---
_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: '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: 2022-07-19T09:33:46Z
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'
...
---
_id: '11500'
abstract:
- lang: eng
text: We report the discovery of diffuse extended Lyα emission from redshift 3.1
to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures
have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep
Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among
the 22 overdense regions identified, five are likely to harbor very extended Lyα
emission at high significance with an average surface brightness of 5 × 10−20
erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these
filaments comes from beyond the circumgalactic medium of any identified Lyα emitter.
Fluorescent Lyα emission powered by the cosmic UV background can only account
for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher
redshift. We find that the bulk of this diffuse emission can be reproduced by
the unresolved Lyα emission of a large population of ultra low-luminosity Lyα
emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function
is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg
s−1, and the clustering of these Lyα emitters is significant (filling factor <
1/6). If these Lyα emitters are powered by star formation, then this implies their
luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1.
These observations provide the first detection of the cosmic web in Lyα emission
in typical filamentary environments and the first observational clue indicating
the existence of a large population of ultra low-luminosity Lyα emitters at high
redshift.
acknowledgement: 'We warmly thank ESO Paranal staff for their great professional support
during all MXDF GTO observing runs. We thank the anonymous referee for a careful
reading of the manuscript and helpful comments. We also thank Matthew Lehnert for
fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant
339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
(FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020
and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV
acknowledges support from the European Research Council under grant agreement ERC-stg-757258
(TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support
from the GDR ISIS through the Projets exploratoires program (project TASTY). AF
acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges
support by The Netherlands Organisation for Scientific Research (NWO) through a
TOP Grant Module 1 under project number 614.001.652. This research made use of the
following open-source software and we are thankful to the developers of these: GNU
Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python
packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras
et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).'
article_number: A107
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: R.
full_name: Bacon, R.
last_name: Bacon
- first_name: D.
full_name: Mary, D.
last_name: Mary
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: J.
full_name: Blaizot, J.
last_name: Blaizot
- first_name: M.
full_name: Maseda, M.
last_name: Maseda
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: S.
full_name: Conseil, S.
last_name: Conseil
- first_name: J.
full_name: Brinchmann, J.
last_name: Brinchmann
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: V.
full_name: Abril-Melgarejo, V.
last_name: Abril-Melgarejo
- first_name: L.
full_name: Boogaard, L.
last_name: Boogaard
- first_name: N. F.
full_name: Bouché, N. F.
last_name: Bouché
- first_name: T.
full_name: Contini, T.
last_name: Contini
- first_name: A.
full_name: Feltre, A.
last_name: Feltre
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: C.
full_name: Herenz, C.
last_name: Herenz
- first_name: W.
full_name: Kollatschny, W.
last_name: Kollatschny
- first_name: H.
full_name: Kusakabe, H.
last_name: Kusakabe
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: L.
full_name: Michel-Dansac, L.
last_name: Michel-Dansac
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: M.
full_name: Roth, M.
last_name: Roth
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: M.
full_name: Steinmetz, M.
last_name: Steinmetz
- first_name: L.
full_name: Tresse, L.
last_name: Tresse
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: A.
full_name: Verhamme, A.
last_name: Verhamme
- first_name: P. M.
full_name: Weilbacher, P. M.
last_name: Weilbacher
- first_name: J.
full_name: Zabl, J.
last_name: Zabl
- first_name: S. L.
full_name: Zoutendijk, S. L.
last_name: Zoutendijk
citation:
ama: 'Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic
web in emission at high redshift. Astronomy & Astrophysics. 2021;647.
doi:10.1051/0004-6361/202039887'
apa: 'Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk,
S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high
redshift. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039887'
chicago: 'Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki,
et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.”
Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039887.'
ieee: 'R. Bacon et al., “The MUSE Extremely Deep Field: The cosmic web in
emission at high redshift,” Astronomy & Astrophysics, vol. 647. EDP
Sciences, 2021.'
ista: 'Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil
S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini
T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac
L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia
T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely
Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics.
647, A107.'
mla: 'Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission
at High Redshift.” Astronomy & Astrophysics, vol. 647, A107, EDP Sciences,
2021, doi:10.1051/0004-6361/202039887.'
short: R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki,
S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F.
Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe,
J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt,
M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L.
Zoutendijk, Astronomy & Astrophysics 647 (2021).
date_created: 2022-07-06T09:31:50Z
date_published: 2021-03-18T00:00:00Z
date_updated: 2022-07-19T09:34:57Z
day: '18'
doi: 10.1051/0004-6361/202039887
extern: '1'
external_id:
arxiv:
- '2102.05516'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: groups: general / cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.05516
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: 'The MUSE Extremely Deep Field: The cosmic web in emission at high redshift'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_id: '11605'
abstract:
- lang: eng
text: "Context. The discovery of moderate differential rotation between the core
and the envelope of evolved solar-like stars could be the signature of a strong
magnetic field trapped inside the radiative interior. The population of intermediate-mass
red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation
modes that behave as acoustic modes in their external envelope and as gravity
modes in their core) could also arise from the effect of an internal magnetic
field. Indeed, stars more massive than about 1.1 solar masses are known to develop
a convective core during their main sequence. The field generated by the dynamo
triggered by this convection could be the progenitor of a strong fossil magnetic
field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims.
Observations of mixed modes can constitute an excellent probe of the deepest layers
of evolved solar-like stars, and magnetic fields in those regions can impact their
propagation. The magnetic perturbation on mixed modes may therefore be visible
in asteroseismic data. To unravel which constraints can be obtained from observations,
we theoretically investigate the effects of a plausible mixed axisymmetric magnetic
field with various amplitudes on the mixed-mode frequencies of evolved solar-like
stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric
magnetic field were computed for dipolar and quadrupolar mixed modes. These computations
were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions.
We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the
presence of a dynamo in the convective core during the main sequence, provoke
significant asymmetries on mixed-mode frequency multiplets during the red giant
branch. We provide constraints and methods for the detectability of such magnetic
signatures. We show that these signatures may be detectable in asteroseismic data
for field amplitudes small enough for the amplitude of the modes not to be affected
by the conversion of gravity into Alfvén waves inside the magnetised interior.
Finally, we infer an upper limit for the strength of the field and the associated
lower limit for the timescale of its action in order to redistribute angular momentum
in stellar interiors."
article_number: A53
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: V.
full_name: Prat, V.
last_name: Prat
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: A.
full_name: Astoul, A.
last_name: Astoul
- first_name: K.
full_name: Augustson, K.
last_name: Augustson
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: L.
full_name: Amard, L.
last_name: Amard
- first_name: C.
full_name: Neiner, C.
last_name: Neiner
citation:
ama: 'Bugnet LA, Prat V, Mathis S, et al. Magnetic signatures on mixed-mode frequencies:
I. An axisymmetric fossil field inside the core of red giants. Astronomy &
Astrophysics. 2021;650. doi:10.1051/0004-6361/202039159'
apa: 'Bugnet, L. A., Prat, V., Mathis, S., Astoul, A., Augustson, K., García, R.
A., … Neiner, C. (2021). Magnetic signatures on mixed-mode frequencies: I. An
axisymmetric fossil field inside the core of red giants. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202039159'
chicago: 'Bugnet, Lisa Annabelle, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.
A. García, S. Mathur, L. Amard, and C. Neiner. “Magnetic Signatures on Mixed-Mode
Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” Astronomy
& Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039159.'
ieee: 'L. A. Bugnet et al., “Magnetic signatures on mixed-mode frequencies:
I. An axisymmetric fossil field inside the core of red giants,” Astronomy &
Astrophysics, vol. 650. EDP Sciences, 2021.'
ista: 'Bugnet LA, Prat V, Mathis S, Astoul A, Augustson K, García RA, Mathur S,
Amard L, Neiner C. 2021. Magnetic signatures on mixed-mode frequencies: I. An
axisymmetric fossil field inside the core of red giants. Astronomy & Astrophysics.
650, A53.'
mla: 'Bugnet, Lisa Annabelle, et al. “Magnetic Signatures on Mixed-Mode Frequencies:
I. An Axisymmetric Fossil Field inside the Core of Red Giants.” Astronomy &
Astrophysics, vol. 650, A53, EDP Sciences, 2021, doi:10.1051/0004-6361/202039159.'
short: L.A. Bugnet, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.A. García, S.
Mathur, L. Amard, C. Neiner, Astronomy & Astrophysics 650 (2021).
date_created: 2022-07-18T12:10:59Z
date_published: 2021-06-07T00:00:00Z
date_updated: 2022-08-19T10:06:33Z
day: '07'
doi: 10.1051/0004-6361/202039159
extern: '1'
external_id:
arxiv:
- '2102.01216'
intvolume: ' 650'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- stars
- oscillations / stars
- magnetic field / stars
- interiors / stars
- evolution / stars
- rotation
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.01216
month: '06'
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: 'Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field
inside the core of red giants'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 650
year: '2021'
...
---
_id: '11606'
abstract:
- lang: eng
text: "Context. Our knowledge of the dynamics of stars has undergone a revolution
through the simultaneous large amount of high-quality photometric observations
collected by space-based asteroseismology and ground-based high-precision spectropolarimetry.
They allowed us to probe the internal rotation of stars and their surface magnetism
in the whole Hertzsprung-Russell diagram. However, new methods should still be
developed to probe the deep magnetic fields in these stars.\r\n\r\nAims. Our goal
is to provide seismic diagnoses that allow us to probe the internal magnetism
of stars.\r\n\r\nMethods. We focused on asymptotic low-frequency gravity modes
and high-frequency acoustic modes. Using a first-order perturbative theory, we
derived magnetic splittings of their frequencies as explicit functions of stellar
parameters.\r\n\r\nResults. As in the case of rotation, we show that asymptotic
gravity and acoustic modes can allow us to probe the different components of the
magnetic field in the cavities in which they propagate. This again demonstrates
the high potential of using mixed-modes when this is possible."
acknowledgement: The authors thank the referee and Pr. J. Christensen-Dalsgaard for
their very constructive comments and remarks that allowed us to improve the article.
St. M., L. B., V. P., and K. A. acknowledge support from the European Research Council
through ERC grant SPIRE 647383. All the members from CEA acknowledge support from
GOLF and PLATO CNES grants of the Astrophysics Division at CEA. S. Mathur acknowledges
support by the Ramon y Cajal fellowship number RYC-2015-17697. We made great use
of the megyr python package for interfacing MESA and GYRE codes.
article_number: A122
article_processing_charge: No
article_type: original
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
- first_name: V.
full_name: Prat, V.
last_name: Prat
- first_name: K.
full_name: Augustson, K.
last_name: Augustson
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: R. A.
full_name: Garcia, R. A.
last_name: Garcia
citation:
ama: Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. Probing the
internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy
& Astrophysics. 2021;647. doi:10.1051/0004-6361/202039180
apa: Mathis, S., Bugnet, L. A., Prat, V., Augustson, K., Mathur, S., & Garcia,
R. A. (2021). Probing the internal magnetism of stars using asymptotic magneto-asteroseismology.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039180
chicago: Mathis, S., Lisa Annabelle Bugnet, V. Prat, K. Augustson, S. Mathur, and
R. A. Garcia. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.”
Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039180.
ieee: S. Mathis, L. A. Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia,
“Probing the internal magnetism of stars using asymptotic magneto-asteroseismology,”
Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021.
ista: Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing
the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy
& Astrophysics. 647, A122.
mla: Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic
Magneto-Asteroseismology.” Astronomy & Astrophysics, vol. 647, A122,
EDP Sciences, 2021, doi:10.1051/0004-6361/202039180.
short: S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy
& Astrophysics 647 (2021).
date_created: 2022-07-18T12:15:27Z
date_published: 2021-03-18T00:00:00Z
date_updated: 2022-08-19T10:11:52Z
day: '18'
doi: 10.1051/0004-6361/202039180
extern: '1'
external_id:
arxiv:
- '2012.11050'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- asteroseismology / waves / stars
- magnetic field / stars
- oscillations / methods
- analytical
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2012.11050
month: '03'
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: Probing the internal magnetism of stars using asymptotic magneto-asteroseismology
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_id: '11608'
abstract:
- lang: eng
text: 'In order to understand stellar evolution, it is crucial to efficiently determine
stellar surface rotation periods. Indeed, while they are of great importance in
stellar models, angular momentum transport processes inside stars are still poorly
understood today. Surface rotation, which is linked to the age of the star, is
one of the constraints needed to improve the way those processes are modelled.
Statistics of the surface rotation periods for a large sample of stars of different
spectral types are thus necessary. An efficient tool to automatically determine
reliable rotation periods is needed when dealing with large samples of stellar
photometric datasets. The objective of this work is to develop such a tool. For
this purpose, machine learning classifiers constitute relevant bases to build
our new methodology. Random forest learning abilities are exploited to automate
the extraction of rotation periods in Kepler light curves. Rotation periods and
complementary parameters are obtained via three different methods: a wavelet analysis,
the autocorrelation function of the light curve, and the composite spectrum. We
trained three different classifiers: one to detect if rotational modulations are
present in the light curve, one to flag close binary or classical pulsators candidates
that can bias our rotation period determination, and finally one classifier to
provide the final rotation period. We tested our machine learning pipeline on
23 431 stars of the Kepler K and M dwarf reference rotation catalogue for which
60% of the stars have been visually inspected. For the sample of 21 707 stars
where all the input parameters are provided to the algorithm, 94.2% of them are
correctly classified (as rotating or not). Among the stars that have a rotation
period in the reference catalogue, the machine learning provides a period that
agrees within 10% of the reference value for 95.3% of the stars. Moreover, the
yield of correct rotation periods is raised to 99.5% after visually inspecting
25.2% of the stars. Over the two main analysis steps, rotation classification
and period selection, the pipeline yields a global agreement with the reference
values of 92.1% and 96.9% before and after visual inspection. Random forest classifiers
are efficient tools to determine reliable rotation periods in large samples of
stars. The methodology presented here could be easily adapted to extract surface
rotation periods for stars with different spectral types or observed by other
instruments such as K2, TESS or by PLATO in the near future.'
acknowledgement: 'We thank Suzanne Aigrain and Joe Llama for providing us with the
simulated data used in Aigrain et al. (2015). S. N. B., L. B. and R. A. G. acknowledge
the support from PLATO and GOLF CNES grants. A. R. G. S. acknowledges the support
from NASA under grant NNX17AF27G. S. M. acknowledges the support from the Spanish
Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697.
P. L. P. and S. M. acknowledge support from the Spanish Ministry of Science and
Innovation with the grant number PID2019-107187GB-I00. This research has made use
of the NASA Exoplanet Archive, which is operated by the California Institute of
Technology, under contract with the National Aeronautics and Space Administration
under the Exoplanet Exploration Program. Software: Python (Van Rossum & Drake 2009),
numpy (Oliphant 2006), pandas (The pandas development team 2020; McKinney 2010),
matplotlib (Hunter 2007), scikit-learn (Pedregosa et al. 2011). The source code
used to obtain the present results can be found at: https://gitlab.com/sybreton/pushkin
; https://gitlab.com/sybreton/ml_surface_rotation_paper .'
article_number: A125
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. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- 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: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: P. L.
full_name: Pallé, P. L.
last_name: Pallé
citation:
ama: 'Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. ROOSTER:
A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy
& Astrophysics. 2021;647. doi:10.1051/0004-6361/202039947'
apa: 'Breton, S. N., Santos, A. R. G., Bugnet, L. A., Mathur, S., García, R. A.,
& Pallé, P. L. (2021). ROOSTER: A machine-learning analysis tool for Kepler
stellar rotation periods. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039947'
chicago: 'Breton, S. N., A. R. G. Santos, Lisa Annabelle Bugnet, S. Mathur, R. A.
García, and P. L. Pallé. “ROOSTER: A Machine-Learning Analysis Tool for Kepler
Stellar Rotation Periods.” Astronomy & Astrophysics. EDP Sciences,
2021. https://doi.org/10.1051/0004-6361/202039947.'
ieee: 'S. N. Breton, A. R. G. Santos, L. A. Bugnet, S. Mathur, R. A. García, and
P. L. Pallé, “ROOSTER: A machine-learning analysis tool for Kepler stellar rotation
periods,” Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021.'
ista: 'Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. 2021. ROOSTER:
A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy
& Astrophysics. 647, A125.'
mla: 'Breton, S. N., et al. “ROOSTER: A Machine-Learning Analysis Tool for Kepler
Stellar Rotation Periods.” Astronomy & Astrophysics, vol. 647, A125,
EDP Sciences, 2021, doi:10.1051/0004-6361/202039947.'
short: S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé,
Astronomy & Astrophysics 647 (2021).
date_created: 2022-07-18T12:21:32Z
date_published: 2021-03-19T00:00:00Z
date_updated: 2022-08-22T08:47:47Z
day: '19'
doi: 10.1051/0004-6361/202039947
extern: '1'
external_id:
arxiv:
- '2101.10152'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'methods: data analysis / stars: solar-type / stars: activity / stars: rotation
/ starspots'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2101.10152
month: '03'
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: 'ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_id: '11609'
abstract:
- lang: eng
text: "Context. Stellar interiors are the seat of efficient transport of angular
momentum all along their evolution. In this context, understanding the dependence
of the turbulent transport triggered by the instabilities of the vertical and
horizontal shears of the differential rotation in stellar radiation zones as a
function of their rotation, stratification, and thermal diffusivity is mandatory.
Indeed, it constitutes one of the cornerstones of the rotational transport and
mixing theory, which is implemented in stellar evolution codes to predict the
rotational and chemical evolutions of stars.\r\n\r\nAims. We investigate horizontal
shear instabilities in rotating stellar radiation zones by considering the full
Coriolis acceleration with both the dimensionless horizontal Coriolis component
f̃ and the vertical component f.\r\n\r\nMethods. We performed a linear stability
analysis using linearized equations derived from the Navier-Stokes and heat transport
equations in the rotating nontraditional f-plane. We considered a horizontal shear
flow with a hyperbolic tangent profile as the base flow. The linear stability
was analyzed numerically in wide ranges of parameters, and we performed an asymptotic
analysis for large vertical wavenumbers using the Wentzel-Kramers-Brillouin-Jeffreys
(WKBJ) approximation for nondiffusive and highly-diffusive fluids.\r\n\r\nResults.
As in the traditional f-plane approximation, we identify two types of instabilities:
the inflectional and inertial instabilities. The inflectional instability is destabilized
as f̃ increases and its maximum growth rate increases significantly, while the
thermal diffusivity stabilizes the inflectional instability similarly to the traditional
case. The inertial instability is also strongly affected; for instance, the inertially
unstable regime is also extended in the nondiffusive limit as 0 < f < 1 + f̃ 2/N2,
where N is the dimensionless Brunt-Väisälä frequency. More strikingly, in the
high thermal diffusivity limit, it is always inertially unstable at any colatitude
θ except at the poles (i.e., 0° < θ < 180°). We also derived the critical Reynolds
numbers for the inertial instability using the asymptotic dispersion relations
obtained from the WKBJ analysis. Using the asymptotic and numerical results, we
propose a prescription for the effective turbulent viscosities induced by the
inertial and inflectional instabilities that can be possibly used in stellar evolution
models. The characteristic time of this turbulence is short enough so that it
is efficient to redistribute angular momentum and to mix chemicals in stellar
radiation zones."
acknowledgement: The authors acknowledge support from the European Research Council
through ERC grant SPIRE 647383 and from GOLF and PLATO CNES grants at the Department
of Astrophysics at CEA Paris-Saclay. We thank the referee, Prof. A. J. Barker, for
his constructive comments that allow us to improve the article.
article_number: A64
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Park, J.
last_name: Park
- first_name: V.
full_name: Prat, V.
last_name: Prat
- 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: 'Park J, Prat V, Mathis S, Bugnet LA. Horizontal shear instabilities in rotating
stellar radiation zones: II. Effects of the full Coriolis acceleration. Astronomy
& Astrophysics. 2021;646. doi:10.1051/0004-6361/202038654'
apa: 'Park, J., Prat, V., Mathis, S., & Bugnet, L. A. (2021). Horizontal shear
instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis
acceleration. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038654'
chicago: 'Park, J., V. Prat, S. Mathis, and Lisa Annabelle Bugnet. “Horizontal Shear
Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis
Acceleration.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202038654.'
ieee: 'J. Park, V. Prat, S. Mathis, and L. A. Bugnet, “Horizontal shear instabilities
in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration,”
Astronomy & Astrophysics, vol. 646. EDP Sciences, 2021.'
ista: 'Park J, Prat V, Mathis S, Bugnet LA. 2021. Horizontal shear instabilities
in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration.
Astronomy & Astrophysics. 646, A64.'
mla: 'Park, J., et al. “Horizontal Shear Instabilities in Rotating Stellar Radiation
Zones: II. Effects of the Full Coriolis Acceleration.” Astronomy & Astrophysics,
vol. 646, A64, EDP Sciences, 2021, doi:10.1051/0004-6361/202038654.'
short: J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy & Astrophysics 646
(2021).
date_created: 2022-07-18T13:24:32Z
date_published: 2021-02-08T00:00:00Z
date_updated: 2022-08-19T10:18:03Z
day: '08'
doi: 10.1051/0004-6361/202038654
extern: '1'
external_id:
arxiv:
- '2006.10660'
intvolume: ' 646'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- hydrodynamics / turbulence / stars
- rotation / stars
- evolution
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2006.10660
month: '02'
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: 'Horizontal shear instabilities in rotating stellar radiation zones: II. Effects
of the full Coriolis acceleration'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 646
year: '2021'
...
---
_id: '13455'
abstract:
- lang: eng
text: The majority of massive stars live in binary or multiple systems and will
interact with a companion during their lifetimes, which helps to explain the observed
diversity of core-collapse supernovae. Donor stars in binary systems can lose
most of their hydrogen-rich envelopes through mass transfer. As a result, not
only are the surface properties affected, but so is the core structure. However,
most calculations of the core-collapse properties of massive stars rely on single-star
models. We present a systematic study of the difference between the pre-supernova
structures of single stars and stars of the same initial mass (11–21 M⊙) that
have been stripped due to stable post-main-sequence mass transfer at solar metallicity.
We present the pre-supernova core composition with novel diagrams that give an
intuitive representation of the isotope distribution. As shown in previous studies,
at the edge of the carbon-oxygen core, the binary-stripped star models contain
an extended gradient of carbon, oxygen, and neon. This layer remains until core
collapse and is more extended in mass for higher initial stellar masses. It originates
from the receding of the convective helium core during core helium burning in
binary-stripped stars, which does not occur in single-star models. We find that
this same evolutionary phase leads to systematic differences in the final density
and nuclear energy generation profiles. Binary-stripped star models have systematically
higher total masses of carbon at the moment of core collapse compared to single-star
models, which likely results in systematically different supernova yields. In
about half of our models, the silicon-burning and oxygen-rich layers merge after
core silicon burning. We discuss the implications of our findings for the “explodability”,
supernova observations, and nucleosynthesis of these stars. Our models are publicly
available and can be readily used as input for detailed supernova simulations.
article_number: A58
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: E.
full_name: Laplace, E.
last_name: Laplace
- first_name: S.
full_name: Justham, S.
last_name: Justham
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- 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: R.
full_name: Farmer, R.
last_name: Farmer
- first_name: D.
full_name: Vartanyan, D.
last_name: Vartanyan
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
citation:
ama: 'Laplace E, Justham S, Renzo M, et al. Different to the core: The pre-supernova
structures of massive single and binary-stripped stars. Astronomy & Astrophysics.
2021;656. doi:10.1051/0004-6361/202140506'
apa: 'Laplace, E., Justham, S., Renzo, M., Götberg, Y. L. L., Farmer, R., Vartanyan,
D., & de Mink, S. E. (2021). Different to the core: The pre-supernova structures
of massive single and binary-stripped stars. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202140506'
chicago: 'Laplace, E., S. Justham, M. Renzo, Ylva Louise Linsdotter Götberg, R.
Farmer, D. Vartanyan, and S. E. de Mink. “Different to the Core: The Pre-Supernova
Structures of Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics.
EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140506.'
ieee: 'E. Laplace et al., “Different to the core: The pre-supernova structures
of massive single and binary-stripped stars,” Astronomy & Astrophysics,
vol. 656. EDP Sciences, 2021.'
ista: 'Laplace E, Justham S, Renzo M, Götberg YLL, Farmer R, Vartanyan D, de Mink
SE. 2021. Different to the core: The pre-supernova structures of massive single
and binary-stripped stars. Astronomy & Astrophysics. 656, A58.'
mla: 'Laplace, E., et al. “Different to the Core: The Pre-Supernova Structures of
Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics,
vol. 656, A58, EDP Sciences, 2021, doi:10.1051/0004-6361/202140506.'
short: E. Laplace, S. Justham, M. Renzo, Y.L.L. Götberg, R. Farmer, D. Vartanyan,
S.E. de Mink, Astronomy & Astrophysics 656 (2021).
date_created: 2023-08-03T10:11:09Z
date_published: 2021-12-02T00:00:00Z
date_updated: 2023-08-21T11:49:15Z
day: '02'
doi: 10.1051/0004-6361/202140506
external_id:
arxiv:
- '2102.05036'
intvolume: ' 656'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/202140506
month: '12'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Different to the core: The pre-supernova structures of massive single and
binary-stripped stars'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 656
year: '2021'
...
---
_id: '13457'
abstract:
- lang: eng
text: "Context. Observations of massive stars in open clusters younger than ∼8 Myr
have shown that a majority of them are in binary systems, most of which will interact
during their life. While these can be used as a proxy of the initial multiplicity
properties, studying populations of massive stars older than ∼20 Myr allows us
to probe the outcome of these interactions after a significant number of systems
have experienced mass and angular momentum transfer and may even have merged.\r\n\r\nAims.
Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity
properties of the massive-star population in the dense core of the ∼40 Myr old
cluster NGC 330 in the Small Magellanic Cloud in order to search for possible
imprints of stellar evolution on the multiplicity properties.\r\n\r\nMethods.
We obtained six epochs of VLT/MUSE observations operated in wide-field mode with
the extended wavelength setup and supported by adaptive optics. We extracted spectra
and measured radial velocities for stars brighter than mF814W = 19. We identified
single-lined spectroscopic binaries through significant RV variability with a
peak-to-peak amplitude larger than 20 km s−1. We also identified double-lined
spectroscopic binaries, and quantified the observational biases for binary detection.
In particular, we took into account that binary systems with similar line strengths
are difficult to detect in our data set.\r\n\r\nResults. The observed spectroscopic
binary fraction among stars brighter than mF814W = 19 (approximately 5.5 M⊙ on
the main sequence) is fSBobs = 13.2 ± 2.0%. Considering period and mass ratio
ranges from log(P) = 0.15−3.5 (about 1.4 to 3160 d), q = 0.1−1.0, and a representative
set of orbital parameter distributions, we find a bias-corrected close binary
fraction of fcl = 34−7+8%. This fraction seems to decline for the fainter stars,
which indicates either that the close binary fraction drops in the B-type domain,
or that the period distribution becomes more heavily weighted toward longer orbital
periods. We further find that both fractions vary strongly in different regions
of the color-magnitude diagram, which corresponds to different evolutionary stages.
This probably reveals the imprint of the binary history of different groups of
stars. In particular, we find that the observed spectroscopic binary fraction
of Be stars (fSBobs = 2 ± 2%) is significantly lower than that of B-type stars
(fSBobs = 9 ± 2%).\r\n\r\nConclusions. We provide the first homogeneous radial
velocity study of a large sample of B-type stars at a low metallicity ([Fe/H]
≲ −1.0). The overall bias-corrected close binary fraction (log(P) < 3.5 d) of
the B-star population in NGC 330 is lower than the fraction reported for younger
Galactic and Large Magellanic Cloud clusters in previous works. More data are
needed, however, to establish whether the observed differences are caused by an
age or a metallicity effect."
article_number: A70
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: G.
full_name: Banyard, G.
last_name: Banyard
- 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: C. J.
full_name: Evans, C. J.
last_name: Evans
- 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: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: F. R. N.
full_name: Schneider, F. R. N.
last_name: Schneider
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
citation:
ama: Bodensteiner J, Sana H, Wang C, et al. The young massive SMC cluster NGC 330
seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy
& Astrophysics. 2021;652. doi:10.1051/0004-6361/202140507
apa: Bodensteiner, J., Sana, H., Wang, C., Langer, N., Mahy, L., Banyard, G., …
Tramper, F. (2021). The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity
properties of the massive-star population. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202140507
chicago: Bodensteiner, J., H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A.
de Koter, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity
Properties of the Massive-Star Population.” Astronomy & Astrophysics.
EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140507.
ieee: J. Bodensteiner et al., “The young massive SMC cluster NGC 330 seen
by MUSE. II. Multiplicity properties of the massive-star population,” Astronomy
& Astrophysics, vol. 652. EDP Sciences, 2021.
ista: Bodensteiner J, Sana H, Wang C, Langer N, Mahy L, Banyard G, de Koter A, de
Mink SE, Evans CJ, Götberg YLL, Patrick LR, Schneider FRN, Tramper F. 2021. The
young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of
the massive-star population. Astronomy & Astrophysics. 652, A70.
mla: Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.
II. Multiplicity Properties of the Massive-Star Population.” Astronomy &
Astrophysics, vol. 652, A70, EDP Sciences, 2021, doi:10.1051/0004-6361/202140507.
short: J. Bodensteiner, H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de
Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, L.R. Patrick, F.R.N. Schneider,
F. Tramper, Astronomy & Astrophysics 652 (2021).
date_created: 2023-08-03T10:11:34Z
date_published: 2021-08-12T00:00:00Z
date_updated: 2023-08-21T11:49:36Z
day: '12'
doi: 10.1051/0004-6361/202140507
extern: '1'
external_id:
arxiv:
- '2104.13409'
intvolume: ' 652'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/202140507
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'
scopus_import: '1'
status: public
title: The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties
of the massive-star population
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 652
year: '2021'
...
---
_id: '11501'
abstract:
- lang: eng
text: We investigated the ultraviolet (UV) spectral properties of faint Lyman-α
emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to
prepare future observations of the faint Universe. We used data from the MUSE
Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint
(median MUV of −18 and down to MUV of −16), low stellar mass (median value of
108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged
spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength,
UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation
rate) properties. We searched for UV spectral features other than Lyα, such as
higher ionization nebular emission lines and absorption features. We successfully
observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission
lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551
doublet either in emission or P-Cygni. We compared the observed spectral properties
of the different mean spectra and find the emission lines to vary with the observational
and physical properties of the LAEs. In particular, the mean spectra of LAEs with
larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes,
and lower stellar masses show the strongest nebular emission. The line ratios
of these lines are similar to those measured in the spectra of local metal-poor
galaxies, while their equivalent widths are weaker compared to the handful of
extreme values detected in individual spectra of z > 2 galaxies. This suggests
that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs.
We publicly released the stacked spectra, as they can serve as empirical templates
for the design of future observations, such as those with the James Webb Space
Telescope and the Extremely Large Telescope.
acknowledgement: 'We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba
Vidal-García for helpful discussions. This work is supported by the ERC advanced
grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR
2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program
for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and
AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported
by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges
support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020
and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003.
HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also
like to thank the organizers and participants of the Leiden Lorentz Center workshop:
Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use
of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB
(Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data
Analysis Framework, Piqueras et al. 2019).'
article_number: A118
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Jayadev
full_name: Pradeep, Jayadev
last_name: Pradeep
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Kasper B.
full_name: Schmidt, Kasper B.
last_name: Schmidt
- first_name: Jeremy
full_name: Blaizot, Jeremy
last_name: Blaizot
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: David
full_name: Carton, David
last_name: Carton
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Wolfram
full_name: Kollatschny, Wolfram
last_name: Kollatschny
- first_name: Raffaella A.
full_name: Marino, Raffaella A.
last_name: Marino
- 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: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Laurence
full_name: Tresse, Laurence
last_name: Tresse
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Peter M.
full_name: Weilbacher, Peter M.
last_name: Weilbacher
citation:
ama: 'Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey:
XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy &
Astrophysics. 2020;641. doi:10.1051/0004-6361/202038133'
apa: 'Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe,
H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The
mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202038133'
chicago: 'Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane
Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field
Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy
& Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202038133.'
ieee: 'A. Feltre et al., “The MUSE Hubble Ultra Deep Field Survey: XV. The
mean rest-UV spectra of Lyα emitters at z > 3,” Astronomy & Astrophysics,
vol. 641. EDP Sciences, 2020.'
ista: 'Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki
L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S,
Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard
J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble
Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z >
3. Astronomy & Astrophysics. 641, A118.'
mla: 'Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean
Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics,
vol. 641, A118, EDP Sciences, 2020, doi:10.1051/0004-6361/202038133.'
short: A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L.
Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard,
S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee,
T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M.
Weilbacher, Astronomy & Astrophysics 641 (2020).
date_created: 2022-07-06T09:38:16Z
date_published: 2020-09-18T00:00:00Z
date_updated: 2022-07-19T09:35:43Z
day: '18'
doi: 10.1051/0004-6361/202038133
extern: '1'
external_id:
arxiv:
- '2007.01878'
intvolume: ' 641'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet:
ISM / ultraviolet: galaxies'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2007.01878
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: 'The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα
emitters at z > 3'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 641
year: '2020'
...
---
_id: '11503'
abstract:
- lang: eng
text: "Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful
probe of the evolution of the intergalactic neutral hydrogen gas fraction. However,
uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks
to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic
Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously
over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes
of M1500 ≈ −17.75). This is a significantly fainter range than in former studies
(M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift
star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift
sample following UV luminosity functions and measured the Lyα emission with MUSE
using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults.
We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the
first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of
XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z −
0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values
are consistent with those in the literature within 1σ at z ≲ 5, but our median
values are systematically lower than reported values over the whole redshift range.
In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα)
≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly
arise from selection biases for Lyman Break Galaxies (LBGs) in the literature:
UV-faint LBGs are more easily selected if they have strong Lyα emission, hence
XLAE is biased towards higher values when those samples are used.\r\nConclusions.
Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously
suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of
a late or patchy reionization process. We compared our results with predictions
from a cosmological galaxy evolution model. We find that a model with a bursty
star formation (SF) can reproduce our observed LAE fractions much better than
models where SF is a smooth function of time."
acknowledgement: We thank the anonymous referee for constructive comments and suggestions.
We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro
for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to
Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima,
Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions.
This work is based on observations taken by VLT, which is operated by European Southern
Observatory. This research made use of Astropy (http://www.astropy.org), which is
a community-developed core Python package for Astronomy (Astropy Collaboration 2013,
2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from
Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship
for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges
support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE.
This work was supported by the project FOGHAR (Agence Nationale de la Recherche,
ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence
Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support
from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid
for Scientic Research 19J01620.
article_number: A12
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Simon
full_name: Conseil, Simon
last_name: Conseil
- first_name: Bruno
full_name: Guiderdoni, Bruno
last_name: Guiderdoni
- first_name: Alyssa B.
full_name: Drake, Alyssa B.
last_name: Drake
- first_name: Edmund
full_name: Christian Herenz, Edmund
last_name: Christian Herenz
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- 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: Raffaella
full_name: Anna Marino, Raffaella
last_name: Anna Marino
- first_name: Kasper
full_name: Borello Schmidt, Kasper
last_name: Borello Schmidt
- first_name: Roser
full_name: Pelló, Roser
last_name: Pelló
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- first_name: Guillaume
full_name: Mahler, Guillaume
last_name: Mahler
citation:
ama: 'Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey:
XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy &
Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340'
apa: 'Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J.,
… Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of
the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/201937340'
chicago: 'Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland
Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field
Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy
& Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340.'
ieee: 'H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV.
Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy &
Astrophysics, vol. 638. EDP Sciences, 2020.'
ista: 'Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto
T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch
P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F,
Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution
of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics.
638, A12.'
mla: 'Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution
of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics,
vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.'
short: H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T.
Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz,
J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló,
M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy & Astrophysics 638
(2020).
date_created: 2022-07-06T09:50:48Z
date_published: 2020-06-03T00:00:00Z
date_updated: 2022-07-19T09:35:20Z
day: '03'
doi: 10.1051/0004-6361/201937340
extern: '1'
external_id:
arxiv:
- '2003.12083'
intvolume: ' 638'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'dark ages / reionization / first stars / early Universe / cosmology: observations
/ galaxies: evolution / galaxies: high-redshift / intergalactic medium'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2003.12083
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: 'The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter
fraction from z = 3 to z = 6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 638
year: '2020'
...
---
_id: '11504'
abstract:
- lang: eng
text: We present spatially resolved maps of six individually-detected Lyman α haloes
(LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature
in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >
MUV > −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic
analysis of the LAHs reveals significant intrahalo variations of the Lyα line
profile. Using a three-dimensional two-component model for the Lyα emission, we
measured the full width at half maximum (FWHM), the peak velocity shift, and the
asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find
that the Lyα line shape is statistically different in the halo compared to the
core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies.
Similarly to object-by-object based studies and a recent resolved study using
lensing, we find a correlation between the peak velocity shift and the width of
the Lyα line both at the interstellar and circum-galactic scales. This trend has
been predicted by radiative transfer simulations of galactic winds as a result
of resonant scattering in outflows. While there is a lack of correlation between
the spectral properties and the spatial scale lengths of our LAHs, we find a correlation
between the width of the line in the LAH and the halo flux fraction. Interestingly,
UV bright galaxies (MUV < −20) show broader, more redshifted, and less asymmetric
Lyα lines in their haloes. The most significant correlation found is for the FWHM
of the line and the UV continuum slope of the galaxy, suggesting that the redder
galaxies have broader Lyα lines. The generally broad and red line shapes found
in the halo component suggest that the Lyα haloes are powered either by scattering
processes through an outflowing medium, fluorescent emission from outflowing cold
clumps of gas, or a mix of both. Considering the large diversity of the Lyα line
profiles observed in our sample and the lack of strong correlation, the interpretation
of our results is still broadly open and underlines the need for realistic spatially
resolved models of the LAHs.
acknowledgement: F.L., R.B., and S.C. acknowledge support from the ERC advanced grant
339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting
grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting
grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds
(PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003.
T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT,
Japan.
article_number: A82
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Adélaïde
full_name: Claeyssens, Adélaïde
last_name: Claeyssens
- first_name: Simon
full_name: Conseil, Simon
last_name: Conseil
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Edmund Christian
full_name: Herenz, Edmund Christian
last_name: Herenz
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
last_name: Marino
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Peter
full_name: Mitchell, Peter
last_name: Mitchell
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Kasper Borello
full_name: Schmidt, Kasper Borello
last_name: Schmidt
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: 'Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey:
XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming
galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339'
apa: 'Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann,
J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially
resolved spectral properties of Lyman α haloes around star-forming galaxies at
z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339'
chicago: 'Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy
Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra
Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes
around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics.
EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937339.'
ieee: 'F. Leclercq et al., “The MUSE Hubble Ultra Deep field survey: XIII.
Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies
at z > 3,” Astronomy & Astrophysics, vol. 635. EDP Sciences, 2020.'
ista: 'Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo
S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino
RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki
L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral
properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy
& Astrophysics. 635, A82.'
mla: 'Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII.
Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies
at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences,
2020, doi:10.1051/0004-6361/201937339.'
short: F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann,
S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz,
H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J.
Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020).
date_created: 2022-07-06T09:56:20Z
date_published: 2020-03-11T00:00:00Z
date_updated: 2022-07-19T09:36:58Z
day: '11'
doi: 10.1051/0004-6361/201937339
extern: '1'
external_id:
arxiv:
- '2002.05731'
intvolume: ' 635'
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/2002.05731
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: 'The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral
properties of Lyman α haloes around star-forming galaxies at z > 3'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 635
year: '2020'
...
---
_id: '13463'
abstract:
- lang: eng
text: 'Present and upcoming time-domain astronomy efforts, in part driven by gravitational-wave
follow-up campaigns, will unveil a variety of rare explosive transients in the
sky. Here, we focus on pulsational pair-instability evolution, which can result
in signatures that are observable with electromagnetic and gravitational waves.
We simulated grids of bare helium stars to characterize the resulting black hole
(BH) masses together with the ejecta composition, velocity, and thermal state.
We find that the stars do not react “elastically” to the thermonuclear ignition
in the core: there is not a one-to-one correspondence between pair-instability
driven ignition and mass ejections, which causes ambiguity as to what is an observable
pulse. In agreement with previous studies, we find that for initial helium core
masses of 37.5 M⊙ ≲ MHe, init ≲ 41 M⊙, corresponding to carbon-oxygen core masses
27.5 M⊙ ≲ MCO ≲ 30.1 M⊙, the explosions are not strong enough to affect the surface.
With increasing initial helium core mass, they become progressively stronger causing
first large radial expansion (41 M⊙ ≲ MHe, init ≲ 42 M⊙, corresponding to 30.1 M⊙ ≲ MCO ≲ 30.8 M⊙)
and, finally, also mass ejection episodes (for MHe, init ≳ 42 M⊙, or MCO ≳ 30.8 M⊙).
The lowest mass helium core to be fully disrupted in a pair-instability supernova
is MHe, init ≃ 80 M⊙, corresponding to MCO ≃ 55 M⊙. Models with MHe, init ≳ 200 M⊙
(MCO ≳ 114 M⊙) reach the photodisintegration regime, resulting in BHs with masses
of MBH ≳ 125 M⊙. Although this is currently considered unlikely, if BHs from these
models form via (weak) explosions, the previously-ejected material might be hit
by the blast wave and convert kinetic energy into observable electromagnetic radiation.
We characterize the hydrogen-free circumstellar material from the pulsational
pair-instability of helium cores by simply assuming that the ejecta maintain a
constant velocity after ejection. We find that our models produce helium-rich
ejecta with mass of 10−3 M⊙ ≲ MCSM ≲ 40 M⊙, the larger values corresponding to
the more massive progenitor stars. These ejecta are typically launched at a few
thousand km s−1 and reach distances of ∼1012 − 1015 cm before the core-collapse
of the star. The delays between mass ejection events and the final collapse span
a wide and mass-dependent range (from subhour to 104 years), and the shells ejected
can also collide with each other, powering supernova impostor events before the
final core-collapse. The range of properties we find suggests a possible connection
with (some) type Ibn supernovae.'
article_number: A56
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: R.
full_name: Farmer, R.
last_name: Farmer
- first_name: S.
full_name: Justham, S.
last_name: Justham
- 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: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
- first_name: P.
full_name: Marchant, P.
last_name: Marchant
- first_name: N.
full_name: Smith, N.
last_name: Smith
citation:
ama: Renzo M, Farmer R, Justham S, et al. Predictions for the hydrogen-free ejecta
of pulsational pair-instability supernovae. Astronomy & Astrophysics.
2020;640. doi:10.1051/0004-6361/202037710
apa: Renzo, M., Farmer, R., Justham, S., Götberg, Y. L. L., de Mink, S. E., Zapartas,
E., … Smith, N. (2020). Predictions for the hydrogen-free ejecta of pulsational
pair-instability supernovae. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/202037710
chicago: Renzo, M., R. Farmer, S. Justham, Ylva Louise Linsdotter Götberg, S. E.
de Mink, E. Zapartas, P. Marchant, and N. Smith. “Predictions for the Hydrogen-Free
Ejecta of Pulsational Pair-Instability Supernovae.” Astronomy & Astrophysics.
EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202037710.
ieee: M. Renzo et al., “Predictions for the hydrogen-free ejecta of pulsational
pair-instability supernovae,” Astronomy & Astrophysics, vol. 640. EDP
Sciences, 2020.
ista: Renzo M, Farmer R, Justham S, Götberg YLL, de Mink SE, Zapartas E, Marchant
P, Smith N. 2020. Predictions for the hydrogen-free ejecta of pulsational pair-instability
supernovae. Astronomy & Astrophysics. 640, A56.
mla: Renzo, M., et al. “Predictions for the Hydrogen-Free Ejecta of Pulsational
Pair-Instability Supernovae.” Astronomy & Astrophysics, vol. 640, A56,
EDP Sciences, 2020, doi:10.1051/0004-6361/202037710.
short: M. Renzo, R. Farmer, S. Justham, Y.L.L. Götberg, S.E. de Mink, E. Zapartas,
P. Marchant, N. Smith, Astronomy & Astrophysics 640 (2020).
date_created: 2023-08-03T10:12:58Z
date_published: 2020-08-12T00:00:00Z
date_updated: 2023-08-09T12:58:41Z
day: '12'
doi: 10.1051/0004-6361/202037710
extern: '1'
external_id:
arxiv:
- '2002.05077'
intvolume: ' 640'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/202037710
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'
scopus_import: '1'
status: public
title: Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 640
year: '2020'
...
---
_id: '13464'
abstract:
- lang: eng
text: Massive binaries that merge as compact objects are the progenitors of gravitational-wave
sources. Most of these binaries experience one or more phases of mass transfer,
during which one of the stars loses all or part of its outer envelope and becomes
a stripped-envelope star. The evolution of the size of these stripped stars is
crucial in determining whether they experience further interactions and understanding
their ultimate fate. We present new calculations of stripped-envelope stars based
on binary evolution models computed with MESA. We use these to investigate their
radius evolution as a function of mass and metallicity. We further discuss their
pre-supernova observable characteristics and potential consequences of their evolution
on the properties of supernovae from stripped stars. At high metallicity, we find
that practically all of the hydrogen-rich envelope is removed, which is in agreement
with earlier findings. Only progenitors with initial masses below 10 M⊙ expand
to large radii (up to 100 R⊙), while more massive progenitors remain compact.
At low metallicity, a substantial amount of hydrogen remains and the progenitors
can, in principle, expand to giant sizes (> 400 R⊙) for all masses we consider.
This implies that they can fill their Roche lobe anew. We show that the prescriptions
commonly used in population synthesis models underestimate the stellar radii by
up to two orders of magnitude. We expect that this has consequences for the predictions
for gravitational-wave sources from double neutron star mergers, particularly
with regard to their metallicity dependence.
article_number: A6
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: E.
full_name: Laplace, E.
last_name: Laplace
- 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: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: S.
full_name: Justham, S.
last_name: Justham
- first_name: R.
full_name: Farmer, R.
last_name: Farmer
citation:
ama: 'Laplace E, Götberg YLL, de Mink SE, Justham S, Farmer R. The expansion of
stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors.
Astronomy & Astrophysics. 2020;637. doi:10.1051/0004-6361/201937300'
apa: 'Laplace, E., Götberg, Y. L. L., de Mink, S. E., Justham, S., & Farmer,
R. (2020). The expansion of stripped-envelope stars: Consequences for supernovae
and gravitational-wave progenitors. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/201937300'
chicago: 'Laplace, E., Ylva Louise Linsdotter Götberg, S. E. de Mink, S. Justham,
and R. Farmer. “The Expansion of Stripped-Envelope Stars: Consequences for Supernovae
and Gravitational-Wave Progenitors.” Astronomy & Astrophysics. EDP
Sciences, 2020. https://doi.org/10.1051/0004-6361/201937300.'
ieee: 'E. Laplace, Y. L. L. Götberg, S. E. de Mink, S. Justham, and R. Farmer, “The
expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave
progenitors,” Astronomy & Astrophysics, vol. 637. EDP Sciences, 2020.'
ista: 'Laplace E, Götberg YLL, de Mink SE, Justham S, Farmer R. 2020. The expansion
of stripped-envelope stars: Consequences for supernovae and gravitational-wave
progenitors. Astronomy & Astrophysics. 637, A6.'
mla: 'Laplace, E., et al. “The Expansion of Stripped-Envelope Stars: Consequences
for Supernovae and Gravitational-Wave Progenitors.” Astronomy & Astrophysics,
vol. 637, A6, EDP Sciences, 2020, doi:10.1051/0004-6361/201937300.'
short: E. Laplace, Y.L.L. Götberg, S.E. de Mink, S. Justham, R. Farmer, Astronomy
& Astrophysics 637 (2020).
date_created: 2023-08-03T10:13:10Z
date_published: 2020-05-01T00:00:00Z
date_updated: 2023-08-09T12:56:32Z
day: '01'
doi: 10.1051/0004-6361/201937300
extern: '1'
external_id:
arxiv:
- '2003.01120'
intvolume: ' 637'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201937300
month: '05'
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 expansion of stripped-envelope stars: Consequences for supernovae and
gravitational-wave progenitors'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 637
year: '2020'
...