---
_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: 2024-10-14T11:39:01Z
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: 2024-10-14T11:39:21Z
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: 2025-01-14T14:11:32Z
day: '02'
doi: 10.1051/0004-6361/202140506
extern: '1'
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'
...
---
_id: '13466'
abstract:
- lang: eng
text: "Context. A majority of massive stars are part of binary systems, a large
fraction of which will inevitably interact during their lives. Binary-interaction
products (BiPs), that is, stars affected by such interaction, are expected to
be commonly present in stellar populations. BiPs are thus a crucial ingredient
in the understanding of stellar evolution.\r\nAims. We aim to identify and characterize
a statistically significant sample of BiPs by studying clusters of 10 − 40 Myr,
an age at which binary population models predict the abundance of BiPs to be highest.
One example of such a cluster is NGC 330 in the Small Magellanic Cloud.\r\nMethods.
Using MUSE WFM-AO observations of NGC 330, we resolved the dense cluster core
for the first time and were able to extract spectra of its entire massive star
population. We developed an automated spectral classification scheme based on
the equivalent widths of spectral lines in the red part of the spectrum.\r\nResults.
We characterize the massive star content of the core of NGC 330, which contains
more than 200 B stars, 2 O stars, 6 A-type supergiants, and 11 red supergiants.
We find a lower limit on the Be star fraction of 32 ± 3% in the whole sample.
It increases to at least 46 ± 10% when we only consider stars brighter than V = 17 mag.
We estimate an age of the cluster core between 35 and 40 Myr and a total cluster
mass of 88−18+17 × 103 M⊙.\r\nConclusions. We find that the population in the
cluster core is different than the population in the outskirts: while the stellar
content in the core appears to be older than the stars in the outskirts, the Be
star fraction and the observed binary fraction are significantly higher. Furthermore,
we detect several BiP candidates that will be subject of future studies."
article_number: A51
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: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- 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: N.
full_name: Langer, N.
last_name: Langer
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- 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, Mahy L, et al. The young massive SMC cluster NGC 330
seen by MUSE. Astronomy & Astrophysics. 2020;634. doi:10.1051/0004-6361/201936743
apa: Bodensteiner, J., Sana, H., Mahy, L., Patrick, L. R., de Koter, A., de Mink,
S. E., … Tramper, F. (2020). The young massive SMC cluster NGC 330 seen by MUSE.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201936743
chicago: Bodensteiner, J., H. Sana, L. Mahy, L. R. Patrick, A. de Koter, S. E. de
Mink, C. J. Evans, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.”
Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201936743.
ieee: J. Bodensteiner et al., “The young massive SMC cluster NGC 330 seen
by MUSE,” Astronomy & Astrophysics, vol. 634. EDP Sciences, 2020.
ista: Bodensteiner J, Sana H, Mahy L, Patrick LR, de Koter A, de Mink SE, Evans
CJ, Götberg YLL, Langer N, Lennon DJ, Schneider FRN, Tramper F. 2020. The young
massive SMC cluster NGC 330 seen by MUSE. Astronomy & Astrophysics. 634, A51.
mla: Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.”
Astronomy & Astrophysics, vol. 634, A51, EDP Sciences, 2020, doi:10.1051/0004-6361/201936743.
short: J. Bodensteiner, H. Sana, L. Mahy, L.R. Patrick, A. de Koter, S.E. de Mink,
C.J. Evans, Y.L.L. Götberg, N. Langer, D.J. Lennon, F.R.N. Schneider, F. Tramper,
Astronomy & Astrophysics 634 (2020).
date_created: 2023-08-03T10:13:29Z
date_published: 2020-02-05T00:00:00Z
date_updated: 2023-08-09T12:50:01Z
day: '05'
doi: 10.1051/0004-6361/201936743
extern: '1'
external_id:
arxiv:
- '1911.03477'
intvolume: ' 634'
keyword:
- 'stars: massive / stars: emission-line / Be / binaries: spectroscopic / blue stragglers
/ Magellanic Clouds'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201936743
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: The young massive SMC cluster NGC 330 seen by MUSE
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 634
year: '2020'
...
---
_id: '13467'
abstract:
- lang: eng
text: Massive stars are often found in binary systems, and it has been argued that
binary products boost the ionizing radiation of stellar populations. Accurate
predictions for binary products are needed to understand and quantify their contribution
to cosmic reionization. We investigate the contribution of stars stripped in binaries
because (1) they are, arguably, the best-understood products of binary evolution,
(2) we recently produced the first radiative transfer calculations for the atmospheres
of these stripped stars that predict their ionizing spectra, and (3) they are
very promising sources because they boost the ionizing emission of stellar populations
at late times. This allows stellar feedback to clear the surroundings such that
a higher fraction of their photons can escape and ionize the intergalactic medium.
Combining our detailed predictions for the ionizing spectra with a simple cosmic
reionization model, we estimate that stripped stars contributed tens of percent
of the photons that caused cosmic reionization of hydrogen, depending on the assumed
escape fractions. More importantly, stripped stars harden the ionizing emission.
We estimate that the spectral index for the ionizing part of the spectrum can
increase to −1 compared to ≲ − 2 for single stars. At high redshift, stripped
stars and massive single stars combined dominate the He II-ionizing emission,
but we expect that active galactic nuclei drive cosmic helium reionization. Further
observational consequences we expect are (1) high ionization states for the intergalactic
gas surrounding stellar systems, such as C IV and Si IV, and (2) additional heating
of the intergalactic medium of up to a few thousand Kelvin. Quantifying these
warrants the inclusion of accurate models for stripped stars and other binary
products in full cosmological simulations.
article_number: A134
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: M.
full_name: McQuinn, M.
last_name: McQuinn
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
- first_name: J. H.
full_name: Groh, J. H.
last_name: Groh
- first_name: C.
full_name: Norman, C.
last_name: Norman
citation:
ama: Götberg YLL, de Mink SE, McQuinn M, Zapartas E, Groh JH, Norman C. Contribution
from stars stripped in binaries to cosmic reionization of hydrogen and helium.
Astronomy & Astrophysics. 2020;634. doi:10.1051/0004-6361/201936669
apa: Götberg, Y. L. L., de Mink, S. E., McQuinn, M., Zapartas, E., Groh, J. H.,
& Norman, C. (2020). Contribution from stars stripped in binaries to cosmic
reionization of hydrogen and helium. Astronomy & Astrophysics. EDP
Sciences. https://doi.org/10.1051/0004-6361/201936669
chicago: Götberg, Ylva Louise Linsdotter, S. E. de Mink, M. McQuinn, E. Zapartas,
J. H. Groh, and C. Norman. “Contribution from Stars Stripped in Binaries to Cosmic
Reionization of Hydrogen and Helium.” Astronomy & Astrophysics. EDP
Sciences, 2020. https://doi.org/10.1051/0004-6361/201936669.
ieee: Y. L. L. Götberg, S. E. de Mink, M. McQuinn, E. Zapartas, J. H. Groh, and
C. Norman, “Contribution from stars stripped in binaries to cosmic reionization
of hydrogen and helium,” Astronomy & Astrophysics, vol. 634. EDP Sciences,
2020.
ista: Götberg YLL, de Mink SE, McQuinn M, Zapartas E, Groh JH, Norman C. 2020. Contribution
from stars stripped in binaries to cosmic reionization of hydrogen and helium.
Astronomy & Astrophysics. 634, A134.
mla: Götberg, Ylva Louise Linsdotter, et al. “Contribution from Stars Stripped in
Binaries to Cosmic Reionization of Hydrogen and Helium.” Astronomy & Astrophysics,
vol. 634, A134, EDP Sciences, 2020, doi:10.1051/0004-6361/201936669.
short: Y.L.L. Götberg, S.E. de Mink, M. McQuinn, E. Zapartas, J.H. Groh, C. Norman,
Astronomy & Astrophysics 634 (2020).
date_created: 2023-08-03T10:13:43Z
date_published: 2020-02-25T00:00:00Z
date_updated: 2024-10-14T12:22:53Z
day: '25'
doi: 10.1051/0004-6361/201936669
extern: '1'
external_id:
arxiv:
- '1911.00543'
intvolume: ' 634'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201936669
month: '02'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Contribution from stars stripped in binaries to cosmic reionization of hydrogen
and helium
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 634
year: '2020'
...
---
_id: '11499'
abstract:
- lang: eng
text: Deep optical spectroscopic surveys of galaxies provide a unique opportunity
to investigate rest-frame ultra-violet (UV) emission line properties of galaxies
at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble
Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other
publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue
of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach
a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line
active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median
MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys.
Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV
emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength
data available in the Hubble legacy fields to derive basic galaxy properties of
our sample through spectral energy distribution fitting techniques. Taking advantage
of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per
pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics
of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately
sub-solar photo-ionisation models, however, we find that including effects of
binary stars lead to degeneracies in most free parameters. Even after considering
extra ionising photons produced by extreme sub-solar metallicity binary stellar
models, photo-ionisation models are unable to reproduce rest-frame He II λ1640
equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models
to match the observed He II λ1640 properties.
acknowledgement: 'The authors wish to thank the referee for constructive comments
that improved the paper substantially. We thank the BPASS team for making the stellar
population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel
Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz
Centre and the scientific organizers of the Characterizing galaxies with spectroscopy
with a view for JWST workshop held at the Lorentz Centre in 2017 October, which
promoted useful discussions in the wider community. TN, JB, and RB acknowledges
the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.
AF acknowledges support from the ERC via an Advanced Grant under grant agreement
no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
(FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract
IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672).
JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research
made use of astropy (http://www.astropy.org) a community-developed core Python package
for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures
were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org).
Facilities: VLT (MUSE).'
article_number: A89
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Wolfram
full_name: Kollatschny, Wolfram
last_name: Kollatschny
- 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: Mieke
full_name: Paalvast, Mieke
last_name: Paalvast
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
citation:
ama: Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission
line properties at z ∼2−4. Astronomy & Astrophysics. 2019;648. doi:10.1051/0004-6361/201834565
apa: Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S.,
Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties
at z ∼2−4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834565
chicago: Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens,
Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640
Emission Line Properties at z ∼2−4.” Astronomy & Astrophysics. EDP
Sciences, 2019. https://doi.org/10.1051/0004-6361/201834565.
ieee: T. Nanayakkara et al., “Exploring He II λ1640 emission line properties
at z ∼2−4,” Astronomy & Astrophysics, vol. 648. EDP Sciences, 2019.
ista: Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A,
Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme
A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &
Astrophysics. 648, A89.
mla: Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties
at z ∼2−4.” Astronomy & Astrophysics, vol. 648, A89, EDP Sciences,
2019, doi:10.1051/0004-6361/201834565.
short: T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A.
Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J.
Richard, A. Verhamme, Astronomy & Astrophysics 648 (2019).
date_created: 2022-07-06T09:07:06Z
date_published: 2019-04-16T00:00:00Z
date_updated: 2022-07-19T09:36:08Z
day: '16'
doi: 10.1051/0004-6361/201834565
extern: '1'
external_id:
arxiv:
- '1902.05960'
intvolume: ' 648'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1902.05960
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'
related_material:
link:
- relation: erratum
url: https://doi.org/10.1051/0004-6361/201834565e
scopus_import: '1'
status: public
title: Exploring He II λ1640 emission line properties at z ∼2−4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 648
year: '2019'
...
---
_id: '11505'
abstract:
- lang: eng
text: "Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic
Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha
luminosity function (LF) based on deep observations of four lensing clusters.
The goal of our project is to set strong constraints on the relative contribution
of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims.
The precise aim of the present study is to further constrain the abundance of
LAEs by taking advantage of the magnification provided by lensing clusters to
build a blindly selected sample of galaxies which is less biased than current
blank field samples in redshift and luminosity. By construction, this sample of
LAEs is complementary to those built from deep blank fields, whether observed
by MUSE or by other facilities, and makes it possible to determine the shape of
the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods.
We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected
luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account
the individual differences in detection conditions between the LAEs when computing
the LF, including lensing configurations, and spatial and spectral morphologies,
the non-parametric 1/Vmax method was adopted. The price to pay to benefit from
magnification is a reduction of the effective volume of the survey, together with
a more complex analysis procedure to properly determine the effective volume Vmax
for each galaxy. In this paper we present a complete procedure for the determination
of the LF based on IFU detections in lensing clusters. This procedure, including
some new methods for masking, effective volume integration and (individual) completeness
determinations, has been fully automated when possible, and it can be easily generalized
to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result
of this analysis, the Lyman-alpha LF has been obtained in four different redshift
bins: 2.9 < z < 6, 7, 2.9 < z < 4.0, 4.0 < z < 5.0, and 5.0 < z < 6.7
with constraints down to log LLyα = 40.5. From our data only, no significant evolution
of LF mean slope can be found. When performing a Schechter analysis also including
data from the literature to complete the present sample towards the brightest
luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08
to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions.
The contribution of the LAE population to the star formation rate density at z ∼ 6
is ≲50% depending on the luminosity limit considered, which is of the same order
as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution
with redshift depends on the assumed escape fraction of Lyman-alpha photons, and
appears to slightly increase with increasing redshift when this fraction is conservatively
set to one. Depending on the intersection between the LAE/LBG populations, the
contribution of the observed galaxies to the ionizing flux may suffice to keep
the universe ionized at z ∼ 6."
acknowledgement: We thank the anonymous referee for their critical review and useful
suggestions. This work has been carried out thanks to the support of the OCEVU Labex
(ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the “Investissements
d’Avenir” French government programme managed by the ANR. Partially funded by the
ERC starting grant CALENDS (JR, VP, BC, JM), the Agence Nationale de la recherche
bearing the reference ANR-13-BS05-0010-02 (FOGHAR), and the “Programme National
de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. GdV, RP, JR, GM, JM, BC,
and VP also acknowledge support by the Programa de Cooperacion Cientifica – ECOS
SUD Program C16U02. NL acknowledges funding from the European Research Council (ERC)
under the European Union’s Horizon 2020 research and innovation programme (grant
agreement No 669253), ABD acknowledges support from the ERC advanced grant “Cosmic
Gas”. LW acknowledges support by the Competitive Fund of the Leibniz Association
through grant SAW-2015-AIP-2, and TG acknowledges support from the European Research
Council under grant agreement ERC-stg-757258 (TRIPLE).. Based on observations made
with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345,
094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also
based on observations obtained with the NASA/ESA Hubble Space Telescope, retrieved
from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science
Institute (STScI). STScI is operated by the Association of Universities for Research
in Astronomy, Inc. under NASA contract NAS 5-26555. This research made use of Astropy,
a community-developed core Python package for Astronomy (Astropy Collaboration 2013).
All plots in this paper were created using Matplotlib (Hunter 2007).
article_number: A3
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: G.
full_name: de La Vieuville, G.
last_name: de La Vieuville
- first_name: D.
full_name: Bina, D.
last_name: Bina
- first_name: R.
full_name: Pello, R.
last_name: Pello
- first_name: G.
full_name: Mahler, G.
last_name: Mahler
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: A. B.
full_name: Drake, A. B.
last_name: Drake
- first_name: E. C.
full_name: Herenz, E. C.
last_name: Herenz
- first_name: F. E.
full_name: Bauer, F. E.
last_name: Bauer
- first_name: B.
full_name: Clément, B.
last_name: Clément
- first_name: D.
full_name: Lagattuta, D.
last_name: Lagattuta
- first_name: N.
full_name: Laporte, N.
last_name: Laporte
- first_name: J.
full_name: Martinez, J.
last_name: Martinez
- first_name: V.
full_name: Patrício, V.
last_name: Patrício
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: J.
full_name: Zabl, J.
last_name: Zabl
- first_name: R. J.
full_name: Bouwens, R. J.
last_name: Bouwens
- first_name: T.
full_name: Contini, T.
last_name: Contini
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: R. A.
full_name: Marino, R. A.
last_name: Marino
- first_name: M. V.
full_name: Maseda, M. V.
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: G.
full_name: Soucail, G.
last_name: Soucail
citation:
ama: de La Vieuville G, Bina D, Pello R, et al. Faint end of the z ∼ 3–7 luminosity
function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy
& Astrophysics. 2019;628. doi:10.1051/0004-6361/201834471
apa: de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A.
B., … Soucail, G. (2019). Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha
emitters behind lensing clusters observed with MUSE. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/201834471
chicago: La Vieuville, G. de, D. Bina, R. Pello, G. Mahler, J. Richard, A. B. Drake,
E. C. Herenz, et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha
Emitters behind Lensing Clusters Observed with MUSE.” Astronomy & Astrophysics.
EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201834471.
ieee: G. de La Vieuville et al., “Faint end of the z ∼ 3–7 luminosity function
of Lyman-alpha emitters behind lensing clusters observed with MUSE,” Astronomy
& Astrophysics, vol. 628. EDP Sciences, 2019.
ista: de La Vieuville G, Bina D, Pello R, Mahler G, Richard J, Drake AB, Herenz
EC, Bauer FE, Clément B, Lagattuta D, Laporte N, Martinez J, Patrício V, Wisotzki
L, Zabl J, Bouwens RJ, Contini T, Garel T, Guiderdoni B, Marino RA, Maseda MV,
Matthee JJ, Schaye J, Soucail G. 2019. Faint end of the z ∼ 3–7 luminosity function
of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy
& Astrophysics. 628, A3.
mla: de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of
Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” Astronomy
& Astrophysics, vol. 628, A3, EDP Sciences, 2019, doi:10.1051/0004-6361/201834471.
short: G. de La Vieuville, D. Bina, R. Pello, G. Mahler, J. Richard, A.B. Drake,
E.C. Herenz, F.E. Bauer, B. Clément, D. Lagattuta, N. Laporte, J. Martinez, V.
Patrício, L. Wisotzki, J. Zabl, R.J. Bouwens, T. Contini, T. Garel, B. Guiderdoni,
R.A. Marino, M.V. Maseda, J.J. Matthee, J. Schaye, G. Soucail, Astronomy &
Astrophysics 628 (2019).
date_created: 2022-07-06T10:09:36Z
date_published: 2019-07-25T00:00:00Z
date_updated: 2022-07-19T09:36:31Z
day: '25'
doi: 10.1051/0004-6361/201834471
extern: '1'
external_id:
arxiv:
- '1905.13696'
intvolume: ' 628'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'gravitational lensing: strong / galaxies: high-redshift / dark ages'
- reionization
- 'first stars / galaxies: clusters: general / galaxies: luminosity function'
- mass function
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1905.13696
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: Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind
lensing clusters observed with MUSE
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 628
year: '2019'
...
---
_id: '11507'
abstract:
- lang: eng
text: 'Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies.
While it originates from many physical processes, for star-forming galaxies the
intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation
produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes
of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star
formation rate (SFR) indicator. However, its resonant nature and susceptibility
to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the
uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating
LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs)
at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα
with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα
as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and
we show that it constrains a well-defined anti-correlation between ionisation
efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0
are easy measurable quantities at high redshift, thus making our relation a practical
tool to estimate intrinsic Lyα and LyC luminosities under well controlled and
simple assumptions. Our results allow observed Lyα luminosities to be used to
compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs.
We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6
to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1
and that our calibration might be even applicable for the most luminous LAEs within
the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1]
= 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily
tested with future observations with JWST which can obtain Hα and Hβ measurements
for high-redshift LAEs.'
acknowledgement: We thank the anonymous referees for multiple comments and suggestions
which have improved the manuscript. JM acknowledges the support of a Huygens PhD
fellowship from Leiden University. We have benefited greatly from the publicly available
programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011;
Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration
2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples
of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017,
2018a) and we also provide the toy model used as a PYTHON script.
article_number: A157
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable:
Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy
& Astrophysics. 2019;623. doi:10.1051/0004-6361/201833075'
apa: 'Sobral, D., & Matthee, J. J. (2019). Predicting Lyα escape fractions with
a simple observable: Lyα in emission as an empirically calibrated star formation
rate indicator. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833075'
chicago: 'Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions
with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
Rate Indicator.” Astronomy & Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201833075.'
ieee: 'D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple
observable: Lyα in emission as an empirically calibrated star formation rate indicator,”
Astronomy & Astrophysics, vol. 623. EDP Sciences, 2019.'
ista: 'Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple
observable: Lyα in emission as an empirically calibrated star formation rate indicator.
Astronomy & Astrophysics. 623, A157.'
mla: 'Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with
a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
Rate Indicator.” Astronomy & Astrophysics, vol. 623, A157, EDP Sciences,
2019, doi:10.1051/0004-6361/201833075.'
short: D. Sobral, J.J. Matthee, Astronomy & Astrophysics 623 (2019).
date_created: 2022-07-06T11:08:16Z
date_published: 2019-03-26T00:00:00Z
date_updated: 2022-07-19T09:37:20Z
day: '26'
doi: 10.1051/0004-6361/201833075
extern: '1'
external_id:
arxiv:
- '1803.08923'
intvolume: ' 623'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies:
evolution / galaxies: formation / galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1803.08923
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: 'Predicting Lyα escape fractions with a simple observable: Lyα in emission
as an empirically calibrated star formation rate indicator'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 623
year: '2019'
...
---
_id: '11614'
abstract:
- lang: eng
text: The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide
full-frame images of almost the entire sky. The amount of stellar data to be analysed
represents hundreds of millions stars, which is several orders of magnitude more
than the number of stars observed by the Convection, Rotation and planetary Transits
satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying
the newly observed stars with near real-time algorithms to better guide the subsequent
detailed studies. In this paper, we present a classification algorithm built to
recognise solar-like pulsators among classical pulsators. This algorithm relies
on the global amount of power contained in the power spectral density (PSD), also
known as the flicker in spectral power density (FliPer). Because each type of
pulsating star has a characteristic background or pulsation pattern, the shape
of the PSD at different frequencies can be used to characterise the type of pulsating
star. The FliPer classifier (FliPerClass) uses different FliPer parameters along
with the effective temperature as input parameters to feed a ML algorithm in order
to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated
data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators
with a 98% accuracy. Among them, solar-like pulsating stars are recognised with
a 99% accuracy, which is of great interest for a further seismic analysis of these
stars, which are like our Sun. Similar results are obtained when we trained our
classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is
part of the large TASC classification pipeline developed by the TESS Data for
Asteroseismology (T’DA) classification working group.
acknowledgement: We thank the enitre T’DA team for useful comments and discussions,
in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James
Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the
support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon
y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support
of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges
the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar
Astrophysics Centre is provided by the Danish National Research Foundation (Grant
DNRF106).
article_number: A79
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: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: G. R.
full_name: Davies, G. R.
last_name: Davies
- first_name: O. J.
full_name: Hall, O. J.
last_name: Hall
- first_name: M. N.
full_name: Lund, M. N.
last_name: Lund
- first_name: B. M.
full_name: Rendle, B. M.
last_name: Rendle
citation:
ama: 'Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like
pulsators among TESS targets. Astronomy & Astrophysics. 2019;624. doi:10.1051/0004-6361/201834780'
apa: 'Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund,
M. N., & Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators
among TESS targets. Astronomy & Astrophysics. EDP Science. https://doi.org/10.1051/0004-6361/201834780'
chicago: 'Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall,
M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators
among TESS Targets.” Astronomy & Astrophysics. EDP Science, 2019. https://doi.org/10.1051/0004-6361/201834780.'
ieee: 'L. A. Bugnet et al., “FliPerClass: In search of solar-like pulsators
among TESS targets,” Astronomy & Astrophysics, vol. 624. EDP Science,
2019.'
ista: 'Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019.
FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy &
Astrophysics. 624, A79.'
mla: 'Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators
among TESS Targets.” Astronomy & Astrophysics, vol. 624, A79, EDP Science,
2019, doi:10.1051/0004-6361/201834780.'
short: L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M.
Rendle, Astronomy & Astrophysics 624 (2019).
date_created: 2022-07-18T14:13:34Z
date_published: 2019-04-19T00:00:00Z
date_updated: 2024-10-14T11:39:57Z
day: '19'
doi: 10.1051/0004-6361/201834780
extern: '1'
external_id:
arxiv:
- '1902.09854'
intvolume: ' 624'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1902.09854
month: '04'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Science
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'FliPerClass: In search of solar-like pulsators among TESS targets'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 624
year: '2019'
...
---
_id: '13468'
abstract:
- lang: eng
text: Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class
of explosions observed following the collapse of the core of massive stars. We
used analytical estimates and population synthesis simulations to assess the fraction
of SNe II progenitors that are expected to have exchanged mass with a companion
prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history
of mass exchange with a binary companion before exploding. The dominant binary
channels leading to SN II progenitors involve the merger of binary stars. Mergers
are expected to produce a diversity of SN II progenitor characteristics, depending
on the evolutionary timing and properties of the merger. Alternatively, SN II
progenitors from interacting binaries may have accreted mass from their companion,
and subsequently been ejected from the binary system after their companion exploded.
We show that the overall fraction of SN II progenitors that are predicted to have
experienced binary interaction is robust against the main physical uncertainties
in our models. However, the relative importance of different binary evolutionary
channels is affected by changing physical assumptions. We further discuss ways
in which binarity might contribute to the observed diversity of SNe II by considering
potential observational signatures arising from each binary channel. For supernovae
which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb
SNe), a surviving non-compact companion would typically indicate that the supernova
progenitor star was in a wide, non-interacting binary. We argue that a significant
fraction of even Type II-P SNe are expected to have gained mass from a companion
prior to explosion.
article_number: A5
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Emmanouil
full_name: Zapartas, Emmanouil
last_name: Zapartas
- first_name: Selma E.
full_name: de Mink, Selma E.
last_name: de Mink
- first_name: Stephen
full_name: Justham, Stephen
last_name: Justham
- first_name: Nathan
full_name: Smith, Nathan
last_name: Smith
- first_name: Alex
full_name: de Koter, Alex
last_name: de Koter
- first_name: Mathieu
full_name: Renzo, Mathieu
last_name: Renzo
- first_name: Iair
full_name: Arcavi, Iair
last_name: Arcavi
- first_name: Rob
full_name: Farmer, Rob
last_name: Farmer
- 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: Silvia
full_name: Toonen, Silvia
last_name: Toonen
citation:
ama: 'Zapartas E, de Mink SE, Justham S, et al. The diverse lives of progenitors
of hydrogen-rich core-collapse supernovae: The role of binary interaction. Astronomy
& Astrophysics. 2019;631. doi:10.1051/0004-6361/201935854'
apa: 'Zapartas, E., de Mink, S. E., Justham, S., Smith, N., de Koter, A., Renzo,
M., … Toonen, S. (2019). The diverse lives of progenitors of hydrogen-rich core-collapse
supernovae: The role of binary interaction. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/201935854'
chicago: 'Zapartas, Emmanouil, Selma E. de Mink, Stephen Justham, Nathan Smith,
Alex de Koter, Mathieu Renzo, Iair Arcavi, Rob Farmer, Ylva Louise Linsdotter
Götberg, and Silvia Toonen. “The Diverse Lives of Progenitors of Hydrogen-Rich
Core-Collapse Supernovae: The Role of Binary Interaction.” Astronomy &
Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201935854.'
ieee: 'E. Zapartas et al., “The diverse lives of progenitors of hydrogen-rich
core-collapse supernovae: The role of binary interaction,” Astronomy &
Astrophysics, vol. 631. EDP Sciences, 2019.'
ista: 'Zapartas E, de Mink SE, Justham S, Smith N, de Koter A, Renzo M, Arcavi I,
Farmer R, Götberg YLL, Toonen S. 2019. The diverse lives of progenitors of hydrogen-rich
core-collapse supernovae: The role of binary interaction. Astronomy & Astrophysics.
631, A5.'
mla: 'Zapartas, Emmanouil, et al. “The Diverse Lives of Progenitors of Hydrogen-Rich
Core-Collapse Supernovae: The Role of Binary Interaction.” Astronomy &
Astrophysics, vol. 631, A5, EDP Sciences, 2019, doi:10.1051/0004-6361/201935854.'
short: E. Zapartas, S.E. de Mink, S. Justham, N. Smith, A. de Koter, M. Renzo, I.
Arcavi, R. Farmer, Y.L.L. Götberg, S. Toonen, Astronomy & Astrophysics 631
(2019).
date_created: 2023-08-03T10:13:52Z
date_published: 2019-11-20T00:00:00Z
date_updated: 2023-08-09T12:36:09Z
day: '20'
doi: 10.1051/0004-6361/201935854
extern: '1'
external_id:
arxiv:
- '1907.06687'
intvolume: ' 631'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201935854
month: '11'
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 diverse lives of progenitors of hydrogen-rich core-collapse supernovae:
The role of binary interaction'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 631
year: '2019'
...
---
_id: '13469'
abstract:
- lang: eng
text: Stars stripped of their envelopes from interaction with a binary companion
emit a significant fraction of their radiation as ionizing photons. They are potentially
important stellar sources of ionizing radiation, however, they are still often
neglected in spectral synthesis simulations or simulations of stellar feedback.
In anticipating the large datasets of galaxy spectra from the upcoming James Webb
Space Telescope, we modeled the radiative contribution from stripped stars by
using detailed evolutionary and spectral models. We estimated their impact on
the integrated spectra and specifically on the emission rates of H I-, He I-,
and He II-ionizing photons from stellar populations. We find that stripped stars
have the largest impact on the ionizing spectrum of a population in which star
formation halted several Myr ago. In such stellar populations, stripped stars
dominate the emission of ionizing photons, mimicking a younger stellar population
in which massive stars are still present. Our models also suggest that stripped
stars have harder ionizing spectra than massive stars. The additional ionizing
radiation, with which stripped stars contribute affects observable properties
that are related to the emission of ionizing photons from stellar populations.
In co-eval stellar populations, the ionizing radiation from stripped stars increases
the ionization parameter and the production efficiency of hydrogen ionizing photons.
They also cause high values for these parameters for about ten times longer than
what is predicted for massive stars. The effect on properties related to non-ionizing
wavelengths is less pronounced, such as on the ultraviolet continuum slope or
stellar contribution to emission lines. However, the hard ionizing radiation from
stripped stars likely introduces a characteristic ionization structure of the
nebula, which leads to the emission of highly ionized elements such as O2+ and
C3+. We, therefore, expect that the presence of stripped stars affects the location
in the BPT diagram and the diagnostic ratio of O III to O II nebular emission
lines. Our models are publicly available through CDS database and on the STARBURST99
website.
article_number: A134
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: J. H.
full_name: Groh, J. H.
last_name: Groh
- first_name: C.
full_name: Leitherer, C.
last_name: Leitherer
- first_name: C.
full_name: Norman, C.
last_name: Norman
citation:
ama: Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. The impact of stars
stripped in binaries on the integrated spectra of stellar populations. Astronomy
& Astrophysics. 2019;629. doi:10.1051/0004-6361/201834525
apa: Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Leitherer, C., & Norman,
C. (2019). The impact of stars stripped in binaries on the integrated spectra
of stellar populations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834525
chicago: Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, C. Leitherer,
and C. Norman. “The Impact of Stars Stripped in Binaries on the Integrated Spectra
of Stellar Populations.” Astronomy & Astrophysics. EDP Sciences, 2019.
https://doi.org/10.1051/0004-6361/201834525.
ieee: Y. L. L. Götberg, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman,
“The impact of stars stripped in binaries on the integrated spectra of stellar
populations,” Astronomy & Astrophysics, vol. 629. EDP Sciences, 2019.
ista: Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. 2019. The impact
of stars stripped in binaries on the integrated spectra of stellar populations.
Astronomy & Astrophysics. 629, A134.
mla: Götberg, Ylva Louise Linsdotter, et al. “The Impact of Stars Stripped in Binaries
on the Integrated Spectra of Stellar Populations.” Astronomy & Astrophysics,
vol. 629, A134, EDP Sciences, 2019, doi:10.1051/0004-6361/201834525.
short: Y.L.L. Götberg, S.E. de Mink, J.H. Groh, C. Leitherer, C. Norman, Astronomy
& Astrophysics 629 (2019).
date_created: 2023-08-03T10:14:00Z
date_published: 2019-09-17T00:00:00Z
date_updated: 2024-10-14T12:22:42Z
day: '17'
doi: 10.1051/0004-6361/201834525
extern: '1'
external_id:
arxiv:
- '1908.06102'
intvolume: ' 629'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201834525
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 impact of stars stripped in binaries on the integrated spectra of stellar
populations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 629
year: '2019'
...