first_name: Alejandro
  full_name: Crespo Gómez, Alejandro
  last_name: Crespo Gómez
- first_name: Mirko
  full_name: Curti, Mirko
  last_name: Curti
- first_name: Andreas
  full_name: Eckart, Andreas
  last_name: Eckart
- first_name: Steven
  full_name: Gillman, Steven
  last_name: Gillman
- first_name: Kevin
  full_name: Hainline, Kevin
  last_name: Hainline
- first_name: Nimisha
  full_name: Kumari, Nimisha
  last_name: Kumari
- first_name: Jens
  full_name: Hjorth, Jens
  last_name: Hjorth
- first_name: Edoardo
  full_name: Iani, Edoardo
  id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
  last_name: Iani
  orcid: 0000-0001-8386-3546
- first_name: Hanae
  full_name: Inami, Hanae
  last_name: Inami
- 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: Álvaro
  full_name: Labiano, Álvaro
  last_name: Labiano
- first_name: Roberto
  full_name: Maiolino, Roberto
  last_name: Maiolino
- first_name: Jens
  full_name: Melinder, Jens
  last_name: Melinder
- first_name: Thibaud
  full_name: Moutard, Thibaud
  last_name: Moutard
- first_name: Florian
  full_name: Peissker, Florian
  last_name: Peissker
- first_name: Marcia
  full_name: Rieke, Marcia
  last_name: Rieke
- first_name: Brant
  full_name: Robertson, Brant
  last_name: Robertson
- first_name: Jan
  full_name: Scholtz, Jan
  last_name: Scholtz
- first_name: Sandro
  full_name: Tacchella, Sandro
  last_name: Tacchella
- first_name: Paul P.
  full_name: Van Der Werf, Paul P.
  last_name: Van Der Werf
- first_name: Fabian
  full_name: Walter, Fabian
  last_name: Walter
- first_name: Christina C.
  full_name: Williams, Christina C.
  last_name: Williams
- first_name: Chris
  full_name: Willott, Chris
  last_name: Willott
- first_name: Joris
  full_name: Witstok, Joris
  last_name: Witstok
- first_name: Hannah
  full_name: Übler, Hannah
  last_name: Übler
- first_name: Yongda
  full_name: Zhu, Yongda
  last_name: Zhu
citation:
  ama: 'Rinaldi P, Pérez-González PG, Rieke GH, et al. Deciphering the nature of Virgil:
    An obscured active galactic nucleus lurking within an apparently normal Lyα emitter
    during cosmic reionization. <i>The Astrophysical Journal</i>. 2025;994(1). doi:<a
    href="https://doi.org/10.3847/1538-4357/ae089c">10.3847/1538-4357/ae089c</a>'
  apa: 'Rinaldi, P., Pérez-González, P. G., Rieke, G. H., Lyu, J., D’Eugenio, F.,
    Wu, Z., … Zhu, Y. (2025). Deciphering the nature of Virgil: An obscured active
    galactic nucleus lurking within an apparently normal Lyα emitter during cosmic
    reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae089c">https://doi.org/10.3847/1538-4357/ae089c</a>'
  chicago: 'Rinaldi, Pierluigi, Pablo G. Pérez-González, George H. Rieke, Jianwei
    Lyu, Francesco D’Eugenio, Zihao Wu, Stefano Carniani, et al. “Deciphering the
    Nature of Virgil: An Obscured Active Galactic Nucleus Lurking within an Apparently
    Normal Lyα Emitter during Cosmic Reionization.” <i>The Astrophysical Journal</i>.
    IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4357/ae089c">https://doi.org/10.3847/1538-4357/ae089c</a>.'
  ieee: 'P. Rinaldi <i>et al.</i>, “Deciphering the nature of Virgil: An obscured
    active galactic nucleus lurking within an apparently normal Lyα emitter during
    cosmic reionization,” <i>The Astrophysical Journal</i>, vol. 994, no. 1. IOP Publishing,
    2025.'
  ista: 'Rinaldi P, Pérez-González PG, Rieke GH, Lyu J, D’Eugenio F, Wu Z, Carniani
    S, Looser TJ, Shivaei I, Boogaard LA, Diaz-Santos T, Colina L, Östlin G, Alberts
    S, Álvarez-Márquez J, Annuziatella M, Aravena M, Bhatawdekar R, Bunker AJ, Caputi
    KI, Charlot S, Crespo Gómez A, Curti M, Eckart A, Gillman S, Hainline K, Kumari
    N, Hjorth J, Iani E, Inami H, Ji Z, Johnson BD, Jones GC, Labiano Á, Maiolino
    R, Melinder J, Moutard T, Peissker F, Rieke M, Robertson B, Scholtz J, Tacchella
    S, Van Der Werf PP, Walter F, Williams CC, Willott C, Witstok J, Übler H, Zhu
    Y. 2025. Deciphering the nature of Virgil: An obscured active galactic nucleus
    lurking within an apparently normal Lyα emitter during cosmic reionization. The
    Astrophysical Journal. 994(1), 86.'
  mla: 'Rinaldi, Pierluigi, et al. “Deciphering the Nature of Virgil: An Obscured
    Active Galactic Nucleus Lurking within an Apparently Normal Lyα Emitter during
    Cosmic Reionization.” <i>The Astrophysical Journal</i>, vol. 994, no. 1, 86, IOP
    Publishing, 2025, doi:<a href="https://doi.org/10.3847/1538-4357/ae089c">10.3847/1538-4357/ae089c</a>.'
  short: P. Rinaldi, P.G. Pérez-González, G.H. Rieke, J. Lyu, F. D’Eugenio, Z. Wu,
    S. Carniani, T.J. Looser, I. Shivaei, L.A. Boogaard, T. Diaz-Santos, L. Colina,
    G. Östlin, S. Alberts, J. Álvarez-Márquez, M. Annuziatella, M. Aravena, R. Bhatawdekar,
    A.J. Bunker, K.I. Caputi, S. Charlot, A. Crespo Gómez, M. Curti, A. Eckart, S.
    Gillman, K. Hainline, N. Kumari, J. Hjorth, E. Iani, H. Inami, Z. Ji, B.D. Johnson,
    G.C. Jones, Á. Labiano, R. Maiolino, J. Melinder, T. Moutard, F. Peissker, M.
    Rieke, B. Robertson, J. Scholtz, S. Tacchella, P.P. Van Der Werf, F. Walter, C.C.
    Williams, C. Willott, J. Witstok, H. Übler, Y. Zhu, The Astrophysical Journal
    994 (2025).
date_created: 2026-04-12T22:01:53Z
date_published: 2025-11-20T00:00:00Z
date_updated: 2026-04-13T07:54:11Z
day: '20'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae089c
file:
- access_level: open_access
  checksum: 5d13b0ad3e9f56cbe29c5de0ba5757c8
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  date_created: 2026-04-13T07:53:00Z
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fulldoi: https://doi.org/10.3847/1538-4357/ae089c
has_accepted_license: '1'
intvolume: '       994'
issue: '1'
language:
- iso: eng
month: '11'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Deciphering the nature of Virgil: An obscured active galactic nucleus lurking
  within an apparently normal Lyα emitter during cosmic reionization'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 994
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '18854'
abstract:
- lang: eng
  text: "Context. One of the surprising early findings with JWST has been the discovery
    of a strong “roll-over” or a softening of the absorption edge of Lyα in a large
    number of galaxies at z ≳ 6, in addition to systematic offsets from photometric
    redshift estimates and fundamental galaxy scaling relations. This has been interpreted
    as strong cumulative damped Lyα absorption (DLA) wings from high column densities
    of neutral atomic hydrogen (H I), signifying major gas accretion events in the
    formation of these galaxies.\r\nAims. To explore this new phenomenon systematically,
    we assembled the JWST/NIRSpec PRImordial gas Mass AssembLy (PRIMAL) legacy survey
    of 584 galaxies at z = 5.0 − 13.4, designed to study the physical properties and
    gas in and around galaxies during the reionization epoch.\r\nMethods. We characterized
    this benchmark sample in full and spectroscopically derived the galaxy redshifts,
    metallicities, star formation rates, and ultraviolet (UV) slopes. We defined a
    new diagnostic, the Lyα damping parameter DLyα, to measure and quantify the net
    effect of Lyα emission strength, the H I fraction in the intergalactic medium,
    or the local H I column density for each source. The JWST-PRIMAL survey is based
    on the spectroscopic DAWN JWST Archive (DJA-Spec). We describe DJA-Spec in this
    paper, detailing the reduction methods, the post-processing steps, and basic analysis
    tools. All the software, reduced spectra, and spectroscopically derived quantities
    and catalogs are made publicly available in dedicated repositories.\r\nResults.
    We find that the fraction of galaxies showing strong integrated DLAs with NHI > 1021 cm−2
    only increases slightly from ≈60% at z ≈ 6 up to ≈65 − 90% at z > 8. Similarly,
    the prevalence and prominence of Lyα emission is found to increase with decreasing
    redshift, in qualitative agreement with previous observational results. Strong
    Lyα emitters (LAEs) are predominantly found to be associated with low-metallicity
    and UV faint galaxies. By contrast, strong DLAs are observed in galaxies with
    a variety of intrinsic physical properties, but predominantly at high redshifts
    and low metallicities.\r\nConclusions. Our results indicate that strong DLAs likely
    reflect a particular early assembly phase of reionization-era galaxies, at which
    point they are largely dominated by pristine H I gas accretion. At z = 8 − 10,
    this gas gradually cools and forms into stars that ionize their local surroundings,
    forming large ionized bubbles and producing strong observed Lyα emission at z < 8."
acknowledgement: 'We would like to thank the referee for a detailed and constructive
  report, greatly improving the presentation of the results in this work. We would
  like to thank Peter Jakobsen for his vision and heroic endeavor in optimally designing
  the JWST/NIRSpec instrument and some of its first on-sky observations and for enlightening
  discussions about the intricacies of the NIRSpec data. Further, we would like to
  thank John Chisholm for helpful clarifications and discussions related to the escape
  fraction of ionizing photons and Aayush Saxena for enlightening conversations on
  the escape and absorption of Lyman-α photons. This work has received funding from
  the Swiss State Secretariat for Education, Research and Innovation (SERI) under
  contract number MB22.00072. The Cosmic Dawn Center (DAWN) is funded by the Danish
  National Research Foundation under grant DNRF140. The data products presented herein
  were retrieved from the DAWN JWST Archive (DJA). DJA is an initiative of the Cosmic
  Dawn Center, which is funded by the Danish National Research Foundation under grant
  DNRF140. P.D. acknowledge support from the NWO grant 016.VIDI.189.162 (“ODIN") and
  warmly thanks the European Commission’s and University of Groningen’s CO-FUND Rosalind
  Franklin program. Support from the ERC Advanced Grant INTERSTELLAR H2020/740120
  is kindly acknowledged (A.F.). S.G. acknowledges financial support from the Villum
  Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. M.K. was supported
  by the ANID BASAL project FB210003. G.E.M. acknowledges financial support from the
  Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. J.W.
  acknowledges support from the Science and Technology Facilities Council (STFC),
  by the ERC through Advanced Grant 695671 “QUENCH”, by the UKRI Frontier Research
  grant RISEandFALL. Support for this work was provided by NASA through the NASA Hubble
  Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in Astronomy,
  Incorporated, under NASA contract NAS5-26555. F.C. acknowledges support from a UKRI
  Frontier Research Guarantee Grant (PI Cullen; grant reference EP/X021025/1). J.H.W.
  acknowledges support by NSF grant AST-2108020 and NASA grants 80NSSC20K0520 and
  80NSSC21K1053. NRT acknowledges support through STFC consolidated grant ST/W000857/1.
  M.J.H. is supported by the Swedish Research Council, VetenskapsrÅdet, and is fellow
  of the Knut & Alice Wallenberg foundation. This work is based in part on observations
  made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from
  the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science
  Institute, which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. Software: This work made
  use of and acknowledge the following software: NumPy (Harris et al. 2020), Matplotlib
  (Hunter 2007), LMfit (Newville et al. 2014), SciPy (Virtanen et al. 2020), grizli
  (Brammer 2023a), Astrodrizzle (Gonzaga et al. 2012), and MsaExp (v0.3; Brammer 2023b).'
article_number: A60
article_processing_charge: No
article_type: original
author:
- first_name: K. E.
  full_name: Heintz, K. E.
  last_name: Heintz
- first_name: G. B.
  full_name: Brammer, G. B.
  last_name: Brammer
- first_name: D.
  full_name: Watson, D.
  last_name: Watson
- first_name: P. A.
  full_name: Oesch, P. A.
  last_name: Oesch
- first_name: L. C.
  full_name: Keating, L. C.
  last_name: Keating
- first_name: M. J.
  full_name: Hayes, M. J.
  last_name: Hayes
- first_name: Unknown
  full_name: Abdurro'Uf, Unknown
  last_name: Abdurro'Uf
- first_name: K. Z.
  full_name: Arellano-Córdova, K. Z.
  last_name: Arellano-Córdova
- first_name: A. C.
  full_name: Carnall, A. C.
  last_name: Carnall
- first_name: C. R.
  full_name: Christiansen, C. R.
  last_name: Christiansen
- first_name: F.
  full_name: Cullen, F.
  last_name: Cullen
- first_name: R.
  full_name: Davé, R.
  last_name: Davé
- first_name: P.
  full_name: Dayal, P.
  last_name: Dayal
- first_name: A.
  full_name: Ferrara, A.
  last_name: Ferrara
- first_name: K.
  full_name: Finlator, K.
  last_name: Finlator
- first_name: J. P.U.
  full_name: Fynbo, J. P.U.
  last_name: Fynbo
- first_name: S. R.
  full_name: Flury, S. R.
  last_name: Flury
- first_name: V.
  full_name: Gelli, V.
  last_name: Gelli
- first_name: S.
  full_name: Gillman, S.
  last_name: Gillman
- first_name: R.
  full_name: Gottumukkala, R.
  last_name: Gottumukkala
- first_name: K.
  full_name: Gould, K.
  last_name: Gould
- first_name: T. R.
  full_name: Greve, T. R.
  last_name: Greve
- first_name: S. E.
  full_name: Hardin, S. E.
  last_name: Hardin
- first_name: T. Y.Y.
  full_name: Hsiao, T. Y.Y.
  last_name: Hsiao
- first_name: A.
  full_name: Hutter, A.
  last_name: Hutter
- first_name: P.
  full_name: Jakobsson, P.
  last_name: Jakobsson
- first_name: M.
  full_name: Killi, M.
  last_name: Killi
- first_name: N.
  full_name: Khosravaninezhad, N.
  last_name: Khosravaninezhad
- first_name: P.
  full_name: Laursen, P.
  last_name: Laursen
- first_name: M. M.
  full_name: Lee, M. M.
  last_name: Lee
- first_name: G. E.
  full_name: Magdis, G. E.
  last_name: Magdis
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: R. P.
  full_name: Naidu, R. P.
  last_name: Naidu
- first_name: D.
  full_name: Narayanan, D.
  last_name: Narayanan
- first_name: C.
  full_name: Pollock, C.
  last_name: Pollock
- first_name: M. K.M.
  full_name: Prescott, M. K.M.
  last_name: Prescott
- first_name: V.
  full_name: Rusakov, V.
  last_name: Rusakov
- first_name: M.
  full_name: Shuntov, M.
  last_name: Shuntov
- first_name: A.
  full_name: Sneppen, A.
  last_name: Sneppen
- first_name: R.
  full_name: Smit, R.
  last_name: Smit
- first_name: N. R.
  full_name: Tanvir, N. R.
  last_name: Tanvir
- first_name: C.
  full_name: Terp, C.
  last_name: Terp
- first_name: S.
  full_name: Toft, S.
  last_name: Toft
- first_name: F.
  full_name: Valentino, F.
  last_name: Valentino
- first_name: A. P.
  full_name: Vijayan, A. P.
  last_name: Vijayan
- first_name: J. R.
  full_name: Weaver, J. R.
  last_name: Weaver
- first_name: J. H.
  full_name: Wise, J. H.
  last_name: Wise
- first_name: J.
  full_name: Witstok, J.
  last_name: Witstok
citation:
  ama: 'Heintz KE, Brammer GB, Watson D, et al. The JWST-PRIMAL archival survey: A
    JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption
    and emission of ∼600 galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>.
    2025;693. doi:<a href="https://doi.org/10.1051/0004-6361/202450243">10.1051/0004-6361/202450243</a>'
  apa: 'Heintz, K. E., Brammer, G. B., Watson, D., Oesch, P. A., Keating, L. C., Hayes,
    M. J., … Witstok, J. (2025). The JWST-PRIMAL archival survey: A JWST/NIRSpec reference
    sample for the physical properties and Lyman-α absorption and emission of ∼600
    galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a
    href="https://doi.org/10.1051/0004-6361/202450243">https://doi.org/10.1051/0004-6361/202450243</a>'
  chicago: 'Heintz, K. E., G. B. Brammer, D. Watson, P. A. Oesch, L. C. Keating, M.
    J. Hayes, Unknown Abdurro’Uf, et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec
    Reference Sample for the Physical Properties and Lyman-α Absorption and Emission
    of ∼600 Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences,
    2025. <a href="https://doi.org/10.1051/0004-6361/202450243">https://doi.org/10.1051/0004-6361/202450243</a>.'
  ieee: 'K. E. Heintz <i>et al.</i>, “The JWST-PRIMAL archival survey: A JWST/NIRSpec
    reference sample for the physical properties and Lyman-α absorption and emission
    of ∼600 galaxies at z = 5.0-13.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 693.
    EDP Sciences, 2025.'
  ista: 'Heintz KE, Brammer GB, Watson D, Oesch PA, Keating LC, Hayes MJ, Abdurro’Uf
    U, Arellano-Córdova KZ, Carnall AC, Christiansen CR, Cullen F, Davé R, Dayal P,
    Ferrara A, Finlator K, Fynbo JPU, Flury SR, Gelli V, Gillman S, Gottumukkala R,
    Gould K, Greve TR, Hardin SE, Hsiao TYY, Hutter A, Jakobsson P, Killi M, Khosravaninezhad
    N, Laursen P, Lee MM, Magdis GE, Matthee JJ, Naidu RP, Narayanan D, Pollock C,
    Prescott MKM, Rusakov V, Shuntov M, Sneppen A, Smit R, Tanvir NR, Terp C, Toft
    S, Valentino F, Vijayan AP, Weaver JR, Wise JH, Witstok J. 2025. The JWST-PRIMAL
    archival survey: A JWST/NIRSpec reference sample for the physical properties and
    Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy &#38;
    Astrophysics. 693, A60.'
  mla: 'Heintz, K. E., et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference
    Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600
    Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 693, A60,
    EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202450243">10.1051/0004-6361/202450243</a>.'
  short: K.E. Heintz, G.B. Brammer, D. Watson, P.A. Oesch, L.C. Keating, M.J. Hayes,
    U. Abdurro’Uf, K.Z. Arellano-Córdova, A.C. Carnall, C.R. Christiansen, F. Cullen,
    R. Davé, P. Dayal, A. Ferrara, K. Finlator, J.P.U. Fynbo, S.R. Flury, V. Gelli,
    S. Gillman, R. Gottumukkala, K. Gould, T.R. Greve, S.E. Hardin, T.Y.Y. Hsiao,
    A. Hutter, P. Jakobsson, M. Killi, N. Khosravaninezhad, P. Laursen, M.M. Lee,
    G.E. Magdis, J.J. Matthee, R.P. Naidu, D. Narayanan, C. Pollock, M.K.M. Prescott,
    V. Rusakov, M. Shuntov, A. Sneppen, R. Smit, N.R. Tanvir, C. Terp, S. Toft, F.
    Valentino, A.P. Vijayan, J.R. Weaver, J.H. Wise, J. Witstok, Astronomy &#38; Astrophysics
    693 (2025).
date_created: 2025-01-19T23:01:52Z
date_published: 2025-01-06T00:00:00Z
date_updated: 2026-02-16T12:07:37Z
day: '06'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450243
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  file_name: 2025_AstronomyAstrophysics_Heintz.pdf
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  relation: main_file
  success: 1
file_date_updated: 2025-01-20T09:17:33Z
fulldoi: https://doi.org/10.1051/0004-6361/202450243
has_accepted_license: '1'
intvolume: '       693'
isi: 1
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical
  properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 693
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '19066'
abstract:
- lang: eng
  text: "We present a sample of 1956 individual stellar clumps at redshift 0.7 < z
    < 10, detected with JWST/NIRCam in 476 galaxies lensed by the galaxy cluster Abell2744.
    The lensed clumps present magnifications ranging between μ = 1.8 and μ = 300.
    We perform simultaneous size-photometry estimates in 20 JWST/NIRCam median and
    broad-band filters from 0.7 to 5 μm.\r\nSpectral energy distribution (SED) fitting
    analyses enable us to recover the physical properties of the clumps. The majority
    of the clumps are spatially resolved and have effective radii in the range Reff
    = 10–700 pc. We restrict this first study to the 1751 post-reionization era clumps
    with redshift < 5.5. We find a significant evolution of the average clump ages,
    star formation rates (SFRs), SFR surface densities, and metallicity with increasing
    redshift, while median stellar mass and stellar mass surface densities are similar
    in the probed redshift range. We observe a strong correlation between the clump
    properties and the properties of their host galaxies, with more massive galaxies
    hosting more massive and older clumps. We find that clumps closer to their host
    galactic centre are on average more massive, while their ages do not show clear
    sign of migration. We find that clumps at cosmic noon sample the upper-mass end
    of the mass function to higher masses than at z > 3, reflecting the rapid increase
    towards the peak of the cosmic star formation history. We conclude that the results
    achieved over the studied redshift range are in agreement with expectation of
    in situ clump formation scenario from large-scale disc fragmentation. "
acknowledgement: 'The authors thank the International Space Science Institute for
  sponsoring the ISSI team: ‘Star Formation within rapidly evolving galaxies’ where
  many ideas discussed in this article have been brainstormed. AA and AC acknowledge
  support by the Swedish research council Vetenskapsrådet (2021-05559). MM acknowledges
  the financial support through grant PRIN-MIUR 2020SKSTHZ. JM and IK acknowledge
  support by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed
  are however those of the author(s) only and do not necessarily reflect those of
  the European Union or the European Research Council. Neither the European Union
  nor the granting authority can be held responsible for them. RPN acknowledges funding
  from JWST programme GO-3516. Support for this work was provided by NASA through
  the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope
  Science Institute, which is operated by the Association of Universities for Research
  in Astronomy, Incorporated, under NASA contract NAS5-26555.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Adélaïde
  full_name: Claeyssens, Adélaïde
  last_name: Claeyssens
- first_name: Angela
  full_name: Adamo, Angela
  last_name: Adamo
- first_name: Matteo
  full_name: Messa, Matteo
  last_name: Messa
- first_name: Miroslava
  full_name: Dessauges-Zavadsky, Miroslava
  last_name: Dessauges-Zavadsky
- first_name: Johan
  full_name: Richard, Johan
  last_name: Richard
- first_name: Ivan
  full_name: Kramarenko, Ivan
  id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
  last_name: Kramarenko
  orcid: 0000-0001-5346-6048
- 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
citation:
  ama: Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic
    time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2025;537(3):2535-2558. doi:<a href="https://doi.org/10.1093/mnras/staf058">10.1093/mnras/staf058</a>
  apa: Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J.,
    Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time
    at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/staf058">https://doi.org/10.1093/mnras/staf058</a>
  chicago: Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky,
    Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing
    Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster
    Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2025. <a href="https://doi.org/10.1093/mnras/staf058">https://doi.org/10.1093/mnras/staf058</a>.
  ieee: A. Claeyssens <i>et al.</i>, “Tracing star formation across cosmic time at
    tens of parsec-scales in the lensing cluster field Abell 2744,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 537, no. 3. Oxford University Press,
    pp. 2535–2558, 2025.
  ista: Claeyssens A, Adamo A, Messa M, Dessauges-Zavadsky M, Richard J, Kramarenko
    I, Matthee JJ, Naidu RP. 2025. Tracing star formation across cosmic time at tens
    of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the
    Royal Astronomical Society. 537(3), 2535–2558.
  mla: Claeyssens, Adélaïde, et al. “Tracing Star Formation across Cosmic Time at
    Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 537, no. 3, Oxford University Press,
    2025, pp. 2535–58, doi:<a href="https://doi.org/10.1093/mnras/staf058">10.1093/mnras/staf058</a>.
  short: A. Claeyssens, A. Adamo, M. Messa, M. Dessauges-Zavadsky, J. Richard, I.
    Kramarenko, J.J. Matthee, R.P. Naidu, Monthly Notices of the Royal Astronomical
    Society 537 (2025) 2535–2558.
date_created: 2025-02-23T23:01:55Z
date_published: 2025-03-01T00:00:00Z
date_updated: 2026-02-16T11:51:48Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1093/mnras/staf058
external_id:
  arxiv:
  - '2410.10974'
  isi:
  - '001420026000001'
file:
- access_level: open_access
  checksum: 431aef05755e6b5472f5e9b4c326cf84
  content_type: application/pdf
  creator: dernst
  date_created: 2025-02-25T06:38:43Z
  date_updated: 2025-02-25T06:38:43Z
  file_id: '19084'
  file_name: 2025_MonthlyNoticesRAS_Claeyssens.pdf
  file_size: 35099276
  relation: main_file
  success: 1
file_date_updated: 2025-02-25T06:38:43Z
fulldoi: https://doi.org/10.1093/mnras/staf058
has_accepted_license: '1'
intvolume: '       537'
isi: 1
issue: '3'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
page: 2535-2558
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
  grant_number: '101076224'
  name: Young galaxies as tracers and agents of cosmic reionization
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Tracing star formation across cosmic time at tens of parsec-scales in the lensing
  cluster field Abell 2744
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: 537
year: '2025'
...
---
OA_place: publisher
OA_type: hybrid
_id: '19069'
abstract:
- lang: eng
  text: "Context. The hydrogen Lyman-alpha (Lyα) line, the brightest rest-frame ultraviolet
    line of high-redshift galaxies, exhibits a large variety of shapes, which is due
    to factors at different scales, from the interstellar medium to the intergalactic
    medium (IGM).\r\nAims. The aim of this work is to provide a systematic inventory
    and classification of the spectral shapes of Lyα emission lines to better understand
    the general population of high-redshift Lyα emitting galaxies (LAEs).\r\nMethods.
    Using the unprecedentedly deep data from the MUSE eXtremely Deep Field (MXDF;
    up to 140 hour exposure time), we selected 477 galaxies observed in the ∼2.8−6.6
    redshift range, 15 of which have a systemic redshift from nebular lines. We developed
    a method to classify Lyα emission lines in four spectral and three spatial categories
    by combining a pure spectral analysis with a narrow-band image analysis. We measured
    spectral properties, such as the peak separation and the blue-to-total flux ratio
    for the double-peaked galaxies.\r\nResults. To ensure a robust sample for statistical
    analysis, we define two unbiased subsets, inclusive and restrictive, by applying
    thresholds for signal-to-noise ratio, peak separation, and Lyα luminosity, yielding
    a final unbiased sample of 206 galaxies. Our analysis reveals that between 32%
    and 51% of the galaxies exhibit double-peaked profiles, with peak separations
    ranging from 150 km s−1 to nearly 1600 km s−1. The fraction of double-peaked galaxies
    seems to evolve dependently with the Lyα luminosity, while we do not see a severe
    decrease in this fraction with redshift, which is expected given the IGM attenuation
    at high redshift. An artificial increase in the number of double-peaked galaxies
    at the highest redshifts may cause the observation of a plateau instead of a decrease.
    A notable number of these double-peaked profiles show blue-dominated spectra,
    suggesting unique gas dynamics and inflow characteristics in some high-redshift
    galaxies. The consequent fraction of blue-dominated spectra needs to be confirmed
    by obtaining new systemic redshift measurements. Among the double-peaked galaxies,
    4% are spurious detections, that is, the blue and red peaks do not come from the
    same spatial location. Around 20% out of the 477 sources of the parent sample
    lie in a complex environment, meaning there are other clumps or galaxies at the
    same redshift within a distance of 30 kpc.\r\nConclusions. Our results suggest
    that the double-peaked LAE fraction may trace the evolution of IGM attenuation,
    but the faintest galaxies must be observed at high redshift. We also need more
    data to confirm the trend seen at low redshift. In addition, it is crucial to
    obtain secure systemic redshifts for LAEs to better constrain the nature of the
    Lyα double-peaked lines. Statistical samples of double-peaked and triple-peaked
    galaxies are a promising probe of the evolution of the physical properties of
    galaxies across cosmic time."
acknowledgement: 'EV and AV acknowledges the support from the SNF grants PP00P2 176808
  and 211023. HK acknowledges support from Japan Society for the Promotion of Science
  (JSPS) Overseas Research Fellowship as well as JSPS Research Fellowships for Young
  Scientists. JP acknowledges funding by the Deutsche Forschungsgemeinschaft, Grant
  Wi 1369/31-1. This work is based on observations taken by VLT, which is operated
  by European Southern Observatory. This research made use of ASTROPY, which is a
  community-developed core Python package for Astronomy (Astropy Collaboration 2013,
  2018, 2022), and other software and packages: MPDAF (Piqueras et al. 2019), PHOTUTILS
  (Bradley 2023), NUMPY (van der Walt et al. 2011), SCIPY (Virtanen et al. 2020).
  The plots in this paper were created using MATPLOTLIB (Hunter 2007).'
article_number: A100
article_processing_charge: No
article_type: original
author:
- first_name: Eloïse
  full_name: Vitte, Eloïse
  last_name: Vitte
- first_name: Anne
  full_name: Verhamme, Anne
  last_name: Verhamme
- first_name: Pascale
  full_name: Hibon, Pascale
  last_name: Hibon
- first_name: Floriane
  full_name: Leclercq, Floriane
  last_name: Leclercq
- first_name: Belén
  full_name: Alcalde Pampliega, Belén
  last_name: Alcalde Pampliega
- first_name: Josephine
  full_name: Kerutt, Josephine
  last_name: Kerutt
- first_name: Haruka
  full_name: Kusakabe, Haruka
  last_name: Kusakabe
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Yucheng
  full_name: Guo, Yucheng
  last_name: Guo
- first_name: Roland
  full_name: Bacon, Roland
  last_name: Bacon
- first_name: Michael
  full_name: Maseda, Michael
  last_name: Maseda
- first_name: Johan
  full_name: Richard, Johan
  last_name: Richard
- first_name: John
  full_name: Pharo, John
  last_name: Pharo
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Leindert
  full_name: Boogaard, Leindert
  last_name: Boogaard
- first_name: Themiya
  full_name: Nanayakkara, Themiya
  last_name: Nanayakkara
- first_name: Thierry
  full_name: Contini, Thierry
  last_name: Contini
citation:
  ama: 'Vitte E, Verhamme A, Hibon P, et al. The MUSE eXtremely Deep Field: Classifying
    the spectral shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>.
    2025;694. doi:<a href="https://doi.org/10.1051/0004-6361/202450426">10.1051/0004-6361/202450426</a>'
  apa: 'Vitte, E., Verhamme, A., Hibon, P., Leclercq, F., Alcalde Pampliega, B., Kerutt,
    J., … Contini, T. (2025). The MUSE eXtremely Deep Field: Classifying the spectral
    shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences.
    <a href="https://doi.org/10.1051/0004-6361/202450426">https://doi.org/10.1051/0004-6361/202450426</a>'
  chicago: 'Vitte, Eloïse, Anne Verhamme, Pascale Hibon, Floriane Leclercq, Belén
    Alcalde Pampliega, Josephine Kerutt, Haruka Kusakabe, et al. “The MUSE EXtremely
    Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202450426">https://doi.org/10.1051/0004-6361/202450426</a>.'
  ieee: 'E. Vitte <i>et al.</i>, “The MUSE eXtremely Deep Field: Classifying the spectral
    shapes of Ly α -emitting galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol.
    694. EDP Sciences, 2025.'
  ista: 'Vitte E, Verhamme A, Hibon P, Leclercq F, Alcalde Pampliega B, Kerutt J,
    Kusakabe H, Matthee JJ, Guo Y, Bacon R, Maseda M, Richard J, Pharo J, Schaye J,
    Boogaard L, Nanayakkara T, Contini T. 2025. The MUSE eXtremely Deep Field: Classifying
    the spectral shapes of Ly α -emitting galaxies. Astronomy &#38; Astrophysics.
    694, A100.'
  mla: 'Vitte, Eloïse, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral
    Shapes of Ly α -Emitting Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol.
    694, A100, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202450426">10.1051/0004-6361/202450426</a>.'
  short: E. Vitte, A. Verhamme, P. Hibon, F. Leclercq, B. Alcalde Pampliega, J. Kerutt,
    H. Kusakabe, J.J. Matthee, Y. Guo, R. Bacon, M. Maseda, J. Richard, J. Pharo,
    J. Schaye, L. Boogaard, T. Nanayakkara, T. Contini, Astronomy &#38; Astrophysics
    694 (2025).
date_created: 2025-02-23T23:01:56Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2026-02-16T12:08:40Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450426
external_id:
  isi:
  - '001417357000009'
file:
- access_level: open_access
  checksum: ed2a5bba313e54ed250be348bd8c1d95
  content_type: application/pdf
  creator: dernst
  date_created: 2025-02-25T07:19:34Z
  date_updated: 2025-02-25T07:19:34Z
  file_id: '19087'
  file_name: 2025_AstronomyAstrophysics_Vitte.pdf
  file_size: 3444203
  relation: main_file
  success: 1
file_date_updated: 2025-02-25T07:19:34Z
fulldoi: https://doi.org/10.1051/0004-6361/202450426
has_accepted_license: '1'
intvolume: '       694'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
  issnl:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting
  galaxies'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 694
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19070'
abstract:
- lang: eng
  text: "Context. Recent observations suggest a significant and rapid buildup of dust
    in galaxies at high redshift (z > 4); this presents new challenges to our understanding
    of galaxy formation in the early Universe. Although our understanding of the physics
    of dust production and destruction in a galaxy’s interstellar medium (ISM) is
    improving, investigating the baryonic processes in the early universe remains
    a complex task owing to the inherent degeneracies in cosmological simulations
    and chemical evolution models.\r\nAims. In this work we characterized the evolution
    of 98 z ∼ 5 star-forming galaxies observed as part of the ALMA Large Program ALPINE
    by constraining the physical processes underpinning the gas and dust production,
    consumption, and destruction in their ISM.\r\nMethods. We made use of chemical
    evolution models to simultaneously reproduce the observed dust and gas content
    of our galaxies, obtained respectively from spectral energy distribution (SED)
    fitting and ionized carbon measurements. For each galaxy we constrained the initial
    gas mass, gas inflows and outflows, and efficiencies of dust growth and destruction.
    We tested these models with both the canonical Chabrier and a top-heavy initial
    mass function (IMF); the latter allowed rapid dust production on shorter timescales.\r\nResults.
    We successfully reproduced the gas and dust content in most of the older galaxies
    (≳600 Myr) regardless of the assumed IMF, predicting dust production primarily
    through Type II supernovae (SNe) and no dust growth in the ISM, as well as moderate
    inflow of primordial gas. In the case of intermediate-age galaxies (300−600 Myr),
    we reproduced the gas and dust content through Type II SNe and dust growth in
    ISM, though we observed an overprediction of dust mass in older galaxies, potentially
    indicating an unaccounted dust destruction mechanism and/or an overestimation
    of the observed dust masses. The number of young galaxies (≲300 Myr) reproduced,
    increases for models assuming top-heavy IMF but with maximal prescriptions of
    dust production. Galactic outflows are required (up to a mass-loading factor of
    2) to reproduce the observed gas and dust mass, and to recover the decreasing
    trend of gas and dust over stellar mass with age. Assuming the Chabrier IMF, models
    are able to reproduce ∼65% of the total sample, while with top-heavy IMF the fraction
    increases to ∼93%, alleviating the tension between the observations and the models.
    Observations from the James Webb Space Telescope (JWST) will allow us to remove
    degeneracies in the diverse intrinsic properties of these galaxies (e.g., star
    formation histories and metallicity), thereby refining our models."
acknowledgement: 'We warmly thank the referee for her/his useful comments and suggestions
  that greatly improved the quality of our paper. P.S., A.N., and M.R. acknowledge
  support from the Narodowe Centrum Nauki (UMO2020/38/E/ST9/00077). M.R. acknowledges
  support from the Foundation for Polish Science (FNP) under the program START 063.2023.
  D.D. acknowledges support from the National Science Center (NCN) grant SONATA (UMO2020/39/D/ST9/00720).
  J. and K.M. are grateful for the support from the Polish National Science Centre
  via grant UMO-018/30/E/ST9/00082. J. acknowledges support from the European Union
  (MSCA EDUCADO, GA 101119830 and WIDERA ExGal-Twin, GA 101158446). M.B. gratefully
  acknowledges support from the ANID BASAL project FB210003 and from the FONDECYT
  regular grant 1211000. This work was supported by the French government through
  the France 2030 investment plan managed by the National Research Agency (ANR), as
  part of the Initiative of Excellence of Université Côte d’Azur under reference number
  ANR-15-IDEX-01. M.H. acknowledges support from the Polish National Science Center
  (UMO-2022/45/N/ST9/01336). E.I. acknowledges funding by ANID FONDECYT Regular 1221846.
  G.E.M. acknowledges the Villum Fonden research grant 13160 “Gas to stars, stars
  to dust: tracing star formation across cosmic time”, grant 37440, “The Hidden Cosmos”,
  and the Cosmic Dawn Center of Excellence funded by the Danish National Research
  Foundation under the grant No. 140.'
article_number: A82
article_processing_charge: Yes
article_type: original
author:
- first_name: P.
  full_name: Sawant, P.
  last_name: Sawant
- first_name: A.
  full_name: Nanni, A.
  last_name: Nanni
- first_name: M.
  full_name: Romano, M.
  last_name: Romano
- first_name: D.
  full_name: Donevski, D.
  last_name: Donevski
- first_name: G.
  full_name: Bruzual, G.
  last_name: Bruzual
- first_name: N.
  full_name: Ysard, N.
  last_name: Ysard
- first_name: B. C.
  full_name: Lemaux, B. C.
  last_name: Lemaux
- first_name: H.
  full_name: Inami, H.
  last_name: Inami
- first_name: F.
  full_name: Calura, F.
  last_name: Calura
- first_name: F.
  full_name: Pozzi, F.
  last_name: Pozzi
- first_name: K.
  full_name: Małek, K.
  last_name: Małek
- first_name: J.
  full_name: Junais, J.
  last_name: Junais
- first_name: M.
  full_name: Boquien, M.
  last_name: Boquien
- first_name: A. L.
  full_name: Faisst, A. L.
  last_name: Faisst
- first_name: M.
  full_name: Hamed, M.
  last_name: Hamed
- first_name: M.
  full_name: Ginolfi, M.
  last_name: Ginolfi
- first_name: G.
  full_name: Zamorani, G.
  last_name: Zamorani
- first_name: G.
  full_name: Lorenzon, G.
  last_name: Lorenzon
- first_name: J.
  full_name: Molina, J.
  last_name: Molina
- first_name: S.
  full_name: Bardelli, S.
  last_name: Bardelli
- first_name: E.
  full_name: Ibar, E.
  last_name: Ibar
- first_name: D.
  full_name: Vergani, D.
  last_name: Vergani
- first_name: Claudia
  full_name: Di Cesare, Claudia
  id: 2d002343-372f-11ef-98ec-a164d20427cb
  last_name: Di Cesare
- first_name: M.
  full_name: Béthermin, M.
  last_name: Béthermin
- first_name: D.
  full_name: Burgarella, D.
  last_name: Burgarella
- first_name: P.
  full_name: Cassata, P.
  last_name: Cassata
- first_name: M.
  full_name: Dessauges-Zavadsky, M.
  last_name: Dessauges-Zavadsky
- first_name: E.
  full_name: D'Onghia, E.
  last_name: D'Onghia
- first_name: Y.
  full_name: Dubois, Y.
  last_name: Dubois
- first_name: G. E.
  full_name: Magdis, G. E.
  last_name: Magdis
- first_name: H.
  full_name: Mendez-Hernandez, H.
  last_name: Mendez-Hernandez
citation:
  ama: 'Sawant P, Nanni A, Romano M, et al. The ALPINE-ALMA [CII] survey: Unveiling
    the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies.
    <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href="https://doi.org/10.1051/0004-6361/202451542">10.1051/0004-6361/202451542</a>'
  apa: 'Sawant, P., Nanni, A., Romano, M., Donevski, D., Bruzual, G., Ysard, N., …
    Mendez-Hernandez, H. (2025). The ALPINE-ALMA [CII] survey: Unveiling the baryon
    evolution in the interstellar medium of z ∼ 5 star-forming galaxies. <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202451542">https://doi.org/10.1051/0004-6361/202451542</a>'
  chicago: 'Sawant, P., A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B.
    C. Lemaux, et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution
    in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202451542">https://doi.org/10.1051/0004-6361/202451542</a>.'
  ieee: 'P. Sawant <i>et al.</i>, “The ALPINE-ALMA [CII] survey: Unveiling the baryon
    evolution in the interstellar medium of z ∼ 5 star-forming galaxies,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.'
  ista: 'Sawant P, Nanni A, Romano M, Donevski D, Bruzual G, Ysard N, Lemaux BC, Inami
    H, Calura F, Pozzi F, Małek K, Junais J, Boquien M, Faisst AL, Hamed M, Ginolfi
    M, Zamorani G, Lorenzon G, Molina J, Bardelli S, Ibar E, Vergani D, Di Cesare
    C, Béthermin M, Burgarella D, Cassata P, Dessauges-Zavadsky M, D’Onghia E, Dubois
    Y, Magdis GE, Mendez-Hernandez H. 2025. The ALPINE-ALMA [CII] survey: Unveiling
    the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies.
    Astronomy &#38; Astrophysics. 694, A82.'
  mla: 'Sawant, P., et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution
    in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38;
    Astrophysics</i>, vol. 694, A82, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202451542">10.1051/0004-6361/202451542</a>.'
  short: P. Sawant, A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B.C. Lemaux,
    H. Inami, F. Calura, F. Pozzi, K. Małek, J. Junais, M. Boquien, A.L. Faisst, M.
    Hamed, M. Ginolfi, G. Zamorani, G. Lorenzon, J. Molina, S. Bardelli, E. Ibar,
    D. Vergani, C. Di Cesare, M. Béthermin, D. Burgarella, P. Cassata, M. Dessauges-Zavadsky,
    E. D’Onghia, Y. Dubois, G.E. Magdis, H. Mendez-Hernandez, Astronomy &#38; Astrophysics
    694 (2025).
date_created: 2025-02-23T23:01:56Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2026-02-16T12:08:24Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202451542
external_id:
  isi:
  - '001414753300028'
file:
- access_level: open_access
  checksum: 792cbcda14148c352dc8c5a26058827d
  content_type: application/pdf
  creator: dernst
  date_created: 2025-02-25T07:05:19Z
  date_updated: 2025-02-25T07:05:19Z
  file_id: '19086'
  file_name: 2025_AstronomyAstrophysics_Sawant.pdf
  file_size: 7624067
  relation: main_file
  success: 1
file_date_updated: 2025-02-25T07:05:19Z
fulldoi: https://doi.org/10.1051/0004-6361/202451542
has_accepted_license: '1'
intvolume: '       694'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar
  medium of z ∼ 5 star-forming galaxies'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 694
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19284'
abstract:
- lang: eng
  text: The Hα nebular emission line is an optimal tracer for recent star formation
    in galaxies. With the advent of JWST, this line has recently become observable
    at z > 3 for the first time. We present a catalog of 1050 Hα emitters at 3.7 < z < 6.7
    in the GOODS fields obtained from a blind search in JWST NIRCam/grism data. We
    made use of the FRESCO survey’s 124 arcmin2 of observations in GOODS-North and
    GOODS-South with the F444W filter, probing Hα at 4.9 < z < 6.7, and the CONGRESS
    survey’s 62 arcmin2 of observations in GOODS-North with F356W, probing Hα at 3.8 < z < 5.1.
    We found an overdensity with 98 sources at z ∼ 4.4 in GOODS-N, and confirmed previously
    reported overdensities at z ∼ 5.2 in GOODS-N and at z ∼ 5.4 and z ∼ 5.9 in GOODS-S.
    We computed the observed Hα luminosity functions (LFs) in three bins centered
    at z ∼ 4.45, 5.30, and 6.15, which are the first such measurements at z > 3 obtained
    based purely on spectroscopic data, robustly tracing galaxy star formation rates
    (SFRs) beyond the peak of the cosmic star formation history. We compared our results
    with theoretical predictions from three different simulations and found good agreement
    at z ∼ 4 − 6. The UV LFs of this spectroscopically confirmed sample are in good
    agreement with pre-JWST measurements obtained with photometrically selected objects.
    Finally, we derived SFR functions and integrated them to compute the evolution
    of the cosmic SFR densities across z ∼ 4 − 6, finding values in good agreement
    with recent UV estimates from Lyman-break galaxies, which imply a continuous decrease
    in SFR density by a factor of three over z ∼ 4 to z ∼ 6. Our work shows the power
    of NIRCam grism observations to efficiently provide new tests for early galaxy
    formation models based on emission line statistics.
acknowledgement: 'This work is based on observations made with the NASA/ESA/CSA James
  Webb Space Telescope. The data were obtained from the Mikulski Archive for Space
  Telescopes at the Space Telescope Science Institute, which is operated by the Association
  of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127
  for JWST. These observations are associated with program Nos. 1895 and 3577. The
  authors sincerely thank the CONGRESS team (PIs: Egami & Sun) for developing their
  observing program with a zero-exclusive-access period. We thank Aswin Vijayan and
  Harley Katz for their help in analyzing the simulation data from FLARES and SPHINX.
  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 (DAWN) is funded by the Danish National Research Foundation under grant
  DNRF140. Support for program #1895 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. Support for this
  work for RPN was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A
  awarded by the Space Telescope Science Institute, which is operated by the Association
  of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
  MS acknowledges support from the European Research Commission Consolidator Grant
  101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and
  from project PID2023-149420NB-I00 funded by MICIU/AEI/10.13039/501100011033 and
  by ERDF/EU.'
article_number: A178
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alba
  full_name: Covelo-Paz, Alba
  last_name: Covelo-Paz
- first_name: Emma
  full_name: Giovinazzo, Emma
  last_name: Giovinazzo
- first_name: Pascal A.
  full_name: Oesch, Pascal A.
  last_name: Oesch
- first_name: Romain A.
  full_name: Meyer, Romain A.
  last_name: Meyer
- first_name: Andrea
  full_name: Weibel, Andrea
  last_name: Weibel
- first_name: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Yoshinobu
  full_name: Fudamoto, Yoshinobu
  last_name: Fudamoto
- first_name: Josephine
  full_name: Kerutt, Josephine
  last_name: Kerutt
- first_name: Jamie
  full_name: Lin, Jamie
  last_name: Lin
- first_name: Jasleen
  full_name: Matharu, Jasleen
  last_name: Matharu
- first_name: Rohan P.
  full_name: Naidu, Rohan P.
  last_name: Naidu
- first_name: Anna
  full_name: Velichko, Anna
  last_name: Velichko
- first_name: Victoria
  full_name: Bollo, Victoria
  last_name: Bollo
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: John
  full_name: Chisholm, John
  last_name: Chisholm
- first_name: Garth D.
  full_name: Illingworth, Garth D.
  last_name: Illingworth
- first_name: Ivan
  full_name: Kramarenko, Ivan
  id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
  last_name: Kramarenko
  orcid: 0000-0001-5346-6048
- first_name: Daniel
  full_name: Magee, Daniel
  last_name: Magee
- first_name: Michael
  full_name: Maseda, Michael
  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: Erica
  full_name: Nelson, Erica
  last_name: Nelson
- first_name: Naveen
  full_name: Reddy, Naveen
  last_name: Reddy
- first_name: Daniel
  full_name: Schaerer, Daniel
  last_name: Schaerer
- first_name: Mauro
  full_name: Stefanon, Mauro
  last_name: Stefanon
- first_name: Mengyuan
  full_name: Xiao, Mengyuan
  last_name: Xiao
citation:
  ama: 'Covelo-Paz A, Giovinazzo E, Oesch PA, et al. An Hα view of galaxy buildup
    in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy.
    <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href="https://doi.org/10.1051/0004-6361/202452363">10.1051/0004-6361/202452363</a>'
  apa: 'Covelo-Paz, A., Giovinazzo, E., Oesch, P. A., Meyer, R. A., Weibel, A., Brammer,
    G., … Xiao, M. (2025). An Hα view of galaxy buildup in the first 2 Gyr: Luminosity
    functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202452363">https://doi.org/10.1051/0004-6361/202452363</a>'
  chicago: 'Covelo-Paz, Alba, Emma Giovinazzo, Pascal A. Oesch, Romain A. Meyer, Andrea
    Weibel, Gabriel Brammer, Yoshinobu Fudamoto, et al. “An Hα View of Galaxy Buildup
    in the First 2 Gyr: Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.”
    <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202452363">https://doi.org/10.1051/0004-6361/202452363</a>.'
  ieee: 'A. Covelo-Paz <i>et al.</i>, “An Hα view of galaxy buildup in the first 2
    Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.'
  ista: 'Covelo-Paz A, Giovinazzo E, Oesch PA, Meyer RA, Weibel A, Brammer G, Fudamoto
    Y, Kerutt J, Lin J, Matharu J, Naidu RP, Velichko A, Bollo V, Bouwens R, Chisholm
    J, Illingworth GD, Kramarenko I, Magee D, Maseda M, Matthee JJ, Nelson E, Reddy
    N, Schaerer D, Stefanon M, Xiao M. 2025. An Hα view of galaxy buildup in the first
    2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. Astronomy
    &#38; Astrophysics. 694, A178.'
  mla: 'Covelo-Paz, Alba, et al. “An Hα View of Galaxy Buildup in the First 2 Gyr:
    Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.” <i>Astronomy
    &#38; Astrophysics</i>, vol. 694, A178, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202452363">10.1051/0004-6361/202452363</a>.'
  short: A. Covelo-Paz, E. Giovinazzo, P.A. Oesch, R.A. Meyer, A. Weibel, G. Brammer,
    Y. Fudamoto, J. Kerutt, J. Lin, J. Matharu, R.P. Naidu, A. Velichko, V. Bollo,
    R. Bouwens, J. Chisholm, G.D. Illingworth, I. Kramarenko, D. Magee, M. Maseda,
    J.J. Matthee, E. Nelson, N. Reddy, D. Schaerer, M. Stefanon, M. Xiao, Astronomy
    &#38; Astrophysics 694 (2025).
date_created: 2025-03-02T23:01:54Z
date_published: 2025-02-12T00:00:00Z
date_updated: 2026-02-16T12:08:59Z
day: '12'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202452363
external_id:
  arxiv:
  - '2409.17241'
  isi:
  - '001420194600001'
file:
- access_level: open_access
  checksum: b1e74644a0cd37550e9a553f8675c93f
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  creator: dernst
  date_created: 2025-03-04T09:29:01Z
  date_updated: 2025-03-04T09:29:01Z
  file_id: '19285'
  file_name: 2025_AstronomyAstrophysics_CoveloPaz.pdf
  file_size: 1865856
  relation: main_file
  success: 1
file_date_updated: 2025-03-04T09:29:01Z
fulldoi: https://doi.org/10.1051/0004-6361/202452363
has_accepted_license: '1'
intvolume: '       694'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
related_material:
  link:
  - relation: software
    url: ' https://github.com/astroalba/fresco'
scopus_import: '1'
status: public
title: 'An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z
  ∼ 4−6.5 from NIRCam/grism spectroscopy'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 694
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '19365'
abstract:
- lang: eng
  text: We present a comprehensive analysis of H i absorption around 96 Lyα emitters
    (LAEs) at z ≈ 3.3 (median Lyα luminosity ≈1042 erg s−1). These LAEs were identified
    within eight MUSE fields, each (math. formular) on the sky and centered on a bright
    background quasar, as part of the MUSEQuBES survey. Using Voigt profile fitting
    for all H i absorbers detected within ±​​​​​​500 km s−1 of these LAEs, we compiled
    a catalog of 800 H i absorption components. Our analysis shows that H i absorption
    is enhanced near the LAEs compared to the intergalactic medium. However, no trend
    is found between the column densities of H i absorbers and their impact parameters
    from the LAEs (spanning ​​​​​​≈54–260 pkpc). Additionally, all galaxies associated
    with Lyman-limit systems have impact parameters >50 pkpc from the quasar sightlines,
    suggesting that true absorber hosts may be too faint to detect. The LAEs show
    an overall H i covering fraction (fc(H i)) of ≈88% for a threshold (math. formular)
    (H i) = 15. Notably, at the same threshold, the LAEs in pairs/groups exhibit a
    100% H i covering fraction out to ≈250 pkpc. In contrast, isolated LAEs consistently
    show a lower fc(H i) of ≈80%. This environmental influence on fc(H i) is also
    evident up to ≈300 km s−1 in differential bins of line-of-sight velocity. We find
    an anticorrelation between fc(H i) and the equivalent width of rest-frame Lyα
    emission (EW0). Based on the Lyα shell model, this could imply that gas-rich galaxies
    tend to reside in gas-rich environments or that the LAEs with higher EW0 are more
    efficient at ionizing their surrounding medium.
acknowledgement: "We would like to thank the anonymous referee for useful comments.
  We thank Marijke Segers, Lorrie Straka, and Monica Turner for their early contributions
  to the MUSEQuBES project. We thank Raghunathan Srianand for useful suggestions.
  E.B. thanks Labanya Kumar Guha and Yucheng Guo for helpful discussions. S.C. gratefully
  acknowledges the fund support from the European Research Council (ERC).\r\n\r\nSoftware:
  NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), Matplotlib (J.
  D. Hunter 2007), and AstroPy (Astropy Collaboration et al. 2013, 2018)."
article_number: '171'
article_processing_charge: Yes
article_type: original
author:
- first_name: Eshita
  full_name: Banerjee, Eshita
  last_name: Banerjee
- first_name: Sowgat
  full_name: Muzahid, Sowgat
  last_name: Muzahid
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Jérémy
  full_name: Blaizot, Jérémy
  last_name: Blaizot
- first_name: Nicolas
  full_name: Bouché, Nicolas
  last_name: Bouché
- first_name: Sebastiano
  full_name: Cantalupo, Sebastiano
  last_name: Cantalupo
- first_name: Sean D.
  full_name: Johnson, Sean D.
  last_name: Johnson
- 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: Anne
  full_name: Verhamme, Anne
  last_name: Verhamme
citation:
  ama: 'Banerjee E, Muzahid S, Schaye J, et al. MUSEQuBES: Connecting H i Absorption
    with Lyα emitters at z ≈ 3.3. <i>The Astrophysical Journal</i>. 2025;980(2). doi:<a
    href="https://doi.org/10.3847/1538-4357/ada7e9">10.3847/1538-4357/ada7e9</a>'
  apa: 'Banerjee, E., Muzahid, S., Schaye, J., Blaizot, J., Bouché, N., Cantalupo,
    S., … Verhamme, A. (2025). MUSEQuBES: Connecting H i Absorption with Lyα emitters
    at z ≈ 3.3. <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ada7e9">https://doi.org/10.3847/1538-4357/ada7e9</a>'
  chicago: 'Banerjee, Eshita, Sowgat Muzahid, Joop Schaye, Jérémy Blaizot, Nicolas
    Bouché, Sebastiano Cantalupo, Sean D. Johnson, Jorryt J Matthee, and Anne Verhamme.
    “MUSEQuBES: Connecting H i Absorption with Lyα Emitters at z ≈ 3.3.” <i>The Astrophysical
    Journal</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4357/ada7e9">https://doi.org/10.3847/1538-4357/ada7e9</a>.'
  ieee: 'E. Banerjee <i>et al.</i>, “MUSEQuBES: Connecting H i Absorption with Lyα
    emitters at z ≈ 3.3,” <i>The Astrophysical Journal</i>, vol. 980, no. 2. IOP Publishing,
    2025.'
  ista: 'Banerjee E, Muzahid S, Schaye J, Blaizot J, Bouché N, Cantalupo S, Johnson
    SD, Matthee JJ, Verhamme A. 2025. MUSEQuBES: Connecting H i Absorption with Lyα
    emitters at z ≈ 3.3. The Astrophysical Journal. 980(2), 171.'
  mla: 'Banerjee, Eshita, et al. “MUSEQuBES: Connecting H i Absorption with Lyα Emitters
    at z ≈ 3.3.” <i>The Astrophysical Journal</i>, vol. 980, no. 2, 171, IOP Publishing,
    2025, doi:<a href="https://doi.org/10.3847/1538-4357/ada7e9">10.3847/1538-4357/ada7e9</a>.'
  short: E. Banerjee, S. Muzahid, J. Schaye, J. Blaizot, N. Bouché, S. Cantalupo,
    S.D. Johnson, J.J. Matthee, A. Verhamme, The Astrophysical Journal 980 (2025).
date_created: 2025-03-09T23:01:26Z
date_published: 2025-02-20T00:00:00Z
date_updated: 2026-02-16T12:42:00Z
day: '20'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ada7e9
external_id:
  isi:
  - '001421001500001'
file:
- access_level: open_access
  checksum: 1d33a8eb59f42a0c7a943c8859e9b883
  content_type: application/pdf
  creator: dernst
  date_created: 2025-03-10T11:54:52Z
  date_updated: 2025-03-10T11:54:52Z
  file_id: '19379'
  file_name: 2025_AstrophysicalJour_Banerjee.pdf
  file_size: 1194131
  relation: main_file
  success: 1
file_date_updated: 2025-03-10T11:54:52Z
fulldoi: https://doi.org/10.3847/1538-4357/ada7e9
has_accepted_license: '1'
intvolume: '       980'
isi: 1
issue: '2'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3'
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: 980
year: '2025'
...