[{"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).","oa":1,"status":"public","article_type":"original","external_id":{"arxiv":["2102.05516"]},"citation":{"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.","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).","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.","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.","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"},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":647,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11500","year":"2021","arxiv":1,"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."}],"extern":"1","title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","publication":"Astronomy & Astrophysics","publisher":"EDP Sciences","oa_version":"Published Version","date_created":"2022-07-06T09:31:50Z","day":"18","language":[{"iso":"eng"}],"month":"03","intvolume":" 647","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.05516"}],"publication_status":"published","date_published":"2021-03-18T00:00:00Z","author":[{"full_name":"Bacon, R.","first_name":"R.","last_name":"Bacon"},{"full_name":"Mary, D.","last_name":"Mary","first_name":"D."},{"last_name":"Garel","first_name":"T.","full_name":"Garel, T."},{"last_name":"Blaizot","first_name":"J.","full_name":"Blaizot, J."},{"last_name":"Maseda","first_name":"M.","full_name":"Maseda, M."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."},{"full_name":"Wisotzki, L.","first_name":"L.","last_name":"Wisotzki"},{"full_name":"Conseil, S.","first_name":"S.","last_name":"Conseil"},{"first_name":"J.","last_name":"Brinchmann","full_name":"Brinchmann, J."},{"last_name":"Leclercq","first_name":"F.","full_name":"Leclercq, F."},{"full_name":"Abril-Melgarejo, V.","last_name":"Abril-Melgarejo","first_name":"V."},{"first_name":"L.","last_name":"Boogaard","full_name":"Boogaard, L."},{"full_name":"Bouché, N. F.","first_name":"N. F.","last_name":"Bouché"},{"first_name":"T.","last_name":"Contini","full_name":"Contini, T."},{"first_name":"A.","last_name":"Feltre","full_name":"Feltre, A."},{"first_name":"B.","last_name":"Guiderdoni","full_name":"Guiderdoni, B."},{"last_name":"Herenz","first_name":"C.","full_name":"Herenz, C."},{"first_name":"W.","last_name":"Kollatschny","full_name":"Kollatschny, W."},{"first_name":"H.","last_name":"Kusakabe","full_name":"Kusakabe, H."},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Michel-Dansac","first_name":"L.","full_name":"Michel-Dansac, L."},{"full_name":"Nanayakkara, T.","first_name":"T.","last_name":"Nanayakkara"},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"full_name":"Roth, M.","last_name":"Roth","first_name":"M."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"M.","last_name":"Steinmetz","full_name":"Steinmetz, M."},{"full_name":"Tresse, L.","last_name":"Tresse","first_name":"L."},{"last_name":"Urrutia","first_name":"T.","full_name":"Urrutia, T."},{"full_name":"Verhamme, A.","last_name":"Verhamme","first_name":"A."},{"first_name":"P. M.","last_name":"Weilbacher","full_name":"Weilbacher, P. M."},{"full_name":"Zabl, J.","last_name":"Zabl","first_name":"J."},{"full_name":"Zoutendijk, S. L.","last_name":"Zoutendijk","first_name":"S. L."}],"doi":"10.1051/0004-6361/202039887","date_updated":"2022-07-19T09:34:57Z","article_processing_charge":"No","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"quality_controlled":"1","article_number":"A107"},{"article_number":"12","article_processing_charge":"No","date_updated":"2022-07-19T09:32:48Z","doi":"10.3847/1538-4357/ac01d7","author":[{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"first_name":"Rychard J.","last_name":"Bouwens","full_name":"Bouwens, Rychard J."},{"full_name":"Riechers, Dominik","first_name":"Dominik","last_name":"Riechers"},{"last_name":"van der Werf","first_name":"Paul","full_name":"van der Werf, Paul"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Stefanon","first_name":"Mauro","full_name":"Stefanon, Mauro"},{"last_name":"Feltre","first_name":"Anna","full_name":"Feltre, Anna"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"first_name":"Manuel","last_name":"Aravena","full_name":"Aravena, Manuel"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Carilli","first_name":"Chris","full_name":"Carilli, Chris"},{"full_name":"Contini, Thierry","last_name":"Contini","first_name":"Thierry"},{"first_name":"Roberto","last_name":"Decarli","full_name":"Decarli, Roberto"},{"last_name":"González-López","first_name":"Jorge","full_name":"González-López, Jorge"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"}],"date_published":"2021-07-20T00:00:00Z","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2105.12489","open_access":"1"}],"intvolume":" 916","day":"20","month":"07","language":[{"iso":"eng"}],"publisher":"IOP Publishing","publication":"The Astrophysical Journal","title":"Measuring the average molecular gas content of star-forming galaxies at z = 3–4","date_created":"2022-07-06T13:05:50Z","oa_version":"Preprint","arxiv":1,"extern":"1","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]."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":916,"year":"2021","_id":"11512","issue":"1","external_id":{"arxiv":["2105.12489"]},"article_type":"original","status":"public","oa":1,"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.","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"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","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).","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.","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"}},{"month":"12","language":[{"iso":"eng"}],"day":"01","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}],"intvolume":" 508","quality_controlled":"1","keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"scopus_import":"1","article_processing_charge":"No","doi":"10.1093/mnras/stab2762","date_updated":"2022-08-18T10:45:56Z","author":[{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"first_name":"Pierre","last_name":"Ocvirk","full_name":"Ocvirk, Pierre"},{"full_name":"Mason, Charlotte","first_name":"Charlotte","last_name":"Mason"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Bosman","first_name":"Sarah E I","full_name":"Bosman, Sarah E I"},{"full_name":"Sorce, Jenny G","first_name":"Jenny G","last_name":"Sorce"},{"full_name":"Lewis, Joseph","first_name":"Joseph","last_name":"Lewis"},{"last_name":"Ahn","first_name":"Kyungjin","full_name":"Ahn, Kyungjin"},{"last_name":"Aubert","first_name":"Dominique","full_name":"Aubert, Dominique"},{"full_name":"Dawoodbhoy, Taha","last_name":"Dawoodbhoy","first_name":"Taha"},{"first_name":"Ilian T","last_name":"Iliev","full_name":"Iliev, Ilian T"},{"last_name":"Shapiro","first_name":"Paul R","full_name":"Shapiro, Paul R"},{"first_name":"Gustavo","last_name":"Yepes","full_name":"Yepes, Gustavo"}],"date_published":"2021-12-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"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.","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","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","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.","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.","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."},"issue":"3","external_id":{"arxiv":["2004.14496"]},"article_type":"original","oa":1,"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.","status":"public","year":"2021","_id":"11522","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":508,"page":"3697-3709","extern":"1","abstract":[{"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.","lang":"eng"}],"arxiv":1,"date_created":"2022-07-07T09:30:21Z","oa_version":"Preprint","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation"},{"language":[{"iso":"eng"}],"month":"07","day":"01","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2102.07779","open_access":"1"}],"intvolume":" 505","quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"doi":"10.1093/mnras/stab1304","date_updated":"2022-08-18T10:49:00Z","article_processing_charge":"No","author":[{"last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Hayes, Matthew","last_name":"Hayes","first_name":"Matthew"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"full_name":"Naidu, Rohan P","last_name":"Naidu","first_name":"Rohan P"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"first_name":"Ricardo","last_name":"Amorín","full_name":"Amorín, Ricardo"}],"date_published":"2021-07-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"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","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.","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.","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.","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.","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"},"article_type":"original","external_id":{"arxiv":["2102.07779"]},"issue":"1","oa":1,"status":"public","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).","year":"2021","_id":"11523","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"1382-1412","volume":505,"extern":"1","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⊙."}],"arxiv":1,"oa_version":"Preprint","date_created":"2022-07-07T09:33:39Z","publisher":"Oxford University Press","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","publication":"Monthly Notices of the Royal Astronomical Society"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"],"scopus_import":"1","quality_controlled":"1","date_published":"2021-07-01T00:00:00Z","author":[{"last_name":"Santos","first_name":"S","full_name":"Santos, S"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Butterworth, J","last_name":"Butterworth","first_name":"J"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"full_name":"Ribeiro, B","last_name":"Ribeiro","first_name":"B"},{"full_name":"da Cunha, E","first_name":"E","last_name":"da Cunha"},{"full_name":"Calhau, J","last_name":"Calhau","first_name":"J"},{"full_name":"Khostovan, A A","first_name":"A A","last_name":"Khostovan"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"first_name":"P","last_name":"Arrabal Haro","full_name":"Arrabal Haro, P"}],"article_processing_charge":"No","doi":"10.1093/mnras/stab1218","date_updated":"2022-08-18T10:51:47Z","intvolume":" 505","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.00007"}],"publication_status":"published","month":"07","language":[{"iso":"eng"}],"day":"01","date_created":"2022-07-07T10:02:59Z","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","publisher":"Oxford University Press","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."}],"extern":"1","arxiv":1,"_id":"11524","year":"2021","volume":505,"page":"1117-1134","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","citation":{"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.","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.","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","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","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.","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."},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","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).","oa":1,"issue":"1","article_type":"original","external_id":{"arxiv":["2105.00007"]}},{"arxiv":1,"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."}],"extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","title":"Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations","publisher":"Oxford University Press","date_created":"2022-07-07T10:07:11Z","oa_version":"Preprint","status":"public","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).","oa":1,"issue":"1","article_type":"original","external_id":{"arxiv":["2103.09250"]},"citation":{"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.","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.","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.","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"},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"volume":504,"page":"16-32","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","_id":"11525","year":"2021","date_published":"2021-06-01T00:00:00Z","author":[{"full_name":"Gallego, Sofia G","last_name":"Gallego","first_name":"Sofia G"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"first_name":"Saeed","last_name":"Sarpas","full_name":"Sarpas, Saeed"},{"full_name":"Duboeuf, Bastien","first_name":"Bastien","last_name":"Duboeuf"},{"last_name":"Lilly","first_name":"Simon","full_name":"Lilly, Simon"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"full_name":"Mauerhofer, Valentin","first_name":"Valentin","last_name":"Mauerhofer"}],"article_processing_charge":"No","doi":"10.1093/mnras/stab796","date_updated":"2022-08-18T10:54:19Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","quality_controlled":"1","day":"01","month":"06","language":[{"iso":"eng"}],"main_file_link":[{"url":"https://arxiv.org/abs/2103.09250","open_access":"1"}],"intvolume":" 504","publication_status":"published"},{"volume":502,"page":"494-509","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","_id":"11526","year":"2021","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).","status":"public","oa":1,"issue":"1","external_id":{"arxiv":["2010.12589"]},"article_type":"original","citation":{"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.","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.","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.","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"},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","publisher":"Oxford University Press","date_created":"2022-07-07T10:11:15Z","oa_version":"Preprint","arxiv":1,"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."}],"extern":"1","intvolume":" 502","main_file_link":[{"url":"https://arxiv.org/abs/2010.12589","open_access":"1"}],"publication_status":"published","day":"01","month":"03","language":[{"iso":"eng"}],"author":[{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"first_name":"Raffaella A","last_name":"Marino","full_name":"Marino, Raffaella A"},{"last_name":"Lilly","first_name":"Simon","full_name":"Lilly, Simon"},{"full_name":"Muzahid, Sowgat","last_name":"Muzahid","first_name":"Sowgat"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"date_published":"2021-03-01T00:00:00Z","article_processing_charge":"No","doi":"10.1093/mnras/staa3277","date_updated":"2022-08-18T10:56:28Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"scopus_import":"1","quality_controlled":"1"},{"publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"intvolume":" 5","language":[{"iso":"eng"}],"month":"07","day":"05","quality_controlled":"1","scopus_import":"1","keyword":["Astronomy and Astrophysics","galaxies","formation - galaxies","evolution - galaxies","star formation - galaxies","abundances"],"doi":"10.1038/s41550-021-01415-y","date_updated":"2022-08-19T08:37:58Z","article_processing_charge":"No","author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"date_published":"2021-07-05T00:00:00Z","year":"2021","_id":"11585","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"984-985","volume":5,"publication_identifier":{"eissn":["2397-3366"]},"citation":{"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.","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."},"external_id":{"arxiv":["1802.06786"]},"article_type":"original","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.","oa":1,"status":"public","oa_version":"Preprint","date_created":"2022-07-14T13:13:39Z","publisher":"Springer Nature","title":"Differences in galaxy colours are not just about the mass","publication":"Nature Astronomy","extern":"1","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."}],"arxiv":1},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","quality_controlled":"1","date_published":"2021-10-21T00:00:00Z","author":[{"first_name":"J.","last_name":"Audenaert","full_name":"Audenaert, J."},{"full_name":"Kuszlewicz, J. S.","first_name":"J. S.","last_name":"Kuszlewicz"},{"last_name":"Handberg","first_name":"R.","full_name":"Handberg, R."},{"first_name":"A.","last_name":"Tkachenko","full_name":"Tkachenko, A."},{"first_name":"D. J.","last_name":"Armstrong","full_name":"Armstrong, D. J."},{"full_name":"Hon, M.","first_name":"M.","last_name":"Hon"},{"full_name":"Kgoadi, R.","first_name":"R.","last_name":"Kgoadi"},{"full_name":"Lund, M. N.","last_name":"Lund","first_name":"M. N."},{"full_name":"Bell, K. J.","first_name":"K. J.","last_name":"Bell"},{"orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"D. M.","last_name":"Bowman","full_name":"Bowman, D. M."},{"full_name":"Johnston, C.","last_name":"Johnston","first_name":"C."},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"first_name":"D.","last_name":"Stello","full_name":"Stello, D."},{"first_name":"L.","last_name":"Molnár","full_name":"Molnár, L."},{"full_name":"Plachy, E.","last_name":"Plachy","first_name":"E."},{"last_name":"Buzasi","first_name":"D.","full_name":"Buzasi, D."},{"full_name":"Aerts, C.","first_name":"C.","last_name":"Aerts"}],"article_processing_charge":"No","date_updated":"2022-08-19T10:01:56Z","doi":"10.3847/1538-3881/ac166a","article_number":"209","month":"10","language":[{"iso":"eng"}],"day":"21","intvolume":" 162","main_file_link":[{"url":"https://arxiv.org/abs/2107.06301","open_access":"1"}],"publication_status":"published","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."}],"extern":"1","arxiv":1,"date_created":"2022-07-18T11:54:55Z","oa_version":"Preprint","publication":"The Astronomical Journal","title":"TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data","publisher":"IOP Publishing","citation":{"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.","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).","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.","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"},"publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"oa":1,"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).","status":"public","issue":"5","external_id":{"arxiv":["2107.06301"]},"article_type":"original","_id":"11604","year":"2021","volume":162,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article"},{"citation":{"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.","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","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","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.","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.","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)."},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"status":"public","external_id":{"arxiv":["2102.01216"]},"article_type":"original","_id":"11605","year":"2021","volume":650,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","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."}],"extern":"1","arxiv":1,"date_created":"2022-07-18T12:10:59Z","oa_version":"Preprint","publication":"Astronomy & Astrophysics","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","publisher":"EDP Sciences","month":"06","language":[{"iso":"eng"}],"day":"07","main_file_link":[{"url":"https://arxiv.org/abs/2102.01216","open_access":"1"}],"intvolume":" 650","publication_status":"published","keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"scopus_import":"1","quality_controlled":"1","date_published":"2021-06-07T00:00:00Z","author":[{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Prat, V.","last_name":"Prat","first_name":"V."},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"first_name":"A.","last_name":"Astoul","full_name":"Astoul, A."},{"last_name":"Augustson","first_name":"K.","full_name":"Augustson, K."},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"first_name":"L.","last_name":"Amard","full_name":"Amard, L."},{"full_name":"Neiner, C.","last_name":"Neiner","first_name":"C."}],"article_processing_charge":"No","date_updated":"2022-08-19T10:06:33Z","doi":"10.1051/0004-6361/202039159","article_number":"A53"},{"arxiv":1,"extern":"1","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."}],"publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","date_created":"2022-07-18T12:15:27Z","oa_version":"Preprint","article_type":"original","external_id":{"arxiv":["2012.11050"]},"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.","oa":1,"status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"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.","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","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","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.","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.","short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy & Astrophysics 647 (2021)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":647,"year":"2021","_id":"11606","article_processing_charge":"No","doi":"10.1051/0004-6361/202039180","date_updated":"2022-08-19T10:11:52Z","date_published":"2021-03-18T00:00:00Z","author":[{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Prat, V.","first_name":"V.","last_name":"Prat"},{"full_name":"Augustson, K.","first_name":"K.","last_name":"Augustson"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"first_name":"R. A.","last_name":"Garcia","full_name":"Garcia, R. A."}],"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"],"scopus_import":"1","article_number":"A122","day":"18","month":"03","language":[{"iso":"eng"}],"publication_status":"published","intvolume":" 647","main_file_link":[{"url":"https://arxiv.org/abs/2012.11050","open_access":"1"}]},{"article_number":"A125","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis / stars: solar-type / stars: activity / stars: rotation / starspots"],"scopus_import":"1","article_processing_charge":"No","date_updated":"2022-08-22T08:47:47Z","doi":"10.1051/0004-6361/202039947","author":[{"first_name":"S. N.","last_name":"Breton","full_name":"Breton, S. N."},{"first_name":"A. R. G.","last_name":"Santos","full_name":"Santos, A. R. G."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"first_name":"P. L.","last_name":"Pallé","full_name":"Pallé, P. L."}],"date_published":"2021-03-19T00:00:00Z","publication_status":"published","intvolume":" 647","main_file_link":[{"url":"https://arxiv.org/abs/2101.10152","open_access":"1"}],"month":"03","language":[{"iso":"eng"}],"day":"19","date_created":"2022-07-18T12:21:32Z","oa_version":"Preprint","publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","title":"ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods","extern":"1","abstract":[{"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.","lang":"eng"}],"arxiv":1,"year":"2021","_id":"11608","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":647,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"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","short":"S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé, Astronomy & Astrophysics 647 (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.","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.","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"},"article_type":"original","external_id":{"arxiv":["2101.10152"]},"oa":1,"status":"public","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 ."},{"publication_status":"published","intvolume":" 646","main_file_link":[{"url":"https://arxiv.org/abs/2006.10660","open_access":"1"}],"day":"08","language":[{"iso":"eng"}],"month":"02","article_number":"A64","doi":"10.1051/0004-6361/202038654","date_updated":"2022-08-19T10:18:03Z","article_processing_charge":"No","date_published":"2021-02-08T00:00:00Z","author":[{"first_name":"J.","last_name":"Park","full_name":"Park, J."},{"first_name":"V.","last_name":"Prat","full_name":"Prat, V."},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"}],"quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","hydrodynamics / turbulence / stars","rotation / stars","evolution"],"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":646,"year":"2021","_id":"11609","article_type":"original","external_id":{"arxiv":["2006.10660"]},"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.","oa":1,"status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"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.","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","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","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.","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.","short":"J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy & Astrophysics 646 (2021)."},"publisher":"EDP Sciences","title":"Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration","publication":"Astronomy & Astrophysics","oa_version":"Preprint","date_created":"2022-07-18T13:24:32Z","arxiv":1,"extern":"1","abstract":[{"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.","lang":"eng"}]},{"month":"06","language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1861-2288"]},"citation":{"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.","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.","ista":"Henzinger MH, Paz A, Schmid S. 2021. On the complexity of weight-dynamic network algorithms. IFIP Networking Conference. IFIP: Networking.","short":"M.H. Henzinger, A. Paz, S. Schmid, in:, IFIP Networking Conference, Institute of Electrical and Electronics Engineers, 2021.","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"},"day":"21","external_id":{"arxiv":["2105.13172"]},"status":"public","oa":1,"year":"2021","publication_status":"published","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.2105.13172","open_access":"1"}],"_id":"11649","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"conference","extern":"1","quality_controlled":"1","scopus_import":"1","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","date_updated":"2023-02-09T09:11:51Z","doi":"10.23919/ifipnetworking52078.2021.9472803","date_published":"2021-06-21T00:00:00Z","author":[{"last_name":"Henzinger","orcid":"0000-0002-5008-6530","first_name":"Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","full_name":"Henzinger, Monika H"},{"first_name":"Ami","last_name":"Paz","full_name":"Paz, Ami"},{"full_name":"Schmid, Stefan","first_name":"Stefan","last_name":"Schmid"}],"arxiv":1,"conference":{"name":"IFIP: Networking","end_date":"2021-06-24","location":" Espoo and Helsinki, Finland","start_date":"2021-06-21"},"date_created":"2022-07-25T11:13:06Z","oa_version":"Preprint","publisher":"Institute of Electrical and Electronics Engineers","publication":"IFIP Networking Conference","title":"On the complexity of weight-dynamic network algorithms"},{"status":"public","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.","oa":1,"article_type":"original","external_id":{"arxiv":["1810.10932"]},"issue":"4","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","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).","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.","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.","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.","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"},"publication_identifier":{"eissn":["1549-6333"],"issn":["1549-6325"]},"volume":17,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11663","year":"2021","arxiv":1,"abstract":[{"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.","lang":"eng"}],"extern":"1","title":"A deamortization approach for dynamic spanner and dynamic maximal matching","publication":"ACM Transactions on Algorithms","publisher":"Association for Computing Machinery","oa_version":"Preprint","date_created":"2022-07-27T11:09:06Z","day":"04","language":[{"iso":"eng"}],"month":"10","main_file_link":[{"url":"https://arxiv.org/abs/1810.10932","open_access":"1"}],"intvolume":" 17","publication_status":"published","date_published":"2021-10-04T00:00:00Z","author":[{"full_name":"Bernstein, Aaron","first_name":"Aaron","last_name":"Bernstein"},{"full_name":"Forster, Sebastian","last_name":"Forster","first_name":"Sebastian"},{"full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","first_name":"Monika H","last_name":"Henzinger","orcid":"0000-0002-5008-6530"}],"doi":"10.1145/3469833","date_updated":"2022-09-09T11:35:44Z","article_processing_charge":"No","scopus_import":"1","quality_controlled":"1","article_number":"29"},{"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2011.00977"}],"intvolume":" 281","language":[{"iso":"eng"}],"month":"12","day":"01","article_number":"104805","quality_controlled":"1","scopus_import":"1","date_updated":"2022-09-12T09:29:29Z","doi":"10.1016/j.ic.2021.104805","article_processing_charge":"No","author":[{"orcid":"0000-0002-5008-6530","last_name":"Henzinger","first_name":"Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","full_name":"Henzinger, Monika H"},{"full_name":"Peng, Pan","last_name":"Peng","first_name":"Pan"}],"date_published":"2021-12-01T00:00:00Z","year":"2021","_id":"11756","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":281,"publication_identifier":{"issn":["0890-5401"]},"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","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.","ista":"Henzinger MH, Peng P. 2021. Constant-time dynamic weight approximation for minimum spanning forest. Information and Computation. 281(12), 104805.","short":"M.H. Henzinger, P. Peng, Information and Computation 281 (2021).","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.","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"},"external_id":{"arxiv":["2011.00977"]},"article_type":"original","issue":"12","status":"public","oa":1,"oa_version":"Preprint","date_created":"2022-08-08T10:58:29Z","publisher":"Elsevier","title":"Constant-time dynamic weight approximation for minimum spanning forest","publication":"Information and Computation","extern":"1","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."}],"arxiv":1},{"conference":{"end_date":"2021-08-11","name":"WADS: Workshop on Algorithms and Data Structures","start_date":"2021-08-09","location":"Virtual"},"article_processing_charge":"No","alternative_title":["LNCS"],"date_updated":"2023-02-10T08:31:50Z","doi":"10.1007/978-3-030-83508-8_34","author":[{"full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","first_name":"Monika H","orcid":"0000-0002-5008-6530","last_name":"Henzinger"},{"full_name":"Wu, Xiaowei","first_name":"Xiaowei","last_name":"Wu"}],"date_published":"2021-08-09T00:00:00Z","quality_controlled":"1","scopus_import":"1","publication_status":"published","intvolume":" 12808","main_file_link":[{"url":"https://arxiv.org/abs/1910.03332","open_access":"1"}],"day":"09","month":"08","language":[{"iso":"eng"}],"publisher":"Springer Nature","publication":"17th International Symposium on Algorithms and Data Structures","title":"Upper and lower bounds for fully retroactive graph problems","date_created":"2022-08-08T13:01:29Z","oa_version":"Preprint","arxiv":1,"extern":"1","abstract":[{"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 𝑂(𝑛1−𝜖) time per operation, for any constant 𝜖>0. Furthermore, We provide RDS with almost tight time per operation. We give fully RDS for maintaining the maximum degree, connectivity and MSF in 𝑂̃ (𝑛) time per operation. We also give an algorithm for the incremental (insertion-only) fully retroactive connectivity with 𝑂̃ (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.","lang":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"conference","volume":12808,"page":"471–484","year":"2021","_id":"11771","external_id":{"arxiv":["1910.03332"]},"oa":1,"status":"public","publication_identifier":{"isbn":["9783030835071"],"issn":["0302-9743"],"eisbn":["9783030835088"],"eissn":["1611-3349"]},"citation":{"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.","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","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.","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."}},{"date_updated":"2024-03-07T15:03:00Z","related_material":{"record":[{"relation":"dissertation_contains","status":"public","id":"14323"}]},"doi":"10.1002/wdev.383","article_processing_charge":"Yes (via OA deal)","author":[{"id":"4CED352A-F248-11E8-B48F-1D18A9856A87","full_name":"Kuzmicz-Kowalska, Katarzyna","last_name":"Kuzmicz-Kowalska","first_name":"Katarzyna"},{"full_name":"Kicheva, Anna","id":"3959A2A0-F248-11E8-B48F-1D18A9856A87","first_name":"Anna","orcid":"0000-0003-4509-4998","last_name":"Kicheva"}],"date_published":"2021-04-15T00:00:00Z","quality_controlled":"1","scopus_import":"1","article_number":"e383","file_date_updated":"2020-11-24T13:11:39Z","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"day":"15","ddc":["570"],"pmid":1,"language":[{"iso":"eng"}],"project":[{"name":"Coordination of Patterning And Growth In the Spinal Cord","grant_number":"680037","_id":"B6FC0238-B512-11E9-945C-1524E6697425","call_identifier":"H2020"},{"_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"}],"isi":1,"month":"04","license":"https://creativecommons.org/licenses/by/4.0/","publication_status":"published","file":[{"content_type":"application/pdf","success":1,"date_created":"2020-11-24T13:11:39Z","relation":"main_file","creator":"dernst","access_level":"open_access","file_size":2527276,"file_name":"2020_WIREs_DevBio_KuzmiczKowalska.pdf","checksum":"f0a7745d48afa09ea7025e876a0145a8","date_updated":"2020-11-24T13:11:39Z","file_id":"8800"}],"abstract":[{"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.","lang":"eng"}],"publisher":"Wiley","title":"Regulation of size and scale in vertebrate spinal cord development","department":[{"_id":"AnKi"}],"publication":"Wiley Interdisciplinary Reviews: Developmental Biology","oa_version":"Published Version","ec_funded":1,"date_created":"2020-05-24T22:01:00Z","external_id":{"isi":["000531419400001"],"pmid":["32391980"]},"article_type":"original","oa":1,"status":"public","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","publication_identifier":{"issn":["17597684"],"eissn":["17597692"]},"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","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).","ista":"Kuzmicz-Kowalska K, Kicheva A. 2021. Regulation of size and scale in vertebrate spinal cord development. Wiley Interdisciplinary Reviews: Developmental Biology., e383.","ieee":"K. Kuzmicz-Kowalska and A. Kicheva, “Regulation of size and scale in vertebrate spinal cord development,” Wiley Interdisciplinary Reviews: Developmental Biology. Wiley, 2021.","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.","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"},"type":"journal_article","user_id":"3E5EF7F0-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","year":"2021","_id":"7883"},{"publication_status":"published","intvolume":" 33","main_file_link":[{"url":"https://arxiv.org/abs/1910.08190","open_access":"1"}],"day":"01","project":[{"call_identifier":"H2020","_id":"25C6DC12-B435-11E9-9278-68D0E5697425","name":"Analysis of quantum many-body systems","grant_number":"694227"}],"language":[{"iso":"eng"}],"month":"01","isi":1,"article_number":"2060009","doi":"10.1142/s0129055x20600090","date_updated":"2023-09-05T16:07:40Z","article_processing_charge":"No","author":[{"id":"3DE6C32A-F248-11E8-B48F-1D18A9856A87","full_name":"Benedikter, Niels P","orcid":"0000-0002-1071-6091","last_name":"Benedikter","first_name":"Niels P"}],"date_published":"2021-01-01T00:00:00Z","quality_controlled":"1","scopus_import":"1","type":"journal_article","user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","volume":33,"year":"2021","_id":"7900","external_id":{"arxiv":["1910.08190"],"isi":["000613313200010"]},"article_type":"original","issue":"1","status":"public","oa":1,"publication_identifier":{"issn":["0129-055X"],"eissn":["1793-6659"]},"citation":{"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).","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","ieee":"N. P. Benedikter, “Bosonic collective excitations in Fermi gases,” Reviews in Mathematical Physics, vol. 33, no. 1. World Scientific, 2021.","chicago":"Benedikter, Niels P. “Bosonic Collective Excitations in Fermi Gases.” Reviews in Mathematical Physics. World Scientific, 2021. https://doi.org/10.1142/s0129055x20600090."},"publisher":"World Scientific","department":[{"_id":"RoSe"}],"title":"Bosonic collective excitations in Fermi gases","publication":"Reviews in Mathematical Physics","oa_version":"Preprint","ec_funded":1,"date_created":"2020-05-28T16:47:55Z","arxiv":1,"abstract":[{"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.","lang":"eng"}]},{"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file_date_updated":"2022-05-16T12:23:40Z","quality_controlled":"1","scopus_import":"1","doi":"10.1007/s00222-021-01041-5","date_updated":"2023-08-21T06:30:30Z","article_processing_charge":"Yes (via OA deal)","author":[{"id":"3DE6C32A-F248-11E8-B48F-1D18A9856A87","full_name":"Benedikter, Niels P","orcid":"0000-0002-1071-6091","last_name":"Benedikter","first_name":"Niels P"},{"full_name":"Nam, Phan Thành","first_name":"Phan Thành","last_name":"Nam"},{"full_name":"Porta, Marcello","last_name":"Porta","first_name":"Marcello"},{"last_name":"Schlein","first_name":"Benjamin","full_name":"Schlein, Benjamin"},{"first_name":"Robert","last_name":"Seiringer","orcid":"0000-0002-6781-0521","full_name":"Seiringer, Robert","id":"4AFD0470-F248-11E8-B48F-1D18A9856A87"}],"date_published":"2021-05-03T00:00:00Z","publication_status":"published","file":[{"file_size":1089319,"checksum":"f38c79dfd828cdc7f49a34b37b83d376","file_name":"2021_InventMath_Benedikter.pdf","file_id":"11386","date_updated":"2022-05-16T12:23:40Z","content_type":"application/pdf","date_created":"2022-05-16T12:23:40Z","success":1,"relation":"main_file","access_level":"open_access","creator":"dernst"}],"intvolume":" 225","project":[{"_id":"B67AFEDC-15C9-11EA-A837-991A96BB2854","name":"IST Austria Open Access Fund"},{"name":"Analysis of quantum many-body systems","grant_number":"694227","_id":"25C6DC12-B435-11E9-9278-68D0E5697425","call_identifier":"H2020"}],"language":[{"iso":"eng"}],"month":"05","isi":1,"day":"03","ddc":["510"],"oa_version":"Published Version","date_created":"2020-05-28T16:48:20Z","ec_funded":1,"publisher":"Springer","department":[{"_id":"RoSe"}],"title":"Correlation energy of a weakly interacting Fermi gas","publication":"Inventiones Mathematicae","abstract":[{"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.","lang":"eng"}],"arxiv":1,"year":"2021","has_accepted_license":"1","_id":"7901","type":"journal_article","user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","page":"885-979","volume":225,"publication_identifier":{"issn":["0020-9910"],"eissn":["1432-1297"]},"citation":{"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.","short":"N.P. Benedikter, P.T. Nam, M. Porta, B. Schlein, R. Seiringer, Inventiones Mathematicae 225 (2021) 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.","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","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.","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."},"external_id":{"arxiv":["2005.08933"],"isi":["000646573600001"]},"article_type":"original","status":"public","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.","oa":1}]