---
_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: '11512'
abstract:
- lang: eng
text: We study the molecular gas content of 24 star-forming galaxies at z = 3–4,
with a median stellar mass of 109.1 M⊙, from the MUSE Hubble Ultra Deep Field
(HUDF) Survey. Selected by their Lyα λ1216 emission and HF160W-band magnitude,
the galaxies show an average $\langle {\mathrm{EW}}_{\mathrm{Ly}\alpha }^{0}\rangle
\approx 20$ Å, below the typical selection threshold for Lyα emitters (${\mathrm{EW}}_{\mathrm{Ly}\alpha
}^{0}\gt 25$ Å), and a rest-frame UV spectrum similar to Lyman-break galaxies.
We use rest-frame optical spectroscopy from KMOS and MOSFIRE, and the UV features
observed with MUSE, to determine the systemic redshifts, which are offset from
Lyα by 〈Δv(Lyα)〉 = 346 km s−1, with a 100 to 600 km s−1 range. Stacking 12CO J
= 4 → 3 and [C i]3P1 → 3P0 (and higher-J CO lines) from the ALMA Spectroscopic
Survey of the HUDF, we determine 3σ upper limits on the line luminosities of 4.0
× 108 K km s−1pc2 and 5.6 × 108 K km s−1pc2, respectively (for a 300 km s−1 line
width). Stacking the 1.2 mm and 3 mm dust-continuum flux densities, we find a
3σ upper limits of 9 μJy and 1.2 μJy, respectively. The inferred gas fractions,
under the assumption of a "Galactic" CO-to-H2 conversion factor and gas-to-dust
ratio, are in tension with previously determined scaling relations. This implies
a substantially higher αCO ≥ 10 and δGDR ≥ 1200, consistent with the subsolar
metallicity estimated for these galaxies ($12+\mathrm{log}({\rm{O}}/{\rm{H}})\approx
7.8\pm 0.2$). The low metallicity of z ≥ 3 star-forming galaxies may thus make
it very challenging to unveil their cold gas through CO or dust emission, warranting
further exploration of alternative tracers, such as [C ii].
acknowledgement: 'We would like to thank the referee for a constructive and helpful
report. L.A.B. is grateful to Corentin Schreiber for assisting with the near-infrared
spectroscopy during the early stages of this work. L.A.B. acknowledges support from
the Leids Kerkhoven-Bosscha Fonds under subsidy numbers 18.2.074 and 19.1.147. D.R.
acknowledges support from the National Science Foundation under grant numbers AST-1614213
and AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt
Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.F.
acknowledges the support from grant PRIN MIUR 201720173ML3WW_001. J.B. 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. H.I. acknowledges support
from JSPS KAKENHI grant No. JP19K23462. This work is based on observations collected
at the European Southern Observatory under ESO programs 094.A-2089(B), 095.A-0010(A),
096.A-0045(A), 096.A-0045(B), 099.A-0858(A), and 0101.A-0725(A). This paper makes
use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership
of ESO (representing its member states), NSF (USA), and NINS (Japan), together with
NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation
with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO,
and NAOJ. The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated Universities,
Inc. This work was supported by a NASA Keck PI Data Award, administered by the NASA
Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck
Observatory from telescope time allocated to the National Aeronautics and Space
Administration through the agency''s scientific partnership with the California
Institute of Technology and the University of California. The Observatory was made
possible by the generous financial support of the W. M. Keck Foundation. The authors
wish to recognize and acknowledge the very significant cultural role and reverence
that the summit of Maunakea has always had within the indigenous Hawaiian community.
We are most fortunate to have the opportunity to conduct observations from this
mountain.'
article_number: '12'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Rychard J.
full_name: Bouwens, Rychard J.
last_name: Bouwens
- first_name: Dominik
full_name: Riechers, Dominik
last_name: Riechers
- first_name: Paul
full_name: van der Werf, Paul
last_name: van der Werf
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- 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: Mauro
full_name: Stefanon, Mauro
last_name: Stefanon
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Manuel
full_name: Aravena, Manuel
last_name: Aravena
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Chris
full_name: Carilli, Chris
last_name: Carilli
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Roberto
full_name: Decarli, Roberto
last_name: Decarli
- first_name: Jorge
full_name: González-López, Jorge
last_name: González-López
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Fabian
full_name: Walter, Fabian
last_name: Walter
citation:
ama: Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular
gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal.
2021;916(1). doi:10.3847/1538-4357/ac01d7
apa: Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R.,
Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content
of star-forming galaxies at z = 3–4. The Astrophysical Journal. IOP Publishing.
https://doi.org/10.3847/1538-4357/ac01d7
chicago: Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der
Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average
Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” The Astrophysical
Journal. IOP Publishing, 2021. https://doi.org/10.3847/1538-4357/ac01d7.
ieee: L. A. Boogaard et al., “Measuring the average molecular gas content
of star-forming galaxies at z = 3–4,” The Astrophysical Journal, vol. 916,
no. 1. IOP Publishing, 2021.
ista: Boogaard LA, Bouwens RJ, Riechers D, van der Werf P, Bacon R, Matthee JJ,
Stefanon M, Feltre A, Maseda M, Inami H, Aravena M, Brinchmann J, Carilli C, Contini
T, Decarli R, González-López J, Nanayakkara T, Walter F. 2021. Measuring the average
molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal.
916(1), 12.
mla: Boogaard, Leindert A., et al. “Measuring the Average Molecular Gas Content
of Star-Forming Galaxies at z = 3–4.” The Astrophysical Journal, vol. 916,
no. 1, 12, IOP Publishing, 2021, doi:10.3847/1538-4357/ac01d7.
short: L.A. Boogaard, R.J. Bouwens, D. Riechers, P. van der Werf, R. Bacon, J.J.
Matthee, M. Stefanon, A. Feltre, M. Maseda, H. Inami, M. Aravena, J. Brinchmann,
C. Carilli, T. Contini, R. Decarli, J. González-López, T. Nanayakkara, F. Walter,
The Astrophysical Journal 916 (2021).
date_created: 2022-07-06T13:05:50Z
date_published: 2021-07-20T00:00:00Z
date_updated: 2022-07-19T09:32:48Z
day: '20'
doi: 10.3847/1538-4357/ac01d7
extern: '1'
external_id:
arxiv:
- '2105.12489'
intvolume: ' 916'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2105.12489
month: '07'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Measuring the average molecular gas content of star-forming galaxies at z =
3–4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 916
year: '2021'
...
---
_id: '11522'
abstract:
- lang: eng
text: The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a
powerful and commonly used probe to constrain the progress of cosmic reionization.
We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring
a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties
of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm
previous studies, i.e. we find a declining Lyα transmission with redshift and
a large sightline-to-sightline variation. However, motivated by the recent discovery
of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the
blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This
low transmission can be attributed not only to the presence of neutral regions
but also to the residual neutral hydrogen within ionized regions, for which a
density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects)
leads to a significantly reduced visibility. Still, we find that ∼1 per cent of
sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow
a transmission of a blue Lyα peak. We discuss our results in the context of the
interpretation of observations.
acknowledgement: The authors thank the referee for constructive feedback that improved
the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing
the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics
Data System, and many open source projects such as trident (Hummels et al. 2017),
IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al.
2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk
et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant
HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., for NASA, under
contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017,
and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support
by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A.
PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G,
and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced
Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a
Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER
under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
programme (grant agreement No. 669253). ITI was supported by the Science and Technology
Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1];
and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414
and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion
of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016).
ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001
(EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak
Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award
AST031). Processing was performed on the Eos and Rhea clusters. Resolution study
simulations were performed on Piz Daint at the Swiss National Supercomputing Center
(PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the
High Performance Computing center of the University of Strasbourg for supporting
this work by providing scientific support and access to computing resources. Part
of the computing resources were funded by the Equipex EquipMeso project (Programme
Investissements d’Avenir) and the CPER Alsacalcul/Big Data.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Pierre
full_name: Ocvirk, Pierre
last_name: Ocvirk
- first_name: Charlotte
full_name: Mason, Charlotte
last_name: Mason
- 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: Sarah E I
full_name: Bosman, Sarah E I
last_name: Bosman
- first_name: Jenny G
full_name: Sorce, Jenny G
last_name: Sorce
- first_name: Joseph
full_name: Lewis, Joseph
last_name: Lewis
- first_name: Kyungjin
full_name: Ahn, Kyungjin
last_name: Ahn
- first_name: Dominique
full_name: Aubert, Dominique
last_name: Aubert
- first_name: Taha
full_name: Dawoodbhoy, Taha
last_name: Dawoodbhoy
- first_name: Ilian T
full_name: Iliev, Ilian T
last_name: Iliev
- first_name: Paul R
full_name: Shapiro, Paul R
last_name: Shapiro
- first_name: Gustavo
full_name: Yepes, Gustavo
last_name: Yepes
citation:
ama: Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the
intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal
Astronomical Society. 2021;508(3):3697-3709. doi:10.1093/mnras/stab2762
apa: Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce,
J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic
medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2762
chicago: Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E
I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties
of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the
Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2762.
ieee: M. Gronke et al., “Lyman-α transmission properties of the intergalactic
medium in the CoDaII simulation,” Monthly Notices of the Royal Astronomical
Society, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.
ista: Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn
K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission
properties of the intergalactic medium in the CoDaII simulation. Monthly Notices
of the Royal Astronomical Society. 508(3), 3697–3709.
mla: Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium
in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society,
vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:10.1093/mnras/stab2762.
short: M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce,
J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes,
Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.
date_created: 2022-07-07T09:30:21Z
date_published: 2021-12-01T00:00:00Z
date_updated: 2022-08-18T10:45:56Z
day: '01'
doi: 10.1093/mnras/stab2762
extern: '1'
external_id:
arxiv:
- '2004.14496'
intvolume: ' 508'
issue: '3'
keyword:
- dark ages
- reionization
- first stars
- intergalactic medium
- 'galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2004.14496
month: '12'
oa: 1
oa_version: Preprint
page: 3697-3709
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 508
year: '2021'
...
---
_id: '11523'
abstract:
- lang: eng
text: We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2).
XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing
≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame
Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations,
and the data reduction. Systemic redshifts are measured from rest-frame optical
lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by
an interstellar medium with little dust, a low metallicity, and a high ionization
state. The ionizing sources are young hot stars that power strong emission lines
in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit
clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption,
a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent
of the Ly α photons escape, of which one quarter on the blue side of the systemic
velocity. A fraction of Ly α photons escape directly at the systemic suggesting
clear channels enabling an ≈10 per cent escape of ionizing photons, consistent
with an inference based on Mg II. A combination of a low effective H I column
density, a low dust content, and young starburst determines whether a star-forming
galaxy is observed as an LAE. The first is possibly related to outflows and/or
a fortunate viewing angle, while we find that the latter two in LAEs are typical
for their stellar mass of 109 M⊙.
acknowledgement: "We thank the referee for constructive comments and suggestions.
We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for
useful discussions and suggestions. It is a pleasure to thank the ESO User Support,
in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and
Lowell Tacconi-Garman for assistance in the preparation and execution of the observations.
Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413,
091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779,
and 102.A-0652. Based on data products from observations made with ESO Telescopes
at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data
products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of
the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through
programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive,
which is a collaboration between the Space Telescope Science Institute (STScI/NASA),
the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian
Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by
the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated
by the Association of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409
and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A,
and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research
School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular
Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY,
MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert
& Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013)
packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of
A. C. J.Matthee (1953–2020)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Matthew
full_name: Hayes, Matthew
last_name: Hayes
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Rohan P
full_name: Naidu, Rohan P
last_name: Naidu
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Ricardo
full_name: Amorín, Ricardo
last_name: Amorín
citation:
ama: 'Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z =
2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the
Royal Astronomical Society. 2021;505(1):1382-1412. doi:10.1093/mnras/stab1304'
apa: 'Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer,
D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What
makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1304'
chicago: 'Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max
Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at
z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of
the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1304.'
ieee: 'J. J. Matthee et al., “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2)
I: What makes a galaxy a Lyman α emitter?,” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.'
ista: 'Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP,
Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER
Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly
Notices of the Royal Astronomical Society. 505(1), 1382–1412.'
mla: 'Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2)
I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:10.1093/mnras/stab1304.'
short: J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P.
Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly
Notices of the Royal Astronomical Society 505 (2021) 1382–1412.
date_created: 2022-07-07T09:33:39Z
date_published: 2021-07-01T00:00:00Z
date_updated: 2022-08-18T10:49:00Z
day: '01'
doi: 10.1093/mnras/stab1304
extern: '1'
external_id:
arxiv:
- '2102.07779'
intvolume: ' 505'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: formation'
- 'galaxies: ISM'
- 'galaxies: starburst'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.07779
month: '07'
oa: 1
oa_version: Preprint
page: 1382-1412
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman
α emitter?'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 505
year: '2021'
...
---
_id: '11524'
abstract:
- lang: eng
text: We measure the evolution of the rest-frame UV luminosity function (LF) and
the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to
z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between
Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11
and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8.
An increasing LLy α cut predominantly lowers the number density of faint MUV and
low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple
assumptions of the faint end slope. For the UV LF, we find a brightening of the
characteristic UV luminosity (M∗UV) with increasing redshift and a decrease of
the characteristic number density (Φ*). For the SMF, we measure a characteristic
stellar mass (M∗⋆/M⊙) increase with increasing redshift, and a Φ* decline. However,
if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0, we find much
milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV)
of the full sample of LAEs shows moderate evolution and the stellar mass density
(ρM) decreases, with both being always lower than the total ρUV and ρM of more
typical galaxies but slowly approaching them with increasing redshift. Overall,
our results indicate that both ρUV and ρM of LAEs slowly approach the measurements
of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in
the epoch of reionization.
acknowledgement: This research made use of Astropy, a community developed core Python
package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool
for manipulating tabular data, was also utilized in this analysis (Taylor 2005).
SG would like to thank Nastasha Wijers for the discussion on the column density
distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science
Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
grant agreement No 864361. GP acknowledges support from the Swiss National Science
Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
full_name: Santos, S
last_name: Santos
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: J
full_name: Butterworth, J
last_name: Butterworth
- first_name: A
full_name: Paulino-Afonso, A
last_name: Paulino-Afonso
- first_name: B
full_name: Ribeiro, B
last_name: Ribeiro
- first_name: E
full_name: da Cunha, E
last_name: da Cunha
- first_name: J
full_name: Calhau, J
last_name: Calhau
- first_name: A A
full_name: Khostovan, A A
last_name: Khostovan
- 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: P
full_name: Arrabal Haro, P
last_name: Arrabal Haro
citation:
ama: Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity
and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly
Notices of the Royal Astronomical Society. 2021;505(1):1117-1134. doi:10.1093/mnras/stab1218
apa: Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha,
E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar
mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of
the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1218
chicago: Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha,
J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution
of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2
to z ∼ 6.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2021. https://doi.org/10.1093/mnras/stab1218.
ieee: S. Santos et al., “The evolution of the UV luminosity and stellar mass
functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” Monthly Notices of the
Royal Astronomical Society, vol. 505, no. 1. Oxford University Press, pp.
1117–1134, 2021.
ista: Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E,
Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the
UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼
6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.
mla: Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions
of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:10.1093/mnras/stab1218.
short: S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha,
J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the
Royal Astronomical Society 505 (2021) 1117–1134.
date_created: 2022-07-07T10:02:59Z
date_published: 2021-07-01T00:00:00Z
date_updated: 2022-08-18T10:51:47Z
day: '01'
doi: 10.1093/mnras/stab1218
extern: '1'
external_id:
arxiv:
- '2105.00007'
intvolume: ' 505'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2105.00007
month: '07'
oa: 1
oa_version: Preprint
page: 1117-1134
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters
from z ∼ 2 to z ∼ 6
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 505
year: '2021'
...
---
_id: '11525'
abstract:
- lang: eng
text: The intensity of the Cosmic UV background (UVB), coming from all sources of
ionizing photons such as star-forming galaxies and quasars, determines the thermal
evolution and ionization state of the intergalactic medium (IGM) and is, therefore,
a critical ingredient for models of cosmic structure formation. Most of the previous
estimates are based on the comparison between observed and simulated Lyman-α forest.
We present the results of an independent method to constrain the product of the
UVB photoionization rate and the covering fraction of Lyman limit systems (LLSs)
by searching for the fluorescent Lyman-α emission produced by self-shielded clouds.
Because the expected surface brightness is well below current sensitivity limits
for direct imaging, we developed a new method based on 3D stacking of the IGM
around Lyman-α emitting galaxies (LAEs) between 2.9 < z < 6.6 using deep MUSE
observations. Combining our results with covering fractions of LLSs obtained from
mock cubes extracted from the EAGLE simulation, we obtain new and independent
constraints on the UVB at z > 3 that are consistent with previous measurements,
with a preference for relatively low UVB intensities at z = 3, and which suggest
a non-monotonic decrease of ΓH I with increasing redshift between 3 < z < 5. This
could suggest a possible tension between some UVB models and current observations
which however require deeper and wider observations in Lyman-α emission and absorption
to be confirmed. Assuming instead a value of UVB from current models, our results
constrain the covering fraction of LLSs at 3 < z < 4.5 to be less than 25 per cent
within 150 kpc from LAEs.
acknowledgement: This research made use of Astropy, a community developed core Python
package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool
for manipulating tabular data, was also utilized in this analysis (Taylor 2005).
SG would like to thank Nastasha Wijers for the discussion on the column density
distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science
Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
grant agreement No 864361. GP acknowledges support from the Swiss National Science
Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sofia G
full_name: Gallego, Sofia G
last_name: Gallego
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Saeed
full_name: Sarpas, Saeed
last_name: Sarpas
- first_name: Bastien
full_name: Duboeuf, Bastien
last_name: Duboeuf
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
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: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Valentin
full_name: Mauerhofer, Valentin
last_name: Mauerhofer
citation:
ama: Gallego SG, Cantalupo S, Sarpas S, et al. Constraining the cosmic UV background
at z > 3 with MUSE Lyman-α emission observations. Monthly Notices of the
Royal Astronomical Society. 2021;504(1):16-32. doi:10.1093/mnras/stab796
apa: Gallego, S. G., Cantalupo, S., Sarpas, S., Duboeuf, B., Lilly, S., Pezzulli,
G., … Mauerhofer, V. (2021). Constraining the cosmic UV background at z >
3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab796
chicago: Gallego, Sofia G, Sebastiano Cantalupo, Saeed Sarpas, Bastien Duboeuf,
Simon Lilly, Gabriele Pezzulli, Raffaella Anna Marino, et al. “Constraining the
Cosmic UV Background at z > 3 with MUSE Lyman-α Emission Observations.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2021.
https://doi.org/10.1093/mnras/stab796.
ieee: S. G. Gallego et al., “Constraining the cosmic UV background at z >
3 with MUSE Lyman-α emission observations,” Monthly Notices of the Royal Astronomical
Society, vol. 504, no. 1. Oxford University Press, pp. 16–32, 2021.
ista: Gallego SG, Cantalupo S, Sarpas S, Duboeuf B, Lilly S, Pezzulli G, Marino
RA, Matthee JJ, Wisotzki L, Schaye J, Richard J, Kusakabe H, Mauerhofer V. 2021.
Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission
observations. Monthly Notices of the Royal Astronomical Society. 504(1), 16–32.
mla: Gallego, Sofia G., et al. “Constraining the Cosmic UV Background at z >
3 with MUSE Lyman-α Emission Observations.” Monthly Notices of the Royal Astronomical
Society, vol. 504, no. 1, Oxford University Press, 2021, pp. 16–32, doi:10.1093/mnras/stab796.
short: S.G. Gallego, S. Cantalupo, S. Sarpas, B. Duboeuf, S. Lilly, G. Pezzulli,
R.A. Marino, J.J. Matthee, L. Wisotzki, J. Schaye, J. Richard, H. Kusakabe, V.
Mauerhofer, Monthly Notices of the Royal Astronomical Society 504 (2021) 16–32.
date_created: 2022-07-07T10:07:11Z
date_published: 2021-06-01T00:00:00Z
date_updated: 2022-08-18T10:54:19Z
day: '01'
doi: 10.1093/mnras/stab796
extern: '1'
external_id:
arxiv:
- '2103.09250'
intvolume: ' 504'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2103.09250
month: '06'
oa: 1
oa_version: Preprint
page: 16-32
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 504
year: '2021'
...
---
_id: '11526'
abstract:
- lang: eng
text: We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which
were selected to be much fainter (20 < iSDSS < 23) than in previous studies of
giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect
H I Ly α nebulae around 100 per cent of our target quasars, with emission extending
to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations
between properties of the nebulae and their host quasars, with the goal of connecting
variations in the properties of the illuminating QSO to the response in nebular
emission. We show that the surface brightness profiles of the nebulae are similar
to those of nebulae around bright quasars, but with a lower normalization. Our
targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than
our bright reference sample, and yet the nebulae around them are only 4.3 times
fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find
significant correlations between the surface brightness of the nebula and the
luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted
as evidence for a substantial contribution from unresolved inner parts of the
nebulae to the narrow components seen in the Ly α lines of some of our faint quasars,
possibly from the inner circumgalactic medium or from the host galaxy’s interstellar
medium.
acknowledgement: The authors thank Daichi Kashino, for providing access to unpublished
zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al.
(2020). GP and SC acknowledge the support of the Swiss National Science Foundation
[grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship,
Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected
at the European Organisation for Astronomical Research in the Southern Hemisphere
under the MUSE GTO programme. The major analysis and production of figures in this
work was conducted in Python, using standard libraries which include NumPy (Harris
et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive
command shell IPython (Pérez & Granger 2007). This research also made use of Astropy,
a community-developed core Python package for Astronomy (Astropy Collaboration et
al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica
sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used
to query galactic extinction maps. topcat, a graphical tool for manipulating tabular
data, was also utilized in this analysis (Taylor 2005). This research has made use
of the "Aladin sky atlas" developed at CDS, Strasbourg Observatory, France (Bonnarel
et al. 2000).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Raffaella A
full_name: Marino, Raffaella A
last_name: Marino
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Sowgat
full_name: Muzahid, Sowgat
last_name: Muzahid
- 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: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar
luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical
Society. 2021;502(1):494-509. doi:10.1093/mnras/staa3277
apa: Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid,
S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant
Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford
University Press. https://doi.org/10.1093/mnras/staa3277
chicago: Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A
Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki.
“Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/staa3277.
ieee: R. Mackenzie et al., “Revealing the impact of quasar luminosity on
giant Lyα nebulae,” Monthly Notices of the Royal Astronomical Society,
vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.
ista: Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee
JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant
Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.
mla: Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant
Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society, vol. 502,
no. 1, Oxford University Press, 2021, pp. 494–509, doi:10.1093/mnras/staa3277.
short: R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid,
J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical
Society 502 (2021) 494–509.
date_created: 2022-07-07T10:11:15Z
date_published: 2021-03-01T00:00:00Z
date_updated: 2022-08-18T10:56:28Z
day: '01'
doi: 10.1093/mnras/staa3277
extern: '1'
external_id:
arxiv:
- '2010.12589'
intvolume: ' 502'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'techniques: imaging spectroscopy'
- intergalactic medium
- 'quasars: emission lines'
- 'quasars: general'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2010.12589
month: '03'
oa: 1
oa_version: Preprint
page: 494-509
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Revealing the impact of quasar luminosity on giant Lyα nebulae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 502
year: '2021'
...
---
_id: '11585'
abstract:
- lang: eng
text: "Observations show that star-forming galaxies reside on a tight three-dimensional
plane between mass, gas-phase metallicity and star formation rate (SFR), which
can be explained by the interplay between metal-poor gas inflows, SFR and outflows.
However, different metals are released on different time-scales, which may affect
the slope of this relation. Here, we use central, star-forming galaxies with Mstar
= 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional
relations between mass, SFR and chemical enrichment using absolute and relative
C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase
α-enhancement is used rather than metallicity. A similar plane also exists for
stellar α-enhancement, implying that present-day specific SFRs are correlated
with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement
plane is even more insensitive to redshift than the plane using metallicity. However,
it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher
SFRs have star formation histories shifted toward late times, are more α-enhanced
and this α-enhancement increases with redshift as observed. These findings suggest
that relations between physical properties inferred from observations may be affected
by systematic variations in α-enhancements."
acknowledgement: We thank the anonymous referee for their constructive comments. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. We
thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
the use of the Topcat software (Taylor 2013) for assisting in rapid exploration
of multi-dimensional datasets and the use of Python and its numpy, matplotlib and
pandas packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Matthee JJ. Differences in galaxy colours are not just about the mass. Nature
Astronomy. 2021;5:984-985. doi:10.1038/s41550-021-01415-y
apa: Matthee, J. J. (2021). Differences in galaxy colours are not just about the
mass. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-021-01415-y
chicago: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the
Mass.” Nature Astronomy. Springer Nature, 2021. https://doi.org/10.1038/s41550-021-01415-y.
ieee: J. J. Matthee, “Differences in galaxy colours are not just about the mass,”
Nature Astronomy, vol. 5. Springer Nature, pp. 984–985, 2021.
ista: Matthee JJ. 2021. Differences in galaxy colours are not just about the mass.
Nature Astronomy. 5, 984–985.
mla: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.”
Nature Astronomy, vol. 5, Springer Nature, 2021, pp. 984–85, doi:10.1038/s41550-021-01415-y.
short: J.J. Matthee, Nature Astronomy 5 (2021) 984–985.
date_created: 2022-07-14T13:13:39Z
date_published: 2021-07-05T00:00:00Z
date_updated: 2022-08-19T08:37:58Z
day: '05'
doi: 10.1038/s41550-021-01415-y
extern: '1'
external_id:
arxiv:
- '1802.06786'
intvolume: ' 5'
keyword:
- Astronomy and Astrophysics
- galaxies
- formation - galaxies
- evolution - galaxies
- star formation - galaxies
- abundances
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.06786
month: '07'
oa: 1
oa_version: Preprint
page: 984-985
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Differences in galaxy colours are not just about the mass
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 5
year: '2021'
...
---
_id: '11604'
abstract:
- lang: eng
text: The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of
millions of stars with time spans ranging from ∼27 days to about 1 yr of continuous
observations. This vast amount of data contains a wealth of information for variability,
exoplanet, and stellar astrophysics studies but requires a number of processing
steps before it can be fully utilized. In order to efficiently process all the
TESS data and make it available to the wider scientific community, the TESS Data
for Asteroseismology working group, as part of the TESS Asteroseismic Science
Consortium, has created an automated open-source processing pipeline to produce
light curves corrected for systematics from the short- and long-cadence raw photometry
data and to classify these according to stellar variability type. We will process
all stars down to a TESS magnitude of 15. This paper is the next in a series detailing
how the pipeline works. Here, we present our methodology for the automatic variability
classification of TESS photometry using an ensemble of supervised learners that
are combined into a metaclassifier. We successfully validate our method using
a carefully constructed labeled sample of Kepler Q9 light curves with a 27.4 days
time span mimicking single-sector TESS observations, on which we obtain an overall
accuracy of 94.9%. We demonstrate that our methodology can successfully classify
stars outside of our labeled sample by applying it to all ∼167,000 stars observed
in Q9 of the Kepler space mission.
acknowledgement: "The research leading to these results has received funding from
the European Research Council (ERC) under the European Union's Horizon 2020 research
and innovation program (grant agreement No. 670519: MAMSIE), from the KU Leuven
Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders
(FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the
BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. D.J.A
acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1).
Funding for the Stellar Astrophysics Centre is provided by The Danish National Research
Foundation (grant agreement No.: DNRF106). R.H. and M.N.L. acknowledge the ESA PRODEX
program. This research was supported by the National Aeronautics and Space Administration
(80NSSC18K1585 and 80NSSC19K0379) awarded through the TESS Guest Investigator Program.
K.J.B. is supported by the National Science Foundation under Award AST-1903828.
J.S.K and K.J.B. were supported by funding from the European Research Council under
the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement
no. 338251 (StellarAges). D.M.B. gratefully acknowledges funding from a senior postdoctoral
fellowship from the Research Foundation Flanders (FWO) with grant agreement No.
1286521N. The research leading to these results has received funding from the Research
Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM). R.A.G. acknowledges
support from the GOLF and PLATO CNES grants. L.M. was supported by the Premium Postdoctoral
Research Program of the Hungarian Academy of Sciences. The research leading to these
results has been supported by the Hungarian National Research, Development, and
Innovation Office (NKFIH) grant KH_18 130405 and the Lendület LP2014-17 and LP2018-7/2020
grants of the Hungarian Academy of Sciences. D.B. acknowledges support from the
NASA TESS Guest Investigator Program under award 80NSSC19K0385.\r\n\r\nThis paper
includes data collected by the TESS mission, which are publicly available from the
Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided
by NASA's Science Mission directorate. This research has made use of NASA's Astrophysics
Data System as well as the NASA/IPAC Extragalactic Database (NED) which is operated
by the Jet Propulsion Laboratory, California Institute of Technology, under contract
with the National Aeronautics and Space Administration. Funding for the TESS Asteroseismic
Science Operations Centre is provided by the Danish National Research Foundation
(Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and the Stellar Astrophysics
Centre (SAC) at Aarhus University. We thank the TESS team and staff and TASC/TASOC
for their support of the present work.\r\n\r\nThis paper includes data collected
by the Kepler mission. Funding for the Kepler and K2 mission was provided by NASA's
Science Mission Directorate. The authors acknowledge the efforts of the Kepler Mission
team in obtaining the light-curve data and data validation products used in this
publication. These data were generated by the Kepler Mission science pipeline through
the efforts of the Kepler Science Operations Center and Science Office. The Kepler
light curves are archived at the Mikulski Archive for Space Telescopes.\r\n\r\nThe
numerical results presented in this work were obtained at the Centre for Scientific
Computing, Aarhus. 37 This research made use of Astropy, a community-developed core
Python package for Astronomy (Astropy Collaboration et al. 2013, 2018).\r\n\r\nSoftware:
Scikit-learn (Pedregosa et al. 2011), Numpy (Harris et al. 2020), Astropy (Astropy
Collaboration et al. 2013, 2018), Scipy (Virtanen et al. 2020), Pandas (McKinney
2010; Pandas Development Team 2020), Lightkurve (Lightkurve Collaboration et al.
2018), XGBoost (Chen & Guestrin 2016), Tensorflow (Abadi et al. 2015)."
article_number: '209'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Audenaert, J.
last_name: Audenaert
- first_name: J. S.
full_name: Kuszlewicz, J. S.
last_name: Kuszlewicz
- first_name: R.
full_name: Handberg, R.
last_name: Handberg
- first_name: A.
full_name: Tkachenko, A.
last_name: Tkachenko
- first_name: D. J.
full_name: Armstrong, D. J.
last_name: Armstrong
- first_name: M.
full_name: Hon, M.
last_name: Hon
- first_name: R.
full_name: Kgoadi, R.
last_name: Kgoadi
- first_name: M. N.
full_name: Lund, M. N.
last_name: Lund
- first_name: K. J.
full_name: Bell, K. J.
last_name: Bell
- 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: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: C.
full_name: Johnston, C.
last_name: Johnston
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: D.
full_name: Stello, D.
last_name: Stello
- first_name: L.
full_name: Molnár, L.
last_name: Molnár
- first_name: E.
full_name: Plachy, E.
last_name: Plachy
- first_name: D.
full_name: Buzasi, D.
last_name: Buzasi
- first_name: C.
full_name: Aerts, C.
last_name: Aerts
citation:
ama: 'Audenaert J, Kuszlewicz JS, Handberg R, et al. TESS Data for Asteroseismology
(T’DA) stellar variability classification pipeline: Setup and application to the
Kepler Q9 data. The Astronomical Journal. 2021;162(5). doi:10.3847/1538-3881/ac166a'
apa: 'Audenaert, J., Kuszlewicz, J. S., Handberg, R., Tkachenko, A., Armstrong,
D. J., Hon, M., … Aerts, C. (2021). TESS Data for Asteroseismology (T’DA) stellar
variability classification pipeline: Setup and application to the Kepler Q9 data.
The Astronomical Journal. IOP Publishing. https://doi.org/10.3847/1538-3881/ac166a'
chicago: 'Audenaert, J., J. S. Kuszlewicz, R. Handberg, A. Tkachenko, D. J. Armstrong,
M. Hon, R. Kgoadi, et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability
Classification Pipeline: Setup and Application to the Kepler Q9 Data.” The
Astronomical Journal. IOP Publishing, 2021. https://doi.org/10.3847/1538-3881/ac166a.'
ieee: 'J. Audenaert et al., “TESS Data for Asteroseismology (T’DA) stellar
variability classification pipeline: Setup and application to the Kepler Q9 data,”
The Astronomical Journal, vol. 162, no. 5. IOP Publishing, 2021.'
ista: 'Audenaert J, Kuszlewicz JS, Handberg R, Tkachenko A, Armstrong DJ, Hon M,
Kgoadi R, Lund MN, Bell KJ, Bugnet LA, Bowman DM, Johnston C, García RA, Stello
D, Molnár L, Plachy E, Buzasi D, Aerts C. 2021. TESS Data for Asteroseismology
(T’DA) stellar variability classification pipeline: Setup and application to the
Kepler Q9 data. The Astronomical Journal. 162(5), 209.'
mla: 'Audenaert, J., et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability
Classification Pipeline: Setup and Application to the Kepler Q9 Data.” The
Astronomical Journal, vol. 162, no. 5, 209, IOP Publishing, 2021, doi:10.3847/1538-3881/ac166a.'
short: J. Audenaert, J.S. Kuszlewicz, R. Handberg, A. Tkachenko, D.J. Armstrong,
M. Hon, R. Kgoadi, M.N. Lund, K.J. Bell, L.A. Bugnet, D.M. Bowman, C. Johnston,
R.A. García, D. Stello, L. Molnár, E. Plachy, D. Buzasi, C. Aerts, The Astronomical
Journal 162 (2021).
date_created: 2022-07-18T11:54:55Z
date_published: 2021-10-21T00:00:00Z
date_updated: 2022-08-19T10:01:56Z
day: '21'
doi: 10.3847/1538-3881/ac166a
extern: '1'
external_id:
arxiv:
- '2107.06301'
intvolume: ' 162'
issue: '5'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2107.06301
month: '10'
oa: 1
oa_version: Preprint
publication: The Astronomical Journal
publication_identifier:
eissn:
- 1538-3881
issn:
- 0004-6256
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline:
Setup and application to the Kepler Q9 data'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 162
year: '2021'
...
---
_id: '11605'
abstract:
- lang: eng
text: "Context. The discovery of moderate differential rotation between the core
and the envelope of evolved solar-like stars could be the signature of a strong
magnetic field trapped inside the radiative interior. The population of intermediate-mass
red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation
modes that behave as acoustic modes in their external envelope and as gravity
modes in their core) could also arise from the effect of an internal magnetic
field. Indeed, stars more massive than about 1.1 solar masses are known to develop
a convective core during their main sequence. The field generated by the dynamo
triggered by this convection could be the progenitor of a strong fossil magnetic
field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims.
Observations of mixed modes can constitute an excellent probe of the deepest layers
of evolved solar-like stars, and magnetic fields in those regions can impact their
propagation. The magnetic perturbation on mixed modes may therefore be visible
in asteroseismic data. To unravel which constraints can be obtained from observations,
we theoretically investigate the effects of a plausible mixed axisymmetric magnetic
field with various amplitudes on the mixed-mode frequencies of evolved solar-like
stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric
magnetic field were computed for dipolar and quadrupolar mixed modes. These computations
were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions.
We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the
presence of a dynamo in the convective core during the main sequence, provoke
significant asymmetries on mixed-mode frequency multiplets during the red giant
branch. We provide constraints and methods for the detectability of such magnetic
signatures. We show that these signatures may be detectable in asteroseismic data
for field amplitudes small enough for the amplitude of the modes not to be affected
by the conversion of gravity into Alfvén waves inside the magnetised interior.
Finally, we infer an upper limit for the strength of the field and the associated
lower limit for the timescale of its action in order to redistribute angular momentum
in stellar interiors."
article_number: A53
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: V.
full_name: Prat, V.
last_name: Prat
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: A.
full_name: Astoul, A.
last_name: Astoul
- first_name: K.
full_name: Augustson, K.
last_name: Augustson
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: L.
full_name: Amard, L.
last_name: Amard
- first_name: C.
full_name: Neiner, C.
last_name: Neiner
citation:
ama: 'Bugnet LA, Prat V, Mathis S, et al. Magnetic signatures on mixed-mode frequencies:
I. An axisymmetric fossil field inside the core of red giants. Astronomy &
Astrophysics. 2021;650. doi:10.1051/0004-6361/202039159'
apa: 'Bugnet, L. A., Prat, V., Mathis, S., Astoul, A., Augustson, K., García, R.
A., … Neiner, C. (2021). Magnetic signatures on mixed-mode frequencies: I. An
axisymmetric fossil field inside the core of red giants. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202039159'
chicago: 'Bugnet, Lisa Annabelle, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.
A. García, S. Mathur, L. Amard, and C. Neiner. “Magnetic Signatures on Mixed-Mode
Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” Astronomy
& Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039159.'
ieee: 'L. A. Bugnet et al., “Magnetic signatures on mixed-mode frequencies:
I. An axisymmetric fossil field inside the core of red giants,” Astronomy &
Astrophysics, vol. 650. EDP Sciences, 2021.'
ista: 'Bugnet LA, Prat V, Mathis S, Astoul A, Augustson K, García RA, Mathur S,
Amard L, Neiner C. 2021. Magnetic signatures on mixed-mode frequencies: I. An
axisymmetric fossil field inside the core of red giants. Astronomy & Astrophysics.
650, A53.'
mla: 'Bugnet, Lisa Annabelle, et al. “Magnetic Signatures on Mixed-Mode Frequencies:
I. An Axisymmetric Fossil Field inside the Core of Red Giants.” Astronomy &
Astrophysics, vol. 650, A53, EDP Sciences, 2021, doi:10.1051/0004-6361/202039159.'
short: L.A. Bugnet, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.A. García, S.
Mathur, L. Amard, C. Neiner, Astronomy & Astrophysics 650 (2021).
date_created: 2022-07-18T12:10:59Z
date_published: 2021-06-07T00:00:00Z
date_updated: 2022-08-19T10:06:33Z
day: '07'
doi: 10.1051/0004-6361/202039159
extern: '1'
external_id:
arxiv:
- '2102.01216'
intvolume: ' 650'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- stars
- oscillations / stars
- magnetic field / stars
- interiors / stars
- evolution / stars
- rotation
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.01216
month: '06'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field
inside the core of red giants'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 650
year: '2021'
...
---
_id: '11606'
abstract:
- lang: eng
text: "Context. Our knowledge of the dynamics of stars has undergone a revolution
through the simultaneous large amount of high-quality photometric observations
collected by space-based asteroseismology and ground-based high-precision spectropolarimetry.
They allowed us to probe the internal rotation of stars and their surface magnetism
in the whole Hertzsprung-Russell diagram. However, new methods should still be
developed to probe the deep magnetic fields in these stars.\r\n\r\nAims. Our goal
is to provide seismic diagnoses that allow us to probe the internal magnetism
of stars.\r\n\r\nMethods. We focused on asymptotic low-frequency gravity modes
and high-frequency acoustic modes. Using a first-order perturbative theory, we
derived magnetic splittings of their frequencies as explicit functions of stellar
parameters.\r\n\r\nResults. As in the case of rotation, we show that asymptotic
gravity and acoustic modes can allow us to probe the different components of the
magnetic field in the cavities in which they propagate. This again demonstrates
the high potential of using mixed-modes when this is possible."
acknowledgement: The authors thank the referee and Pr. J. Christensen-Dalsgaard for
their very constructive comments and remarks that allowed us to improve the article.
St. M., L. B., V. P., and K. A. acknowledge support from the European Research Council
through ERC grant SPIRE 647383. All the members from CEA acknowledge support from
GOLF and PLATO CNES grants of the Astrophysics Division at CEA. S. Mathur acknowledges
support by the Ramon y Cajal fellowship number RYC-2015-17697. We made great use
of the megyr python package for interfacing MESA and GYRE codes.
article_number: A122
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: V.
full_name: Prat, V.
last_name: Prat
- first_name: K.
full_name: Augustson, K.
last_name: Augustson
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: R. A.
full_name: Garcia, R. A.
last_name: Garcia
citation:
ama: Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. Probing the
internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy
& Astrophysics. 2021;647. doi:10.1051/0004-6361/202039180
apa: Mathis, S., Bugnet, L. A., Prat, V., Augustson, K., Mathur, S., & Garcia,
R. A. (2021). Probing the internal magnetism of stars using asymptotic magneto-asteroseismology.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039180
chicago: Mathis, S., Lisa Annabelle Bugnet, V. Prat, K. Augustson, S. Mathur, and
R. A. Garcia. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.”
Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039180.
ieee: S. Mathis, L. A. Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia,
“Probing the internal magnetism of stars using asymptotic magneto-asteroseismology,”
Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021.
ista: Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing
the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy
& Astrophysics. 647, A122.
mla: Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic
Magneto-Asteroseismology.” Astronomy & Astrophysics, vol. 647, A122,
EDP Sciences, 2021, doi:10.1051/0004-6361/202039180.
short: S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy
& Astrophysics 647 (2021).
date_created: 2022-07-18T12:15:27Z
date_published: 2021-03-18T00:00:00Z
date_updated: 2022-08-19T10:11:52Z
day: '18'
doi: 10.1051/0004-6361/202039180
extern: '1'
external_id:
arxiv:
- '2012.11050'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- asteroseismology / waves / stars
- magnetic field / stars
- oscillations / methods
- analytical
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2012.11050
month: '03'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Probing the internal magnetism of stars using asymptotic magneto-asteroseismology
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_id: '11608'
abstract:
- lang: eng
text: 'In order to understand stellar evolution, it is crucial to efficiently determine
stellar surface rotation periods. Indeed, while they are of great importance in
stellar models, angular momentum transport processes inside stars are still poorly
understood today. Surface rotation, which is linked to the age of the star, is
one of the constraints needed to improve the way those processes are modelled.
Statistics of the surface rotation periods for a large sample of stars of different
spectral types are thus necessary. An efficient tool to automatically determine
reliable rotation periods is needed when dealing with large samples of stellar
photometric datasets. The objective of this work is to develop such a tool. For
this purpose, machine learning classifiers constitute relevant bases to build
our new methodology. Random forest learning abilities are exploited to automate
the extraction of rotation periods in Kepler light curves. Rotation periods and
complementary parameters are obtained via three different methods: a wavelet analysis,
the autocorrelation function of the light curve, and the composite spectrum. We
trained three different classifiers: one to detect if rotational modulations are
present in the light curve, one to flag close binary or classical pulsators candidates
that can bias our rotation period determination, and finally one classifier to
provide the final rotation period. We tested our machine learning pipeline on
23 431 stars of the Kepler K and M dwarf reference rotation catalogue for which
60% of the stars have been visually inspected. For the sample of 21 707 stars
where all the input parameters are provided to the algorithm, 94.2% of them are
correctly classified (as rotating or not). Among the stars that have a rotation
period in the reference catalogue, the machine learning provides a period that
agrees within 10% of the reference value for 95.3% of the stars. Moreover, the
yield of correct rotation periods is raised to 99.5% after visually inspecting
25.2% of the stars. Over the two main analysis steps, rotation classification
and period selection, the pipeline yields a global agreement with the reference
values of 92.1% and 96.9% before and after visual inspection. Random forest classifiers
are efficient tools to determine reliable rotation periods in large samples of
stars. The methodology presented here could be easily adapted to extract surface
rotation periods for stars with different spectral types or observed by other
instruments such as K2, TESS or by PLATO in the near future.'
acknowledgement: 'We thank Suzanne Aigrain and Joe Llama for providing us with the
simulated data used in Aigrain et al. (2015). S. N. B., L. B. and R. A. G. acknowledge
the support from PLATO and GOLF CNES grants. A. R. G. S. acknowledges the support
from NASA under grant NNX17AF27G. S. M. acknowledges the support from the Spanish
Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697.
P. L. P. and S. M. acknowledge support from the Spanish Ministry of Science and
Innovation with the grant number PID2019-107187GB-I00. This research has made use
of the NASA Exoplanet Archive, which is operated by the California Institute of
Technology, under contract with the National Aeronautics and Space Administration
under the Exoplanet Exploration Program. Software: Python (Van Rossum & Drake 2009),
numpy (Oliphant 2006), pandas (The pandas development team 2020; McKinney 2010),
matplotlib (Hunter 2007), scikit-learn (Pedregosa et al. 2011). The source code
used to obtain the present results can be found at: https://gitlab.com/sybreton/pushkin
; https://gitlab.com/sybreton/ml_surface_rotation_paper .'
article_number: A125
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S. N.
full_name: Breton, S. N.
last_name: Breton
- first_name: A. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: P. L.
full_name: Pallé, P. L.
last_name: Pallé
citation:
ama: 'Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. ROOSTER:
A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy
& Astrophysics. 2021;647. doi:10.1051/0004-6361/202039947'
apa: 'Breton, S. N., Santos, A. R. G., Bugnet, L. A., Mathur, S., García, R. A.,
& Pallé, P. L. (2021). ROOSTER: A machine-learning analysis tool for Kepler
stellar rotation periods. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039947'
chicago: 'Breton, S. N., A. R. G. Santos, Lisa Annabelle Bugnet, S. Mathur, R. A.
García, and P. L. Pallé. “ROOSTER: A Machine-Learning Analysis Tool for Kepler
Stellar Rotation Periods.” Astronomy & Astrophysics. EDP Sciences,
2021. https://doi.org/10.1051/0004-6361/202039947.'
ieee: 'S. N. Breton, A. R. G. Santos, L. A. Bugnet, S. Mathur, R. A. García, and
P. L. Pallé, “ROOSTER: A machine-learning analysis tool for Kepler stellar rotation
periods,” Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021.'
ista: 'Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. 2021. ROOSTER:
A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy
& Astrophysics. 647, A125.'
mla: 'Breton, S. N., et al. “ROOSTER: A Machine-Learning Analysis Tool for Kepler
Stellar Rotation Periods.” Astronomy & Astrophysics, vol. 647, A125,
EDP Sciences, 2021, doi:10.1051/0004-6361/202039947.'
short: S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé,
Astronomy & Astrophysics 647 (2021).
date_created: 2022-07-18T12:21:32Z
date_published: 2021-03-19T00:00:00Z
date_updated: 2022-08-22T08:47:47Z
day: '19'
doi: 10.1051/0004-6361/202039947
extern: '1'
external_id:
arxiv:
- '2101.10152'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'methods: data analysis / stars: solar-type / stars: activity / stars: rotation
/ starspots'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2101.10152
month: '03'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_id: '11609'
abstract:
- lang: eng
text: "Context. Stellar interiors are the seat of efficient transport of angular
momentum all along their evolution. In this context, understanding the dependence
of the turbulent transport triggered by the instabilities of the vertical and
horizontal shears of the differential rotation in stellar radiation zones as a
function of their rotation, stratification, and thermal diffusivity is mandatory.
Indeed, it constitutes one of the cornerstones of the rotational transport and
mixing theory, which is implemented in stellar evolution codes to predict the
rotational and chemical evolutions of stars.\r\n\r\nAims. We investigate horizontal
shear instabilities in rotating stellar radiation zones by considering the full
Coriolis acceleration with both the dimensionless horizontal Coriolis component
f̃ and the vertical component f.\r\n\r\nMethods. We performed a linear stability
analysis using linearized equations derived from the Navier-Stokes and heat transport
equations in the rotating nontraditional f-plane. We considered a horizontal shear
flow with a hyperbolic tangent profile as the base flow. The linear stability
was analyzed numerically in wide ranges of parameters, and we performed an asymptotic
analysis for large vertical wavenumbers using the Wentzel-Kramers-Brillouin-Jeffreys
(WKBJ) approximation for nondiffusive and highly-diffusive fluids.\r\n\r\nResults.
As in the traditional f-plane approximation, we identify two types of instabilities:
the inflectional and inertial instabilities. The inflectional instability is destabilized
as f̃ increases and its maximum growth rate increases significantly, while the
thermal diffusivity stabilizes the inflectional instability similarly to the traditional
case. The inertial instability is also strongly affected; for instance, the inertially
unstable regime is also extended in the nondiffusive limit as 0 < f < 1 + f̃ 2/N2,
where N is the dimensionless Brunt-Väisälä frequency. More strikingly, in the
high thermal diffusivity limit, it is always inertially unstable at any colatitude
θ except at the poles (i.e., 0° < θ < 180°). We also derived the critical Reynolds
numbers for the inertial instability using the asymptotic dispersion relations
obtained from the WKBJ analysis. Using the asymptotic and numerical results, we
propose a prescription for the effective turbulent viscosities induced by the
inertial and inflectional instabilities that can be possibly used in stellar evolution
models. The characteristic time of this turbulence is short enough so that it
is efficient to redistribute angular momentum and to mix chemicals in stellar
radiation zones."
acknowledgement: The authors acknowledge support from the European Research Council
through ERC grant SPIRE 647383 and from GOLF and PLATO CNES grants at the Department
of Astrophysics at CEA Paris-Saclay. We thank the referee, Prof. A. J. Barker, for
his constructive comments that allow us to improve the article.
article_number: A64
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Park, J.
last_name: Park
- first_name: V.
full_name: Prat, V.
last_name: Prat
- first_name: S.
full_name: Mathis, S.
last_name: Mathis
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: 'Park J, Prat V, Mathis S, Bugnet LA. Horizontal shear instabilities in rotating
stellar radiation zones: II. Effects of the full Coriolis acceleration. Astronomy
& Astrophysics. 2021;646. doi:10.1051/0004-6361/202038654'
apa: 'Park, J., Prat, V., Mathis, S., & Bugnet, L. A. (2021). Horizontal shear
instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis
acceleration. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038654'
chicago: 'Park, J., V. Prat, S. Mathis, and Lisa Annabelle Bugnet. “Horizontal Shear
Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis
Acceleration.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202038654.'
ieee: 'J. Park, V. Prat, S. Mathis, and L. A. Bugnet, “Horizontal shear instabilities
in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration,”
Astronomy & Astrophysics, vol. 646. EDP Sciences, 2021.'
ista: 'Park J, Prat V, Mathis S, Bugnet LA. 2021. Horizontal shear instabilities
in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration.
Astronomy & Astrophysics. 646, A64.'
mla: 'Park, J., et al. “Horizontal Shear Instabilities in Rotating Stellar Radiation
Zones: II. Effects of the Full Coriolis Acceleration.” Astronomy & Astrophysics,
vol. 646, A64, EDP Sciences, 2021, doi:10.1051/0004-6361/202038654.'
short: J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy & Astrophysics 646
(2021).
date_created: 2022-07-18T13:24:32Z
date_published: 2021-02-08T00:00:00Z
date_updated: 2022-08-19T10:18:03Z
day: '08'
doi: 10.1051/0004-6361/202038654
extern: '1'
external_id:
arxiv:
- '2006.10660'
intvolume: ' 646'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- hydrodynamics / turbulence / stars
- rotation / stars
- evolution
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2006.10660
month: '02'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Horizontal shear instabilities in rotating stellar radiation zones: II. Effects
of the full Coriolis acceleration'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 646
year: '2021'
...
---
_id: '11649'
abstract:
- lang: eng
text: 'While operating communication networks adaptively may improve utilization
and performance, frequent adjustments also introduce an algorithmic challenge:
the re-optimization of traffic engineering solutions is time-consuming and may
limit the granularity at which a network can be adjusted. This paper is motivated
by question whether the reactivity of a network can be improved by re-optimizing
solutions dynamically rather than from scratch, especially if inputs such as link
weights do not change significantly. This paper explores to what extent dynamic
algorithms can be used to speed up fundamental tasks in network operations. We
specifically investigate optimizations related to traffic engineering (namely
shortest paths and maximum flow computations), but also consider spanning tree
and matching applications. While prior work on dynamic graph algorithms focusses
on link insertions and deletions, we are interested in the practical problem of
link weight changes. We revisit existing upper bounds in the weight-dynamic model,
and present several novel lower bounds on the amortized runtime for recomputing
solutions. In general, we find that the potential performance gains depend on
the application, and there are also strict limitations on what can be achieved,
even if link weights change only slightly.'
article_processing_charge: No
arxiv: 1
author:
- first_name: Monika H
full_name: Henzinger, Monika H
id: 540c9bbd-f2de-11ec-812d-d04a5be85630
last_name: Henzinger
orcid: 0000-0002-5008-6530
- first_name: Ami
full_name: Paz, Ami
last_name: Paz
- first_name: Stefan
full_name: Schmid, Stefan
last_name: Schmid
citation:
ama: 'Henzinger MH, Paz A, Schmid S. On the complexity of weight-dynamic network
algorithms. In: IFIP Networking Conference. Institute of Electrical and
Electronics Engineers; 2021. doi:10.23919/ifipnetworking52078.2021.9472803'
apa: 'Henzinger, M. H., Paz, A., & Schmid, S. (2021). On the complexity of weight-dynamic
network algorithms. In IFIP Networking Conference. Espoo and Helsinki,
Finland: Institute of Electrical and Electronics Engineers. https://doi.org/10.23919/ifipnetworking52078.2021.9472803'
chicago: Henzinger, Monika H, Ami Paz, and Stefan Schmid. “On the Complexity of
Weight-Dynamic Network Algorithms.” In IFIP Networking Conference. Institute
of Electrical and Electronics Engineers, 2021. https://doi.org/10.23919/ifipnetworking52078.2021.9472803.
ieee: M. H. Henzinger, A. Paz, and S. Schmid, “On the complexity of weight-dynamic
network algorithms,” in IFIP Networking Conference, Espoo and Helsinki,
Finland, 2021.
ista: 'Henzinger MH, Paz A, Schmid S. 2021. On the complexity of weight-dynamic
network algorithms. IFIP Networking Conference. IFIP: Networking.'
mla: Henzinger, Monika H., et al. “On the Complexity of Weight-Dynamic Network Algorithms.”
IFIP Networking Conference, Institute of Electrical and Electronics Engineers,
2021, doi:10.23919/ifipnetworking52078.2021.9472803.
short: M.H. Henzinger, A. Paz, S. Schmid, in:, IFIP Networking Conference, Institute
of Electrical and Electronics Engineers, 2021.
conference:
end_date: 2021-06-24
location: ' Espoo and Helsinki, Finland'
name: 'IFIP: Networking'
start_date: 2021-06-21
date_created: 2022-07-25T11:13:06Z
date_published: 2021-06-21T00:00:00Z
date_updated: 2023-02-09T09:11:51Z
day: '21'
doi: 10.23919/ifipnetworking52078.2021.9472803
extern: '1'
external_id:
arxiv:
- '2105.13172'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.2105.13172'
month: '06'
oa: 1
oa_version: Preprint
publication: IFIP Networking Conference
publication_identifier:
eissn:
- 1861-2288
publication_status: published
publisher: Institute of Electrical and Electronics Engineers
quality_controlled: '1'
scopus_import: '1'
status: public
title: On the complexity of weight-dynamic network algorithms
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2021'
...
---
_id: '11663'
abstract:
- lang: eng
text: "Many dynamic graph algorithms have an amortized update time, rather than
a stronger worst-case guarantee. But amortized data structures are not suitable
for real-time systems, where each individual operation has to be executed quickly.
For this reason, there exist many recent randomized results that aim to provide
a guarantee stronger than amortized expected. The strongest possible guarantee
for a randomized algorithm is that it is always correct (Las Vegas) and has high-probability
worst-case update time, which gives a bound on the time for each individual operation
that holds with high probability.\r\n\r\nIn this article, we present the first
polylogarithmic high-probability worst-case time bounds for the dynamic spanner
and the dynamic maximal matching problem.\r\n\r\n(1)\r\n\r\nFor dynamic spanner,
the only known o(n) worst-case bounds were O(n3/4) high-probability worst-case
update time for maintaining a 3-spanner and O(n5/9) for maintaining a 5-spanner.
We give a O(1)k log3 (n) high-probability worst-case time bound for maintaining
a (2k-1)-spanner, which yields the first worst-case polylog update time for all
constant k. (All the results above maintain the optimal tradeoff of stretch 2k-1
and Õ(n1+1/k) edges.)\r\n\r\n(2)\r\n\r\nFor dynamic maximal matching, or dynamic
2-approximate maximum matching, no algorithm with o(n) worst-case time bound was
known and we present an algorithm with O(log 5 (n)) high-probability worst-case
time; similar worst-case bounds existed only for maintaining a matching that was
(2+ϵ)-approximate, and hence not maximal.\r\n\r\nOur results are achieved using
a new approach for converting amortized guarantees to worst-case ones for randomized
data structures by going through a third type of guarantee, which is a middle
ground between the two above: An algorithm is said to have worst-case expected
update time ɑ if for every update σ, the expected time to process σ is at most
ɑ. Although stronger than amortized expected, the worst-case expected guarantee
does not resolve the fundamental problem of amortization: A worst-case expected
update time of O(1) still allows for the possibility that every 1/f(n) updates
requires ϴ (f(n)) time to process, for arbitrarily high f(n). In this article,
we present a black-box reduction that converts any data structure with worst-case
expected update time into one with a high-probability worst-case update time:
The query time remains the same, while the update time increases by a factor of
O(log 2(n)).\r\n\r\nThus, we achieve our results in two steps:\r\n\r\n(1) First,
we show how to convert existing dynamic graph algorithms with amortized expected
polylogarithmic running times into algorithms with worst-case expected polylogarithmic
running times.\r\n\r\n(2) Then, we use our black-box reduction to achieve the
polylogarithmic high-probability worst-case time bound. All our algorithms are
Las-Vegas-type algorithms."
acknowledgement: 'The conference version of this article [10] had an error in the
analysis of the dynamic matching algorithm. In particular, Lemma 4.5 assumed an
independence between adversarial updates to the hierarchy that is in fact true,
but which requires a sophisticated proof. We are very grateful to the anonymous
reviewers of Transactions on Algorithms for pointing out this mistake in our analysis.
The mistake is fixed in Section 4.5. Almost the entire fix is a matter of analysis:
the only change to the algorithm itself is the introduction of responsible bits
in Algorithm 2. The first author would like to thank Mikkel Thorup and Alan Roytman
for a very helpful discussion of the proof of Theorem 1.1.'
article_number: '29'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Aaron
full_name: Bernstein, Aaron
last_name: Bernstein
- first_name: Sebastian
full_name: Forster, Sebastian
last_name: Forster
- first_name: Monika H
full_name: Henzinger, Monika H
id: 540c9bbd-f2de-11ec-812d-d04a5be85630
last_name: Henzinger
orcid: 0000-0002-5008-6530
citation:
ama: Bernstein A, Forster S, Henzinger MH. A deamortization approach for dynamic
spanner and dynamic maximal matching. ACM Transactions on Algorithms. 2021;17(4).
doi:10.1145/3469833
apa: Bernstein, A., Forster, S., & Henzinger, M. H. (2021). A deamortization
approach for dynamic spanner and dynamic maximal matching. ACM Transactions
on Algorithms. Association for Computing Machinery. https://doi.org/10.1145/3469833
chicago: Bernstein, Aaron, Sebastian Forster, and Monika H Henzinger. “A Deamortization
Approach for Dynamic Spanner and Dynamic Maximal Matching.” ACM Transactions
on Algorithms. Association for Computing Machinery, 2021. https://doi.org/10.1145/3469833.
ieee: A. Bernstein, S. Forster, and M. H. Henzinger, “A deamortization approach
for dynamic spanner and dynamic maximal matching,” ACM Transactions on Algorithms,
vol. 17, no. 4. Association for Computing Machinery, 2021.
ista: Bernstein A, Forster S, Henzinger MH. 2021. A deamortization approach for
dynamic spanner and dynamic maximal matching. ACM Transactions on Algorithms.
17(4), 29.
mla: Bernstein, Aaron, et al. “A Deamortization Approach for Dynamic Spanner and
Dynamic Maximal Matching.” ACM Transactions on Algorithms, vol. 17, no.
4, 29, Association for Computing Machinery, 2021, doi:10.1145/3469833.
short: A. Bernstein, S. Forster, M.H. Henzinger, ACM Transactions on Algorithms
17 (2021).
date_created: 2022-07-27T11:09:06Z
date_published: 2021-10-04T00:00:00Z
date_updated: 2022-09-09T11:35:44Z
day: '04'
doi: 10.1145/3469833
extern: '1'
external_id:
arxiv:
- '1810.10932'
intvolume: ' 17'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1810.10932
month: '10'
oa: 1
oa_version: Preprint
publication: ACM Transactions on Algorithms
publication_identifier:
eissn:
- 1549-6333
issn:
- 1549-6325
publication_status: published
publisher: Association for Computing Machinery
quality_controlled: '1'
scopus_import: '1'
status: public
title: A deamortization approach for dynamic spanner and dynamic maximal matching
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 17
year: '2021'
...
---
_id: '11756'
abstract:
- lang: eng
text: We give two fully dynamic algorithms that maintain a (1 + ε)-approximation
of the weight M of a minimum spanning forest (MSF) of an n-node graph G with edges
weights in [1, W ], for any ε > 0. (1) Our deterministic algorithm takes O (W
2 log W /ε3) worst-case update time, which is O (1) if both W and ε are constants.
(2) Our randomized (Monte-Carlo style) algorithm works with high probability and
runs in worst-case O (log W /ε4) update time if W = O ((m∗)1/6/log2/3 n), where
m∗ is the minimum number of edges in the graph throughout all the updates. It
works even against an adaptive adversary. We complement our algorithmic results
with two cell-probe lower bounds for dynamically maintaining an approximation
of the weight of an MSF of a graph.
article_number: '104805'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Monika H
full_name: Henzinger, Monika H
id: 540c9bbd-f2de-11ec-812d-d04a5be85630
last_name: Henzinger
orcid: 0000-0002-5008-6530
- first_name: Pan
full_name: Peng, Pan
last_name: Peng
citation:
ama: Henzinger MH, Peng P. Constant-time dynamic weight approximation for minimum
spanning forest. Information and Computation. 2021;281(12). doi:10.1016/j.ic.2021.104805
apa: Henzinger, M. H., & Peng, P. (2021). Constant-time dynamic weight approximation
for minimum spanning forest. Information and Computation. Elsevier. https://doi.org/10.1016/j.ic.2021.104805
chicago: Henzinger, Monika H, and Pan Peng. “Constant-Time Dynamic Weight Approximation
for Minimum Spanning Forest.” Information and Computation. Elsevier, 2021.
https://doi.org/10.1016/j.ic.2021.104805.
ieee: M. H. Henzinger and P. Peng, “Constant-time dynamic weight approximation for
minimum spanning forest,” Information and Computation, vol. 281, no. 12.
Elsevier, 2021.
ista: Henzinger MH, Peng P. 2021. Constant-time dynamic weight approximation for
minimum spanning forest. Information and Computation. 281(12), 104805.
mla: Henzinger, Monika H., and Pan Peng. “Constant-Time Dynamic Weight Approximation
for Minimum Spanning Forest.” Information and Computation, vol. 281, no.
12, 104805, Elsevier, 2021, doi:10.1016/j.ic.2021.104805.
short: M.H. Henzinger, P. Peng, Information and Computation 281 (2021).
date_created: 2022-08-08T10:58:29Z
date_published: 2021-12-01T00:00:00Z
date_updated: 2022-09-12T09:29:29Z
day: '01'
doi: 10.1016/j.ic.2021.104805
extern: '1'
external_id:
arxiv:
- '2011.00977'
intvolume: ' 281'
issue: '12'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2011.00977
month: '12'
oa: 1
oa_version: Preprint
publication: Information and Computation
publication_identifier:
issn:
- 0890-5401
publication_status: published
publisher: Elsevier
quality_controlled: '1'
scopus_import: '1'
status: public
title: Constant-time dynamic weight approximation for minimum spanning forest
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 281
year: '2021'
...
---
_id: '11771'
abstract:
- lang: eng
text: "Classic dynamic data structure problems maintain a data structure subject
to a sequence S of updates and they answer queries using the latest version of
the data structure, i.e., the data structure after processing the whole sequence.
To handle operations that change the sequence S of updates, Demaine et al. [7]
introduced retroactive data structures (RDS). A retroactive operation modifies
the update sequence S in a given position t, called time, and either creates or
cancels an update in S at time t. A fully retroactive data structure supports
queries at any time t: a query at time t is answered using only the updates of
S up to time t. While efficient RDS have been proposed for classic data structures,
e.g., stack, priority queue and binary search tree, the retroactive version of
graph problems are rarely studied.\r\n\r\nIn this paper we study retroactive graph
problems including connectivity, minimum spanning forest (MSF), maximum degree,
etc. We show that under the OMv conjecture (proposed by Henzinger et al. [15]),
there does not exist fully RDS maintaining connectivity or MSF, or incremental
fully RDS maintaining the maximum degree with \U0001D442(\U0001D45B1−\U0001D716)
time per operation, for any constant \U0001D716>0. Furthermore, We provide RDS
with almost tight time per operation. We give fully RDS for maintaining the maximum
degree, connectivity and MSF in \U0001D442̃ (\U0001D45B) time per operation. We
also give an algorithm for the incremental (insertion-only) fully retroactive
connectivity with \U0001D442̃ (1) time per operation, showing that the lower bound
cannot be extended to this setting.\r\n\r\nWe also study a restricted version
of RDS, where the only change to S is the swap of neighboring updates and show
that for this problem we can beat the above hardness result. This also implies
the first non-trivial dynamic Reeb graph computation algorithm."
alternative_title:
- LNCS
article_processing_charge: No
arxiv: 1
author:
- first_name: Monika H
full_name: Henzinger, Monika H
id: 540c9bbd-f2de-11ec-812d-d04a5be85630
last_name: Henzinger
orcid: 0000-0002-5008-6530
- first_name: Xiaowei
full_name: Wu, Xiaowei
last_name: Wu
citation:
ama: 'Henzinger MH, Wu X. Upper and lower bounds for fully retroactive graph problems.
In: 17th International Symposium on Algorithms and Data Structures. Vol
12808. Springer Nature; 2021:471–484. doi:10.1007/978-3-030-83508-8_34'
apa: 'Henzinger, M. H., & Wu, X. (2021). Upper and lower bounds for fully retroactive
graph problems. In 17th International Symposium on Algorithms and Data Structures
(Vol. 12808, pp. 471–484). Virtual: Springer Nature. https://doi.org/10.1007/978-3-030-83508-8_34'
chicago: Henzinger, Monika H, and Xiaowei Wu. “Upper and Lower Bounds for Fully
Retroactive Graph Problems.” In 17th International Symposium on Algorithms
and Data Structures, 12808:471–484. Springer Nature, 2021. https://doi.org/10.1007/978-3-030-83508-8_34.
ieee: M. H. Henzinger and X. Wu, “Upper and lower bounds for fully retroactive graph
problems,” in 17th International Symposium on Algorithms and Data Structures,
Virtual, 2021, vol. 12808, pp. 471–484.
ista: 'Henzinger MH, Wu X. 2021. Upper and lower bounds for fully retroactive graph
problems. 17th International Symposium on Algorithms and Data Structures. WADS:
Workshop on Algorithms and Data Structures, LNCS, vol. 12808, 471–484.'
mla: Henzinger, Monika H., and Xiaowei Wu. “Upper and Lower Bounds for Fully Retroactive
Graph Problems.” 17th International Symposium on Algorithms and Data Structures,
vol. 12808, Springer Nature, 2021, pp. 471–484, doi:10.1007/978-3-030-83508-8_34.
short: M.H. Henzinger, X. Wu, in:, 17th International Symposium on Algorithms and
Data Structures, Springer Nature, 2021, pp. 471–484.
conference:
end_date: 2021-08-11
location: Virtual
name: 'WADS: Workshop on Algorithms and Data Structures'
start_date: 2021-08-09
date_created: 2022-08-08T13:01:29Z
date_published: 2021-08-09T00:00:00Z
date_updated: 2023-02-10T08:31:50Z
day: '09'
doi: 10.1007/978-3-030-83508-8_34
extern: '1'
external_id:
arxiv:
- '1910.03332'
intvolume: ' 12808'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1910.03332
month: '08'
oa: 1
oa_version: Preprint
page: 471–484
publication: 17th International Symposium on Algorithms and Data Structures
publication_identifier:
eisbn:
- '9783030835088'
eissn:
- 1611-3349
isbn:
- '9783030835071'
issn:
- 0302-9743
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Upper and lower bounds for fully retroactive graph problems
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 12808
year: '2021'
...
---
_id: '7883'
abstract:
- lang: eng
text: All vertebrates have a spinal cord with dimensions and shape specific to their
species. Yet how species‐specific organ size and shape are achieved is a fundamental
unresolved question in biology. The formation and sculpting of organs begins during
embryonic development. As it develops, the spinal cord extends in anterior–posterior
direction in synchrony with the overall growth of the body. The dorsoventral (DV)
and apicobasal lengths of the spinal cord neuroepithelium also change, while at
the same time a characteristic pattern of neural progenitor subtypes along the
DV axis is established and elaborated. At the basis of these changes in tissue
size and shape are biophysical determinants, such as the change in cell number,
cell size and shape, and anisotropic tissue growth. These processes are controlled
by global tissue‐scale regulators, such as morphogen signaling gradients as well
as mechanical forces. Current challenges in the field are to uncover how these
tissue‐scale regulatory mechanisms are translated to the cellular and molecular
level, and how regulation of distinct cellular processes gives rise to an overall
defined size. Addressing these questions will help not only to achieve a better
understanding of how size is controlled, but also of how tissue size is coordinated
with the specification of pattern.
acknowledgement: 'Austrian Academy of Sciences, Grant/Award Number: DOC fellowship
for Katarzyna Kuzmicz-Kowalska; Austrian Science Fund, Grant/Award Number: F78 (Stem
Cell Modulation); H2020 European Research Council, Grant/Award Number: 680037'
article_number: e383
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Katarzyna
full_name: Kuzmicz-Kowalska, Katarzyna
id: 4CED352A-F248-11E8-B48F-1D18A9856A87
last_name: Kuzmicz-Kowalska
- first_name: Anna
full_name: Kicheva, Anna
id: 3959A2A0-F248-11E8-B48F-1D18A9856A87
last_name: Kicheva
orcid: 0000-0003-4509-4998
citation:
ama: 'Kuzmicz-Kowalska K, Kicheva A. Regulation of size and scale in vertebrate
spinal cord development. Wiley Interdisciplinary Reviews: Developmental Biology.
2021. doi:10.1002/wdev.383'
apa: 'Kuzmicz-Kowalska, K., & Kicheva, A. (2021). Regulation of size and scale
in vertebrate spinal cord development. Wiley Interdisciplinary Reviews: Developmental
Biology. Wiley. https://doi.org/10.1002/wdev.383'
chicago: 'Kuzmicz-Kowalska, Katarzyna, and Anna Kicheva. “Regulation of Size and
Scale in Vertebrate Spinal Cord Development.” Wiley Interdisciplinary Reviews:
Developmental Biology. Wiley, 2021. https://doi.org/10.1002/wdev.383.'
ieee: 'K. Kuzmicz-Kowalska and A. Kicheva, “Regulation of size and scale in vertebrate
spinal cord development,” Wiley Interdisciplinary Reviews: Developmental Biology.
Wiley, 2021.'
ista: 'Kuzmicz-Kowalska K, Kicheva A. 2021. Regulation of size and scale in vertebrate
spinal cord development. Wiley Interdisciplinary Reviews: Developmental Biology.,
e383.'
mla: 'Kuzmicz-Kowalska, Katarzyna, and Anna Kicheva. “Regulation of Size and Scale
in Vertebrate Spinal Cord Development.” Wiley Interdisciplinary Reviews: Developmental
Biology, e383, Wiley, 2021, doi:10.1002/wdev.383.'
short: 'K. Kuzmicz-Kowalska, A. Kicheva, Wiley Interdisciplinary Reviews: Developmental
Biology (2021).'
date_created: 2020-05-24T22:01:00Z
date_published: 2021-04-15T00:00:00Z
date_updated: 2024-03-07T15:03:00Z
day: '15'
ddc:
- '570'
department:
- _id: AnKi
doi: 10.1002/wdev.383
ec_funded: 1
external_id:
isi:
- '000531419400001'
pmid:
- '32391980'
file:
- access_level: open_access
checksum: f0a7745d48afa09ea7025e876a0145a8
content_type: application/pdf
creator: dernst
date_created: 2020-11-24T13:11:39Z
date_updated: 2020-11-24T13:11:39Z
file_id: '8800'
file_name: 2020_WIREs_DevBio_KuzmiczKowalska.pdf
file_size: 2527276
relation: main_file
success: 1
file_date_updated: 2020-11-24T13:11:39Z
has_accepted_license: '1'
isi: 1
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '04'
oa: 1
oa_version: Published Version
pmid: 1
project:
- _id: B6FC0238-B512-11E9-945C-1524E6697425
call_identifier: H2020
grant_number: '680037'
name: Coordination of Patterning And Growth In the Spinal Cord
- _id: 267AF0E4-B435-11E9-9278-68D0E5697425
name: The role of morphogens in the regulation of neural tube growth
- _id: 059DF620-7A3F-11EA-A408-12923DDC885E
grant_number: F07802
name: Morphogen control of growth and pattern in the spinal cord
publication: 'Wiley Interdisciplinary Reviews: Developmental Biology'
publication_identifier:
eissn:
- '17597692'
issn:
- '17597684'
publication_status: published
publisher: Wiley
quality_controlled: '1'
related_material:
record:
- id: '14323'
relation: dissertation_contains
status: public
scopus_import: '1'
status: public
title: Regulation of size and scale in vertebrate spinal cord development
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 3E5EF7F0-F248-11E8-B48F-1D18A9856A87
year: '2021'
...
---
_id: '7900'
abstract:
- lang: eng
text: Hartree–Fock theory has been justified as a mean-field approximation for fermionic
systems. However, it suffers from some defects in predicting physical properties,
making necessary a theory of quantum correlations. Recently, bosonization of many-body
correlations has been rigorously justified as an upper bound on the correlation
energy at high density with weak interactions. We review the bosonic approximation,
deriving an effective Hamiltonian. We then show that for systems with Coulomb
interaction this effective theory predicts collective excitations (plasmons) in
accordance with the random phase approximation of Bohm and Pines, and with experimental
observation.
article_number: '2060009'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Niels P
full_name: Benedikter, Niels P
id: 3DE6C32A-F248-11E8-B48F-1D18A9856A87
last_name: Benedikter
orcid: 0000-0002-1071-6091
citation:
ama: Benedikter NP. Bosonic collective excitations in Fermi gases. Reviews in
Mathematical Physics. 2021;33(1). doi:10.1142/s0129055x20600090
apa: Benedikter, N. P. (2021). Bosonic collective excitations in Fermi gases. Reviews
in Mathematical Physics. World Scientific. https://doi.org/10.1142/s0129055x20600090
chicago: Benedikter, Niels P. “Bosonic Collective Excitations in Fermi Gases.” Reviews
in Mathematical Physics. World Scientific, 2021. https://doi.org/10.1142/s0129055x20600090.
ieee: N. P. Benedikter, “Bosonic collective excitations in Fermi gases,” Reviews
in Mathematical Physics, vol. 33, no. 1. World Scientific, 2021.
ista: Benedikter NP. 2021. Bosonic collective excitations in Fermi gases. Reviews
in Mathematical Physics. 33(1), 2060009.
mla: Benedikter, Niels P. “Bosonic Collective Excitations in Fermi Gases.” Reviews
in Mathematical Physics, vol. 33, no. 1, 2060009, World Scientific, 2021,
doi:10.1142/s0129055x20600090.
short: N.P. Benedikter, Reviews in Mathematical Physics 33 (2021).
date_created: 2020-05-28T16:47:55Z
date_published: 2021-01-01T00:00:00Z
date_updated: 2023-09-05T16:07:40Z
day: '01'
department:
- _id: RoSe
doi: 10.1142/s0129055x20600090
ec_funded: 1
external_id:
arxiv:
- '1910.08190'
isi:
- '000613313200010'
intvolume: ' 33'
isi: 1
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1910.08190
month: '01'
oa: 1
oa_version: Preprint
project:
- _id: 25C6DC12-B435-11E9-9278-68D0E5697425
call_identifier: H2020
grant_number: '694227'
name: Analysis of quantum many-body systems
publication: Reviews in Mathematical Physics
publication_identifier:
eissn:
- 1793-6659
issn:
- 0129-055X
publication_status: published
publisher: World Scientific
quality_controlled: '1'
scopus_import: '1'
status: public
title: Bosonic collective excitations in Fermi gases
type: journal_article
user_id: c635000d-4b10-11ee-a964-aac5a93f6ac1
volume: 33
year: '2021'
...
---
_id: '7901'
abstract:
- lang: eng
text: We derive rigorously the leading order of the correlation energy of a Fermi
gas in a scaling regime of high density and weak interaction. The result verifies
the prediction of the random-phase approximation. Our proof refines the method
of collective bosonization in three dimensions. We approximately diagonalize an
effective Hamiltonian describing approximately bosonic collective excitations
around the Hartree–Fock state, while showing that gapless and non-collective excitations
have only a negligible effect on the ground state energy.
acknowledgement: We thank Christian Hainzl for helpful discussions and a referee for
very careful reading of the paper and many helpful suggestions. NB and RS were supported
by the European Research Council (ERC) under the European Union’s Horizon 2020 research
and innovation programme (grant agreement No. 694227). Part of the research of NB
was conducted on the RZD18 Nice–Milan–Vienna–Moscow. NB thanks Elliott H. Lieb and
Peter Otte for explanations about the Luttinger model. PTN has received funding
from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under
Germany’s Excellence Strategy (EXC-2111-390814868). MP acknowledges financial support
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation programme (ERC StG MaMBoQ, grant agreement No. 802901).
BS gratefully acknowledges financial support from the NCCR SwissMAP, from the Swiss
National Science Foundation through the Grant “Dynamical and energetic properties
of Bose-Einstein condensates” and from the European Research Council through the
ERC-AdG CLaQS (grant agreement No. 834782). All authors acknowledge support for
workshop participation from Mathematisches Forschungsinstitut Oberwolfach (Leibniz
Association). NB, PTN, BS, and RS acknowledge support for workshop participation
from Fondation des Treilles.
article_processing_charge: Yes (via OA deal)
article_type: original
arxiv: 1
author:
- first_name: Niels P
full_name: Benedikter, Niels P
id: 3DE6C32A-F248-11E8-B48F-1D18A9856A87
last_name: Benedikter
orcid: 0000-0002-1071-6091
- first_name: Phan Thành
full_name: Nam, Phan Thành
last_name: Nam
- first_name: Marcello
full_name: Porta, Marcello
last_name: Porta
- first_name: Benjamin
full_name: Schlein, Benjamin
last_name: Schlein
- first_name: Robert
full_name: Seiringer, Robert
id: 4AFD0470-F248-11E8-B48F-1D18A9856A87
last_name: Seiringer
orcid: 0000-0002-6781-0521
citation:
ama: Benedikter NP, Nam PT, Porta M, Schlein B, Seiringer R. Correlation energy
of a weakly interacting Fermi gas. Inventiones Mathematicae. 2021;225:885-979.
doi:10.1007/s00222-021-01041-5
apa: Benedikter, N. P., Nam, P. T., Porta, M., Schlein, B., & Seiringer, R.
(2021). Correlation energy of a weakly interacting Fermi gas. Inventiones Mathematicae.
Springer. https://doi.org/10.1007/s00222-021-01041-5
chicago: Benedikter, Niels P, Phan Thành Nam, Marcello Porta, Benjamin Schlein,
and Robert Seiringer. “Correlation Energy of a Weakly Interacting Fermi Gas.”
Inventiones Mathematicae. Springer, 2021. https://doi.org/10.1007/s00222-021-01041-5.
ieee: N. P. Benedikter, P. T. Nam, M. Porta, B. Schlein, and R. Seiringer, “Correlation
energy of a weakly interacting Fermi gas,” Inventiones Mathematicae, vol.
225. Springer, pp. 885–979, 2021.
ista: Benedikter NP, Nam PT, Porta M, Schlein B, Seiringer R. 2021. Correlation
energy of a weakly interacting Fermi gas. Inventiones Mathematicae. 225, 885–979.
mla: Benedikter, Niels P., et al. “Correlation Energy of a Weakly Interacting Fermi
Gas.” Inventiones Mathematicae, vol. 225, Springer, 2021, pp. 885–979,
doi:10.1007/s00222-021-01041-5.
short: N.P. Benedikter, P.T. Nam, M. Porta, B. Schlein, R. Seiringer, Inventiones
Mathematicae 225 (2021) 885–979.
date_created: 2020-05-28T16:48:20Z
date_published: 2021-05-03T00:00:00Z
date_updated: 2023-08-21T06:30:30Z
day: '03'
ddc:
- '510'
department:
- _id: RoSe
doi: 10.1007/s00222-021-01041-5
ec_funded: 1
external_id:
arxiv:
- '2005.08933'
isi:
- '000646573600001'
file:
- access_level: open_access
checksum: f38c79dfd828cdc7f49a34b37b83d376
content_type: application/pdf
creator: dernst
date_created: 2022-05-16T12:23:40Z
date_updated: 2022-05-16T12:23:40Z
file_id: '11386'
file_name: 2021_InventMath_Benedikter.pdf
file_size: 1089319
relation: main_file
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file_date_updated: 2022-05-16T12:23:40Z
has_accepted_license: '1'
intvolume: ' 225'
isi: 1
language:
- iso: eng
month: '05'
oa: 1
oa_version: Published Version
page: 885-979
project:
- _id: B67AFEDC-15C9-11EA-A837-991A96BB2854
name: IST Austria Open Access Fund
- _id: 25C6DC12-B435-11E9-9278-68D0E5697425
call_identifier: H2020
grant_number: '694227'
name: Analysis of quantum many-body systems
publication: Inventiones Mathematicae
publication_identifier:
eissn:
- 1432-1297
issn:
- 0020-9910
publication_status: published
publisher: Springer
quality_controlled: '1'
scopus_import: '1'
status: public
title: Correlation energy of a weakly interacting Fermi gas
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 4359f0d1-fa6c-11eb-b949-802e58b17ae8
volume: 225
year: '2021'
...