---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21252'
abstract:
- lang: eng
text: "Context. Recent observational results from asteroseismic studies show that
an important fraction of solar-like stars do not present detectable stochastically
excited acoustic oscillations. This non-detectability seems to correlate with
a high rotation rate in the convective envelope and a high surface magnetic activity.
At the same time, the properties of stellar convection are affected by rotation
and magnetism.\r\nAims. We investigate the role of rotation in the excitation
of acoustic modes in the convective envelope of solar-like stars, to evaluate
its impact on the energy injected in the oscillations.\r\nMethods. We derived
theoretical prescriptions for the excitation of acoustic waves in the convective
envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory
to model the influence of rotation on convection. We used the MESA stellar evolution
code and the GYRE stellar oscillation code to estimate the power injected in the
oscillations from our theoretical prescriptions.\r\nResults. We demonstrate that
the power injected in the acoustic modes is insensitive to rotation if a Gaussian
time-correlation function is assumed, while it can decrease by up to 60% for a
Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that
the modification of the excitation rate by rotation depends not only on the rotation
rate but also on the radial and angular orders of the considered oscillation mode.
This result can allow for better constraints on the properties of stellar convection
by studying observationally acoustic mode excitation.\r\nConclusions. These results
demonstrate how important it is to take into account the modification of stellar
convection by rotation when evaluating the amplitude of the stellar oscillations
it stochastically excites. They open the path for understanding the large variety
of observed acoustic-mode amplitudes at the surface of solar-like stars as a function
of surface rotation rates."
acknowledgement: 'The authors thank the referee for detailed comments that allow them
to improve their work. The authors thank Jordan Philidet and Kevin Belkacem for
fruitful discussions. L.B. and Stéphane M. acknowledge support from the European
Research Council (ERC) under the Horizon Europe program (Synergy Grant agreement
101071505: 4D-STAR), from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from
PNPS (CNRS/INSU). While partially funded by the European Union, views and opinions
expressed are however those of the author 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. Savita M. acknowledges
support from the Spanish Ministry of Science and Innovation with the grant no. PID2019-107061GB-C66
and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023
(CEX2019-000920-S).'
article_number: A25
article_processing_charge: Yes
article_type: original
author:
- first_name: L.
full_name: Bessila, L.
last_name: Bessila
- first_name: A.
full_name: Deckx van Ruys, A.
last_name: Deckx van Ruys
- first_name: V.
full_name: Buriasco, V.
last_name: Buriasco
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
citation:
ama: Bessila L, Deckx van Ruys A, Buriasco V, et al. The impact of rotation on the
stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy
& Astrophysics. 2025;700. doi:10.1051/0004-6361/202452093
apa: Bessila, L., Deckx van Ruys, A., Buriasco, V., Mathis, S., Bugnet, L. A., García,
R. A., & Mathur, S. (2025). The impact of rotation on the stochastic excitation
of stellar acoustic modes in solar-like pulsators. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202452093
chicago: Bessila, L., A. Deckx van Ruys, V. Buriasco, S. Mathis, Lisa Annabelle
Bugnet, R. A. García, and S. Mathur. “The Impact of Rotation on the Stochastic
Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452093.
ieee: L. Bessila et al., “The impact of rotation on the stochastic excitation
of stellar acoustic modes in solar-like pulsators,” Astronomy & Astrophysics,
vol. 700. EDP Sciences, 2025.
ista: Bessila L, Deckx van Ruys A, Buriasco V, Mathis S, Bugnet LA, García RA, Mathur
S. 2025. The impact of rotation on the stochastic excitation of stellar acoustic
modes in solar-like pulsators. Astronomy & Astrophysics. 700, A25.
mla: Bessila, L., et al. “The Impact of Rotation on the Stochastic Excitation of
Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy & Astrophysics,
vol. 700, A25, EDP Sciences, 2025, doi:10.1051/0004-6361/202452093.
short: L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A.
García, S. Mathur, Astronomy & Astrophysics 700 (2025).
date_created: 2026-02-16T15:46:59Z
date_published: 2025-08-01T00:00:00Z
date_updated: 2026-02-17T13:10:18Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202452093
file:
- access_level: open_access
checksum: b8a0927307c1d82025bcb5af47b20b26
content_type: application/pdf
creator: dernst
date_created: 2026-02-17T13:07:45Z
date_updated: 2026-02-17T13:07:45Z
file_id: '21306'
file_name: 2025_AstronomyAstrophysics_Bessila.pdf
file_size: 7161755
relation: main_file
success: 1
file_date_updated: 2026-02-17T13:07:45Z
has_accepted_license: '1'
intvolume: ' 700'
language:
- iso: eng
month: '08'
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'
status: public
title: The impact of rotation on the stochastic excitation of stellar acoustic modes
in solar-like pulsators
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: 700
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19844'
abstract:
- lang: eng
text: "Context. Rapidly rotating classical OBe stars have been proposed as the products
of binary interactions, and the fraction of Be stars with compact companions implies
that at least some are. However, to constrain the interaction physics spinning
up the OBe stars, a large sample of homogeneously analyzed OBe stars with well-determined
binary characteristics and orbital parameters are required.\r\n\r\nAims. We investigated
the multiplicity properties of a sample of 18 Oe, 62 Be, and two Of?p stars observed
within the BLOeM survey in the Small Magellanic Cloud. We analyzed the first nine
epochs of spectroscopic observations obtained over approximately three months
in 2023.\r\n\r\nMethods. Radial velocities (RVs) of all stars were measured using
cross-correlation based on different sets of absorption and emission lines. Applying
commonly used binarity criteria, we classified objects as binaries, binary candidates,
and apparently single (RV stable) objects. We further inspected the spectra for
double-lined spectroscopic binaries and cross-matched with catalogs of X-ray sources
and photometric binaries.\r\n\r\nResults. We classify 14 OBe stars as binaries,
and an additional 11 as binary candidates. The two Of?p stars are apparently single.
We find two more objects that are most likely currently interacting binaries.
Without those, the observed binary fraction for the remaining OBe sample of 78
stars is fobs+candOBe = 0.18 ± 0.04 (fobs+candOBe = 0.32±0.05 including candidates).
This binary fraction is less than half of that measured for OB stars in BLOeM.
Combined with the lower fraction of SB2s, this suggests that OBe stars do indeed
have fundamentally different present-day binary properties than OB stars. We find
no evidence for OBe binaries with massive compact companions, in contrast to expectations
from binary population synthesis.\r\n\r\nConclusions. Our results support the
binary scenario as an important formation channel for OBe stars, as post-interaction
binaries may have been disrupted or the stripped companions of OBe stars are harder
to detect. Further observations are required to characterize the detected binaries,
their orbital parameters, and the nature of their companions."
acknowledgement: 'The research leading to these results has received funding from
the European Research Council (ERC) under the European Union’s Horizon 2020 and
Horizon Europe research and innovation programme (grant agreement numbers 772225:
MULTIPLES, and 945806) and is supported by the Deutsche Forschungsgemeinschaft (DFG,
German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1-390900948
(the Heidelberg STRUCTURES Excellence Cluster). DMB gratefully acknowledges funding
from UK Research and Innovation (UKRI) in the form of a Frontier Research grant
under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; grant
number: EP/Y031059/1), and a Royal Society University Research Fellowship (URF;
grant number: URF\R1\231631). RGI is funded by STFC grant ST/Y002350/1 as part of
the BRIDGCE UK network, and thanks IReNA colleagues for stimulating discussions.
Z.K. acknowledges support from JSPS Kakenhi Grant-in-Aid for Scientific Research
(23K19071). IM acknowledges support from the Australian Research Council (ARC) Centre
of Excellence for GravitationalWave Discovery (OzGrav), through project number CE230100016.
DP acknowledges financial support by the Deutsches Zentrum für Luft und Raumfahrt
(DLR) grant FKZ 50OR2005. DFR is thankful for the support of CAPES-Br and FAPERJ/DSC-10
(SEI-260003/001630/2023). AACS and VR are supported by the German Deutsche Forschungsgemeinschaft
(DFG) under Project-ID 445674056 (Emmy Noether Research Group SA4064/1-1, PI Sander).
AACS and VR are further supported by funding from the Federal Ministry of Education
and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the
Excellence Strategy of the German Federal and State Governments. JIV acknowledges
support from the European Research Council for the ERC Advanced Grant 101054731.
LRP acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033.
GH acknowledges support from grants PID2021-122397NB-C21/PID2022-136640NB-C22 funded
by MCIN/AEI/FEDER/10.13039/501100011033. J.K. thanks for the support of a grant
GA CR 22-34467S. This project has received funding from the European Research Council
(ERC) under the European Union’s Horizon 2020 research and innovation programme
(grant agreement 101164755/METAL) and was supported by the Israel Science Foundation
(ISF) under grant number 2434/24.'
article_number: A38
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: M.
full_name: Fabry, M.
last_name: Fabry
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: R. G.
full_name: Izzard, R. G.
last_name: Izzard
- first_name: S.
full_name: Janssens, S.
last_name: Janssens
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Kubát, J.
last_name: Kubát
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: G.
full_name: Maravelias, G.
last_name: Maravelias
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: D. F.
full_name: Rocha, D. F.
last_name: Rocha
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: R.
full_name: Valli, R.
last_name: Valli
- first_name: A.
full_name: Vigna-Gómez, A.
last_name: Vigna-Gómez
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: X. T.
full_name: Xu, X. T.
last_name: Xu
citation:
ama: 'Bodensteiner J, Shenar T, Sana H, et al. Binarity at LOw Metallicity (BLOeM):
Multiplicity properties of Oe and Be stars. Astronomy & Astrophysics.
2025;698. doi:10.1051/0004-6361/202452623'
apa: 'Bodensteiner, J., Shenar, T., Sana, H., Britavskiy, N., Crowther, P. A., Langer,
N., … Xu, X. T. (2025). Binarity at LOw Metallicity (BLOeM): Multiplicity properties
of Oe and Be stars. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452623'
chicago: 'Bodensteiner, J., T. Shenar, H. Sana, N. Britavskiy, P. A. Crowther, N.
Langer, D. J. Lennon, et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
Properties of Oe and Be Stars.” Astronomy & Astrophysics. EDP Sciences,
2025. https://doi.org/10.1051/0004-6361/202452623.'
ieee: 'J. Bodensteiner et al., “Binarity at LOw Metallicity (BLOeM): Multiplicity
properties of Oe and Be stars,” Astronomy & Astrophysics, vol. 698.
EDP Sciences, 2025.'
ista: 'Bodensteiner J, Shenar T, Sana H, Britavskiy N, Crowther PA, Langer N, Lennon
DJ, Mahy L, Patrick LR, Villaseñor JI, Abdul-Masih M, Bowman DM, De Koter A, De
Mink SE, Deshmukh K, Fabry M, Gilkis A, Götberg YLL, Holgado G, Izzard RG, Janssens
S, Kalari VM, Keszthelyi Z, Kubát J, Mandel I, Maravelias G, Oskinova LM, Pauli
D, Ramachandran V, Rocha DF, Renzo M, Sander AAC, Schneider FRN, Schootemeijer
A, Sen K, Stoop M, Toonen S, Van Loon JT, Valli R, Vigna-Gómez A, Vink JS, Wang
C, Xu XT. 2025. Binarity at LOw Metallicity (BLOeM): Multiplicity properties of
Oe and Be stars. Astronomy & Astrophysics. 698, A38.'
mla: 'Bodensteiner, J., et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
Properties of Oe and Be Stars.” Astronomy & Astrophysics, vol. 698,
A38, EDP Sciences, 2025, doi:10.1051/0004-6361/202452623.'
short: J. Bodensteiner, T. Shenar, H. Sana, N. Britavskiy, P.A. Crowther, N. Langer,
D.J. Lennon, L. Mahy, L.R. Patrick, J.I. Villaseñor, M. Abdul-Masih, D.M. Bowman,
A. De Koter, S.E. De Mink, K. Deshmukh, M. Fabry, A. Gilkis, Y.L.L. Götberg, G.
Holgado, R.G. Izzard, S. Janssens, V.M. Kalari, Z. Keszthelyi, J. Kubát, I. Mandel,
G. Maravelias, L.M. Oskinova, D. Pauli, V. Ramachandran, D.F. Rocha, M. Renzo,
A.A.C. Sander, F.R.N. Schneider, A. Schootemeijer, K. Sen, M. Stoop, S. Toonen,
J.T. Van Loon, R. Valli, A. Vigna-Gómez, J.S. Vink, C. Wang, X.T. Xu, Astronomy
& Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:30Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-04-16T08:17:17Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452623
external_id:
arxiv:
- '2502.02641'
isi:
- '001497903100011'
file:
- access_level: open_access
checksum: 51d79c82f6030180fb7c5d7ba01b2da8
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T07:54:57Z
date_updated: 2025-06-23T07:54:57Z
file_id: '19866'
file_name: 2025_AstronomyAstrophysics_Bodensteiner.pdf
file_size: 2404827
relation: main_file
success: 1
file_date_updated: 2025-06-23T07:54:57Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
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: 'Binarity at LOw Metallicity (BLOeM): Multiplicity properties of Oe and Be
stars'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 698
year: '2025'
...
---
_id: '17889'
abstract:
- lang: eng
text: The increasingly neutral intergalactic gas at z > 6 impacts the Lyman-α (Lyα)
flux observed from galaxies. One luminous galaxy, COLA1, stands out because of
its unique double-peaked Lyα line at z = 6.6, unseen in any simulation of reionization.
Here, we present JWST/NIRCam wide-field slitless spectroscopy in a 21 arcmin2
field centered on COLA1. We find 141 galaxies spectroscopically selected through
the [O III] doublet at 5.35 < z < 6.95, with 40 of these sources showing Hβ. For
COLA1, we additionally detect [O III]4363 as well as Hγ. We measure a systemic
redshift of z = 6.5917 for COLA1, confirming the classical double-peak nature
of the Lyα profile. This implies that it resides in a highly ionized bubble and
that it is leaking ionizing photons with a high escape fraction of fesc(LyC) = 20–50%,
making it a prime laboratory to study Lyman continuum escape in the Epoch of Reionization.
COLA1 shows all the signs of a prolific ionizer with a Lyα escape fraction of
81 ± 5%, Balmer decrement indicating no dust, a steep UV slope (βUV = −3.2 ± 0.4),
and a star-formation surface density ≳10× that of typical galaxies at similar
redshift. We detect five galaxies in COLA1’s close environment (Δz < 0.02). Exploiting
the high spectroscopic completeness inherent to grism surveys, and using mock
simulations that fully mimic the selection function, we show that the number of
detected companions is very typical for a normal similarly UV-bright (MUV ∼ −21.3)
galaxy – that is, the ionized bubble around COLA1 is unlikely to be due to an
excessively large over-density. Instead, the measured ionizing properties suggest
that COLA1 by itself might be powering the bubble required to explain its double-peaked
Lyα profile (Rion ≈ 0.7 pMpc), with only minor contributions from detected neighbors
(−19.5 ≲ MUV ≲ −17.5).
acknowledgement: 'The authors acknowledge the financial support from the MICIU with
funding from the European Union NextGenerationEU and Generalitat Valenciana in the
call Programa de Planes Complementarios de I+D+i (PRTR 2022) Project (VAL-JPAS),
reference ASFAE/2022/025. This work has been funded by project PID2019-109592GBI00/AEI/10.13039/501100011033
from the Spanish Ministerio de Ciencia e Innovación (MCIN)-Agencia Estatal de Investigación,
by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Innovació
Universitats, Ciència i Societat Digital de la Generalitat Valenciana. It has also
be funded by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Educació,
Universitats, i Ocupació de la Generalitat Valenciana. 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. ST acknowledges support by the Royal Society Research
Grant G125142. AH acknowledges support by the VILLUM FONDEN under grant 37459. The
Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under
grant DNRF140. We acknowledge funding from JWST program GO-1933. 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.
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
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 # 1933. The specific observations analyzed
can be accessed via https://doi.org/10.17909/s9ht-7n34.'
article_number: A44
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: Alberto
full_name: Torralba-Torregrosa, Alberto
last_name: Torralba-Torregrosa
- 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: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Anne
full_name: Hutter, Anne
last_name: Hutter
- first_name: Pablo
full_name: Arnalte-Mur, Pablo
last_name: Arnalte-Mur
- first_name: Siddhartha
full_name: Gurung-López, Siddhartha
last_name: Gurung-López
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- first_name: Daichi
full_name: Kashino, Daichi
last_name: Kashino
- first_name: Charlie
full_name: Conroy, Charlie
last_name: Conroy
- first_name: David
full_name: Sobral, David
last_name: Sobral
citation:
ama: 'Torralba-Torregrosa A, Matthee JJ, Naidu RP, et al. Anatomy of an ionized
bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter
COLA1 and its environment. Astronomy and Astrophysics. 2024;689. doi:10.1051/0004-6361/202450318'
apa: 'Torralba-Torregrosa, A., Matthee, J. J., Naidu, R. P., Mackenzie, R., Pezzulli,
G., Hutter, A., … Sobral, D. (2024). Anatomy of an ionized bubble: NIRCam grism
spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment.
Astronomy and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202450318'
chicago: 'Torralba-Torregrosa, Alberto, Jorryt J Matthee, Rohan P. Naidu, Ruari
Mackenzie, Gabriele Pezzulli, Anne Hutter, Pablo Arnalte-Mur, et al. “Anatomy
of an Ionized Bubble: NIRCam Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman-
α Emitter COLA1 and Its Environment.” Astronomy and Astrophysics. EDP Sciences,
2024. https://doi.org/10.1051/0004-6361/202450318.'
ieee: 'A. Torralba-Torregrosa et al., “Anatomy of an ionized bubble: NIRCam
grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its
environment,” Astronomy and Astrophysics, vol. 689. EDP Sciences, 2024.'
ista: 'Torralba-Torregrosa A, Matthee JJ, Naidu RP, Mackenzie R, Pezzulli G, Hutter
A, Arnalte-Mur P, Gurung-López S, Tacchella S, Oesch P, Kashino D, Conroy C, Sobral
D. 2024. Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6
double-peaked Lyman- α emitter COLA1 and its environment. Astronomy and Astrophysics.
689, A44.'
mla: 'Torralba-Torregrosa, Alberto, et al. “Anatomy of an Ionized Bubble: NIRCam
Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman- α Emitter COLA1 and Its
Environment.” Astronomy and Astrophysics, vol. 689, A44, EDP Sciences,
2024, doi:10.1051/0004-6361/202450318.'
short: A. Torralba-Torregrosa, J.J. Matthee, R.P. Naidu, R. Mackenzie, G. Pezzulli,
A. Hutter, P. Arnalte-Mur, S. Gurung-López, S. Tacchella, P. Oesch, D. Kashino,
C. Conroy, D. Sobral, Astronomy and Astrophysics 689 (2024).
date_created: 2024-09-08T22:01:11Z
date_published: 2024-09-01T00:00:00Z
date_updated: 2025-09-08T09:20:52Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450318
external_id:
arxiv:
- '2404.10040'
isi:
- '001303205700016'
file:
- access_level: open_access
checksum: a6c0df287c75e8929db9f42badeac859
content_type: application/pdf
creator: dernst
date_created: 2024-09-11T07:35:00Z
date_updated: 2024-09-11T07:35:00Z
file_id: '18055'
file_name: 2024_AstronomyAstrophysics_TorralbaTorregrosa.pdf
file_size: 6225413
relation: main_file
success: 1
file_date_updated: 2024-09-11T07:35:00Z
has_accepted_license: '1'
intvolume: ' 689'
isi: 1
language:
- iso: eng
month: '09'
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'
scopus_import: '1'
status: public
title: 'Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked
Lyman- α emitter COLA1 and its environment'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 689
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18447'
abstract:
- lang: eng
text: We present the first results on the spatial distribution of star formation
in 454 star-forming galaxies just after the epoch of reionisation (4.8 < z < 6.5)
using Hα emission-line maps and F444W imaging that traces the stellar continuum
from the JWST FRESCO NIRCam Slitless Spectroscopy Survey. The Hα equivalent width
profiles of star-forming galaxies across the main sequence at z ∼ 5.3 with stellar
masses 6.8≤ log(M*/M⊙) < 11.1 increase with radius, which provides direct evidence
for the inside-out growth of star-forming galaxies just after the epoch of reionisation.
GALFIT was used to calculate half-light radii, Reff, and central surface densities
within 1 kiloparsec, Σ1kpc of Hα and the continuum. At a fixed stellar mass of
Log(M*/M⊙) = 9.5, Σ1kpc, Hα is 1.04 ± 0.05 times higher than Σ1kpc, C, Reff, Hα
is 1.18 ± 0.03 times larger than Reff, C and both Reff measurements are smaller
than 1 kiloparsec. These measurements suggest the rapid build-up of compact bulges
via star formation just after the epoch of reionisation. By comparison to analogous
work done at lower redshifts with Hubble Space Telescope WFC3 slitless spectroscopy
as part of the 3D-HST (z ∼ 1) and CLEAR (z ∼ 0.5) surveys, we find that Reff(z)
evolves at the same pace for Hα and the continuum, but Σ1kpc(z) evolves faster
for Hα than the stellar continuum. As a function of the Hubble parameter, Reff, Hα/Reff,C = 1.1h(z)
and Σ1 kpc, Hα/Σ1 kpc,C = h(z)1.3. These parametrisations suggest that the inside-out
growth of the disk starts to dominate the inside-out growth of the bulge towards
lower redshifts. This is supported by the redshift evolution in the EW(Hα) profiles
from FRESCO, 3D-HST, and CLEAR at fixed stellar mass and when star-forming progenitors
are traced, in which in EW(Hα) rapidly increases with radius within the half-light
radius at z ∼ 5.3, but EW(Hα) increases only significantly with radius in the
outer disk at z ∼ 0.5.
acknowledgement: "JM is grateful to the Cosmic Dawn Center for the DAWN Fellowship.
JM thanks Adam Muzzin, Viola Gelli and Anne Hutter for useful discussions that led
to improvements in the analysis presented in this paper. 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\r\nSpace 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 program #1895. Support for program JWST-GO-1895
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.\r\nThis 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. RPN thanks the NASA Hubble
Fellowshp Program for the Hubble Fellowship. DM acknowledges funding from JWST-GO-01895.013,
provided through a grant from the STScI under NASA contract NAS5-03127."
article_number: A64
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: Jasleen
full_name: Matharu, Jasleen
last_name: Matharu
- first_name: Erica J.
full_name: Nelson, Erica J.
last_name: Nelson
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Natalie
full_name: Allen, Natalie
last_name: Allen
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: John
full_name: Chisholm, John
last_name: Chisholm
- first_name: Alba
full_name: Covelo-Paz, Alba
last_name: Covelo-Paz
- first_name: Yoshinobu
full_name: Fudamoto, Yoshinobu
last_name: Fudamoto
- first_name: Emma
full_name: Giovinazzo, Emma
last_name: Giovinazzo
- first_name: Thomas
full_name: Herard-Demanche, Thomas
last_name: Herard-Demanche
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Danilo
full_name: Marchesini, Danilo
last_name: Marchesini
- first_name: Romain A.
full_name: Meyer, Romain A.
last_name: Meyer
- first_name: Gonzalo
full_name: Prieto-Lyon, Gonzalo
last_name: Prieto-Lyon
- first_name: Naveen
full_name: Reddy, Naveen
last_name: Reddy
- first_name: Marko
full_name: Shuntov, Marko
last_name: Shuntov
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
- first_name: Mengyuan
full_name: Xiao, Mengyuan
last_name: Xiao
citation:
ama: Matharu J, Nelson EJ, Brammer G, et al. A first look at spatially resolved
star formation at 4.8 < z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy.
Astronomy and Astrophysics. 2024;690. doi:10.1051/0004-6361/202450522
apa: Matharu, J., Nelson, E. J., Brammer, G., Oesch, P. A., Allen, N., Shivaei,
I., … Xiao, M. (2024). A first look at spatially resolved star formation at 4.8
< z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy. Astronomy
and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202450522
chicago: Matharu, Jasleen, Erica J. Nelson, Gabriel Brammer, Pascal A. Oesch, Natalie
Allen, Irene Shivaei, Rohan P. Naidu, et al. “A First Look at Spatially Resolved
Star Formation at 4.8 < z < 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.”
Astronomy and Astrophysics. EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202450522.
ieee: J. Matharu et al., “A first look at spatially resolved star formation
at 4.8 < z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy,” Astronomy
and Astrophysics, vol. 690. EDP Sciences, 2024.
ista: Matharu J, Nelson EJ, Brammer G, Oesch PA, Allen N, Shivaei I, Naidu RP, Chisholm
J, Covelo-Paz A, Fudamoto Y, Giovinazzo E, Herard-Demanche T, Kerutt J, Kramarenko
I, Marchesini D, Meyer RA, Prieto-Lyon G, Reddy N, Shuntov M, Weibel A, Wuyts
S, Xiao M. 2024. A first look at spatially resolved star formation at 4.8 <
z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy. Astronomy and Astrophysics.
690, A64.
mla: Matharu, Jasleen, et al. “A First Look at Spatially Resolved Star Formation
at 4.8 < z < 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” Astronomy
and Astrophysics, vol. 690, A64, EDP Sciences, 2024, doi:10.1051/0004-6361/202450522.
short: J. Matharu, E.J. Nelson, G. Brammer, P.A. Oesch, N. Allen, I. Shivaei, R.P.
Naidu, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, E. Giovinazzo, T. Herard-Demanche,
J. Kerutt, I. Kramarenko, D. Marchesini, R.A. Meyer, G. Prieto-Lyon, N. Reddy,
M. Shuntov, A. Weibel, S. Wuyts, M. Xiao, Astronomy and Astrophysics 690 (2024).
date_created: 2024-10-20T22:02:06Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:22:57Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202450522
external_id:
arxiv:
- '2404.17629'
isi:
- '001322237700004'
file:
- access_level: open_access
checksum: 10ae78291aa9fa9a9e64724c42d91588
content_type: application/pdf
creator: dernst
date_created: 2024-10-21T11:45:35Z
date_updated: 2024-10-21T11:45:35Z
file_id: '18457'
file_name: 2024_AstronomyAstrophysics_Matharu.pdf
file_size: 825494
relation: main_file
success: 1
file_date_updated: 2024-10-21T11:45:35Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
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'
scopus_import: '1'
status: public
title: A first look at spatially resolved star formation at 4.8 < z < 6.5 with JWST
FRESCO NIRCam 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: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18448'
abstract:
- lang: eng
text: "Aims. This paper utilises the James Webb Space Telescope (JWST) Mid-Infrared
Instrument (MIRI) to extend the observational studies of dust and polycyclic aromatic
hydrocarbon (PAH) emission to a new mass and star formation rate (SFR) parameter
space beyond our local Universe. The combination of fully sampled spectral energy
distributions (SEDs) with multiple mid-infrared (mid-IR) bands and the unprecedented
sensitivity of MIRI allows us to investigate dust obscuration and PAH behaviour
from z = 0.7 up to z = 2 in typical main-sequence galaxies. Our focus is on constraining
the evolution of PAH strength and the dust-obscured luminosity fraction before
and during cosmic noon, the epoch of peak star formation activity in the Universe.\r\n\r\nMethods.
In this study, we utilise MIRI multi-band imaging data from the SMILES survey
(5 to 25 μm), complemented with NIRCam photometry from the JADES survey (1 to
5 μm), available HST photometry (0.4 to 0.9 μm), and spectroscopic redshifts from
the FRESCO and JADES surveys in GOODS-S for 443 star-forming (without dominant
active galactic nucleus (AGN)) galaxies at z = 0.7 − 2.0. This redshift range
was chosen to ensure that the MIRI data cover mid-IR dust emission. Our methodology
involved employing ultraviolet (UV) to IR energy balance SED fitting to robustly
constrain the fraction of dust mass in PAHs and dust-obscured luminosity. Additionally,
we inferred dust sizes from MIRI 15 μm imaging data, enhancing our understanding
of the physical characteristics of dust within these galaxies.\r\n\r\nResults.
We find a strong correlation between the fraction of dust in PAHs (PAH fraction,
qPAH) with stellar mass. Moreover, the sub-sample with robust qPAH measurements
(N = 216) shows a similar behaviour between qPAH and gas-phase metallicity to
that at z ∼ 0, suggesting a universal relation: qPAH is constant (∼3.4%) above
a metallicity of Z ∼ 0.5 Z⊙ and decreases to < 1% at metallicities ≲0.3 Z⊙. This
indicates that metallicity is a good indicator of the interstellar medium properties
that affect the balance between the formation and destruction of PAHs. The lack
of a redshift evolution from z ∼ 0 − 2 also implies that above Z ∼ 0.5 Z⊙ the
PAH emission effectively traces obscured luminosity and the previous locally calibrated
PAH-SFR calibrations remain applicable in this metallicity regime. We observe
a strong correlation between the obscured UV luminosity fraction (ratio of obscured
to total luminosity) and stellar mass. Above the stellar mass of M* > 5 × 109
M⊙, on average, more than half of the emitted luminosity is obscured, while there
exists a non-negligible population of lower-mass galaxies with > 50% obscured
fractions. At a fixed mass, the obscured fraction correlates with SFR surface
density. This is a result of higher dust covering fractions in galaxies with more
compact star-forming regions. Similarly, galaxies with high IRX (IR to UV luminosity)
at a given mass or UV continuum slope (β) tend to have higher ΣSFR and shallower
attenuation curves, owing to their higher effective dust optical depths and more
compact star-forming regions."
acknowledgement: IS thanks the members of the JWST/MIRI instrument team for their
exceptional efforts and for providing an outstanding experience during the commissioning
period of JWST, which fostered numerous fruitful discussions and significantly enhanced
the quality of data reduction in this study. IS also thanks Karin Sandstrom and
Joel Leja for their insightful discussions during the scientific development of
this work. Additionally, IS acknowledges the contribution of Andras Gáspar to the
construction of the F560W PSF utilised in this research. This work was supported
in part by NASA grant NNX13AD82G. Part of this research has been funded by Atraccíon
de Talento Grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain. AJB and
AC 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). 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. PGP-G acknowledges
support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia
e Innovación CIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. SA
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. 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 PID 1207, 1080, 1081, 1895,
1220, 1286, 1287, 1963. Based on observations made with the NASA/ESA Hubble Space
Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration
between the Space Telescope Science Institute (STScI/NASA), the Space Telescope
European Coordinating Facility (ST-ECF/ESAC/ESA) and the Canadian Astronomy Data
Centre (CADC/NRC/CSA).
article_number: A89
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: Irene
full_name: Shivaei, Irene
last_name: Shivaei
- first_name: Stacey
full_name: Alberts, Stacey
last_name: Alberts
- first_name: Michael
full_name: Florian, Michael
last_name: Florian
- first_name: George
full_name: Rieke, George
last_name: Rieke
- first_name: Stijn
full_name: Wuyts, Stijn
last_name: Wuyts
- first_name: Sarah
full_name: Bodansky, Sarah
last_name: Bodansky
- first_name: Andrew J.
full_name: Bunker, Andrew J.
last_name: Bunker
- first_name: Alex J.
full_name: Cameron, Alex J.
last_name: Cameron
- first_name: Mirko
full_name: Curti, Mirko
last_name: Curti
- first_name: Francesco
full_name: Da'Eugenio, Francesco
last_name: Da'Eugenio
- first_name: Ugne
full_name: Dudzevičiūte, Ugne
last_name: Dudzevičiūte
- first_name: Zhiyuan
full_name: Ji, Zhiyuan
last_name: Ji
- first_name: Benjamin D.
full_name: Johnson, Benjamin D.
last_name: Johnson
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
orcid: 0000-0001-5346-6048
- first_name: Jianwei
full_name: Lyu, Jianwei
last_name: Lyu
- 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: Jane
full_name: Morrison, Jane
last_name: Morrison
- first_name: Rohan
full_name: Naidu, Rohan
last_name: Naidu
- first_name: Pablo G.
full_name: Pérez-González, Pablo G.
last_name: Pérez-González
- first_name: Naveen
full_name: Reddy, Naveen
last_name: Reddy
- first_name: Brant
full_name: Robertson, Brant
last_name: Robertson
- first_name: Yang
full_name: Sun, Yang
last_name: Sun
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Katherine
full_name: Whitaker, Katherine
last_name: Whitaker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
- first_name: Christopher N.A.
full_name: Willmer, Christopher N.A.
last_name: Willmer
- first_name: Joris
full_name: Witstok, Joris
last_name: Witstok
- first_name: Mengyuan
full_name: Xiao, Mengyuan
last_name: Xiao
- first_name: Yongda
full_name: Zhu, Yongda
last_name: Zhu
citation:
ama: Shivaei I, Alberts S, Florian M, et al. A new census of dust and polycyclic
aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. Astronomy and Astrophysics.
2024;690. doi:10.1051/0004-6361/202449579
apa: Shivaei, I., Alberts, S., Florian, M., Rieke, G., Wuyts, S., Bodansky, S.,
… Zhu, Y. (2024). A new census of dust and polycyclic aromatic hydrocarbons at
z = 0.7-2 with JWST MIRI. Astronomy and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202449579
chicago: Shivaei, Irene, Stacey Alberts, Michael Florian, George Rieke, Stijn Wuyts,
Sarah Bodansky, Andrew J. Bunker, et al. “A New Census of Dust and Polycyclic
Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” Astronomy and Astrophysics.
EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202449579.
ieee: I. Shivaei et al., “A new census of dust and polycyclic aromatic hydrocarbons
at z = 0.7-2 with JWST MIRI,” Astronomy and Astrophysics, vol. 690. EDP
Sciences, 2024.
ista: Shivaei I, Alberts S, Florian M, Rieke G, Wuyts S, Bodansky S, Bunker AJ,
Cameron AJ, Curti M, Da’Eugenio F, Dudzevičiūte U, Ji Z, Johnson BD, Kramarenko
I, Lyu J, Matthee JJ, Morrison J, Naidu R, Pérez-González PG, Reddy N, Robertson
B, Sun Y, Tacchella S, Whitaker K, Williams CC, Willmer CNA, Witstok J, Xiao M,
Zhu Y. 2024. A new census of dust and polycyclic aromatic hydrocarbons at z =
0.7-2 with JWST MIRI. Astronomy and Astrophysics. 690, A89.
mla: Shivaei, Irene, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons
at z = 0.7-2 with JWST MIRI.” Astronomy and Astrophysics, vol. 690, A89,
EDP Sciences, 2024, doi:10.1051/0004-6361/202449579.
short: I. Shivaei, S. Alberts, M. Florian, G. Rieke, S. Wuyts, S. Bodansky, A.J.
Bunker, A.J. Cameron, M. Curti, F. Da’Eugenio, U. Dudzevičiūte, Z. Ji, B.D. Johnson,
I. Kramarenko, J. Lyu, J.J. Matthee, J. Morrison, R. Naidu, P.G. Pérez-González,
N. Reddy, B. Robertson, Y. Sun, S. Tacchella, K. Whitaker, C.C. Williams, C.N.A.
Willmer, J. Witstok, M. Xiao, Y. Zhu, Astronomy and Astrophysics 690 (2024).
date_created: 2024-10-20T22:02:06Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2026-03-05T11:19:11Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202449579
external_id:
arxiv:
- '2402.07989'
isi:
- '001381135700006'
file:
- access_level: open_access
checksum: f399be98968b9ca5611c832a9b1eee2b
content_type: application/pdf
creator: dernst
date_created: 2024-10-21T11:52:29Z
date_updated: 2024-10-21T11:52:29Z
file_id: '18458'
file_name: 2024_AstronomyAstrophysics_Shivaei.pdf
file_size: 10777358
relation: main_file
success: 1
file_date_updated: 2024-10-21T11:52:29Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
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'
scopus_import: '1'
status: public
title: A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with
JWST MIRI
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
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18492'
abstract:
- lang: eng
text: 'Surveys in the Milky Way and Large Magellanic Cloud have revealed that the
majority of massive stars will interact with companions during their lives. However,
knowledge of the binary properties of massive stars at low metallicity, and therefore
in conditions approaching those of the Early Universe, remain sparse. We present
the Binarity at LOw Metallicity (BLOeM) campaign, an ESO large programme designed
to obtain 25 epochs of spectroscopy for 929 massive stars in the Small Magellanic
Cloud, allowing us to probe multiplicity in the lowest-metallicity conditions
to date (Z = 0.2 Z⊙). BLOeM will provide (i) the binary fraction, (ii) the orbital
configurations of systems with periods of P ≲ 3 yr, (iii) dormant black-hole binary
candidates (OB+BH), and (iv) a legacy database of physical parameters of massive
stars at low metallicity. Main sequence (OB-type) and evolved (OBAF-type) massive
stars are observed with the LR02 setup of the GIRAFFE instrument of the Very Large
Telescope (3960–4570 Å resolving power R = 6200; typical signal-to-noise ratio(S/N)
≈70–100). This paper utilises the first nine epochs obtained over a three-month
time period. We describe the survey and data reduction, perform a spectral classification
of the stacked spectra, and construct a Hertzsprung-Russell diagram of the sample
via spectral-type and photometric calibrations. Our detailed classification reveals
that the sample covers spectral types from O4 to F5, spanning the effective temperature
and luminosity ranges 6.5 ≲ Teff/kK ≲ 45 and 3.7 < log L/L⊙ < 6.1 and initial
masses of 8 ≲ Mini ≲ 80 M⊙. The sample comprises 159 O-type stars, 331 early B-type
(B0–3) dwarfs and giants (luminosity classes V–III), 303 early B-type supergiants
(II–I), and 136 late-type BAF supergiants. At least 82 stars are OBe stars: 20
O-type and 62 B-type (13% and 11% of the respective samples). In addition, the
sample includes 4 high-mass X-ray binaries, 3 stars resembling luminous blue variables,
2 bloated stripped-star candidates, 2 candidate magnetic stars, and 74 eclipsing
binaries.'
acknowledgement: 'The research leading to these results has received funding from
the European Research Council (ERC) under the European Union’s Horizon 2020 research
and innovation programme (grant agreement numbers 772225: MULTIPLES). PAC and JMB
are supported by the Science and Technology Facilities Council research grant ST/V000853/1
(PI. V. Dhillon). DMB gratefully acknowledges support from UK Research and Innovation
(UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon
Europe funding guarantee (SYMPHONY; PI Bowman; grant number: EP/Y031059/1), and
a Royal Society University Research Fellowship (PI Bowman; grant number: URF\R1\231631).
ZK acknowledges support from JSPS Kakenhi Grant-in-Aid for Scientific Research (23K19071).
IM acknowledges support from the Australian Research Council (ARC) Centre of Excellence
for Gravitational Wave Discovery (OzGrav), through project number CE230100016. AACS,
VR, RRL, and MBP are funded by the Deutsche Forschungsgemeinschaft (DFG, German
Research Foundation) in the form of an Emmy Noether Research Group – Project-ID
445674056 (SA4064/1-1, PI Sander). GGT and JJ are supported by the German Deutsche
Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1, PI Sander)
VR, GGT, and AACS further acknowledge support from the Federal Ministry of Education
and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the
Excellence Strategy of the German Federal and State Governments. ECS acknowledges
financial support by the Federal Ministry for Economic Affairs and Climate Action
(BMWK) via the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt,
DLR) grant 50 OR 2306 (PI: Ramachandran/Sander). This work has received funding
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation programme (Grant agreement No. 945806) and is supported
by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s
Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES Excellence Cluster).
LMO is thankful for the funding provided by the DFG grant 443790621. This paper
benefited from discussions at the International Space Science Institute (ISSI) in
Bern through ISSI International Team project 512 (Multiwavelength View on Massive
Stars in the Era of Multimessenger Astronomy). DP acknowledges financial support
by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005. JIV acknowledges
the European Research Council for support from the ERC Advanced grant ERC-2021-ADG101054731.
JSV is supported by STFC (Science and Technology Facilities Council) funding under
grant number ST/V000233/1. GH, SS-D, SRB and AH acknowledge support from the State
Research Agency (AEI) of the Spanish Ministry of Science and Innovation (MICIN)
and the European Regional Development Fund, FEDER under grants PID2021-122397NB-C21
and CEX2019-000920-S. SRB also acknowledges financial support by NextGeneration
EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-ULL. DFR is thankful
for the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). F.N.,
and L.R.P. acknowledge support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41
funded by MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. MG acknowledges
financial support from the grants PID2021-125485NB-C22, CEX2019-000918-M funded
by MCIN/AEI/10.13039/501100011033 (State Agency for Research of the Spanish Ministry
of Science and Innovation) and SGR-2021-01069 (AGAUR). GM acknowledges funding support
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation programme (Grant agreement No. 772086). JMA acknowledges
support from the Spanish Government Ministerio de Ciencia e Innovación and Agencia
Estatal de Investigación (10.13 039/501 100 011 033) through grant PID2022-136640
NB-C22 and from the Consejo Superior de Investigaciones Científicas (CSIC) through
grant 2022-AEP 005. MP is supported by the BEKKER fellowship BPN/BEK/2022/1/00106
from the Polish National Agency for Academic Exchange. KS is funded by the National
Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. JM acknowledges
support from a Royal Society-Science Foundation Ireland University Research Fellowship.
SJ acknowledges support from the FWO PhD fellowship under project 11E1721N. FB acknowledges
the support of the European Research Council (ERC) Horizon Europe under grant agreement
number 101044048.'
article_number: A289
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: L. A.
full_name: Almeida, L. A.
last_name: Almeida
- first_name: F.
full_name: Backs, F.
last_name: Backs
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: J. M.
full_name: Bestenlehner, J. M.
last_name: Bestenlehner
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: V. A.
full_name: Bronner, V. A.
last_name: Bronner
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: M.
full_name: Fabry, M.
last_name: Fabry
- first_name: M.
full_name: Gieles, M.
last_name: Gieles
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: G.
full_name: González-Torà, G.
last_name: González-Torà
- first_name: G.
full_name: Gräfener, G.
last_name: Gräfener
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: C.
full_name: Hawcroft, C.
last_name: Hawcroft
- first_name: V.
full_name: Hénault-Brunet, V.
last_name: Hénault-Brunet
- first_name: A.
full_name: Herrero, A.
last_name: Herrero
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: S.
full_name: Janssens, S.
last_name: Janssens
- first_name: C.
full_name: Johnston, C.
last_name: Johnston
- first_name: J.
full_name: Josiek, J.
last_name: Josiek
- first_name: S.
full_name: Justham, S.
last_name: Justham
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z. Z.
full_name: Katabi, Z. Z.
last_name: Katabi
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: J.
full_name: Kubát, J.
last_name: Kubát
- first_name: B.
full_name: Kubátová, B.
last_name: Kubátová
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: R. R.
full_name: Lefever, R. R.
last_name: Lefever
- first_name: B.
full_name: Ludwig, B.
last_name: Ludwig
- first_name: J.
full_name: Mackey, J.
last_name: Mackey
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: J.
full_name: Maíz Apellániz, J.
last_name: Maíz Apellániz
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: G.
full_name: Maravelias, G.
last_name: Maravelias
- first_name: P.
full_name: Marchant, P.
last_name: Marchant
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: F.
full_name: Najarro, F.
last_name: Najarro
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: A. J.G.
full_name: O'Grady, A. J.G.
last_name: O'Grady
- first_name: R.
full_name: Ovadia, R.
last_name: Ovadia
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Pawlak, M.
last_name: Pawlak
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: D. F.
full_name: Rocha, D. F.
last_name: Rocha
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: T.
full_name: Sayada, T.
last_name: Sayada
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: E. C.
full_name: Schösser, E. C.
last_name: Schösser
- first_name: C.
full_name: Schürmann, C.
last_name: Schürmann
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: S.
full_name: Shahaf, S.
last_name: Shahaf
- first_name: S.
full_name: Simón-Díaz, S.
last_name: Simón-Díaz
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: J. Th
full_name: Van Loon, J. Th
last_name: Van Loon
- first_name: R.
full_name: Valli, R.
last_name: Valli
- first_name: L. A.C.
full_name: Van Son, L. A.C.
last_name: Van Son
- first_name: A.
full_name: Vigna-Gómez, A.
last_name: Vigna-Gómez
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: R.
full_name: Willcox, R.
last_name: Willcox
citation:
ama: 'Shenar T, Bodensteiner J, Sana H, et al. Binarity at LOw Metallicity (BLOeM):
A spectroscopic VLT monitoring survey of massive stars in the SMC. Astronomy
and Astrophysics. 2024;690. doi:10.1051/0004-6361/202451586'
apa: 'Shenar, T., Bodensteiner, J., Sana, H., Crowther, P. A., Lennon, D. J., Abdul-Masih,
M., … Willcox, R. (2024). Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC. Astronomy and Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202451586'
chicago: 'Shenar, T., J. Bodensteiner, H. Sana, P. A. Crowther, D. J. Lennon, M.
Abdul-Masih, L. A. Almeida, et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic
VLT Monitoring Survey of Massive Stars in the SMC.” Astronomy and Astrophysics.
EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202451586.'
ieee: 'T. Shenar et al., “Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC,” Astronomy and Astrophysics,
vol. 690. EDP Sciences, 2024.'
ista: 'Shenar T, Bodensteiner J, Sana H, Crowther PA, Lennon DJ, Abdul-Masih M,
Almeida LA, Backs F, Berlanas SR, Bernini-Peron M, Bestenlehner JM, Bowman DM,
Bronner VA, Britavskiy N, De Koter A, De Mink SE, Deshmukh K, Evans CJ, Fabry
M, Gieles M, Gilkis A, González-Torà G, Gräfener G, Götberg YLL, Hawcroft C, Hénault-Brunet
V, Herrero A, Holgado G, Janssens S, Johnston C, Josiek J, Justham S, Kalari VM,
Katabi ZZ, Keszthelyi Z, Klencki J, Kubát J, Kubátová B, Langer N, Lefever RR,
Ludwig B, Mackey J, Mahy L, Maíz Apellániz J, Mandel I, Maravelias G, Marchant
P, Menon A, Najarro F, Oskinova LM, O’Grady AJG, Ovadia R, Patrick LR, Pauli D,
Pawlak M, Ramachandran V, Renzo M, Rocha DF, Sander AAC, Sayada T, Schneider FRN,
Schootemeijer A, Schösser EC, Schürmann C, Sen K, Shahaf S, Simón-Díaz S, Stoop
M, Toonen S, Tramper F, Van Loon JT, Valli R, Van Son LAC, Vigna-Gómez A, Villaseñor
JI, Vink JS, Wang C, Willcox R. 2024. Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC. Astronomy and Astrophysics.
690, A289.'
mla: 'Shenar, T., et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic VLT
Monitoring Survey of Massive Stars in the SMC.” Astronomy and Astrophysics,
vol. 690, A289, EDP Sciences, 2024, doi:10.1051/0004-6361/202451586.'
short: T. Shenar, J. Bodensteiner, H. Sana, P.A. Crowther, D.J. Lennon, M. Abdul-Masih,
L.A. Almeida, F. Backs, S.R. Berlanas, M. Bernini-Peron, J.M. Bestenlehner, D.M.
Bowman, V.A. Bronner, N. Britavskiy, A. De Koter, S.E. De Mink, K. Deshmukh, C.J.
Evans, M. Fabry, M. Gieles, A. Gilkis, G. González-Torà, G. Gräfener, Y.L.L. Götberg,
C. Hawcroft, V. Hénault-Brunet, A. Herrero, G. Holgado, S. Janssens, C. Johnston,
J. Josiek, S. Justham, V.M. Kalari, Z.Z. Katabi, Z. Keszthelyi, J. Klencki, J.
Kubát, B. Kubátová, N. Langer, R.R. Lefever, B. Ludwig, J. Mackey, L. Mahy, J.
Maíz Apellániz, I. Mandel, G. Maravelias, P. Marchant, A. Menon, F. Najarro, L.M.
Oskinova, A.J.G. O’Grady, R. Ovadia, L.R. Patrick, D. Pauli, M. Pawlak, V. Ramachandran,
M. Renzo, D.F. Rocha, A.A.C. Sander, T. Sayada, F.R.N. Schneider, A. Schootemeijer,
E.C. Schösser, C. Schürmann, K. Sen, S. Shahaf, S. Simón-Díaz, M. Stoop, S. Toonen,
F. Tramper, J.T. Van Loon, R. Valli, L.A.C. Van Son, A. Vigna-Gómez, J.I. Villaseñor,
J.S. Vink, C. Wang, R. Willcox, Astronomy and Astrophysics 690 (2024).
date_created: 2024-11-03T23:01:44Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:31:11Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202451586
external_id:
arxiv:
- '2407.14593'
isi:
- '001336770600014'
file:
- access_level: open_access
checksum: b378b36726591f3479a927d924ab8e77
content_type: application/pdf
creator: dernst
date_created: 2024-11-04T09:52:26Z
date_updated: 2024-11-04T09:52:26Z
file_id: '18500'
file_name: 2024_AstronomyAstrophysics_Shenar.pdf
file_size: 4267349
relation: main_file
success: 1
file_date_updated: 2024-11-04T09:52:26Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
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'
scopus_import: '1'
status: public
title: 'Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey
of massive stars in the SMC'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
OA_type: diamond
_id: '18493'
abstract:
- lang: eng
text: "Context. The escape of Lyman-α photons at redshifts greater than two is an
ongoing subject of study and an important quantity to further understanding of
Lyman-α emitters (LAEs), the transmission of Lyman-α photons through the interstellar
medium and intergalactic medium, and the impact these LAEs have on cosmic reionisation.\r\n\r\nAims.
This study aims to assess the Lyman-α escape fraction, fesc, Lyα, over the redshift
range 2.9 < z < 6.7, focusing on Very Large Telescope/Multi Unit Spectroscopic
Explorer (VLT/MUSE) selected, gravitationally lensed, intrinsically faint LAEs.
These galaxies are of particular interest as the potential drivers of cosmic reionisation.\r\n\r\nMethods.
We assessed fesc, Lyα in two ways: through an individual study of 96 LAEs behind
the A2744 lensing cluster, with James Webb Space Telescope/Near-Infrared Camera
(JWST/NIRCam) and HST data, and through a study of the global evolution of fesc, Lyα
using the state-of-the-art luminosity functions for LAEs and the UV-selected ‘parent’
population (dust-corrected). We compared these studies to those in the literature
based on brighter samples.\r\n\r\nResults. We find a negligible redshift evolution
of fesc, Lyα for our individual galaxies; it is likely that it was washed out
by significant intrinsic scatter. We observed a more significant evolution towards
higher escape fractions with decreasing UV magnitude and fit this relation. When
comparing the two luminosity functions to derive fesc, Lyα in a global sense,
we saw agreement with previous literature when integrating the luminosity functions
to a bright limit. However, when integrating using a faint limit equivalent to
the observational limits of our samples, we observed enhanced values of fesc, Lyα,
particularly around z ∼ 6, where fesc, Lyα becomes consistent with 100% escape.
This indicates for the faint regimes we sampled that galaxies towards reionisation
tend to allow very large fractions of Lyman-α photons to escape. We interpret
this as evidence of a lack of any significant dust in these populations; our sample
is likely dominated by young, highly star-forming chemically unevolved galaxies.
Finally, we assessed the contribution of the LAE population to reionisation using
our latest values for fesc, Lyα and the LAE luminosity density. The dependence
on the escape fraction of Lyman continuum photons is strong, but for values similar
to those observed recently in z ∼ 3 LAEs and high-redshift analogues, LAEs could
provide all the ionising emissivity necessary for reionisation."
acknowledgement: "This work is done based on observations made with ESO Telescopes
at the La Silla Paranal Observatory under programme IDs 060.A-9345, 092.A-0472,
094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also
based on observations obtained with the\r\nNASA/ESA Hubble Space Telescope, retrieved
from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science
Institute (STScI). STScI is operated by the Association of Universities for Research
in Astronomy, Inc. under NASA contract NAS 5-26555. All plots in this paper were
created using Matplotlib (Hunter 2007). Part of this work was supported by the French
CNRS, the Aix-Marseille University, the French Programme National de Cosmologie
et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This
work also received support from the French government under the France 2030 investment
plan, as part of the Excellence Initiative of Aix-Marseille University - A*MIDEX
(AMX-19-IET-008 - IPhU).\r\nFinancial support from the World Laboratory, the Odon
Vallet Foundation and VNSC is gratefully acknowledged. Tran Thi Thai was funded
by Vingroup JSC and supported by the Master, PhD Scholarship Programme of Vingroup
Innovation Foundation (VINIF), Institute of Big Data, code VINIF.2023.TS.108. This
research was funded by Vingroup Innovation Foundation under project code VINIF.2023.DA.057."
article_number: A302
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: I.
full_name: Goovaerts, I.
last_name: Goovaerts
- first_name: T. T.
full_name: Thai, T. T.
last_name: Thai
- first_name: R.
full_name: Pello, R.
last_name: Pello
- first_name: P.
full_name: Tuan-Anh, P.
last_name: Tuan-Anh
- first_name: N.
full_name: Laporte, N.
last_name: Laporte
- 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: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: J.
full_name: Pharo, J.
last_name: Pharo
citation:
ama: Goovaerts I, Thai TT, Pello R, et al. Charting the Lyman-α escape fraction
in the range 2.9 < z < 6.7 and consequences for the LAE reionisation contribution.
Astronomy and Astrophysics. 2024;690. doi:10.1051/0004-6361/202451432
apa: Goovaerts, I., Thai, T. T., Pello, R., Tuan-Anh, P., Laporte, N., Matthee,
J. J., … Pharo, J. (2024). Charting the Lyman-α escape fraction in the range 2.9
< z < 6.7 and consequences for the LAE reionisation contribution. Astronomy
and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451432
chicago: Goovaerts, I., T. T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, Jorryt J
Matthee, T. Nanayakkara, and J. Pharo. “Charting the Lyman-α Escape Fraction in
the Range 2.9 < z < 6.7 and Consequences for the LAE Reionisation Contribution.”
Astronomy and Astrophysics. EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202451432.
ieee: I. Goovaerts et al., “Charting the Lyman-α escape fraction in the range
2.9 < z < 6.7 and consequences for the LAE reionisation contribution,”
Astronomy and Astrophysics, vol. 690. EDP Sciences, 2024.
ista: Goovaerts I, Thai TT, Pello R, Tuan-Anh P, Laporte N, Matthee JJ, Nanayakkara
T, Pharo J. 2024. Charting the Lyman-α escape fraction in the range 2.9 <
z < 6.7 and consequences for the LAE reionisation contribution. Astronomy
and Astrophysics. 690, A302.
mla: Goovaerts, I., et al. “Charting the Lyman-α Escape Fraction in the Range 2.9
< z < 6.7 and Consequences for the LAE Reionisation Contribution.” Astronomy
and Astrophysics, vol. 690, A302, EDP Sciences, 2024, doi:10.1051/0004-6361/202451432.
short: I. Goovaerts, T.T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, J.J. Matthee,
T. Nanayakkara, J. Pharo, Astronomy and Astrophysics 690 (2024).
date_created: 2024-11-03T23:01:45Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:28:28Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202451432
external_id:
arxiv:
- '2408.00517'
isi:
- '001339205700015'
file:
- access_level: open_access
checksum: 4007e2b0fadf93bea61c5bec3fc97e87
content_type: application/pdf
creator: dernst
date_created: 2024-11-04T08:04:44Z
date_updated: 2024-11-04T08:04:44Z
file_id: '18495'
file_name: 2024_AstronomyAstrophysics_Goovaerts.pdf
file_size: 2008461
relation: main_file
success: 1
file_date_updated: 2024-11-04T08:04:44Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
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'
scopus_import: '1'
status: public
title: Charting the Lyman-α escape fraction in the range 2.9 < z < 6.7 and consequences
for the LAE reionisation contribution
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
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 and 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
and 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
and 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 and 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 and Astrophysics.
690, A255.
mla: Di Cesare, Claudia, et al. “Carbon Envelopes around Merging Galaxies at z ~
4.5.” Astronomy and 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 and Astrophysics 690 (2024).
corr_author: '1'
date_created: 2024-11-10T23:02:00Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:35:57Z
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
content_type: application/pdf
creator: dernst
date_created: 2024-11-11T08:54:11Z
date_updated: 2024-11-11T08:54:11Z
file_id: '18533'
file_name: 2024_AstronomyAstrophysics_diCesare.pdf
file_size: 8033864
relation: main_file
success: 1
file_date_updated: 2024-11-11T08:54:11Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
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'
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: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18528'
abstract:
- lang: eng
text: The recent measurement of magnetic field strength inside the radiative interior
of red giant stars has opened the way toward full 3D characterization of the geometry
of stable large-scale magnetic fields. However, current measurements, which are
limited to dipolar (ℓ = 1) mixed modes, do not properly constrain the topology
of magnetic fields due to degeneracies on the observed magnetic field signature
on such ℓ = 1 mode frequencies. Efforts focused toward unambiguous detections
of magnetic field configurations are now key to better understand angular momentum
transport in stars. We investigated the detectability of complex magnetic field
topologies (such as the ones observed at the surface of stars with a radiative
envelope with spectropolarimetry) inside the radiative interior of red giants.
We focused on a field composed of a combination of a dipole and a quadrupole (quadrudipole)
and on an offset field. We explored the potential of probing such magnetic field
topologies from a combined measurement of magnetic signatures on ℓ = 1 and quadrupolar
(ℓ = 2) mixed mode oscillation frequencies. We first derived the asymptotic theoretical
formalism for computing the asymmetric signature in the frequency pattern for
ℓ = 2 modes due to a quadrudipole magnetic field. To access asymmetry parameters
for more complex magnetic field topologies, we numerically performed a grid search
over the parameter space to map the degeneracy of the signatures of given topologies.
We demonstrate the crucial role played by ℓ = 2 mixed modes in accessing internal
magnetic fields with a quadrupolar component. The degeneracy of the quadrudipole
compared to pure dipolar fields is lifted when considering magnetic asymmetries
in both ℓ = 1 and ℓ = 2 mode frequencies. In addition to the analytical derivation
for the quadrudipole, we present the prospect for complex magnetic field inversions
using magnetic sensitivity kernels from standard perturbation analysis for forward
modeling. Using this method, we explored the detectability of offset magnetic
fields from ℓ = 1 and ℓ = 2 frequencies and demonstrate that offset fields may
be mistaken for weak and centered magnetic fields, resulting in underestimating
the magnetic field strength in stellar cores. We emphasize the need to characterize
ℓ = 2 mixed-mode frequencies, (along with the currently characterized ℓ = 1 mixed
modes), to unveil the higher-order components of the geometry of buried magnetic
fields and to better constrain angular momentum transport inside stars.
acknowledgement: The authors thank S. Mathis, L. Barrault, S. Torres, A. Cristea,
and K. M. Smith for very useful discussions. This project has received funding from
the European Union’s Horizon 2020 research and innovation programme under the Marie
Skłodowska-Curíe grant agreement No 101034413. The authors thank the anonymous referee
for valuable comments and suggestions to improve the manuscript.
article_number: A217
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Srijan B
full_name: Das, Srijan B
id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
last_name: Das
orcid: 0000-0003-0896-7972
- first_name: Lukas
full_name: Einramhof, Lukas
id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c
last_name: Einramhof
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: Das SB, Einramhof L, Bugnet LA. Unveiling complex magnetic field configurations
in red giant stars. Astronomy and Astrophysics. 2024;690. doi:10.1051/0004-6361/202450918
apa: Das, S. B., Einramhof, L., & Bugnet, L. A. (2024). Unveiling complex magnetic
field configurations in red giant stars. Astronomy and Astrophysics. EDP
Sciences. https://doi.org/10.1051/0004-6361/202450918
chicago: Das, Srijan B, Lukas Einramhof, and Lisa Annabelle Bugnet. “Unveiling Complex
Magnetic Field Configurations in Red Giant Stars.” Astronomy and Astrophysics.
EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202450918.
ieee: S. B. Das, L. Einramhof, and L. A. Bugnet, “Unveiling complex magnetic field
configurations in red giant stars,” Astronomy and Astrophysics, vol. 690.
EDP Sciences, 2024.
ista: Das SB, Einramhof L, Bugnet LA. 2024. Unveiling complex magnetic field configurations
in red giant stars. Astronomy and Astrophysics. 690, A217.
mla: Das, Srijan B., et al. “Unveiling Complex Magnetic Field Configurations in
Red Giant Stars.” Astronomy and Astrophysics, vol. 690, A217, EDP Sciences,
2024, doi:10.1051/0004-6361/202450918.
short: S.B. Das, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics 690 (2024).
corr_author: '1'
date_created: 2024-11-10T23:02:00Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:36:39Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202450918
ec_funded: 1
external_id:
arxiv:
- '2405.20133'
isi:
- '001336485200015'
file:
- access_level: open_access
checksum: d43bbe6ed8ce4512e65e2d0d87070cf6
content_type: application/pdf
creator: dernst
date_created: 2024-11-11T09:01:11Z
date_updated: 2024-11-11T09:01:11Z
file_id: '18534'
file_name: 2024_AstronomyAstrophysics_Das.pdf
file_size: 5306256
relation: main_file
success: 1
file_date_updated: 2024-11-11T09:01:11Z
has_accepted_license: '1'
intvolume: ' 690'
isi: 1
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
publication: Astronomy and Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Unveiling complex magnetic field configurations in red giant stars
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18904'
abstract:
- lang: eng
text: The Planetary Transits and Oscillations of stars mission (PLATO) will allow
us to measure surface rotation and monitor photometric activity of tens of thousands
of main sequence solar-type and subgiant stars. This paper is the first of a series
dedicated to the preparation of the analysis of stellar surface rotation and photospheric
activity with the near-future PLATO data. We describe in this work the strategy
that will be implemented in the PLATO pipeline to measure stellar surface rotation,
photometric activity, and long-term modulations. The algorithms are applied on
both noise-free and noisy simulations of solar-type stars, which include activity
cycles, latitudinal differential rotation, and spot evolution. PLATO simulated
systematics are included in the noisy light curves. We show that surface rotation
periods can be recovered with confidence for most of the stars with only six months
of observations and that the recovery rate of the analysis significantly improves
as additional observations are collected. This means that the first PLATO data
release will already provide a substantial set of measurements for this quantity,
with a significant refinement on their quality as the instrument obtains longer
light curves. Measuring the Schwabe-like magnetic activity cycle during the mission
will require that the same field be observed over a significant timescale (more
than four years). Nevertheless, PLATO will provide a vast and robust sample of
solar-type stars with constraints on the activity-cycle length. Such a sample
is lacking from previous missions dedicated to space photometry.
acknowledgement: 'This work presents results from the European Space Agency (ESA)
space mission PLATO. The PLATO payload, the PLATO Ground Segment and PLATO data
processing are joint developments of ESA and the PLATO Mission Consortium (PMC).
Funding for the PMC is provided at national levels, in particular by countries participating
in the PLATO Multilateral Agreement (Austria, Belgium, Czech Republic, Denmark,
France, Germany, Italy, Netherlands, Portugal, Spain, Sweden, Switzerland, Norway,
and United Kingdom) and institutions from Brazil. Members of the PLATO Consortium
can be found at https://platomission.com. The ESA PLATO mission website is https://www.cosmos.esa.int/plato.
The authors thank the teams working for PLATO for all their work. They acknowledge
the critical reading and the constructive comments from the anonymous referee that
significantly allowed improving the original version of this paper. They finally
thank R. Samadi for helpful advice and suggestions concerning the PSLS abilities.
S.N.B, A.F.L, S.Me, I.P and E.C acknowledge support from PLATO ASI-INAF agreement
no. 2022-28-HH.0 “PLATO Fase D”. S.N.B, L.A, A.S.B, Q.N, and A.S acknowledge financial
support by ERC Whole Sun Synergy grant #810218. S.N.B, R.A.G, L.A, A.S.B, Q.N.,
D.B.P, E.P, and A.S acknowledge the support from PLATO CNES grant. R.A.G, D.B.P,
and E.P acknowledge the support from SoHO/GOLF CNES grant. A.S.B, Q.N, and A.S acknowledge
the support from INSU/PNST grant and Solar Orbiter CNES grant. A.S acknowledges
funding from from the European Union’s Horizon-2020 research and innovation program
(grant agreement no. 776403 ExoplANETS-A) and the Programme National de Planétologie
(PNP). A.R.G.S acknowledges the support from the FCT through national funds and
FEDER through COMPETE2020 (UIDB/04434/2020, UIDP/04434/2020, 2022.03993.PTDC) and
the support from the FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001.
S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN)
with the Ramón y Cajal fellowship no. RYC-2015-17697 and through AEI under the Severo
Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.Ma acknowledges
support from the Spanish Ministry of Science and Innovation (MICINN) with the grant
no. PID2019-107187GB-I00. M.J.G., K.B., R.M.O, J.P, O.R., C.R. acknowledge support
from CNES. The computations were performed with the IRFU/CEA Saclay server facilities,
funded by ERC Synergy grant WholeSun No.810218, the P2IO Labex emergence project
FlarePredict, and CNES PLATO funds. Software:star-privateer (this work), pyspot
(Aigrain et al. 2015), PSLS (Samadi et al. 2019), numpy (Harris et al. 2020), matplotlib
(Hunter 2007), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration 2022),
pandas (Wes McKinney 2010; The pandas development team 2020), scikit-learn (Pedregosa
et al. 2011).'
article_number: A229
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S. N.
full_name: Breton, S. N.
last_name: Breton
- first_name: A. F.
full_name: Lanza, A. F.
last_name: Lanza
- first_name: S.
full_name: Messina, S.
last_name: Messina
- first_name: I.
full_name: Pagano, I.
last_name: Pagano
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: E.
full_name: Corsaro, E.
last_name: Corsaro
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: A. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- first_name: S.
full_name: Aigrain, S.
last_name: Aigrain
- first_name: L.
full_name: Amard, L.
last_name: Amard
- first_name: A. S.
full_name: Brun, A. S.
last_name: Brun
- first_name: L.
full_name: Degott, L.
last_name: Degott
- first_name: Q.
full_name: Noraz, Q.
last_name: Noraz
- first_name: D. B.
full_name: Palakkatharappil, D. B.
last_name: Palakkatharappil
- first_name: E.
full_name: Panetier, E.
last_name: Panetier
- first_name: A.
full_name: Strugarek, A.
last_name: Strugarek
- first_name: K.
full_name: Belkacem, K.
last_name: Belkacem
- first_name: M.-J
full_name: Goupil, M.-J
last_name: Goupil
- first_name: R. M.
full_name: Ouazzani, R. M.
last_name: Ouazzani
- first_name: J.
full_name: Philidet, J.
last_name: Philidet
- first_name: C.
full_name: Renié, C.
last_name: Renié
- first_name: O.
full_name: Roth, O.
last_name: Roth
citation:
ama: Breton SN, Lanza AF, Messina S, et al. Measuring stellar surface rotation and
activity with the PLATO mission. I. Strategy and application to simulated light
curves. Astronomy and Astrophysics. 2024;689. doi:10.1051/0004-6361/202449893
apa: Breton, S. N., Lanza, A. F., Messina, S., Pagano, I., Bugnet, L. A., Corsaro,
E., … Roth, O. (2024). Measuring stellar surface rotation and activity with the
PLATO mission. I. Strategy and application to simulated light curves. Astronomy
and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202449893
chicago: Breton, S. N., A. F. Lanza, S. Messina, I. Pagano, Lisa Annabelle Bugnet,
E. Corsaro, R. A. García, et al. “Measuring Stellar Surface Rotation and Activity
with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.”
Astronomy and Astrophysics. EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202449893.
ieee: S. N. Breton et al., “Measuring stellar surface rotation and activity
with the PLATO mission. I. Strategy and application to simulated light curves,”
Astronomy and Astrophysics, vol. 689. EDP Sciences, 2024.
ista: Breton SN, Lanza AF, Messina S, Pagano I, Bugnet LA, Corsaro E, García RA,
Mathur S, Santos ARG, Aigrain S, Amard L, Brun AS, Degott L, Noraz Q, Palakkatharappil
DB, Panetier E, Strugarek A, Belkacem K, Goupil M-J, Ouazzani RM, Philidet J,
Renié C, Roth O. 2024. Measuring stellar surface rotation and activity with the
PLATO mission. I. Strategy and application to simulated light curves. Astronomy
and Astrophysics. 689, A229.
mla: Breton, S. N., et al. “Measuring Stellar Surface Rotation and Activity with
the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” Astronomy
and Astrophysics, vol. 689, A229, EDP Sciences, 2024, doi:10.1051/0004-6361/202449893.
short: S.N. Breton, A.F. Lanza, S. Messina, I. Pagano, L.A. Bugnet, E. Corsaro,
R.A. García, S. Mathur, A.R.G. Santos, S. Aigrain, L. Amard, A.S. Brun, L. Degott,
Q. Noraz, D.B. Palakkatharappil, E. Panetier, A. Strugarek, K. Belkacem, M.-J.
Goupil, R.M. Ouazzani, J. Philidet, C. Renié, O. Roth, Astronomy and Astrophysics
689 (2024).
date_created: 2025-01-27T13:12:44Z
date_published: 2024-09-01T00:00:00Z
date_updated: 2025-09-09T12:04:24Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202449893
external_id:
arxiv:
- '2407.03709'
isi:
- '001366206400007'
file:
- access_level: open_access
checksum: 5c871ba7370a507ed6ea9fb2304d8263
content_type: application/pdf
creator: dernst
date_created: 2025-01-27T13:18:41Z
date_updated: 2025-01-27T13:18:41Z
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file_name: 2024_AstronomyAstrophysics_Breton.pdf
file_size: 6212007
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intvolume: ' 689'
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month: '09'
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'
scopus_import: '1'
status: public
title: Measuring stellar surface rotation and activity with the PLATO mission. I.
Strategy and application to simulated light curves
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 689
year: '2024'
...
---
_id: '15336'
abstract:
- lang: eng
text: Submillimeter surveys toward overdense regions in the early Universe are essential
for uncovering the obscured star formation and the cold gas content of assembling
galaxies within massive dark matter halos. In this work, we present deep ALMA
mosaic observations covering an area of ∼2′×2′ around MUSE Quasar Nebula 01 (MQN01),
one of the largest and brightest Ly-α emitting nebulae discovered thus far; it
surrounds a radio-quiet quasar at z ≃ 3.25. Our observations target the 1.2 and
the 3 mm dust continuum as well as the carbon monoxide CO(4–3) transition in galaxies
in the vicinity of the quasar. We identify a robust sample of 11 CO-line-emitting
galaxies (including a closely separated quasar companion) that lie within ±4000 km s−1
of the quasar systemic redshift. A fraction of these objects were missed in previous
deep rest-frame optical/UV surveys, which highlights the critical role of (sub)millimeter
imaging. We also detect a total of 11 sources revealed in the dust continuum at
1.2 mm; six of them have either high-fidelity spectroscopic redshift information
from rest-frame UV metal absorptions or the CO(4–3) line that places them in the
same narrow redshift range. A comparison of the CO luminosity function and 1.2
mm number count density with those of the general fields points to a galaxy overdensity
of δ > 10. We find evidence of a systematic flattening at the bright end of the
CO luminosity function with respect to the trend measured in blank fields. Our
findings reveal that galaxies in dense regions at z ∼ 3 are more massive and significantly
richer in molecular gas than galaxies in fields, which enables a faster and accelerated
assembly. This is the first in a series of studies aimed at characterizing one
of the densest regions of the Universe found so far at z > 3.
acknowledgement: 'We thank the anonymous referee for the careful reading of the paper
and useful suggestions which improved the manuscript. We thank Dr. Leindert Boogaard
for sharing data and providing support in the data analysis process. This paper
makes use of the following ALMA data: ADS/JAO.ALMA#2021.1.00793.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 project was supported by the European Research Council (ERC) Consolidator
Grant 864361 (CosmicWeb) and by Fondazione Cariplo grant no. 2020-0902. M.M. was
supported in part by grant HST-GO-17065. This research made use of Astropy (http://www.astropy.org),
a community-developed core Python package for Astronomy (Astropy Collaboration 2013,
2018), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter
2007), and Statsmodel (Seabold & Perktold 2010).'
article_number: A119
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: A.
full_name: Pensabene, A.
last_name: Pensabene
- first_name: S.
full_name: Cantalupo, S.
last_name: Cantalupo
- first_name: C.
full_name: Cicone, C.
last_name: Cicone
- first_name: R.
full_name: Decarli, R.
last_name: Decarli
- first_name: M.
full_name: Galbiati, M.
last_name: Galbiati
- first_name: M.
full_name: Ginolfi, M.
last_name: Ginolfi
- first_name: S.
full_name: De Beer, S.
last_name: De Beer
- first_name: M.
full_name: Fossati, M.
last_name: Fossati
- first_name: M.
full_name: Fumagalli, M.
last_name: Fumagalli
- first_name: T.
full_name: Lazeyras, T.
last_name: Lazeyras
- first_name: G.
full_name: Pezzulli, G.
last_name: Pezzulli
- first_name: A.
full_name: Travascio, A.
last_name: Travascio
- first_name: W.
full_name: Wang, W.
last_name: Wang
- 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: M. V.
full_name: Maseda, M. V.
last_name: Maseda
citation:
ama: 'Pensabene A, Cantalupo S, Cicone C, et al. ALMA survey of a massive node of
the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. Astronomy
and Astrophysics. 2024;684. doi:10.1051/0004-6361/202348659'
apa: 'Pensabene, A., Cantalupo, S., Cicone, C., Decarli, R., Galbiati, M., Ginolfi,
M., … Maseda, M. V. (2024). ALMA survey of a massive node of the Cosmic Web at
z ∼ 3: I. Discovery of a large overdensity of CO emitters. Astronomy and Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202348659'
chicago: 'Pensabene, A., S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi,
S. De Beer, et al. “ALMA Survey of a Massive Node of the Cosmic Web at z ∼ 3:
I. Discovery of a Large Overdensity of CO Emitters.” Astronomy and Astrophysics.
EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202348659.'
ieee: 'A. Pensabene et al., “ALMA survey of a massive node of the Cosmic
Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters,” Astronomy
and Astrophysics, vol. 684. EDP Sciences, 2024.'
ista: 'Pensabene A, Cantalupo S, Cicone C, Decarli R, Galbiati M, Ginolfi M, De
Beer S, Fossati M, Fumagalli M, Lazeyras T, Pezzulli G, Travascio A, Wang W, Matthee
JJ, Maseda MV. 2024. ALMA survey of a massive node of the Cosmic Web at z ∼ 3:
I. Discovery of a large overdensity of CO emitters. Astronomy and Astrophysics.
684, A119.'
mla: 'Pensabene, A., et al. “ALMA Survey of a Massive Node of the Cosmic Web at
z ∼ 3: I. Discovery of a Large Overdensity of CO Emitters.” Astronomy and Astrophysics,
vol. 684, A119, EDP Sciences, 2024, doi:10.1051/0004-6361/202348659.'
short: A. Pensabene, S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi,
S. De Beer, M. Fossati, M. Fumagalli, T. Lazeyras, G. Pezzulli, A. Travascio,
W. Wang, J.J. Matthee, M.V. Maseda, Astronomy and Astrophysics 684 (2024).
date_created: 2024-04-21T22:00:53Z
date_published: 2024-04-01T00:00:00Z
date_updated: 2025-09-04T13:42:50Z
day: '01'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.1051/0004-6361/202348659
external_id:
arxiv:
- '2401.04765'
isi:
- '001199982500009'
file:
- access_level: open_access
checksum: ab48775b6946cebfa27ddded5a68fdd2
content_type: application/pdf
creator: dernst
date_created: 2024-04-23T06:59:18Z
date_updated: 2024-04-23T06:59:18Z
file_id: '15341'
file_name: 2024_AstronomyAstrophysics_Pensabene.pdf
file_size: 4410627
relation: main_file
success: 1
file_date_updated: 2024-04-23T06:59:18Z
has_accepted_license: '1'
intvolume: ' 684'
isi: 1
language:
- iso: eng
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'
scopus_import: '1'
status: public
title: 'ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of
a large overdensity of CO emitters'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 684
year: '2024'
...
---
_id: '14103'
abstract:
- lang: eng
text: Observations of individual massive stars, super-luminous supernovae, gamma-ray
bursts, and gravitational wave events involving spectacular black hole mergers
indicate that the low-metallicity Universe is fundamentally different from our
own Galaxy. Many transient phenomena will remain enigmatic until we achieve a
firm understanding of the physics and evolution of massive stars at low metallicity
(Z). The Hubble Space Telescope has devoted 500 orbits to observing ∼250 massive
stars at low Z in the ultraviolet (UV) with the COS and STIS spectrographs under
the ULLYSES programme. The complementary X-Shooting ULLYSES (XShootU) project
provides an enhanced legacy value with high-quality optical and near-infrared
spectra obtained with the wide-wavelength coverage X-shooter spectrograph at ESO’s
Very Large Telescope. We present an overview of the XShootU project, showing that
combining ULLYSES UV and XShootU optical spectra is critical for the uniform determination
of stellar parameters such as effective temperature, surface gravity, luminosity,
and abundances, as well as wind properties such as mass-loss rates as a function
of Z. As uncertainties in stellar and wind parameters percolate into many adjacent
areas of astrophysics, the data and modelling of the XShootU project is expected
to be a game changer for our physical understanding of massive stars at low Z.
To be able to confidently interpret James Webb Space Telescope spectra of the
first stellar generations, the individual spectra of low-Z stars need to be understood,
which is exactly where XShootU can deliver.
article_number: A154
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorick S.
full_name: Vink, Jorick S.
last_name: Vink
- first_name: A.
full_name: Mehner, A.
last_name: Mehner
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: A.
full_name: Fullerton, A.
last_name: Fullerton
- first_name: M.
full_name: Garcia, M.
last_name: Garcia
- first_name: F.
full_name: Martins, F.
last_name: Martins
- first_name: N.
full_name: Morrell, N.
last_name: Morrell
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: N.
full_name: St-Louis, N.
last_name: St-Louis
- first_name: A.
full_name: ud-Doula, A.
last_name: ud-Doula
- first_name: A. A. C.
full_name: Sander, A. A. C.
last_name: Sander
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: J.-C.
full_name: Bouret, J.-C.
last_name: Bouret
- first_name: B.
full_name: Kubátová, B.
last_name: Kubátová
- first_name: P.
full_name: Marchant, P.
last_name: Marchant
- first_name: L. P.
full_name: Martins, L. P.
last_name: Martins
- first_name: A.
full_name: Wofford, A.
last_name: Wofford
- first_name: J. Th.
full_name: van Loon, J. Th.
last_name: van Loon
- first_name: O.
full_name: Grace Telford, O.
last_name: Grace Telford
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: C.
full_name: Erba, C.
last_name: Erba
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: T.
full_name: Alkousa, T.
last_name: Alkousa
- first_name: F.
full_name: Backs, F.
last_name: Backs
- first_name: C. L.
full_name: Barbosa, C. L.
last_name: Barbosa
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: J. M.
full_name: Bestenlehner, J. M.
last_name: Bestenlehner
- first_name: R.
full_name: Blomme, R.
last_name: Blomme
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: S. A.
full_name: Brands, S. A.
last_name: Brands
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: A.
full_name: David-Uraz, A.
last_name: David-Uraz
- first_name: F. A.
full_name: Driessen, F. A.
last_name: Driessen
- first_name: K.
full_name: Dsilva, K.
last_name: Dsilva
- first_name: S.
full_name: Geen, S.
last_name: Geen
- first_name: V. M. A.
full_name: Gómez-González, V. M. A.
last_name: Gómez-González
- first_name: L.
full_name: Grassitelli, L.
last_name: Grassitelli
- first_name: W.-R.
full_name: Hamann, W.-R.
last_name: Hamann
- first_name: C.
full_name: Hawcroft, C.
last_name: Hawcroft
- first_name: A.
full_name: Herrero, A.
last_name: Herrero
- first_name: E. R.
full_name: Higgins, E. R.
last_name: Higgins
- first_name: D.
full_name: John Hillier, D.
last_name: John Hillier
- first_name: R.
full_name: Ignace, R.
last_name: Ignace
- first_name: A. G.
full_name: Istrate, A. G.
last_name: Istrate
- first_name: L.
full_name: Kaper, L.
last_name: Kaper
- first_name: N. D.
full_name: Kee, N. D.
last_name: Kee
- first_name: C.
full_name: Kehrig, C.
last_name: Kehrig
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: A.
full_name: de Koter, A.
last_name: de Koter
- first_name: R.
full_name: Kuiper, R.
last_name: Kuiper
- first_name: E.
full_name: Laplace, E.
last_name: Laplace
- first_name: C. J. K.
full_name: Larkin, C. J. K.
last_name: Larkin
- first_name: R. R.
full_name: Lefever, R. R.
last_name: Lefever
- first_name: C.
full_name: Leitherer, C.
last_name: Leitherer
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: J.
full_name: Maíz Apellániz, J.
last_name: Maíz Apellániz
- first_name: G.
full_name: Maravelias, G.
last_name: Maravelias
- first_name: W.
full_name: Marcolino, W.
last_name: Marcolino
- first_name: A. F.
full_name: McLeod, A. F.
last_name: McLeod
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: F.
full_name: Najarro, F.
last_name: Najarro
- first_name: M. S.
full_name: Oey, M. S.
last_name: Oey
- first_name: T. N.
full_name: Parsons, T. N.
last_name: Parsons
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M. G.
full_name: Pedersen, M. G.
last_name: Pedersen
- first_name: R. K.
full_name: Prinja, R. K.
last_name: Prinja
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: M. C.
full_name: Ramírez-Tannus, M. C.
last_name: Ramírez-Tannus
- first_name: G. N.
full_name: Sabhahit, G. N.
last_name: Sabhahit
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: S.
full_name: Reyero Serantes, S.
last_name: Reyero Serantes
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: G. S.
full_name: Stringfellow, G. S.
last_name: Stringfellow
- first_name: N.
full_name: Sudnik, N.
last_name: Sudnik
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: L.
full_name: Wang, L.
last_name: Wang
citation:
ama: 'Vink JS, Mehner A, Crowther PA, et al. X-shooting ULLYSES: Massive stars at
low metallicity. I. Project description. Astronomy & Astrophysics.
2023;675. doi:10.1051/0004-6361/202245650'
apa: 'Vink, J. S., Mehner, A., Crowther, P. A., Fullerton, A., Garcia, M., Martins,
F., … Wang, L. (2023). X-shooting ULLYSES: Massive stars at low metallicity. I.
Project description. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202245650'
chicago: 'Vink, Jorick S., A. Mehner, P. A. Crowther, A. Fullerton, M. Garcia, F.
Martins, N. Morrell, et al. “X-Shooting ULLYSES: Massive Stars at Low Metallicity.
I. Project Description.” Astronomy & Astrophysics. EDP Sciences, 2023.
https://doi.org/10.1051/0004-6361/202245650.'
ieee: 'J. S. Vink et al., “X-shooting ULLYSES: Massive stars at low metallicity.
I. Project description,” Astronomy & Astrophysics, vol. 675. EDP Sciences,
2023.'
ista: 'Vink JS, Mehner A, Crowther PA, Fullerton A, Garcia M, Martins F, Morrell
N, Oskinova LM, St-Louis N, ud-Doula A, Sander AAC, Sana H, Bouret J-C, Kubátová
B, Marchant P, Martins LP, Wofford A, van Loon JT, Grace Telford O, Götberg YLL,
Bowman DM, Erba C, Kalari VM, Abdul-Masih M, Alkousa T, Backs F, Barbosa CL, Berlanas
SR, Bernini-Peron M, Bestenlehner JM, Blomme R, Bodensteiner J, Brands SA, Evans
CJ, David-Uraz A, Driessen FA, Dsilva K, Geen S, Gómez-González VMA, Grassitelli
L, Hamann W-R, Hawcroft C, Herrero A, Higgins ER, John Hillier D, Ignace R, Istrate
AG, Kaper L, Kee ND, Kehrig C, Keszthelyi Z, Klencki J, de Koter A, Kuiper R,
Laplace E, Larkin CJK, Lefever RR, Leitherer C, Lennon DJ, Mahy L, Maíz Apellániz
J, Maravelias G, Marcolino W, McLeod AF, de Mink SE, Najarro F, Oey MS, Parsons
TN, Pauli D, Pedersen MG, Prinja RK, Ramachandran V, Ramírez-Tannus MC, Sabhahit
GN, Schootemeijer A, Reyero Serantes S, Shenar T, Stringfellow GS, Sudnik N, Tramper
F, Wang L. 2023. X-shooting ULLYSES: Massive stars at low metallicity. I. Project
description. Astronomy & Astrophysics. 675, A154.'
mla: 'Vink, Jorick S., et al. “X-Shooting ULLYSES: Massive Stars at Low Metallicity.
I. Project Description.” Astronomy & Astrophysics, vol. 675, A154,
EDP Sciences, 2023, doi:10.1051/0004-6361/202245650.'
short: J.S. Vink, A. Mehner, P.A. Crowther, A. Fullerton, M. Garcia, F. Martins,
N. Morrell, L.M. Oskinova, N. St-Louis, A. ud-Doula, A.A.C. Sander, H. Sana, J.-C.
Bouret, B. Kubátová, P. Marchant, L.P. Martins, A. Wofford, J.T. van Loon, O.
Grace Telford, Y.L.L. Götberg, D.M. Bowman, C. Erba, V.M. Kalari, M. Abdul-Masih,
T. Alkousa, F. Backs, C.L. Barbosa, S.R. Berlanas, M. Bernini-Peron, J.M. Bestenlehner,
R. Blomme, J. Bodensteiner, S.A. Brands, C.J. Evans, A. David-Uraz, F.A. Driessen,
K. Dsilva, S. Geen, V.M.A. Gómez-González, L. Grassitelli, W.-R. Hamann, C. Hawcroft,
A. Herrero, E.R. Higgins, D. John Hillier, R. Ignace, A.G. Istrate, L. Kaper,
N.D. Kee, C. Kehrig, Z. Keszthelyi, J. Klencki, A. de Koter, R. Kuiper, E. Laplace,
C.J.K. Larkin, R.R. Lefever, C. Leitherer, D.J. Lennon, L. Mahy, J. Maíz Apellániz,
G. Maravelias, W. Marcolino, A.F. McLeod, S.E. de Mink, F. Najarro, M.S. Oey,
T.N. Parsons, D. Pauli, M.G. Pedersen, R.K. Prinja, V. Ramachandran, M.C. Ramírez-Tannus,
G.N. Sabhahit, A. Schootemeijer, S. Reyero Serantes, T. Shenar, G.S. Stringfellow,
N. Sudnik, F. Tramper, L. Wang, Astronomy & Astrophysics 675 (2023).
date_created: 2023-08-21T10:12:35Z
date_published: 2023-07-01T00:00:00Z
date_updated: 2023-08-22T11:01:07Z
day: '01'
doi: 10.1051/0004-6361/202245650
extern: '1'
external_id:
arxiv:
- '2305.06376'
intvolume: ' 675'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/202245650
month: '07'
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: 'X-shooting ULLYSES: Massive stars at low metallicity. I. Project description'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 675
year: '2023'
...
---
_id: '14256'
abstract:
- lang: eng
text: "Context. Space asteroseismology is revolutionizing our knowledge of the internal
structure and dynamics of stars. A breakthrough is ongoing with the recent discoveries
of signatures of strong magnetic fields in the core of red giant stars. The key
signature for such a detection is the asymmetry these fields induce in the frequency
splittings of observed dipolar mixed gravito-acoustic modes.\r\nAims. We investigate
the ability of the observed asymmetries of the frequency splittings of dipolar
mixed modes to constrain the geometrical properties of deep magnetic fields.\r\nMethods.
We used the powerful analytical Racah-Wigner algebra used in quantum mechanics
to characterize the geometrical couplings of dipolar mixed oscillation modes with
various realistically plausible topologies of fossil magnetic fields. We also
computed the induced perturbation of their frequencies.\r\nResults. First, in
the case of an oblique magnetic dipole, we provide the exact analytical expression
of the asymmetry as a function of the angle between the rotation and magnetic
axes. Its value provides a direct measure of this angle. Second, considering a
combination of axisymmetric dipolar and quadrupolar fields, we show how the asymmetry
is blind to the unraveling of the relative strength and sign of each component.
Finally, in the case of a given multipole, we show that a negative asymmetry is
a signature of non-axisymmetric topologies.\r\nConclusions. Asymmetries of dipolar
mixed modes provide a key bit of information on the geometrical topology of deep
fossil magnetic fields, but this is insufficient on its own. Asteroseismic constraints
should therefore be combined with spectropolarimetric observations and numerical
simulations, which aim to predict the more probable stable large-scale geometries."
acknowledgement: The authors are grateful to the referee for her/his detailed and
constructive report, which has allowed us to improve our article. S. M. acknowledges
support from the CNES GOLF-SOHO and PLATO grants at CEA/DAp and PNPS (CNRS/INSU).
We thank R. A. Garcia for fruitful discussions and suggestions.
article_number: L9
article_processing_charge: Yes (in subscription journal)
article_type: letter_note
arxiv: 1
author:
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: 'Mathis S, Bugnet LA. Asymmetries of frequency splittings of dipolar mixed
modes: A window on the topology of deep magnetic fields. Astronomy and Astrophysics.
2023;676. doi:10.1051/0004-6361/202346832'
apa: 'Mathis, S., & Bugnet, L. A. (2023). Asymmetries of frequency splittings
of dipolar mixed modes: A window on the topology of deep magnetic fields. Astronomy
and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202346832'
chicago: 'Mathis, S., and Lisa Annabelle Bugnet. “Asymmetries of Frequency Splittings
of Dipolar Mixed Modes: A Window on the Topology of Deep Magnetic Fields.” Astronomy
and Astrophysics. EDP Sciences, 2023. https://doi.org/10.1051/0004-6361/202346832.'
ieee: 'S. Mathis and L. A. Bugnet, “Asymmetries of frequency splittings of dipolar
mixed modes: A window on the topology of deep magnetic fields,” Astronomy and
Astrophysics, vol. 676. EDP Sciences, 2023.'
ista: 'Mathis S, Bugnet LA. 2023. Asymmetries of frequency splittings of dipolar
mixed modes: A window on the topology of deep magnetic fields. Astronomy and Astrophysics.
676, L9.'
mla: 'Mathis, S., and Lisa Annabelle Bugnet. “Asymmetries of Frequency Splittings
of Dipolar Mixed Modes: A Window on the Topology of Deep Magnetic Fields.” Astronomy
and Astrophysics, vol. 676, L9, EDP Sciences, 2023, doi:10.1051/0004-6361/202346832.'
short: S. Mathis, L.A. Bugnet, Astronomy and Astrophysics 676 (2023).
date_created: 2023-09-03T22:01:15Z
date_published: 2023-08-01T00:00:00Z
date_updated: 2023-09-06T11:05:58Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202346832
external_id:
arxiv:
- '2306.11587'
isi:
- '001046037700007'
file:
- access_level: open_access
checksum: 7b30d26fb2b7bcb5b5be1414950615f9
content_type: application/pdf
creator: dernst
date_created: 2023-09-06T07:13:19Z
date_updated: 2023-09-06T07:13:19Z
file_id: '14271'
file_name: 2023_AstronomyAstrophysics_Mathis.pdf
file_size: 458120
relation: main_file
success: 1
file_date_updated: 2023-09-06T07:13:19Z
has_accepted_license: '1'
intvolume: ' 676'
isi: 1
language:
- iso: eng
month: '08'
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'
scopus_import: '1'
status: public
title: 'Asymmetries of frequency splittings of dipolar mixed modes: A window on the
topology of deep magnetic fields'
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: c635000d-4b10-11ee-a964-aac5a93f6ac1
volume: 676
year: '2023'
...
---
_id: '15193'
abstract:
- lang: eng
text: We report on Imaging X-ray polarimetry explorer (IXPE) observations of the
Be-transient X-ray pulsar LS V +44 17/RX J0440.9+4431 made at two luminosity levels
during the giant outburst in January–February 2023. Considering the observed spectral
variability and changes in the pulse profiles, the source was likely caught in
supercritical and subcritical states with significantly different emission-region
geometry, associated with the presence of accretion columns and hot spots, respectively.
We focus here on the pulse-phase-resolved polarimetric analysis and find that
the observed dependencies of the polarization degree and polarization angle (PA)
on the pulse phase are indeed drastically different for the two observations.
The observed differences, if interpreted within the framework of the rotating
vector model (RVM), imply dramatic variations in the spin axis inclination, the
position angle, and the magnetic colatitude by tens of degrees within the space
of just a few days. We suggest that the apparent changes in the observed PA phase
dependence are predominantly related to the presence of an unpulsed polarized
component in addition to the polarized radiation associated with the pulsar itself.
We then show that the observed PA phase dependence in both observations can be
explained with a single set of RVM parameters defining the pulsar’s geometry.
We also suggest that the additional polarized component is likely produced by
scattering of the pulsar radiation in the equatorial disk wind.
article_number: A57
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Victor
full_name: Doroshenko, Victor
last_name: Doroshenko
- first_name: Juri
full_name: Poutanen, Juri
last_name: Poutanen
- first_name: Jeremy
full_name: Heyl, Jeremy
last_name: Heyl
- first_name: Sergey S.
full_name: Tsygankov, Sergey S.
last_name: Tsygankov
- first_name: Ilaria
full_name: Caiazzo, Ilaria
id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
last_name: Caiazzo
orcid: 0000-0002-4770-5388
- first_name: Roberto
full_name: Turolla, Roberto
last_name: Turolla
- first_name: Alexandra
full_name: Veledina, Alexandra
last_name: Veledina
- first_name: Martin C.
full_name: Weisskopf, Martin C.
last_name: Weisskopf
- first_name: Sofia V.
full_name: Forsblom, Sofia V.
last_name: Forsblom
- first_name: Denis
full_name: González-Caniulef, Denis
last_name: González-Caniulef
- first_name: Vladislav
full_name: Loktev, Vladislav
last_name: Loktev
- first_name: Christian
full_name: Malacaria, Christian
last_name: Malacaria
- first_name: Alexander A.
full_name: Mushtukov, Alexander A.
last_name: Mushtukov
- first_name: Valery F.
full_name: Suleimanov, Valery F.
last_name: Suleimanov
- first_name: Alexander A.
full_name: Lutovinov, Alexander A.
last_name: Lutovinov
- first_name: Ilya A.
full_name: Mereminskiy, Ilya A.
last_name: Mereminskiy
- first_name: Sergey V.
full_name: Molkov, Sergey V.
last_name: Molkov
- first_name: Alexander
full_name: Salganik, Alexander
last_name: Salganik
- first_name: Andrea
full_name: Santangelo, Andrea
last_name: Santangelo
- first_name: Andrei V.
full_name: Berdyugin, Andrei V.
last_name: Berdyugin
- first_name: Vadim
full_name: Kravtsov, Vadim
last_name: Kravtsov
- first_name: Anagha P.
full_name: Nitindala, Anagha P.
last_name: Nitindala
- first_name: Iván
full_name: Agudo, Iván
last_name: Agudo
- first_name: Lucio A.
full_name: Antonelli, Lucio A.
last_name: Antonelli
- first_name: Matteo
full_name: Bachetti, Matteo
last_name: Bachetti
- first_name: Luca
full_name: Baldini, Luca
last_name: Baldini
- first_name: Wayne H.
full_name: Baumgartner, Wayne H.
last_name: Baumgartner
- first_name: Ronaldo
full_name: Bellazzini, Ronaldo
last_name: Bellazzini
- first_name: Stefano
full_name: Bianchi, Stefano
last_name: Bianchi
- first_name: Stephen D.
full_name: Bongiorno, Stephen D.
last_name: Bongiorno
- first_name: Raffaella
full_name: Bonino, Raffaella
last_name: Bonino
- first_name: Alessandro
full_name: Brez, Alessandro
last_name: Brez
- first_name: Niccolò
full_name: Bucciantini, Niccolò
last_name: Bucciantini
- first_name: Fiamma
full_name: Capitanio, Fiamma
last_name: Capitanio
- first_name: Simone
full_name: Castellano, Simone
last_name: Castellano
- first_name: Elisabetta
full_name: Cavazzuti, Elisabetta
last_name: Cavazzuti
- first_name: Chien-Ting
full_name: Chen, Chien-Ting
last_name: Chen
- first_name: Stefano
full_name: Ciprini, Stefano
last_name: Ciprini
- first_name: Enrico
full_name: Costa, Enrico
last_name: Costa
- first_name: Alessandra
full_name: De Rosa, Alessandra
last_name: De Rosa
- first_name: Ettore
full_name: Del Monte, Ettore
last_name: Del Monte
- first_name: Laura
full_name: Di Gesu, Laura
last_name: Di Gesu
- first_name: Niccolò
full_name: Di Lalla, Niccolò
last_name: Di Lalla
- first_name: Alessandro
full_name: Di Marco, Alessandro
last_name: Di Marco
- first_name: Immacolata
full_name: Donnarumma, Immacolata
last_name: Donnarumma
- first_name: Michal
full_name: Dovčiak, Michal
last_name: Dovčiak
- first_name: Steven R.
full_name: Ehlert, Steven R.
last_name: Ehlert
- first_name: Teruaki
full_name: Enoto, Teruaki
last_name: Enoto
- first_name: Yuri
full_name: Evangelista, Yuri
last_name: Evangelista
- first_name: Sergio
full_name: Fabiani, Sergio
last_name: Fabiani
- first_name: Riccardo
full_name: Ferrazzoli, Riccardo
last_name: Ferrazzoli
- first_name: Javier A.
full_name: García, Javier A.
last_name: García
- first_name: Shuichi
full_name: Gunji, Shuichi
last_name: Gunji
- first_name: Kiyoshi
full_name: Hayashida, Kiyoshi
last_name: Hayashida
- first_name: Wataru
full_name: Iwakiri, Wataru
last_name: Iwakiri
- first_name: Svetlana G.
full_name: Jorstad, Svetlana G.
last_name: Jorstad
- first_name: Philip
full_name: Kaaret, Philip
last_name: Kaaret
- first_name: Vladimir
full_name: Karas, Vladimir
last_name: Karas
- first_name: Fabian
full_name: Kislat, Fabian
last_name: Kislat
- first_name: Takao
full_name: Kitaguchi, Takao
last_name: Kitaguchi
- first_name: Jeffery J.
full_name: Kolodziejczak, Jeffery J.
last_name: Kolodziejczak
- first_name: Henric
full_name: Krawczynski, Henric
last_name: Krawczynski
- first_name: Fabio
full_name: La Monaca, Fabio
last_name: La Monaca
- first_name: Luca
full_name: Latronico, Luca
last_name: Latronico
- first_name: Ioannis
full_name: Liodakis, Ioannis
last_name: Liodakis
- first_name: Simone
full_name: Maldera, Simone
last_name: Maldera
- first_name: Alberto
full_name: Manfreda, Alberto
last_name: Manfreda
- first_name: Frédéric
full_name: Marin, Frédéric
last_name: Marin
- first_name: Andrea
full_name: Marinucci, Andrea
last_name: Marinucci
- first_name: Alan P.
full_name: Marscher, Alan P.
last_name: Marscher
- first_name: Herman L.
full_name: Marshall, Herman L.
last_name: Marshall
- first_name: Francesco
full_name: Massaro, Francesco
last_name: Massaro
- first_name: Giorgio
full_name: Matt, Giorgio
last_name: Matt
- first_name: Ikuyuki
full_name: Mitsuishi, Ikuyuki
last_name: Mitsuishi
- first_name: Tsunefumi
full_name: Mizuno, Tsunefumi
last_name: Mizuno
- first_name: Fabio
full_name: Muleri, Fabio
last_name: Muleri
- first_name: Michela
full_name: Negro, Michela
last_name: Negro
- first_name: Chi-Yung
full_name: Ng, Chi-Yung
last_name: Ng
- first_name: Stephen L.
full_name: O’Dell, Stephen L.
last_name: O’Dell
- first_name: Nicola
full_name: Omodei, Nicola
last_name: Omodei
- first_name: Chiara
full_name: Oppedisano, Chiara
last_name: Oppedisano
- first_name: Alessandro
full_name: Papitto, Alessandro
last_name: Papitto
- first_name: George G.
full_name: Pavlov, George G.
last_name: Pavlov
- first_name: Abel L.
full_name: Peirson, Abel L.
last_name: Peirson
- first_name: Matteo
full_name: Perri, Matteo
last_name: Perri
- first_name: Melissa
full_name: Pesce-Rollins, Melissa
last_name: Pesce-Rollins
- first_name: Pierre-Olivier
full_name: Petrucci, Pierre-Olivier
last_name: Petrucci
- first_name: Maura
full_name: Pilia, Maura
last_name: Pilia
- first_name: Andrea
full_name: Possenti, Andrea
last_name: Possenti
- first_name: Simonetta
full_name: Puccetti, Simonetta
last_name: Puccetti
- first_name: Brian D.
full_name: Ramsey, Brian D.
last_name: Ramsey
- first_name: John
full_name: Rankin, John
last_name: Rankin
- first_name: Ajay
full_name: Ratheesh, Ajay
last_name: Ratheesh
- first_name: Oliver J.
full_name: Roberts, Oliver J.
last_name: Roberts
- first_name: Roger W.
full_name: Romani, Roger W.
last_name: Romani
- first_name: Carmelo
full_name: Sgrò, Carmelo
last_name: Sgrò
- first_name: Patrick
full_name: Slane, Patrick
last_name: Slane
- first_name: Paolo
full_name: Soffitta, Paolo
last_name: Soffitta
- first_name: Gloria
full_name: Spandre, Gloria
last_name: Spandre
- first_name: Douglas A.
full_name: Swartz, Douglas A.
last_name: Swartz
- first_name: Toru
full_name: Tamagawa, Toru
last_name: Tamagawa
- first_name: Fabrizio
full_name: Tavecchio, Fabrizio
last_name: Tavecchio
- first_name: Roberto
full_name: Taverna, Roberto
last_name: Taverna
- first_name: Yuzuru
full_name: Tawara, Yuzuru
last_name: Tawara
- first_name: Allyn F.
full_name: Tennant, Allyn F.
last_name: Tennant
- first_name: Nicholas E.
full_name: Thomas, Nicholas E.
last_name: Thomas
- first_name: Francesco
full_name: Tombesi, Francesco
last_name: Tombesi
- first_name: Alessio
full_name: Trois, Alessio
last_name: Trois
- first_name: Jacco
full_name: Vink, Jacco
last_name: Vink
- first_name: Kinwah
full_name: Wu, Kinwah
last_name: Wu
- first_name: Fei
full_name: Xie, Fei
last_name: Xie
- first_name: Silvia
full_name: Zane, Silvia
last_name: Zane
citation:
ama: Doroshenko V, Poutanen J, Heyl J, et al. Complex variations in X-ray polarization
in the X-ray pulsar LS V +44 17/RX J0440.9+4431. Astronomy & Astrophysics.
2023;677. doi:10.1051/0004-6361/202347088
apa: Doroshenko, V., Poutanen, J., Heyl, J., Tsygankov, S. S., Caiazzo, I., Turolla,
R., … Zane, S. (2023). Complex variations in X-ray polarization in the X-ray pulsar
LS V +44 17/RX J0440.9+4431. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202347088
chicago: Doroshenko, Victor, Juri Poutanen, Jeremy Heyl, Sergey S. Tsygankov, Ilaria
Caiazzo, Roberto Turolla, Alexandra Veledina, et al. “Complex Variations in X-Ray
Polarization in the X-Ray Pulsar LS V +44 17/RX J0440.9+4431.” Astronomy &
Astrophysics. EDP Sciences, 2023. https://doi.org/10.1051/0004-6361/202347088.
ieee: V. Doroshenko et al., “Complex variations in X-ray polarization in
the X-ray pulsar LS V +44 17/RX J0440.9+4431,” Astronomy & Astrophysics,
vol. 677. EDP Sciences, 2023.
ista: Doroshenko V et al. 2023. Complex variations in X-ray polarization in the
X-ray pulsar LS V +44 17/RX J0440.9+4431. Astronomy & Astrophysics. 677, A57.
mla: Doroshenko, Victor, et al. “Complex Variations in X-Ray Polarization in the
X-Ray Pulsar LS V +44 17/RX J0440.9+4431.” Astronomy & Astrophysics,
vol. 677, A57, EDP Sciences, 2023, doi:10.1051/0004-6361/202347088.
short: V. Doroshenko, J. Poutanen, J. Heyl, S.S. Tsygankov, I. Caiazzo, R. Turolla,
A. Veledina, M.C. Weisskopf, S.V. Forsblom, D. González-Caniulef, V. Loktev, C.
Malacaria, A.A. Mushtukov, V.F. Suleimanov, A.A. Lutovinov, I.A. Mereminskiy,
S.V. Molkov, A. Salganik, A. Santangelo, A.V. Berdyugin, V. Kravtsov, A.P. Nitindala,
I. Agudo, L.A. Antonelli, M. Bachetti, L. Baldini, W.H. Baumgartner, R. Bellazzini,
S. Bianchi, S.D. Bongiorno, R. Bonino, A. Brez, N. Bucciantini, F. Capitanio,
S. Castellano, E. Cavazzuti, C.-T. Chen, S. Ciprini, E. Costa, A. De Rosa, E.
Del Monte, L. Di Gesu, N. Di Lalla, A. Di Marco, I. Donnarumma, M. Dovčiak, S.R.
Ehlert, T. Enoto, Y. Evangelista, S. Fabiani, R. Ferrazzoli, J.A. García, S. Gunji,
K. Hayashida, W. Iwakiri, S.G. Jorstad, P. Kaaret, V. Karas, F. Kislat, T. Kitaguchi,
J.J. Kolodziejczak, H. Krawczynski, F. La Monaca, L. Latronico, I. Liodakis, S.
Maldera, A. Manfreda, F. Marin, A. Marinucci, A.P. Marscher, H.L. Marshall, F.
Massaro, G. Matt, I. Mitsuishi, T. Mizuno, F. Muleri, M. Negro, C.-Y. Ng, S.L.
O’Dell, N. Omodei, C. Oppedisano, A. Papitto, G.G. Pavlov, A.L. Peirson, M. Perri,
M. Pesce-Rollins, P.-O. Petrucci, M. Pilia, A. Possenti, S. Puccetti, B.D. Ramsey,
J. Rankin, A. Ratheesh, O.J. Roberts, R.W. Romani, C. Sgrò, P. Slane, P. Soffitta,
G. Spandre, D.A. Swartz, T. Tamagawa, F. Tavecchio, R. Taverna, Y. Tawara, A.F.
Tennant, N.E. Thomas, F. Tombesi, A. Trois, J. Vink, K. Wu, F. Xie, S. Zane, Astronomy
& Astrophysics 677 (2023).
date_created: 2024-03-26T09:46:01Z
date_published: 2023-09-04T00:00:00Z
date_updated: 2024-04-02T06:57:11Z
day: '04'
doi: 10.1051/0004-6361/202347088
extern: '1'
external_id:
arxiv:
- '2306.02116'
intvolume: ' 677'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/202347088
month: '09'
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: Complex variations in X-ray polarization in the X-ray pulsar LS V +44 17/RX
J0440.9+4431
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: 677
year: '2023'
...
---
_id: '11488'
abstract:
- lang: eng
text: Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic
medium (CGM) at high redshifts. In this work, we aim to explore the existence
of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters
(LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5,
and spectroscopic redshifts were assigned or constrained for all the sources thanks
to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit
Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes
21 galaxies that are purely F775W-magnitude selected within the redshift range
z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding
any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly
more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs
and four non-LAHs. We report the first individual detections of extended Lyα emission
around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which
is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected
galaxies generally have a large amount of hydrogen in their CGM. We derived the
mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections
and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint
redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding
gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz,
is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7.
Assuming that Lyα emission and absorption arise in the same gas, this suggests,
based on abundance matching, that LAHs trace the same gas as damped Lyα systems
(DLAs) and sub-DLAs.
acknowledgement: 'We thank the anonymous referee for constructive comments and suggestions.
We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard,
Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds
Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving
insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful
suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges
support from Swiss Government Excellence Scholarships and Japan Society for the
Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are
supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC
Starting Grant 757258“TRIPLE”. This work was supported by the Programme National
Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and
CNES. 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), and other
software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris
et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).'
article_number: A44
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Sofia G.
full_name: Gallego, Sofia G.
last_name: Gallego
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- 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: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Roser
full_name: Pelló, Roser
last_name: Pelló
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Laurence
full_name: Tresse, Laurence
last_name: Tresse
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Eloïse
full_name: Vitte, Eloïse
last_name: Vitte
citation:
ama: 'Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual
detections of Lyα haloes around rest-frame UV-selected galaxies at z
≃ 2.9–4.4. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142302'
apa: 'Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq,
F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of
Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142302'
chicago: 'Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz
Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field:
Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies
at z ≃ 2.9–4.4.” Astronomy & Astrophysics. EDP Sciences, 2022.
https://doi.org/10.1051/0004-6361/202142302.'
ieee: 'H. Kusakabe et al., “The MUSE eXtremely Deep Field: Individual detections
of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4,”
Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.'
ista: 'Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon
R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló
R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field:
Individual detections of Lyα haloes around rest-frame UV-selected galaxies
at z ≃ 2.9–4.4. Astronomy & Astrophysics. 660, A44.'
mla: 'Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections
of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.”
Astronomy & Astrophysics, vol. 660, A44, EDP Sciences, 2022, doi:10.1051/0004-6361/202142302.'
short: H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq,
R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara,
R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy & Astrophysics
660 (2022).
date_created: 2022-07-05T14:27:26Z
date_published: 2022-04-07T00:00:00Z
date_updated: 2022-07-19T09:33:24Z
day: '07'
doi: 10.1051/0004-6361/202142302
extern: '1'
external_id:
arxiv:
- '2201.07257'
intvolume: ' 660'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2201.07257
month: '04'
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 MUSE eXtremely Deep Field: Individual detections of Lyα haloes
around rest-frame UV-selected galaxies at z ≃ 2.9–4.4'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 660
year: '2022'
...
---
_id: '11490'
abstract:
- lang: eng
text: Directly characterising the first generations of stars in distant galaxies
is a key quest of observational cosmology. We present a case study of ID53 at
z = 4.77, the UV-brightest (but L⋆) star-forming galaxy at z > 3 in the MUSE eXtremely
Deep Field with a mass of ≈109 M⊙. In addition to very strong Lyman-α (Lyα) emission,
we clearly detect the (stellar) continuum and an N V P Cygni feature, interstellar
absorption, fine-structure emission and nebular C IV emission lines in the 140
h spectrum. Continuum emission from two spatially resolved components in Hubble
Space Telescope data are blended in the MUSE data, but we show that the nebular
C IV emission originates from a subcomponent of the galaxy. The UV spectrum can
be fit with recent BPASS stellar population models combined with single-burst
or continuous star formation histories (SFHs), a standard initial mass function,
and an attenuation law. Models with a young age and low metallicity (log10(age/yr)
= 6.5–7.6 and [Z/H] = −2.15 to −1.15) are preferred, but the details depend on
the assumed SFH. The intrinsic Hα luminosity of the best-fit models is an order
of magnitude higher than the Hα luminosity inferred from Spitzer/IRAC data, which
either suggests a high escape fraction of ionising photons, a high relative attenuation
of nebular to stellar dust, or a complex SFH. The metallicity appears lower than
the metallicity in more massive galaxies at z = 3 − 5, consistent with the scenario
according to which younger galaxies have lower metallicities. This chemical immaturity
likely facilitates Lyα escape, explaining why the Lyα equivalent width is anti-correlated
with stellar metallicity. Finally, we stress that uncertainties in SFHs impose
a challenge for future inferences of the stellar metallicity of young galaxies.
This highlights the need for joint (spatially resolved) analyses of stellar spectra
and photo-ionisation models.
acknowledgement: We thank the referee for thoughtful and constructive comments that
have improved the quality of this manuscript. Based on observations collected at
the European Southern Observatory under ESO programme 1101.A-0127. This work made
use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as
described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges
the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from
Australian Research Council Laureate Fellowship FL180100060.
article_number: A10
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
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: 'Matthee JJ, Feltre A, Maseda M, et al. Deciphering stellar metallicities in
the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely
Deep Field. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142187'
apa: 'Matthee, J. J., Feltre, A., Maseda, M., Nanayakkara, T., Boogaard, L., Bacon,
R., … Wisotzki, L. (2022). Deciphering stellar metallicities in the early universe:
Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142187'
chicago: 'Matthee, Jorryt J, Anna Feltre, Michael Maseda, Themiya Nanayakkara, Leindert
Boogaard, Roland Bacon, Anne Verhamme, et al. “Deciphering Stellar Metallicities
in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely
Deep Field.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142187.'
ieee: 'J. J. Matthee et al., “Deciphering stellar metallicities in the early
universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep
Field,” Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.'
ista: 'Matthee JJ, Feltre A, Maseda M, Nanayakkara T, Boogaard L, Bacon R, Verhamme
A, Leclercq F, Kusakabe H, Urrutia T, Wisotzki L. 2022. Deciphering stellar metallicities
in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely
Deep Field. Astronomy & Astrophysics. 660, A10.'
mla: 'Matthee, Jorryt J., et al. “Deciphering Stellar Metallicities in the Early
Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep
Field.” Astronomy & Astrophysics, vol. 660, A10, EDP Sciences, 2022,
doi:10.1051/0004-6361/202142187.'
short: J.J. Matthee, A. Feltre, M. Maseda, T. Nanayakkara, L. Boogaard, R. Bacon,
A. Verhamme, F. Leclercq, H. Kusakabe, T. Urrutia, L. Wisotzki, Astronomy &
Astrophysics 660 (2022).
date_created: 2022-07-05T15:25:35Z
date_published: 2022-03-30T00:00:00Z
date_updated: 2024-10-14T11:31:22Z
day: '30'
doi: 10.1051/0004-6361/202142187
extern: '1'
external_id:
arxiv:
- '2111.14855'
intvolume: ' 660'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / techniques: spectroscopic / galaxies: stellar content
/ galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2111.14855
month: '03'
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: 'Deciphering stellar metallicities in the early universe: Case study of a young
galaxy at z = 4.77 in the MUSE eXtremely Deep Field'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 660
year: '2022'
...
---
_id: '11497'
abstract:
- lang: eng
text: "Context. The hydrogen Lyman α line is often the only measurable feature in
optical spectra of high-redshift galaxies. Its shape and strength are influenced
by radiative transfer processes and the properties of the underlying stellar population.
High equivalent widths of several hundred Å are especially hard to explain by
models and could point towards unusual stellar populations, for example with low
metallicities, young stellar ages, and a top-heavy initial mass function. Other
aspects influencing equivalent widths are the morphology of the galaxy and its
gas properties.\r\nAims. The aim of this study is to better understand the connection
between the Lyman α rest-frame equivalent width (EW0) and spectral properties
as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms
for a statistical sample of galaxies and by assessing the fraction of objects
with large equivalent widths.\r\nMethods. We used integral field spectroscopy
from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data
from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission
lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour
exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum
counterparts in archival HST data. We fitted the UV continuum photometric images
using the Galfit software to gain morphological information on the rest-UV emission
and fitted the spectra obtained from MUSE to determine the double peak fraction,
asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults.
The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of
objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16%
for the full sample. This includes objects without HST continuum counterparts
(one-third of our sample), for which we give lower limits for EW0. The object
with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower
limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman
α spectral or UV continuum morphological properties.\r\nConclusions. The survey
depth has to be taken into account when studying EW0 distributions. We find that
in general, high EW0 objects can have a wide range of spectral and UV morphological
properties, which might reflect that the underlying causes for high EW0 values
are equally varied."
acknowledgement: We thank the referee for thoughtful and constructive comments that
have improved the quality of this manuscript. Based on observations collected at
the European Southern Observatory under ESO programme 1101.A-0127. This work made
use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as
described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges
the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from
Australian Research Council Laureate Fellowship FL180100060.
article_number: '183'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Kerutt, J.
last_name: Kerutt
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: A.
full_name: Verhamme, A.
last_name: Verhamme
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: E. C.
full_name: Herenz, E. C.
last_name: Herenz
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: T.
full_name: Hashimoto, T.
last_name: Hashimoto
- first_name: M.
full_name: Maseda, M.
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: H.
full_name: Kusakabe, H.
last_name: Kusakabe
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: V.
full_name: Mauerhofer, V.
last_name: Mauerhofer
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: E.
full_name: Vitte, E.
last_name: Vitte
citation:
ama: Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters
in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 2022;659. doi:10.1051/0004-6361/202141900
apa: Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz,
E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202141900
chicago: Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C.
Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide
and MUSE-Deep.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141900.
ieee: J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.
ista: Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia
T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J,
Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of
Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 659,
183.
mla: Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and
MUSE-Deep.” Astronomy & Astrophysics, vol. 659, 183, EDP Sciences,
2022, doi:10.1051/0004-6361/202141900.
short: J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz,
T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye,
J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy
& Astrophysics 659 (2022).
date_created: 2022-07-06T08:17:27Z
date_published: 2022-03-25T00:00:00Z
date_updated: 2022-07-19T09:47:16Z
day: '25'
doi: 10.1051/0004-6361/202141900
extern: '1'
external_id:
arxiv:
- '2202.06642'
intvolume: ' 659'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2202.06642
month: '03'
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: Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 659
year: '2022'
...
---
_id: '11602'
abstract:
- lang: eng
text: During the survey phase of the Kepler mission, several thousand stars were
observed in short cadence, allowing for the detection of solar-like oscillations
in more than 500 main-sequence and subgiant stars. These detections showed the
power of asteroseismology in determining fundamental stellar parameters. However,
the Kepler Science Office discovered an issue in the calibration that affected
half of the store of short-cadence data, leading to a new data release (DR25)
with corrections on the light curves. In this work, we re-analyzed the one-month
time series of the Kepler survey phase to search for solar-like oscillations that
might have been missed when using the previous data release. We studied the seismic
parameters of 99 stars, among which there are 46 targets with new reported solar-like
oscillations, increasing, by around 8%, the known sample of solar-like stars with
an asteroseismic analysis of the short-cadence data from this mission. The majority
of these stars have mid- to high-resolution spectroscopy publicly available with
the LAMOST and APOGEE surveys, respectively, as well as precise Gaia parallaxes.
We computed the masses and radii using seismic scaling relations and we find that
this new sample features massive stars (above 1.2 M⊙ and up to 2 M⊙) and subgiants.
We determined the granulation parameters and amplitude of the modes, which agree
with the scaling relations derived for dwarfs and subgiants. The stars studied
here are slightly fainter than the previously known sample of main-sequence and
subgiants with asteroseismic detections. We also studied the surface rotation
and magnetic activity levels of those stars. Our sample of 99 stars has similar
levels of activity compared to the previously known sample and is in the same
range as the Sun between the minimum and maximum of its activity cycle. We find
that for seven stars, a possible blend could be the reason for the non-detection
with the early data release. Finally, we compared the radii obtained from the
scaling relations with the Gaia ones and we find that the Gaia radii are overestimated
by 4.4%, on average, compared to the seismic radii, with a scatter of 12.3% and
a decreasing trend according to the evolutionary stage. In addition, for homogeneity
purposes, we re-analyzed the DR25 of the main-sequence and subgiant stars with
solar-like oscillations that were previously detected and, as a result, we provide
the global seismic parameters for a total of 525 stars.
acknowledgement: 'This paper includes data collected by the Kepler mission. Funding
for the Kepler mission is provided by the NASA Science Mission directorate. Some
of the data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. S. M. acknowledges
support by the Spanish Ministry of Science and Innovation with the Ramon y Cajal
fellowship number RYC-2015-17697 and the grant number PID2019-107187GB-I00. R. A.
G. and S. N. B acknowledge the support from PLATO and GOLF CNES grants. A. R. G.
S. acknowledges the support from National Aeronautics and Space Administration under
Grant NNX17AF27G and STFC consolidated grant ST/T000252/1. D.H. acknowledges support
from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration
(80NSSC19K0597), and the National Science Foundation (AST-1717000). M.S. is supported
by the Research Corporation for Science Advancement through Scialog award #26080.
Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope
LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences.
Funding for the project has been provided by the National Development and Reform
Commission. LAMOST is operated and managed by the National Astronomical Observatories,
Chinese Academy of Sciences.'
article_number: A31
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Breton, S.
last_name: Breton
- first_name: A. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- first_name: B.
full_name: Mosser, B.
last_name: Mosser
- first_name: D.
full_name: Huber, D.
last_name: Huber
- first_name: M.
full_name: Sayeed, M.
last_name: Sayeed
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: A.
full_name: Chontos, A.
last_name: Chontos
citation:
ama: Mathur S, García RA, Breton S, et al. Detections of solar-like oscillations
in dwarfs and subgiants with Kepler DR25 short-cadence data. Astronomy &
Astrophysics. 2022;657. doi:10.1051/0004-6361/202141168
apa: Mathur, S., García, R. A., Breton, S., Santos, A. R. G., Mosser, B., Huber,
D., … Chontos, A. (2022). Detections of solar-like oscillations in dwarfs and
subgiants with Kepler DR25 short-cadence data. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202141168
chicago: Mathur, S., R. A. García, S. Breton, A. R. G. Santos, B. Mosser, D. Huber,
M. Sayeed, Lisa Annabelle Bugnet, and A. Chontos. “Detections of Solar-like Oscillations
in Dwarfs and Subgiants with Kepler DR25 Short-Cadence Data.” Astronomy &
Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141168.
ieee: S. Mathur et al., “Detections of solar-like oscillations in dwarfs
and subgiants with Kepler DR25 short-cadence data,” Astronomy & Astrophysics,
vol. 657. EDP Sciences, 2022.
ista: Mathur S, García RA, Breton S, Santos ARG, Mosser B, Huber D, Sayeed M, Bugnet
LA, Chontos A. 2022. Detections of solar-like oscillations in dwarfs and subgiants
with Kepler DR25 short-cadence data. Astronomy & Astrophysics. 657, A31.
mla: Mathur, S., et al. “Detections of Solar-like Oscillations in Dwarfs and Subgiants
with Kepler DR25 Short-Cadence Data.” Astronomy & Astrophysics, vol.
657, A31, EDP Sciences, 2022, doi:10.1051/0004-6361/202141168.
short: S. Mathur, R.A. García, S. Breton, A.R.G. Santos, B. Mosser, D. Huber, M.
Sayeed, L.A. Bugnet, A. Chontos, Astronomy & Astrophysics 657 (2022).
date_created: 2022-07-18T11:41:59Z
date_published: 2022-01-01T00:00:00Z
date_updated: 2022-08-19T09:56:58Z
day: '01'
doi: 10.1051/0004-6361/202141168
extern: '1'
external_id:
arxiv:
- '2109.14058'
intvolume: ' 657'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2109.14058
month: '01'
oa: 1
oa_version: Preprint
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: Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25
short-cadence data
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 657
year: '2022'
...
---
_id: '11621'
abstract:
- lang: eng
text: "Context. Asteroseismology has revealed small core-to-surface rotation contrasts
in stars in the whole Hertzsprung–Russell diagram. This is the signature of strong
transport of angular momentum (AM) in stellar interiors. One of the plausible
candidates to efficiently carry AM is magnetic fields with various topologies
that could be present in stellar radiative zones. Among them, strong axisymmetric
azimuthal (toroidal) magnetic fields have received a lot of interest. Indeed,
if they are subject to the so-called Tayler instability, the accompanying triggered
Maxwell stresses can transport AM efficiently. In addition, the electromotive
force induced by the fluctuations of magnetic and velocity fields could potentially
sustain a dynamo action that leads to the regeneration of the initial strong axisymmetric
azimuthal magnetic field.\r\n\r\nAims. The key question we aim to answer is whether
we can detect signatures of these deep strong azimuthal magnetic fields. The only
way to answer this question is asteroseismology, and the best laboratories of
study are intermediate-mass and massive stars with external radiative envelopes.
Most of these are rapid rotators during their main sequence. Therefore, we have
to study stellar pulsations propagating in stably stratified, rotating, and potentially
strongly magnetised radiative zones, namely magneto-gravito-inertial (MGI) waves.\r\n\r\nMethods.
We generalise the traditional approximation of rotation (TAR) by simultaneously
taking general axisymmetric differential rotation and azimuthal magnetic fields
into account. Both the Coriolis acceleration and the Lorentz force are therefore
treated in a non-perturbative way. Using this new formalism, we derive the asymptotic
properties of MGI waves and their period spacings.\r\n\r\nResults. We find that
toroidal magnetic fields induce a shift in the period spacings of gravity (g)
and Rossby (r) modes. An equatorial azimuthal magnetic field with an amplitude
of the order of 105 G leads to signatures that are detectable in period spacings
for high-radial-order g and r modes in γ Doradus (γ Dor) and slowly pulsating
B (SPB) stars. More complex hemispheric configurations are more difficult to observe,
particularly when they are localised out of the propagation region of MGI modes,
which can be localised in an equatorial belt.\r\n\r\nConclusions. The magnetic
TAR, which takes into account toroidal magnetic fields in a non-perturbative way,
is derived. This new formalism allows us to assess the effects of the magnetic
field in γ Dor and SPB stars on g and r modes. We find that these effects should
be detectable for equatorial fields thanks to modern space photometry using observations
from Kepler, TESS CVZ, and PLATO."
acknowledgement: 'We thank the referee for her/his positive and constructive report,
which has allowed us to improve the quality of our article. H.D. and S.M. acknowledge
support from the CNES PLATO grant at CEA/DAp. T.V.R. gratefully acknowledges support
from the Research Foundation Flanders (FWO) under grant agreement No. 12ZB620N and
V414021N. This research was supported in part by the National Science Foundation
under Grant No. NSF PHY-1748958. C.A. is supported by the KU Leuven Research Council
(grant C16/18/005: PARADISE) as well as from the BELgian federal Science Policy
Office (BELSPO) through a PLATO PRODEX grant.'
article_number: A133
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: H.
full_name: Dhouib, H.
last_name: Dhouib
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: T.
full_name: Van Reeth, T.
last_name: Van Reeth
- first_name: C.
full_name: Aerts, C.
last_name: Aerts
citation:
ama: 'Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. Detecting deep axisymmetric
toroidal magnetic fields in stars: The traditional approximation of rotation for
differentially rotating deep spherical shells with a general azimuthal magnetic
field. Astronomy & Astrophysics. 2022;661. doi:10.1051/0004-6361/202142956'
apa: 'Dhouib, H., Mathis, S., Bugnet, L. A., Van Reeth, T., & Aerts, C. (2022).
Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional
approximation of rotation for differentially rotating deep spherical shells with
a general azimuthal magnetic field. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202142956'
chicago: 'Dhouib, H., S. Mathis, Lisa Annabelle Bugnet, T. Van Reeth, and C. Aerts.
“Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional
Approximation of Rotation for Differentially Rotating Deep Spherical Shells with
a General Azimuthal Magnetic Field.” Astronomy & Astrophysics. EDP
Sciences, 2022. https://doi.org/10.1051/0004-6361/202142956.'
ieee: 'H. Dhouib, S. Mathis, L. A. Bugnet, T. Van Reeth, and C. Aerts, “Detecting
deep axisymmetric toroidal magnetic fields in stars: The traditional approximation
of rotation for differentially rotating deep spherical shells with a general azimuthal
magnetic field,” Astronomy & Astrophysics, vol. 661. EDP Sciences,
2022.'
ista: 'Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. 2022. Detecting deep
axisymmetric toroidal magnetic fields in stars: The traditional approximation
of rotation for differentially rotating deep spherical shells with a general azimuthal
magnetic field. Astronomy & Astrophysics. 661, A133.'
mla: 'Dhouib, H., et al. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in
Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep
Spherical Shells with a General Azimuthal Magnetic Field.” Astronomy &
Astrophysics, vol. 661, A133, EDP Sciences, 2022, doi:10.1051/0004-6361/202142956.'
short: H. Dhouib, S. Mathis, L.A. Bugnet, T. Van Reeth, C. Aerts, Astronomy &
Astrophysics 661 (2022).
date_created: 2022-07-19T08:04:15Z
date_published: 2022-05-19T00:00:00Z
date_updated: 2022-08-22T07:58:54Z
day: '19'
doi: 10.1051/0004-6361/202142956
extern: '1'
external_id:
arxiv:
- '2202.10026'
intvolume: ' 661'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- magnetohydrodynamics (MHD) / waves / stars
- 'rotation / stars: magnetic field / stars'
- oscillations / methods
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2202.10026
month: '05'
oa: 1
oa_version: Preprint
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: 'Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional
approximation of rotation for differentially rotating deep spherical shells with
a general azimuthal magnetic field'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 661
year: '2022'
...
---
_id: '11498'
abstract:
- lang: eng
text: Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase
abundances, metallicities, and ionization parameters of the emitting star-forming
galaxies and their environments. The strongest main UV emission line, Lyα, has
been instrumental in advancing the general knowledge of galaxy formation in the
early universe. However, observing Lyα emission becomes increasingly challenging
at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic
media increases. Secondary weaker UV emission lines provide important alternative
methods for studying galaxy properties at high redshift. We present a large sample
of rest-frame UV emission line sources at intermediate redshift for calibrating
and exploring the connection between secondary UV lines and the emitting galaxies’
physical properties and their Lyα emission. The sample of 2052 emission line sources
with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and
MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were
selected through untargeted source detection (i.e., no preselection of sources
as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes.
We searched optimally extracted one-dimensional spectra of the full sample for
UV emission features via emission line template matching, resulting in a sample
of more than 100 rest-frame UV emission line detections. We show that the detection
efficiency of (non-Lyα) UV emission lines increases with survey depth, and that
the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and
[Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 +
C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III]
λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity
offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548
+ C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range
of 250−500 km s−1 which is in agreement with previous results from the literature.
The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III]
λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase
abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization
Model Probability Density Functions” to infer physical parameters of the full
sample and individual systems based on photoionization model parameter grids and
observational constraints from our UV emission line searches. This reveals that
the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal
mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added
catalogs of the full sample of MUSE objects studied in this work and a collection
of UV line emitters from the literature are provided with this paper.
acknowledgement: 'We would like to thank Charlotte Mason for useful discussions and
for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing
the observational data for the comparison sample studied by Steidel et al. (2014),
also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and
we acknowledge support by the Competitive Fund of the Leibniz Association through
grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001.
JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research
Council (NWO). GM received funding from the European Union’s Horizon 2020 research
and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS
– DLV-896778. This paper is based on observations collected at the European Organisation
for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B),
095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090,
097.A-0160, and 098.A-0017. This paper also makes use of observations made with
the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of
the following programs and open-source packages for Python and we are thankful to
their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013,
2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy
(van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).'
article_number: A80
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: J.
full_name: Kerutt, J.
last_name: Kerutt
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: A.
full_name: Feltre, A.
last_name: Feltre
- first_name: M. V.
full_name: Maseda, M. V.
last_name: Maseda
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: R.
full_name: Bacon, R.
last_name: Bacon
- first_name: L. A.
full_name: Boogaard, L. A.
last_name: Boogaard
- first_name: S.
full_name: Conseil, S.
last_name: Conseil
- first_name: T.
full_name: Contini, T.
last_name: Contini
- first_name: E. C.
full_name: Herenz, E. C.
last_name: Herenz
- first_name: W.
full_name: Kollatschny, W.
last_name: Kollatschny
- first_name: M.
full_name: Krumpe, M.
last_name: Krumpe
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: G.
full_name: Mahler, G.
last_name: Mahler
- 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: V.
full_name: Mauerhofer, V.
last_name: Mauerhofer
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
citation:
ama: Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame
UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4.
Astronomy & Astrophysics. 2021;654. doi:10.1051/0004-6361/202140876
apa: Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda,
M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines
in 2052 galaxies observed with MUSE at 1.5 < z < 6.4. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140876
chicago: Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda,
T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines
in 2052 Galaxies Observed with MUSE at 1.5 < z < 6.4.” Astronomy &
Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140876.
ieee: K. B. Schmidt et al., “Recovery and analysis of rest-frame UV emission
lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4,” Astronomy
& Astrophysics, vol. 654. EDP Sciences, 2021.
ista: Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara
T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe
M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021.
Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed
with MUSE at 1.5 < z < 6.4. Astronomy & Astrophysics. 654, A80.
mla: Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines
in 2052 Galaxies Observed with MUSE at 1.5 < z < 6.4.” Astronomy &
Astrophysics, vol. 654, A80, EDP Sciences, 2021, doi:10.1051/0004-6361/202140876.
short: K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda,
T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz,
W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer,
J. Richard, J. Schaye, Astronomy & Astrophysics 654 (2021).
date_created: 2022-07-06T08:49:03Z
date_published: 2021-10-15T00:00:00Z
date_updated: 2022-07-19T09:34:36Z
day: '15'
doi: 10.1051/0004-6361/202140876
extern: '1'
external_id:
arxiv:
- '2108.01713'
intvolume: ' 654'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and
bands / methods: observational / techniques: imaging spectroscopy'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2108.01713
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: Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed
with MUSE at 1.5 < z < 6.4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 654
year: '2021'
...