---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21341'
abstract:
- lang: eng
text: We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation
between the stellar mass, metallicity, and star formation rate (SFR) known as
the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800
[O III] selected galaxies from deep NIRCam grism surveys, we present our stacked
measurements of direct-Te metallicities, which we used to test recent strong-line
metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for
M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However,
there are significant inconsistencies between observations and hydrodynamical
simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations,
which cannot be attributed to selection effects. With simple models, we show that
the effect of an [O III] flux-limited sample on the observed shape of the MZR
is strongly dependent on the FMR. If the FMR is similar to the one in the local
Universe, the intrinsic high-redshift MZR should be even flatter than is observed.
In turn, a 3D relation where SFR correlates positively with metallicity at fixed
mass would imply an intrinsically steeper MZR. Our measurements indicate that
metallicity variations at fixed mass show little dependence on the SFR, suggesting
a flat intrinsic MZR. This could indicate that the low-mass galaxies at these
redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass
galaxies. However, being limited by our stacking analysis, we are yet to probe
the scatter in the MZR and its dependence on SFR. Large carefully selected samples
of galaxies with robust metallicity measurements can put tight constraints on
the high-redshift FMR and help us to understand the interplay between gas flows,
star formation, and feedback in early galaxies.
acknowledgement: 'We thank the anonymous referee for the insightful comments that
helped improving this paper. 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 Associations of Universities for Research in Astronomy, Inc., under NASA contract
NAS 5-03127 for JWST. These observations were taken under programmes # 1243, # 1933
and # 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. GK acknowledges
support from the Foundation MERAC. APV acknowledge support from the Sussex Astronomy
Centre STFC Consolidated Grant (ST/X001040/1).'
article_number: A165
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- 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: Aswin P.
full_name: Vijayan, Aswin P.
last_name: Vijayan
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Rongmon
full_name: Bordoloi, Rongmon
last_name: Bordoloi
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: A. Lola
full_name: Danhaive, A. Lola
last_name: Danhaive
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: David
full_name: Sobral, David
last_name: Sobral
citation:
ama: Kotiwale G, Matthee JJ, Kashino D, et al. Rapid, out-of-equilibrium metal enrichment
indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy.
Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202556597
apa: Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa,
A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment
indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556597
chicago: Kotiwale, Gauri, Jorryt J Matthee, Daichi Kashino, Aswin P. Vijayan, Alberto
Torralba Torregrosa, Claudia Di Cesare, Edoardo Iani, et al. “Rapid, out-of-Equilibrium
Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam
Grism Spectroscopy.” Astronomy & Astrophysics. EDP Sciences, 2026.
https://doi.org/10.1051/0004-6361/202556597.
ieee: G. Kotiwale et al., “Rapid, out-of-equilibrium metal enrichment indicated
by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,”
Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.
ista: Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare
C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive
AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026.
Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity
relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy & Astrophysics.
706, A165.
mla: Kotiwale, Gauri, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated
by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.”
Astronomy & Astrophysics, vol. 706, A165, EDP Sciences, 2026, doi:10.1051/0004-6361/202556597.
short: G. Kotiwale, J.J. Matthee, D. Kashino, A.P. Vijayan, A. Torralba Torregrosa,
C. Di Cesare, E. Iani, R. Bordoloi, J. Leja, M.V. Maseda, S. Tacchella, I. Shivaei,
K.E. Heintz, A.L. Danhaive, S. Mascia, I. Kramarenko, B. Navarrete, R. Mackenzie,
R.P. Naidu, D. Sobral, Astronomy & Astrophysics 706 (2026).
corr_author: '1'
date_created: 2026-02-22T23:01:35Z
date_published: 2026-02-01T00:00:00Z
date_updated: 2026-02-24T07:49:42Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202556597
external_id:
arxiv:
- '2510.19959'
file:
- access_level: open_access
checksum: 6f5849d29ad43bee32f90152f6fc0294
content_type: application/pdf
creator: dernst
date_created: 2026-02-24T07:46:47Z
date_updated: 2026-02-24T07:46:47Z
file_id: '21355'
file_name: 2026_AstronomyAstrophysics_Kotiwale.pdf
file_size: 6531719
relation: main_file
success: 1
file_date_updated: 2026-02-24T07:46:47Z
has_accepted_license: '1'
intvolume: ' 706'
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: 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: Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity
relation at z ∼ 6 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: 706
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21451'
abstract:
- lang: eng
text: The population of the little red dots (LRDs) may represent a key phase of
supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging
as a key component to explain the most striking properties of LRDs, such as strong
Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect
the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra
of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra
reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission.
We revealed a forest of optical [Fe II] lines, which we argue are emerging from
a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K.
The broad wings of Hα and Hβ have an exponential profile due to electron scattering
in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an
indicator of collisional excitation and resonant scattering dominating the Balmer
line emission. A narrow Hγ component, unseen in the other two Balmer lines due
to outshining by the broad components, could trace the ISM of a normal host galaxy
with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer
transitions, producing a characteristic P Cygni profile in the line centers suggesting
outflowing motions. This same layer is responsible for shaping the Balmer break.
The broadband spectrum can be reasonably matched by a simple photoionized slab
model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy
that could explain the narrow [O III], with only a subdominant contribution to
the UV continuum. Our findings indicate that Balmer lines are not directly tracing
the gas kinematics near the SMBH and that the BH mass scale is likely much lower
than virial indicators suggest.
acknowledgement: 'We thank the scientific referee for useful and constructive comments.
We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics
of gaseous envelopes and accretion into black holes. 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. This work is based in part on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the
Mikulski Archive for Space Telescopes at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated
with program #5664. 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.'
article_number: A75
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Gabriel B.
full_name: Brammer, Gabriel B.
last_name: Brammer
- first_name: Seok Jun
full_name: Chang, Seok Jun
last_name: Chang
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Vasily
full_name: Kokorev, Vasily
last_name: Kokorev
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Yilun
full_name: Ma, Yilun
last_name: Ma
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Erica
full_name: Nelson, Erica
last_name: Nelson
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- first_name: Robert A.
full_name: Simcoe, Robert A.
last_name: Simcoe
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer
of a little red dot as the source of [Fe ii] and collisional Balmer lines with
scattering wings. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557537
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa,
Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot
as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557537
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan
P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm
Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer
Lines with Scattering Wings.” Astronomy & Astrophysics. EDP Sciences,
2026. https://doi.org/10.1051/0004-6361/202557537.
ieee: A. Torralba Torregrosa et al., “The warm outer layer of a little red
dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,”
Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer
GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene
JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete
B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little
red dot as the source of [Fe ii] and collisional Balmer lines with scattering
wings. Astronomy & Astrophysics. 707, A75.
mla: Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red
Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.”
Astronomy & Astrophysics, vol. 707, A75, EDP Sciences, 2026, doi:10.1051/0004-6361/202557537.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa,
G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare,
A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko,
Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy
& Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:59:16Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557537
external_id:
arxiv:
- '2510.00103'
file:
- access_level: open_access
checksum: fcab9cb3dcf1d68612e1fdc8191643c1
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:57:49Z
date_updated: 2026-03-16T10:57:49Z
file_id: '21460'
file_name: 2026_AstronomyAstrophysics_Torralba2.pdf
file_size: 2510157
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:57:49Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
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: The warm outer layer of a little red dot as the source of [Fe ii] and collisional
Balmer lines with scattering wings
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21452'
abstract:
- lang: eng
text: Galaxies exhibit a tight correlation between their star formation rate (SFR)
and stellar mass over a wide redshift range known as the star-forming main sequence
(SFMS). With JWST, the SFMS can now be investigated at high redshifts down to
masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα
emission, which allow us to probe the variability in the star formation histories.
We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5
with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell
2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little
Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α,
with α = 0.45). After we corrected this for the Hα-flux limited nature of our
survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09,
whereas current data on their own are inconclusive on the mass dependence of the
scatter. These slopes differ significantly from the slope of ∼1 that is expected
from the observed evolution of the galaxy stellar mass function and from simulations.
When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic
scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010
M⊙). This difference might be explained by a (combination of) luminosity-dependent
SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated
dust attenuation in high-mass galaxies. Future deep observations with different
facilities can quantify these processes, which will enable us to achieve better
insights into the variability of the star formation histories.
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion,
Pierluigi Rinaldi for his help with data handling and Luca Graziani and William
McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. 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. 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 # 3516. We acknowledge funding from JWST program GO-3516. Software
used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant
2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy
Collaboration 2013)."
article_number: A129
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- 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: Alberto
full_name: Torralba, Alberto
last_name: Torralba
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Jeremy
full_name: Blaizot, Jeremy
last_name: Blaizot
- first_name: Joakim
full_name: Rosdahl, Joakim
last_name: Rosdahl
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Angela
full_name: Adamo, Angela
last_name: Adamo
- first_name: Alba
full_name: Covelo-Paz, Alba
last_name: Covelo-Paz
- first_name: Lukas J.
full_name: Furtak, Lukas J.
last_name: Furtak
- first_name: Kasper E.
full_name: Heintz, Kasper E.
last_name: Heintz
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Michael
full_name: Romano, Michael
last_name: Romano
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
citation:
ama: 'Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming
main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557790'
apa: 'Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko,
I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence
at z ∼ 5: Reconciling observations with simulations. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557790'
chicago: 'Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba,
Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter
of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.”
Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557790.'
ieee: 'C. Di Cesare et al., “The slope and scatter of the star-forming main
sequence at z ∼ 5: Reconciling observations with simulations,” Astronomy &
Astrophysics, vol. 707. EDP Sciences, 2026.'
ista: 'Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I,
Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz
KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The
slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations
with simulations. Astronomy & Astrophysics. 707, A129.'
mla: 'Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main
Sequence at z ∼ 5: Reconciling Observations with Simulations.” Astronomy &
Astrophysics, vol. 707, A129, EDP Sciences, 2026, doi:10.1051/0004-6361/202557790.'
short: C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko,
J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak,
K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-15T23:01:36Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T10:52:44Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202557790
external_id:
arxiv:
- '2510.19044'
file:
- access_level: open_access
checksum: c056b00ce7324849754521fde10fb7ca
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T10:48:07Z
date_updated: 2026-03-16T10:48:07Z
file_id: '21459'
file_name: 2026_AstronomyAstrophysics_DiCesare.pdf
file_size: 1821411
relation: main_file
success: 1
file_date_updated: 2026-03-16T10:48:07Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
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: 'The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling
observations with simulations'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21481'
abstract:
- lang: eng
text: 'The Hα emission line in galaxies is a powerful tracer of their recent star
formation activity. With the advent of JWST, we are now able to routinely observe
Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation
rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs
leads to biased results because high-redshift galaxies are commonly characterized
by low metallicities and bursty star formation histories, affecting the conversion
factor between the Hα luminosity (LHα) and the SFR. We developed a set of new
SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3
with very little error. We used the SPHINX cosmological simulations to select
a sample of star-forming galaxies representative of the Hα-emitter population
observed with JWST. We then derived linear corrections to the classical SFR(Hα)
calibrations that took variations in the physical properties (e.g., stellar metallicities)
among individual galaxies into account. We obtained two new SFR(Hα) calibrations
that compared to the classical calibrations reduce the root mean squared error
(RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively.
Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show
that the new calibrations affect the high-redshift galaxy population statistics:
(i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed
slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.'
acknowledgement: "We thank the anonymous referee for the insightful comments that
helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene
Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala
for useful comments and productive discussions. We gratefully acknowledge support
from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de
Lyon for the computing resources.\r\nFunded 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. This work made extensive use of several open-source software packages,
and we gratefully acknowledge the efforts of their authors: numpy (Harris et al.
2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez
& Granger 2007), and scikit-learn (Pedregosa et al. 2011)."
article_number: A184
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: J.
full_name: Rosdahl, J.
last_name: Rosdahl
- first_name: J.
full_name: Blaizot, J.
last_name: Blaizot
- 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: H.
full_name: Katz, H.
last_name: Katz
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
citation:
ama: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as
a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 2026;707. doi:10.1051/0004-6361/202557114
apa: Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., & Di
Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological
simulations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557114
chicago: Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and
Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557114.
ieee: I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare,
“H α as a tracer of star formation in the SPHINX cosmological simulations,” Astronomy
& Astrophysics, vol. 707. EDP Sciences, 2026.
ista: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026.
H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy
& Astrophysics. 707, A184.
mla: Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological
Simulations.” Astronomy & Astrophysics, vol. 707, A184, EDP Sciences,
2026, doi:10.1051/0004-6361/202557114.
short: I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare,
Astronomy & Astrophysics 707 (2026).
corr_author: '1'
date_created: 2026-03-23T14:58:03Z
date_published: 2026-03-05T00:00:00Z
date_updated: 2026-03-23T15:46:31Z
day: '05'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202557114
external_id:
arxiv:
- '2509.05403'
file:
- access_level: open_access
checksum: 7429076b381dd498084f40ffd199e714
content_type: application/pdf
creator: dernst
date_created: 2026-03-23T15:44:09Z
date_updated: 2026-03-23T15:44:09Z
file_id: '21492'
file_name: 2026_AstronomyAstrophysics_Kramarenko.pdf
file_size: 904565
relation: main_file
success: 1
file_date_updated: 2026-03-23T15:44:09Z
has_accepted_license: '1'
intvolume: ' 707'
language:
- iso: eng
month: '03'
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'
status: public
title: H α as a tracer of star formation in the SPHINX cosmological simulations
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21045'
abstract:
- lang: eng
text: 'The abundant population of little red dots (LRDs), compact objects with red
UV to optical colors and broad Balmer lines at high redshift, is revealing new
insights into the properties of early active galactic nuclei (AGN). Perhaps the
most surprising features of this population are the presence of Balmer absorption
and ubiquitous strong Balmer breaks. Recent models link these features to an active
supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We
present a stringent test of such models using VLT/MUSE observations of A2744-45924,
the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744
lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula
(h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc.
The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα)
compared to Lyα nebulae typically observed around quasars of similar luminosity.
We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial
shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and
Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered
by star formation. In the environment of A2744-45924, we identified four extended
Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations
based on Hα emission, and show no evidence for radiation from A2744-45924 affecting
its surroundings. The lack of strong, compact, and broad Lyα and the absence of
a luminous extended halo, suggest that the UV AGN light is obscured by dense gas
cloaking the SMBH with a covering factor close to unity.'
acknowledgement: 'We thank the anonymous referee for constructive and useful comments.
We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected
at the European Organisation for Astronomical Research in the Southern Hemisphere
under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224).
Views and opinions expressed are however those of the author(s) only and do not
necessarily reflect those of the European Union or the European Research Council.
Neither the European Union nor the granting authority can be held responsible for
them. We acknowledge funding from JWST program GO-3516. This work is based in part
on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data
were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations
are associated with program #3516. MG thanks the Max Planck Society for support
through the MPRG. FDE acknowledges support by the Science and Technology Facilities
Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI
Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant
SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.'
article_number: A147
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba Torregrosa, Alberto
id: 018f0249-0e87-11f0-b167-cbce08fbd541
last_name: Torralba Torregrosa
orcid: 0000-0001-5586-6950
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Sara
full_name: Mascia, Sara
id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29
last_name: Mascia
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: Anna Christina
full_name: Eilers, Anna Christina
last_name: Eilers
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Edoardo
full_name: Iani, Edoardo
id: 4053390a-6b68-11ef-9828-a3b8adef8d0a
last_name: Iani
orcid: 0000-0001-8386-3546
- first_name: Yuzo
full_name: Ishikawa, Yuzo
last_name: Ishikawa
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Benjamín
full_name: Navarrete, Benjamín
id: aa14a535-50c9-11ef-b52e-e0c373d10148
last_name: Navarrete
- first_name: Gauri
full_name: Kotiwale, Gauri
id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875
last_name: Kotiwale
citation:
ama: Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for
an extremely bright little red dot. Indications of enshrouded supermassive black
hole growth. Astronomy & Astrophysics. 2026;705. doi:10.1051/0004-6361/202555596
apa: Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke,
M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555596
chicago: Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya
Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo
for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive
Black Hole Growth.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202555596.
ieee: A. Torralba Torregrosa et al., “A weak Ly α halo for an extremely bright
little red dot. Indications of enshrouded supermassive black hole growth,” Astronomy
& Astrophysics, vol. 705. EDP Sciences, 2026.
ista: Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia
S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie
R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely
bright little red dot. Indications of enshrouded supermassive black hole growth.
Astronomy & Astrophysics. 705, A147.
mla: Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright
Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” Astronomy
& Astrophysics, vol. 705, A147, EDP Sciences, 2026, doi:10.1051/0004-6361/202555596.
short: A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke,
S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa,
R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy & Astrophysics
705 (2026).
corr_author: '1'
das_tickbox: '1'
date_created: 2026-01-25T23:01:41Z
date_published: 2026-01-14T00:00:00Z
date_updated: 2026-07-08T06:38:23Z
day: '14'
ddc:
- '520'
department:
- _id: JoMa
- _id: GradSch
doi: 10.1051/0004-6361/202555596
external_id:
arxiv:
- '2505.09542'
file:
- access_level: open_access
checksum: 3782e03bc0843438aae8487f6af779c5
content_type: application/pdf
creator: dernst
date_created: 2026-02-16T07:35:03Z
date_updated: 2026-02-16T07:35:03Z
file_id: '21224'
file_name: 2026_AstronomyAstrophysics_Torralba.pdf
file_size: 2259914
relation: main_file
success: 1
file_date_updated: 2026-02-16T07:35:03Z
has_accepted_license: '1'
intvolume: ' 705'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
project:
- _id: bd9b2118-d553-11ed-ba76-db24564edfea
grant_number: '101076224'
name: Young galaxies as tracers and agents of cosmic reionization
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded
supermassive black hole growth
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 705
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '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.
Astronomy & Astrophysics. 2025;701. doi:10.1051/0004-6361/202553760
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. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202553760
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.” Astronomy
& Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202553760.
ieee: S. Mascia et al., “Little impact of mergers and galaxy morphology on
the production and escape of ionizing photons in the early Universe,” Astronomy
& Astrophysics, 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 & 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.” Astronomy
& Astrophysics, vol. 701, A122, EDP Sciences, 2025, doi:10.1051/0004-6361/202553760.
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
& 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
file_id: '21166'
file_name: 2025_AstronomyAstrophysics_Mascia.pdf
file_size: 9994234
relation: main_file
success: 1
file_date_updated: 2026-02-09T07:28:08Z
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: '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. The Astrophysical Journal. 2025;988(2). doi:10.3847/1538-4357/ade886
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. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ade886
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.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ade886.
ieee: J. J. Matthee et al., “Environmental evidence for overly massive Black
Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” The
Astrophysical Journal, 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.” The
Astrophysical Journal, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:10.3847/1538-4357/ade886.
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
content_type: application/pdf
creator: dernst
date_created: 2026-02-09T08:20:14Z
date_updated: 2026-02-09T08:20:14Z
file_id: '21168'
file_name: 2025_AstrophysicalJournal_Matthee.pdf
file_size: 6237415
relation: main_file
success: 1
file_date_updated: 2026-02-09T08:20:14Z
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'
...
---
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.
Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202451542'
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. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451542'
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.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202451542.'
ieee: 'P. Sawant et al., “The ALPINE-ALMA [CII] survey: Unveiling the baryon
evolution in the interstellar medium of z ∼ 5 star-forming galaxies,” Astronomy
& Astrophysics, 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 & 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.” Astronomy &
Astrophysics, vol. 694, A82, EDP Sciences, 2025, doi:10.1051/0004-6361/202451542.'
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 & 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'
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doi: 10.1051/0004-6361/202451542
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month: '02'
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oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
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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'
...
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OA_type: hybrid
_id: '18527'
abstract:
- lang: eng
text: "Context. Galaxies evolve through a dynamic exchange of material with their
immediate surrounding environment, the so-called circumgalactic medium (CGM).
Understanding the physics of gas flows and the nature of the CGM is fundamental
to studying galaxy evolution, especially at 4 ≤ z ≤ 6 (i.e., after the Epoch of
Reionization) when galaxies rapidly assembled their masses and reached their chemical
maturity. Galactic outflows are predicted to enrich the CGM with metals, although
it has also been suggested that gas stripping in systems undergoing a major merger
may play a role.\r\n\r\nAims. In this work, we explore the metal enrichment of
the medium around merging galaxies at z ∼ 4.5, observed by the ALMA Large Program
to INvestigate [CII] at Early times (ALPINE). To do so, we study the nature of
the [CII] 158 μm emission in the CGM around these systems, using simulations to
help disentangle the mechanisms contributing to the CGM metal pollution.\r\n\r\nMethods.
By adopting an updated classification of major merger systems in the ALPINE survey,
we selected and analyzed merging galaxies whose components can be spatially and/or
spectrally resolved in a robust way. This makes it possible to distinguish between
the [CII] emission coming from the single components of the system and that coming
from the system as a whole. We also made use of the dustyGadget cosmological simulation
to select synthetic analogs of observed galaxies and guide the interpretation
of the observational results.\r\n\r\nResults. We find a large diffuse [CII] envelope
(≳20 kpc) embedding all the merging systems, with at least 25% of the total [CII]
emission coming from the medium between the galaxies. Using predictions from dustyGadget,
we suggest that this emission has a multi-fold nature, with dynamical interactions
between galaxies playing a major role in stripping the gas and enriching the medium
with heavy elements."
acknowledgement: 'The authors would like to thank the anonymous referee for the useful
suggestions which improved this article. This paper is based on data obtained with
the ALMA Observatory, under Large Program 2017.1.00428.L. 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. CDC would like to thank the GESO group at the European Southern Observatory
(ESO) for the useful discussions while preparing this manuscript. The simulated
data underlying this article will be shared on reasonable request to the corresponding
author. CDC acknowledged support from Sapienza University of Rome program “Bando
per la mobilità individuale all’estero” (DR n.1607 del 14 June 2021) during the
visiting period (June-November 2022) at ESO Garching, Germany. LG and RS acknowledge
support from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly
(FLAGS) funded by the European Union – Next Generation EU, and from the Amaldi Research
Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:B81I18001170001).
MR acknowledges support from the Narodowe Centrum Nauki (UMO-2020/38/E/ST9/00077)
and support from the Foundation for Polish Science (FNP) under the program START
063.2023. We have benefited from the publicly available software CASA and CARTA
and programming language Python, including the numpy (https://numpy.org), matplotlib
(https://matplotlib.org), scipy (https://scipy.org) and astropy (http://www.astropy.org)
packages. '
article_number: A255
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia
full_name: Di Cesare, Claudia
id: 2d002343-372f-11ef-98ec-a164d20427cb
last_name: Di Cesare
- first_name: M.
full_name: Ginolfi, M.
last_name: Ginolfi
- first_name: L.
full_name: Graziani, L.
last_name: Graziani
- first_name: R.
full_name: Schneider, R.
last_name: Schneider
- first_name: M.
full_name: Romano, M.
last_name: Romano
- first_name: G.
full_name: Popping, G.
last_name: Popping
citation:
ama: Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. Carbon
envelopes around merging galaxies at z ~ 4.5. Astronomy & Astrophysics.
2024;690. doi:10.1051/0004-6361/202449164
apa: Di Cesare, C., Ginolfi, M., Graziani, L., Schneider, R., Romano, M., &
Popping, G. (2024). Carbon envelopes around merging galaxies at z ~ 4.5. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202449164
chicago: Di Cesare, Claudia, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and
G. Popping. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” Astronomy
& Astrophysics. EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202449164.
ieee: C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping,
“Carbon envelopes around merging galaxies at z ~ 4.5,” Astronomy & Astrophysics,
vol. 690. EDP Sciences, 2024.
ista: Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. 2024.
Carbon envelopes around merging galaxies at z ~ 4.5. Astronomy & Astrophysics.
690, A255.
mla: Di Cesare, Claudia, et al. “Carbon Envelopes around Merging Galaxies at z ~
4.5.” Astronomy & Astrophysics, vol. 690, A255, EDP Sciences, 2024,
doi:10.1051/0004-6361/202449164.
short: C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, G. Popping,
Astronomy & Astrophysics 690 (2024).
corr_author: '1'
das_tickbox: '1'
date_created: 2024-11-10T23:02:00Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2026-07-08T06:44:39Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202449164
external_id:
arxiv:
- '2401.03020'
isi:
- '001332213700013'
file:
- access_level: open_access
checksum: 24c65a64047aba156f39b01425269bdb
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creator: dernst
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intvolume: ' 690'
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language:
- iso: eng
month: '10'
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: Carbon envelopes around merging galaxies at z ~ 4.5
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: 690
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...