[{"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa_version":"Preprint","month":"07","article_number":"12","publication":"The Astrophysical Journal","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.12489"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"oa":1,"date_published":"2021-07-20T00:00:00Z","type":"journal_article","publisher":"IOP Publishing","article_type":"original","quality_controlled":"1","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-06T13:05:50Z","title":"Measuring the average molecular gas content of star-forming galaxies at z = 3–4","intvolume":" 916","_id":"11512","scopus_import":"1","author":[{"first_name":"Leindert A.","last_name":"Boogaard","full_name":"Boogaard, Leindert A."},{"full_name":"Bouwens, Rychard J.","last_name":"Bouwens","first_name":"Rychard J."},{"last_name":"Riechers","first_name":"Dominik","full_name":"Riechers, Dominik"},{"last_name":"van der Werf","first_name":"Paul","full_name":"van der Werf, Paul"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Stefanon, Mauro","first_name":"Mauro","last_name":"Stefanon"},{"first_name":"Anna","last_name":"Feltre","full_name":"Feltre, Anna"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"full_name":"Aravena, Manuel","last_name":"Aravena","first_name":"Manuel"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"full_name":"Carilli, Chris","first_name":"Chris","last_name":"Carilli"},{"full_name":"Contini, Thierry","last_name":"Contini","first_name":"Thierry"},{"first_name":"Roberto","last_name":"Decarli","full_name":"Decarli, Roberto"},{"first_name":"Jorge","last_name":"González-López","full_name":"González-López, Jorge"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Fabian","last_name":"Walter","full_name":"Walter, Fabian"}],"issue":"1","volume":916,"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.","extern":"1","arxiv":1,"doi":"10.3847/1538-4357/ac01d7","day":"20","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]."}],"date_updated":"2022-07-19T09:32:48Z","year":"2021","citation":{"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).","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.","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.","ama":"Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. 2021;916(1). doi:10.3847/1538-4357/ac01d7","apa":"Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R., Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac01d7","chicago":"Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” The Astrophysical Journal. IOP Publishing, 2021. https://doi.org/10.3847/1538-4357/ac01d7.","ieee":"L. A. Boogaard et al., “Measuring the average molecular gas content of star-forming galaxies at z = 3–4,” The Astrophysical Journal, vol. 916, no. 1. IOP Publishing, 2021."},"external_id":{"arxiv":["2105.12489"]}},{"day":"01","doi":"10.1093/mnras/stab1304","arxiv":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⊙."}],"year":"2021","citation":{"ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412.","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:10.1093/mnras/stab1304.","short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","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.","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.","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","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"},"date_updated":"2022-08-18T10:49:00Z","external_id":{"arxiv":["2102.07779"]},"volume":505,"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).","extern":"1","article_processing_charge":"No","date_created":"2022-07-07T09:33:39Z","publication_status":"published","intvolume":" 505","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","scopus_import":"1","_id":"11523","issue":"1","author":[{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Hayes","first_name":"Matthew","full_name":"Hayes, Matthew"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"full_name":"Naidu, Rohan P","first_name":"Rohan P","last_name":"Naidu"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"full_name":"Amorín, Ricardo","last_name":"Amorín","first_name":"Ricardo"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"1382-1412","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2021-07-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.07779"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"07","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"language":[{"iso":"eng"}]},{"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."}],"arxiv":1,"doi":"10.1093/mnras/stab1218","day":"01","external_id":{"arxiv":["2105.00007"]},"date_updated":"2022-08-18T10:51:47Z","citation":{"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.","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.","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.","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","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."},"year":"2021","extern":"1","volume":505,"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).","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","intvolume":" 505","publication_status":"published","date_created":"2022-07-07T10:02:59Z","article_processing_charge":"No","author":[{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"first_name":"D","last_name":"Sobral","full_name":"Sobral, D"},{"first_name":"J","last_name":"Butterworth","full_name":"Butterworth, J"},{"full_name":"Paulino-Afonso, A","first_name":"A","last_name":"Paulino-Afonso"},{"full_name":"Ribeiro, B","last_name":"Ribeiro","first_name":"B"},{"full_name":"da Cunha, E","first_name":"E","last_name":"da Cunha"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"},{"full_name":"Khostovan, A A","first_name":"A A","last_name":"Khostovan"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"last_name":"Arrabal Haro","first_name":"P","full_name":"Arrabal Haro, P"}],"issue":"1","_id":"11524","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"1117-1134","quality_controlled":"1","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2021-07-01T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2105.00007","open_access":"1"}],"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"]},{"author":[{"full_name":"Gallego, Sofia G","last_name":"Gallego","first_name":"Sofia G"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"last_name":"Sarpas","first_name":"Saeed","full_name":"Sarpas, Saeed"},{"last_name":"Duboeuf","first_name":"Bastien","full_name":"Duboeuf, Bastien"},{"last_name":"Lilly","first_name":"Simon","full_name":"Lilly, Simon"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Raffaella Anna","last_name":"Marino","full_name":"Marino, Raffaella Anna"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"first_name":"Valentin","last_name":"Mauerhofer","full_name":"Mauerhofer, Valentin"}],"issue":"1","_id":"11525","scopus_import":"1","title":"Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations","intvolume":" 504","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T10:07:11Z","page":"16-32","quality_controlled":"1","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["2103.09250"]},"date_updated":"2022-08-18T10:54:19Z","citation":{"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.","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","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","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."},"year":"2021","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."}],"arxiv":1,"doi":"10.1093/mnras/stab796","day":"01","extern":"1","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).","volume":504,"publication":"Monthly Notices of the Royal Astronomical Society","month":"06","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_published":"2021-06-01T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2103.09250","open_access":"1"}]},{"publication":"Monthly Notices of the Royal Astronomical Society","month":"03","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2021-03-01T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2010.12589"}],"issue":"1","author":[{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Marino, Raffaella A","last_name":"Marino","first_name":"Raffaella A"},{"full_name":"Lilly, Simon","last_name":"Lilly","first_name":"Simon"},{"last_name":"Muzahid","first_name":"Sowgat","full_name":"Muzahid, Sowgat"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"}],"scopus_import":"1","_id":"11526","intvolume":" 502","title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","article_processing_charge":"No","date_created":"2022-07-07T10:11:15Z","publication_status":"published","quality_controlled":"1","page":"494-509","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["2010.12589"]},"year":"2021","citation":{"ama":"Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 2021;502(1):494-509. doi:10.1093/mnras/staa3277","apa":"Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid, S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3277","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.","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.","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.","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."},"date_updated":"2022-08-18T10:56:28Z","abstract":[{"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.","lang":"eng"}],"day":"01","arxiv":1,"doi":"10.1093/mnras/staa3277","extern":"1","volume":502,"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)."},{"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).","volume":162,"extern":"1","day":"21","arxiv":1,"doi":"10.3847/1538-3881/ac166a","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."}],"citation":{"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.","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).","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.","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.","ama":"Audenaert J, Kuszlewicz JS, Handberg R, et al. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. The Astronomical Journal. 2021;162(5). doi:10.3847/1538-3881/ac166a","apa":"Audenaert, J., Kuszlewicz, J. S., Handberg, R., Tkachenko, A., Armstrong, D. J., Hon, M., … Aerts, C. (2021). TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. The Astronomical Journal. IOP Publishing. https://doi.org/10.3847/1538-3881/ac166a"},"year":"2021","date_updated":"2022-08-19T10:01:56Z","external_id":{"arxiv":["2107.06301"]},"publisher":"IOP Publishing","article_type":"original","quality_controlled":"1","date_created":"2022-07-18T11:54:55Z","article_processing_charge":"No","publication_status":"published","intvolume":" 162","title":"TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data","scopus_import":"1","_id":"11604","issue":"5","author":[{"full_name":"Audenaert, J.","first_name":"J.","last_name":"Audenaert"},{"full_name":"Kuszlewicz, J. S.","last_name":"Kuszlewicz","first_name":"J. S."},{"full_name":"Handberg, R.","last_name":"Handberg","first_name":"R."},{"full_name":"Tkachenko, A.","last_name":"Tkachenko","first_name":"A."},{"first_name":"D. J.","last_name":"Armstrong","full_name":"Armstrong, D. J."},{"first_name":"M.","last_name":"Hon","full_name":"Hon, M."},{"full_name":"Kgoadi, R.","first_name":"R.","last_name":"Kgoadi"},{"full_name":"Lund, M. N.","first_name":"M. N.","last_name":"Lund"},{"first_name":"K. J.","last_name":"Bell","full_name":"Bell, K. J."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"last_name":"Bowman","first_name":"D. M.","full_name":"Bowman, D. M."},{"full_name":"Johnston, C.","first_name":"C.","last_name":"Johnston"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"first_name":"D.","last_name":"Stello","full_name":"Stello, D."},{"full_name":"Molnár, L.","last_name":"Molnár","first_name":"L."},{"last_name":"Plachy","first_name":"E.","full_name":"Plachy, E."},{"full_name":"Buzasi, D.","last_name":"Buzasi","first_name":"D."},{"first_name":"C.","last_name":"Aerts","full_name":"Aerts, C."}],"main_file_link":[{"url":"https://arxiv.org/abs/2107.06301","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"oa":1,"type":"journal_article","date_published":"2021-10-21T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"oa_version":"Preprint","article_number":"209","month":"10","publication":"The Astronomical Journal"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"A53","month":"06","oa_version":"Preprint","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2102.01216","open_access":"1"}],"type":"journal_article","date_published":"2021-06-07T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Prat","first_name":"V.","full_name":"Prat, V."},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"last_name":"Astoul","first_name":"A.","full_name":"Astoul, A."},{"first_name":"K.","last_name":"Augustson","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."},{"full_name":"Amard, L.","last_name":"Amard","first_name":"L."},{"full_name":"Neiner, C.","first_name":"C.","last_name":"Neiner"}],"scopus_import":"1","_id":"11605","intvolume":" 650","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","date_created":"2022-07-18T12:10:59Z","article_processing_charge":"No","publication_status":"published","extern":"1","volume":650,"external_id":{"arxiv":["2102.01216"]},"year":"2021","citation":{"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).","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.","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","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."},"date_updated":"2022-08-19T10:06:33Z","abstract":[{"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.","lang":"eng"}],"day":"07","doi":"10.1051/0004-6361/202039159","arxiv":1},{"quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","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"},{"last_name":"Prat","first_name":"V.","full_name":"Prat, V."},{"full_name":"Augustson, K.","last_name":"Augustson","first_name":"K."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"first_name":"R. A.","last_name":"Garcia","full_name":"Garcia, R. A."}],"scopus_import":"1","_id":"11606","intvolume":" 647","title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","article_processing_charge":"No","date_created":"2022-07-18T12:15:27Z","publication_status":"published","extern":"1","volume":647,"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.","external_id":{"arxiv":["2012.11050"]},"citation":{"mla":"Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” Astronomy & Astrophysics, vol. 647, A122, EDP Sciences, 2021, doi:10.1051/0004-6361/202039180.","short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy & Astrophysics 647 (2021).","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.","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","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.","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."},"year":"2021","date_updated":"2022-08-19T10:11:52Z","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."}],"day":"18","doi":"10.1051/0004-6361/202039180","arxiv":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"A122","month":"03","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2012.11050","open_access":"1"}],"type":"journal_article","date_published":"2021-03-18T00:00:00Z","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"title":"ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods","intvolume":" 647","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-18T12:21:32Z","author":[{"full_name":"Breton, S. N.","last_name":"Breton","first_name":"S. N."},{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Pallé","first_name":"P. L.","full_name":"Pallé, P. L."}],"_id":"11608","scopus_import":"1","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","abstract":[{"lang":"eng","text":"In order to understand stellar evolution, it is crucial to efficiently determine stellar surface rotation periods. Indeed, while they are of great importance in stellar models, angular momentum transport processes inside stars are still poorly understood today. Surface rotation, which is linked to the age of the star, is one of the constraints needed to improve the way those processes are modelled. Statistics of the surface rotation periods for a large sample of stars of different spectral types are thus necessary. An efficient tool to automatically determine reliable rotation periods is needed when dealing with large samples of stellar photometric datasets. The objective of this work is to develop such a tool. For this purpose, machine learning classifiers constitute relevant bases to build our new methodology. Random forest learning abilities are exploited to automate the extraction of rotation periods in Kepler light curves. Rotation periods and complementary parameters are obtained via three different methods: a wavelet analysis, the autocorrelation function of the light curve, and the composite spectrum. We trained three different classifiers: one to detect if rotational modulations are present in the light curve, one to flag close binary or classical pulsators candidates that can bias our rotation period determination, and finally one classifier to provide the final rotation period. We tested our machine learning pipeline on 23 431 stars of the Kepler K and M dwarf reference rotation catalogue for which 60% of the stars have been visually inspected. For the sample of 21 707 stars where all the input parameters are provided to the algorithm, 94.2% of them are correctly classified (as rotating or not). Among the stars that have a rotation period in the reference catalogue, the machine learning provides a period that agrees within 10% of the reference value for 95.3% of the stars. Moreover, the yield of correct rotation periods is raised to 99.5% after visually inspecting 25.2% of the stars. Over the two main analysis steps, rotation classification and period selection, the pipeline yields a global agreement with the reference values of 92.1% and 96.9% before and after visual inspection. Random forest classifiers are efficient tools to determine reliable rotation periods in large samples of stars. The methodology presented here could be easily adapted to extract surface rotation periods for stars with different spectral types or observed by other instruments such as K2, TESS or by PLATO in the near future."}],"doi":"10.1051/0004-6361/202039947","arxiv":1,"day":"19","external_id":{"arxiv":["2101.10152"]},"date_updated":"2022-08-22T08:47:47Z","year":"2021","citation":{"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.","short":"S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé, Astronomy & Astrophysics 647 (2021).","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.","ama":"Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy & Astrophysics. 2021;647. doi:10.1051/0004-6361/202039947","apa":"Breton, S. N., Santos, A. R. G., Bugnet, L. A., Mathur, S., García, R. A., & Pallé, P. L. (2021). ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039947"},"extern":"1","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 .","volume":647,"month":"03","article_number":"A125","oa_version":"Preprint","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis / stars: solar-type / stars: activity / stars: rotation / starspots"],"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_published":"2021-03-19T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2101.10152"}]},{"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"type":"journal_article","date_published":"2021-02-08T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2006.10660","open_access":"1"}],"article_number":"A64","month":"02","oa_version":"Preprint","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","hydrodynamics / turbulence / stars","rotation / stars","evolution"],"language":[{"iso":"eng"}],"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"}],"day":"08","arxiv":1,"doi":"10.1051/0004-6361/202038654","external_id":{"arxiv":["2006.10660"]},"citation":{"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","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.","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.","short":"J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy & Astrophysics 646 (2021).","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."},"year":"2021","date_updated":"2022-08-19T10:18:03Z","extern":"1","volume":646,"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.","intvolume":" 646","title":"Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration","article_processing_charge":"No","date_created":"2022-07-18T13:24:32Z","publication_status":"published","author":[{"full_name":"Park, J.","last_name":"Park","first_name":"J."},{"first_name":"V.","last_name":"Prat","full_name":"Prat, V."},{"full_name":"Mathis, S.","last_name":"Mathis","first_name":"S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"}],"scopus_import":"1","_id":"11609","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1"},{"publication":"The Astrophysical Journal","oa_version":"Preprint","month":"12","article_number":"277","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_published":"2021-12-29T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2107.10933"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"13453","scopus_import":"1","author":[{"first_name":"M.","last_name":"Renzo","full_name":"Renzo, M."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"}],"issue":"2","publication_status":"published","article_processing_charge":"No","date_created":"2023-08-03T10:10:48Z","title":"Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi","intvolume":" 923","quality_controlled":"1","publisher":"American Astronomical Society","article_type":"original","date_updated":"2023-08-21T11:59:34Z","citation":{"mla":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The Astrophysical Journal, vol. 923, no. 2, 277, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac29c5.","short":"M. Renzo, Y.L.L. Götberg, The Astrophysical Journal 923 (2021).","ista":"Renzo M, Götberg YLL. 2021. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 923(2), 277.","ama":"Renzo M, Götberg YLL. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 2021;923(2). doi:10.3847/1538-4357/ac29c5","apa":"Renzo, M., & Götberg, Y. L. L. (2021). Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac29c5","ieee":"M. Renzo and Y. L. L. Götberg, “Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi,” The Astrophysical Journal, vol. 923, no. 2. American Astronomical Society, 2021.","chicago":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac29c5."},"year":"2021","external_id":{"arxiv":["2107.10933"]},"doi":"10.3847/1538-4357/ac29c5","arxiv":1,"day":"29","abstract":[{"text":"Most massive stars are born in binaries close enough for mass transfer episodes. These modify the appearance, structure, and future evolution of both stars. We compute the evolution of a 100-day-period binary, consisting initially of a 25 M⊙ star and a 17 M⊙ star, which experiences stable mass transfer. We focus on the impact of mass accretion on the surface composition, internal rotation, and structure of the accretor. To anchor our models, we show that our accretor broadly reproduces the properties of ζ Ophiuchi, which has long been proposed to have accreted mass before being ejected as a runaway star when the companion exploded. We compare our accretor to models of single rotating stars and find that the later and stronger spin-up provided by mass accretion produces significant differences. Specifically, the core of the accretor retains higher spin at the end of the main sequence, and a convective layer develops that changes its density profile. Moreover, the surface of the accretor star is polluted by CNO-processed material donated by the companion. Our models show effects of mass accretion in binaries that are not captured in single rotating stellar models. This possibly impacts the further evolution (either in a binary or as single stars), the final collapse, and the resulting spin of the compact object.","lang":"eng"}],"volume":923,"extern":"1"},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2109.14817"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2021-12-03T00:00:00Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","oa_version":"Preprint","article_number":"241","month":"12","volume":922,"extern":"1","citation":{"short":"T.L.S. Wong, J. Schwab, Y.L.L. Götberg, The Astrophysical Journal 922 (2021).","mla":"Wong, Tin Long Sunny, et al. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” The Astrophysical Journal, vol. 922, no. 2, 241, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac27ae.","ista":"Wong TLS, Schwab J, Götberg YLL. 2021. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 922(2), 241.","apa":"Wong, T. L. S., Schwab, J., & Götberg, Y. L. L. (2021). Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac27ae","ama":"Wong TLS, Schwab J, Götberg YLL. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 2021;922(2). doi:10.3847/1538-4357/ac27ae","ieee":"T. L. S. Wong, J. Schwab, and Y. L. L. Götberg, “Pre-explosion properties of Helium star donors to thermonuclear supernovae,” The Astrophysical Journal, vol. 922, no. 2. American Astronomical Society, 2021.","chicago":"Wong, Tin Long Sunny, Josiah Schwab, and Ylva Louise Linsdotter Götberg. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac27ae."},"year":"2021","date_updated":"2023-08-21T11:52:05Z","external_id":{"arxiv":["2109.14817"]},"day":"03","arxiv":1,"doi":"10.3847/1538-4357/ac27ae","abstract":[{"lang":"eng","text":"Helium star–carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code MESA, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to near-UV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultra-massive WD in a multiday orbit. However, extending our binary models to initial CO WD masses of up to 1.2 M⊙, we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star–WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition."}],"quality_controlled":"1","publisher":"American Astronomical Society","article_type":"original","scopus_import":"1","_id":"13454","issue":"2","author":[{"full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny","last_name":"Wong"},{"first_name":"Josiah","last_name":"Schwab","full_name":"Schwab, Josiah"},{"full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"}],"date_created":"2023-08-03T10:10:58Z","article_processing_charge":"No","publication_status":"published","intvolume":" 922","title":"Pre-explosion properties of Helium star donors to thermonuclear supernovae"},{"volume":656,"external_id":{"arxiv":["2102.05036"]},"date_updated":"2023-08-21T11:49:15Z","citation":{"chicago":"Laplace, E., S. Justham, M. Renzo, Ylva Louise Linsdotter Götberg, R. Farmer, D. Vartanyan, and S. E. de Mink. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140506.","ieee":"E. Laplace et al., “Different to the core: The pre-supernova structures of massive single and binary-stripped stars,” Astronomy & Astrophysics, vol. 656. EDP Sciences, 2021.","ama":"Laplace E, Justham S, Renzo M, et al. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. 2021;656. doi:10.1051/0004-6361/202140506","apa":"Laplace, E., Justham, S., Renzo, M., Götberg, Y. L. L., Farmer, R., Vartanyan, D., & de Mink, S. E. (2021). Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140506","ista":"Laplace E, Justham S, Renzo M, Götberg YLL, Farmer R, Vartanyan D, de Mink SE. 2021. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. 656, A58.","short":"E. Laplace, S. Justham, M. Renzo, Y.L.L. Götberg, R. Farmer, D. Vartanyan, S.E. de Mink, Astronomy & Astrophysics 656 (2021).","mla":"Laplace, E., et al. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics, vol. 656, A58, EDP Sciences, 2021, doi:10.1051/0004-6361/202140506."},"year":"2021","abstract":[{"lang":"eng","text":"The majority of massive stars live in binary or multiple systems and will interact with a companion during their lifetimes, which helps to explain the observed diversity of core-collapse supernovae. Donor stars in binary systems can lose most of their hydrogen-rich envelopes through mass transfer. As a result, not only are the surface properties affected, but so is the core structure. However, most calculations of the core-collapse properties of massive stars rely on single-star models. We present a systematic study of the difference between the pre-supernova structures of single stars and stars of the same initial mass (11–21 M⊙) that have been stripped due to stable post-main-sequence mass transfer at solar metallicity. We present the pre-supernova core composition with novel diagrams that give an intuitive representation of the isotope distribution. As shown in previous studies, at the edge of the carbon-oxygen core, the binary-stripped star models contain an extended gradient of carbon, oxygen, and neon. This layer remains until core collapse and is more extended in mass for higher initial stellar masses. It originates from the receding of the convective helium core during core helium burning in binary-stripped stars, which does not occur in single-star models. We find that this same evolutionary phase leads to systematic differences in the final density and nuclear energy generation profiles. Binary-stripped star models have systematically higher total masses of carbon at the moment of core collapse compared to single-star models, which likely results in systematically different supernova yields. In about half of our models, the silicon-burning and oxygen-rich layers merge after core silicon burning. We discuss the implications of our findings for the “explodability”, supernova observations, and nucleosynthesis of these stars. Our models are publicly available and can be readily used as input for detailed supernova simulations."}],"doi":"10.1051/0004-6361/202140506","arxiv":1,"day":"02","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","author":[{"full_name":"Laplace, E.","last_name":"Laplace","first_name":"E."},{"last_name":"Justham","first_name":"S.","full_name":"Justham, S."},{"full_name":"Renzo, M.","last_name":"Renzo","first_name":"M."},{"full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"R.","last_name":"Farmer","full_name":"Farmer, R."},{"full_name":"Vartanyan, D.","last_name":"Vartanyan","first_name":"D."},{"full_name":"de Mink, S. E.","last_name":"de Mink","first_name":"S. E."}],"_id":"13455","scopus_import":"1","title":"Different to the core: The pre-supernova structures of massive single and binary-stripped stars","intvolume":" 656","publication_status":"published","article_processing_charge":"No","date_created":"2023-08-03T10:11:09Z","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/202140506"}],"date_published":"2021-12-02T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication":"Astronomy & Astrophysics","month":"12","article_number":"A58","oa_version":"Published Version"},{"volume":918,"extern":"1","citation":{"ama":"Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. The Astrophysical Journal. 2021;918(1). doi:10.3847/1538-4357/ac0af6","apa":"Berzin, E., Secunda, A., Cen, R., Menegas, A., & Götberg, Y. L. L. (2021). Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac0af6","chicago":"Berzin, Elizabeth, Amy Secunda, Renyue Cen, Alexander Menegas, and Ylva Louise Linsdotter Götberg. “Spectral Signatures of Population III and Envelope-Stripped Stars in Galaxies at the Epoch of Reionization.” The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac0af6.","ieee":"E. Berzin, A. Secunda, R. Cen, A. Menegas, and Y. L. L. Götberg, “Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization,” The Astrophysical Journal, vol. 918, no. 1. American Astronomical Society, 2021.","mla":"Berzin, Elizabeth, et al. “Spectral Signatures of Population III and Envelope-Stripped Stars in Galaxies at the Epoch of Reionization.” The Astrophysical Journal, vol. 918, no. 1, 5, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac0af6.","short":"E. Berzin, A. Secunda, R. Cen, A. Menegas, Y.L.L. Götberg, The Astrophysical Journal 918 (2021).","ista":"Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. 2021. Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. The Astrophysical Journal. 918(1), 5."},"year":"2021","date_updated":"2023-08-21T11:44:50Z","external_id":{"arxiv":["2102.08408"]},"day":"27","arxiv":1,"doi":"10.3847/1538-4357/ac0af6","abstract":[{"lang":"eng","text":"While most simulations of the epoch of reionization have focused on single-stellar populations in star-forming dwarf galaxies, products of binary evolution are expected to significantly contribute to emissions of hydrogen-ionizing photons. Among these products are stripped stars (or helium stars), which have their envelopes stripped from interactions with binary companions, leaving an exposed helium core. Previous work has suggested these stripped stars can dominate the Lyman Continuum (LyC) photon output of high-redshift, low-luminosity galaxies post-starburst. Other sources of hard radiation in the early universe include zero-metallicity Population iii stars, which may have similar spectral energy distribution (SED) properties to galaxies with radiation dominated by stripped-star emissions. Here, we use four metrics (the power-law exponent over wavelength intervals 240–500 Å, 600–900 Å, and 1200–2000 Å, and the ratio of total luminosity in FUV wavelengths to LyC wavelengths) to compare the SEDs of simulated galaxies with only single-stellar evolution, galaxies containing stripped stars, and galaxies containing Population iii stars, with four different initial mass functions (IMFs). We find that stripped stars significantly alter SEDs in the LyC range of galaxies at the epoch of reionization. SEDs in galaxies with stripped stars have lower power-law indices in the LyC range and lower FUV to LyC luminosity ratios. These differences in SEDs are present at all considered luminosities (${M}_{\\mathrm{UV}}\\gt -15$, AB system), and are most pronounced for lower-luminosity galaxies. Intrinsic SEDs as well as those with interstellar medium absorption of galaxies with stripped stars and Population iii stars are found to be distinct for all tested Population iii IMFs."}],"quality_controlled":"1","publisher":"American Astronomical Society","article_type":"original","scopus_import":"1","_id":"13456","issue":"1","author":[{"last_name":"Berzin","first_name":"Elizabeth","full_name":"Berzin, Elizabeth"},{"last_name":"Secunda","first_name":"Amy","full_name":"Secunda, Amy"},{"full_name":"Cen, Renyue","last_name":"Cen","first_name":"Renyue"},{"full_name":"Menegas, Alexander","first_name":"Alexander","last_name":"Menegas"},{"full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"}],"date_created":"2023-08-03T10:11:24Z","article_processing_charge":"No","publication_status":"published","intvolume":" 918","title":"Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization","main_file_link":[{"url":"https://doi.org/10.3847/1538-4357/ac0af6","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2021-08-27T00:00:00Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","oa_version":"Published Version","article_number":"5","month":"08"},{"publication":"Astronomy & Astrophysics","article_number":"A70","month":"08","oa_version":"Published Version","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2021-08-12T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/202140507","open_access":"1"}],"author":[{"first_name":"J.","last_name":"Bodensteiner","full_name":"Bodensteiner, J."},{"full_name":"Sana, H.","last_name":"Sana","first_name":"H."},{"full_name":"Wang, C.","first_name":"C.","last_name":"Wang"},{"first_name":"N.","last_name":"Langer","full_name":"Langer, N."},{"full_name":"Mahy, L.","last_name":"Mahy","first_name":"L."},{"full_name":"Banyard, G.","last_name":"Banyard","first_name":"G."},{"first_name":"A.","last_name":"de Koter","full_name":"de Koter, A."},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"full_name":"Evans, C. J.","last_name":"Evans","first_name":"C. J."},{"last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"last_name":"Patrick","first_name":"L. R.","full_name":"Patrick, L. R."},{"first_name":"F. R. N.","last_name":"Schneider","full_name":"Schneider, F. R. N."},{"last_name":"Tramper","first_name":"F.","full_name":"Tramper, F."}],"scopus_import":"1","_id":"13457","intvolume":" 652","title":"The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population","article_processing_charge":"No","date_created":"2023-08-03T10:11:34Z","publication_status":"published","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","external_id":{"arxiv":["2104.13409"]},"year":"2021","citation":{"short":"J. Bodensteiner, H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, L.R. Patrick, F.R.N. Schneider, F. Tramper, Astronomy & Astrophysics 652 (2021).","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” Astronomy & Astrophysics, vol. 652, A70, EDP Sciences, 2021, doi:10.1051/0004-6361/202140507.","ista":"Bodensteiner J, Sana H, Wang C, Langer N, Mahy L, Banyard G, de Koter A, de Mink SE, Evans CJ, Götberg YLL, Patrick LR, Schneider FRN, Tramper F. 2021. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. 652, A70.","apa":"Bodensteiner, J., Sana, H., Wang, C., Langer, N., Mahy, L., Banyard, G., … Tramper, F. (2021). The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140507","ama":"Bodensteiner J, Sana H, Wang C, et al. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. 2021;652. doi:10.1051/0004-6361/202140507","chicago":"Bodensteiner, J., H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140507.","ieee":"J. Bodensteiner et al., “The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population,” Astronomy & Astrophysics, vol. 652. EDP Sciences, 2021."},"date_updated":"2023-08-21T11:49:36Z","abstract":[{"lang":"eng","text":"Context. Observations of massive stars in open clusters younger than ∼8 Myr have shown that a majority of them are in binary systems, most of which will interact during their life. While these can be used as a proxy of the initial multiplicity properties, studying populations of massive stars older than ∼20 Myr allows us to probe the outcome of these interactions after a significant number of systems have experienced mass and angular momentum transfer and may even have merged.\r\n\r\nAims. Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity properties of the massive-star population in the dense core of the ∼40 Myr old cluster NGC 330 in the Small Magellanic Cloud in order to search for possible imprints of stellar evolution on the multiplicity properties.\r\n\r\nMethods. We obtained six epochs of VLT/MUSE observations operated in wide-field mode with the extended wavelength setup and supported by adaptive optics. We extracted spectra and measured radial velocities for stars brighter than mF814W = 19. We identified single-lined spectroscopic binaries through significant RV variability with a peak-to-peak amplitude larger than 20 km s−1. We also identified double-lined spectroscopic binaries, and quantified the observational biases for binary detection. In particular, we took into account that binary systems with similar line strengths are difficult to detect in our data set.\r\n\r\nResults. The observed spectroscopic binary fraction among stars brighter than mF814W = 19 (approximately 5.5 M⊙ on the main sequence) is fSBobs = 13.2 ± 2.0%. Considering period and mass ratio ranges from log(P) = 0.15−3.5 (about 1.4 to 3160 d), q = 0.1−1.0, and a representative set of orbital parameter distributions, we find a bias-corrected close binary fraction of fcl = 34−7+8%. This fraction seems to decline for the fainter stars, which indicates either that the close binary fraction drops in the B-type domain, or that the period distribution becomes more heavily weighted toward longer orbital periods. We further find that both fractions vary strongly in different regions of the color-magnitude diagram, which corresponds to different evolutionary stages. This probably reveals the imprint of the binary history of different groups of stars. In particular, we find that the observed spectroscopic binary fraction of Be stars (fSBobs = 2 ± 2%) is significantly lower than that of B-type stars (fSBobs = 9 ± 2%).\r\n\r\nConclusions. We provide the first homogeneous radial velocity study of a large sample of B-type stars at a low metallicity ([Fe/H] ≲ −1.0). The overall bias-corrected close binary fraction (log(P) < 3.5 d) of the B-star population in NGC 330 is lower than the fraction reported for younger Galactic and Large Magellanic Cloud clusters in previous works. More data are needed, however, to establish whether the observed differences are caused by an age or a metallicity effect."}],"day":"12","doi":"10.1051/0004-6361/202140507","arxiv":1,"extern":"1","volume":652},{"external_id":{"arxiv":["2104.03317"]},"year":"2021","citation":{"ista":"Vartanyan D, Laplace E, Renzo M, Götberg YLL, Burrows A, de Mink SE. 2021. Binary-stripped stars as core-collapse supernovae progenitors. The Astrophysical Journal Letters. 916(1), L5.","short":"D. Vartanyan, E. Laplace, M. Renzo, Y.L.L. Götberg, A. Burrows, S.E. de Mink, The Astrophysical Journal Letters 916 (2021).","mla":"Vartanyan, David, et al. “Binary-Stripped Stars as Core-Collapse Supernovae Progenitors.” The Astrophysical Journal Letters, vol. 916, no. 1, L5, American Astronomical Society, 2021, doi:10.3847/2041-8213/ac0b42.","chicago":"Vartanyan, David, Eva Laplace, Mathieu Renzo, Ylva Louise Linsdotter Götberg, Adam Burrows, and Selma E. de Mink. “Binary-Stripped Stars as Core-Collapse Supernovae Progenitors.” The Astrophysical Journal Letters. American Astronomical Society, 2021. https://doi.org/10.3847/2041-8213/ac0b42.","ieee":"D. Vartanyan, E. Laplace, M. Renzo, Y. L. L. Götberg, A. Burrows, and S. E. de Mink, “Binary-stripped stars as core-collapse supernovae progenitors,” The Astrophysical Journal Letters, vol. 916, no. 1. American Astronomical Society, 2021.","ama":"Vartanyan D, Laplace E, Renzo M, Götberg YLL, Burrows A, de Mink SE. Binary-stripped stars as core-collapse supernovae progenitors. The Astrophysical Journal Letters. 2021;916(1). doi:10.3847/2041-8213/ac0b42","apa":"Vartanyan, D., Laplace, E., Renzo, M., Götberg, Y. L. L., Burrows, A., & de Mink, S. E. (2021). Binary-stripped stars as core-collapse supernovae progenitors. The Astrophysical Journal Letters. American Astronomical Society. https://doi.org/10.3847/2041-8213/ac0b42"},"date_updated":"2023-08-21T11:37:48Z","abstract":[{"text":"Most massive stars experience binary interactions in their lifetimes that can alter both the surface and core structure of the stripped star with significant effects on their ultimate fate as core-collapse supernovae. However, core-collapse supernovae simulations to date have focused almost exclusively on the evolution of single stars. We present a systematic simulation study of single and binary-stripped stars with the same initial mass as candidates for core-collapse supernovae (11–21 M⊙). Generally, we find that binary-stripped stars core tend to have a smaller compactness parameter, with a more prominent, deeper silicon/oxygen interface, and explode preferentially to the corresponding single stars of the same initial mass. Such a dichotomy of behavior between these two modes of evolution would have important implications for supernovae statistics, including the final neutron star masses, explosion energies, and nucleosynthetic yields. Binary-stripped remnants are also well poised to populate the possible mass gap between the heaviest neutron stars and the lightest black holes. Our work presents an improvement along two fronts, as we self-consistently account for the pre-collapse stellar evolution and the subsequent explosion outcome. Even so, our results emphasize the need for more detailed stellar evolutionary models to capture the sensitive nature of explosion outcome.","lang":"eng"}],"day":"23","doi":"10.3847/2041-8213/ac0b42","arxiv":1,"extern":"1","volume":916,"issue":"1","author":[{"last_name":"Vartanyan","first_name":"David","full_name":"Vartanyan, David"},{"full_name":"Laplace, Eva","last_name":"Laplace","first_name":"Eva"},{"full_name":"Renzo, Mathieu","first_name":"Mathieu","last_name":"Renzo"},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"first_name":"Adam","last_name":"Burrows","full_name":"Burrows, Adam"},{"full_name":"de Mink, Selma E.","first_name":"Selma E.","last_name":"de Mink"}],"scopus_import":"1","_id":"13458","intvolume":" 916","title":"Binary-stripped stars as core-collapse supernovae progenitors","date_created":"2023-08-03T10:11:45Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","article_type":"original","publisher":"American Astronomical Society","type":"journal_article","date_published":"2021-07-23T00:00:00Z","oa":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2104.03317"}],"publication":"The Astrophysical Journal Letters","article_number":"L5","month":"07","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}]},{"oa_version":"Preprint","month":"05","article_number":"248","publication":"The Astronomical Journal","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"oa":1,"date_published":"2021-05-04T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/2103.13642","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_status":"published","date_created":"2023-08-03T10:11:57Z","article_processing_charge":"No","title":"The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy","intvolume":" 161","_id":"13459","scopus_import":"1","author":[{"full_name":"Wang, Luqian","first_name":"Luqian","last_name":"Wang"},{"last_name":"Gies","first_name":"Douglas R.","full_name":"Gies, Douglas R."},{"first_name":"Geraldine J.","last_name":"Peters","full_name":"Peters, Geraldine J."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter"},{"last_name":"Chojnowski","first_name":"S. Drew","full_name":"Chojnowski, S. Drew"},{"full_name":"Lester, Kathryn V.","first_name":"Kathryn V.","last_name":"Lester"},{"last_name":"Howell","first_name":"Steve B.","full_name":"Howell, Steve B."}],"issue":"5","publisher":"American Astronomical Society","article_type":"original","quality_controlled":"1","arxiv":1,"doi":"10.3847/1538-3881/abf144","day":"04","abstract":[{"lang":"eng","text":"The B emission-line stars are rapid rotators that were probably spun up by mass and angular momentum accretion through mass transfer in an interacting binary. Mass transfer will strip the donor star of its envelope to create a small and hot subdwarf remnant. Here we report on Hubble Space Telescope/STIS far-ultraviolet spectroscopy of a sample of Be stars that reveals the presence of the hot sdO companion through the calculation of cross-correlation functions of the observed and model spectra. We clearly detect the spectral signature of the sdO star in 10 of the 13 stars in the sample, and the spectral signals indicate that the sdO stars are hot, relatively faint, and slowly rotating as predicted by models. A comparison of their temperatures and radii with evolutionary tracks indicates that the sdO stars occupy the relatively long-lived, He-core burning stage. Only 1 of the 10 detections was a known binary prior to this investigation, which emphasizes the difficulty of finding such Be+sdO binaries through optical spectroscopy. However, these results and others indicate that many Be stars probably host hot subdwarf companions."}],"date_updated":"2023-08-21T11:35:50Z","citation":{"mla":"Wang, Luqian, et al. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” The Astronomical Journal, vol. 161, no. 5, 248, American Astronomical Society, 2021, doi:10.3847/1538-3881/abf144.","short":"L. Wang, D.R. Gies, G.J. Peters, Y.L.L. Götberg, S.D. Chojnowski, K.V. Lester, S.B. Howell, The Astronomical Journal 161 (2021).","ista":"Wang L, Gies DR, Peters GJ, Götberg YLL, Chojnowski SD, Lester KV, Howell SB. 2021. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. The Astronomical Journal. 161(5), 248.","ama":"Wang L, Gies DR, Peters GJ, et al. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. The Astronomical Journal. 2021;161(5). doi:10.3847/1538-3881/abf144","apa":"Wang, L., Gies, D. R., Peters, G. J., Götberg, Y. L. L., Chojnowski, S. D., Lester, K. V., & Howell, S. B. (2021). The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. The Astronomical Journal. American Astronomical Society. https://doi.org/10.3847/1538-3881/abf144","ieee":"L. Wang et al., “The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy,” The Astronomical Journal, vol. 161, no. 5. American Astronomical Society, 2021.","chicago":"Wang, Luqian, Douglas R. Gies, Geraldine J. Peters, Ylva Louise Linsdotter Götberg, S. Drew Chojnowski, Kathryn V. Lester, and Steve B. Howell. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” The Astronomical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-3881/abf144."},"year":"2021","external_id":{"arxiv":["2103.13642"]},"volume":161,"extern":"1"},{"volume":126,"extern":"1","year":"2021","citation":{"ista":"Fyffe CL, Potter E, Fugger S, Orr A, Fatichi S, Loarte E, Medina K, Hellström RÅ, Bernat M, Aubry‐Wake C, Gurgiser W, Perry LB, Suarez W, Quincey DJ, Pellicciotti F. 2021. The energy and mass balance of Peruvian Glaciers. Journal of Geophysical Research: Atmospheres. 126(23), e2021JD034911.","short":"C.L. Fyffe, E. Potter, S. Fugger, A. Orr, S. Fatichi, E. Loarte, K. Medina, R.Å. Hellström, M. Bernat, C. Aubry‐Wake, W. Gurgiser, L.B. Perry, W. Suarez, D.J. Quincey, F. Pellicciotti, Journal of Geophysical Research: Atmospheres 126 (2021).","mla":"Fyffe, Catriona L., et al. “The Energy and Mass Balance of Peruvian Glaciers.” Journal of Geophysical Research: Atmospheres, vol. 126, no. 23, e2021JD034911, American Geophysical Union, 2021, doi:10.1029/2021jd034911.","ieee":"C. L. Fyffe et al., “The energy and mass balance of Peruvian Glaciers,” Journal of Geophysical Research: Atmospheres, vol. 126, no. 23. American Geophysical Union, 2021.","chicago":"Fyffe, Catriona L., Emily Potter, Stefan Fugger, Andrew Orr, Simone Fatichi, Edwin Loarte, Katy Medina, et al. “The Energy and Mass Balance of Peruvian Glaciers.” Journal of Geophysical Research: Atmospheres. American Geophysical Union, 2021. https://doi.org/10.1029/2021jd034911.","apa":"Fyffe, C. L., Potter, E., Fugger, S., Orr, A., Fatichi, S., Loarte, E., … Pellicciotti, F. (2021). The energy and mass balance of Peruvian Glaciers. Journal of Geophysical Research: Atmospheres. American Geophysical Union. https://doi.org/10.1029/2021jd034911","ama":"Fyffe CL, Potter E, Fugger S, et al. The energy and mass balance of Peruvian Glaciers. Journal of Geophysical Research: Atmospheres. 2021;126(23). doi:10.1029/2021jd034911"},"date_updated":"2023-02-28T13:31:08Z","day":"16","doi":"10.1029/2021jd034911","abstract":[{"lang":"eng","text":"Peruvian glaciers are important contributors to dry season runoff for agriculture and hydropower, but they are at risk of disappearing due to climate change. We applied a physically based, energy balance melt model at five on-glacier sites within the Peruvian Cordilleras Blanca and Vilcanota. Net shortwave radiation dominates the energy balance, and despite this flux being higher in the dry season, melt rates are lower due to losses from net longwave radiation and the latent heat flux. The sensible heat flux is a relatively small contributor to melt energy. At three of the sites the wet season snowpack was discontinuous, forming and melting within a daily to weekly timescale, and resulting in highly variable melt rates closely related to precipitation dynamics. Cold air temperatures due to a strong La Niña year at Shallap Glacier (Cordillera Blanca) resulted in a continuous wet season snowpack, significantly reducing wet season ablation. Sublimation was most important at the highest site in the accumulation zone of the Quelccaya Ice Cap (Cordillera Vilcanota), accounting for 81% of ablation, compared to 2%–4% for the other sites. Air temperature and precipitation inputs were perturbed to investigate the climate sensitivity of the five glaciers. At the lower sites warmer air temperatures resulted in a switch from snowfall to rain, so that ablation was increased via the decrease in albedo and increase in net shortwave radiation. At the top of Quelccaya Ice Cap warming caused melting to replace sublimation so that ablation increased nonlinearly with air temperature."}],"quality_controlled":"1","publisher":"American Geophysical Union","article_type":"original","scopus_import":"1","_id":"12583","issue":"23","author":[{"last_name":"Fyffe","first_name":"Catriona L.","full_name":"Fyffe, Catriona L."},{"last_name":"Potter","first_name":"Emily","full_name":"Potter, Emily"},{"full_name":"Fugger, Stefan","last_name":"Fugger","first_name":"Stefan"},{"full_name":"Orr, Andrew","first_name":"Andrew","last_name":"Orr"},{"first_name":"Simone","last_name":"Fatichi","full_name":"Fatichi, Simone"},{"first_name":"Edwin","last_name":"Loarte","full_name":"Loarte, Edwin"},{"last_name":"Medina","first_name":"Katy","full_name":"Medina, Katy"},{"full_name":"Hellström, Robert Å.","last_name":"Hellström","first_name":"Robert Å."},{"full_name":"Bernat, Maud","first_name":"Maud","last_name":"Bernat"},{"first_name":"Caroline","last_name":"Aubry‐Wake","full_name":"Aubry‐Wake, Caroline"},{"first_name":"Wolfgang","last_name":"Gurgiser","full_name":"Gurgiser, Wolfgang"},{"first_name":"L. Baker","last_name":"Perry","full_name":"Perry, L. Baker"},{"first_name":"Wilson","last_name":"Suarez","full_name":"Suarez, Wilson"},{"full_name":"Quincey, Duncan J.","last_name":"Quincey","first_name":"Duncan J."},{"id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70","full_name":"Pellicciotti, Francesca","first_name":"Francesca","last_name":"Pellicciotti"}],"date_created":"2023-02-20T08:10:43Z","article_processing_charge":"No","publication_status":"published","intvolume":" 126","title":"The energy and mass balance of Peruvian Glaciers","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1029/2021JD034911"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2021-12-16T00:00:00Z","publication_identifier":{"eissn":["2169-8996"],"issn":["2169-897X"]},"oa":1,"keyword":["Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Geophysics"],"language":[{"iso":"eng"}],"publication":"Journal of Geophysical Research: Atmospheres","oa_version":"Published Version","article_number":"e2021JD034911","month":"12"},{"title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","intvolume":" 641","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-06T09:38:16Z","author":[{"full_name":"Feltre, Anna","first_name":"Anna","last_name":"Feltre"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"last_name":"Bacon","first_name":"Roland","full_name":"Bacon, Roland"},{"last_name":"Pradeep","first_name":"Jayadev","full_name":"Pradeep, Jayadev"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"full_name":"Schmidt, Kasper B.","first_name":"Kasper B.","last_name":"Schmidt"},{"full_name":"Blaizot, Jeremy","first_name":"Jeremy","last_name":"Blaizot"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"first_name":"Leindert","last_name":"Boogaard","full_name":"Boogaard, Leindert"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Carton, David","last_name":"Carton","first_name":"David"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"last_name":"Kollatschny","first_name":"Wolfram","full_name":"Kollatschny, Wolfram"},{"full_name":"Marino, Raffaella A.","last_name":"Marino","first_name":"Raffaella A."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Tresse, Laurence","first_name":"Laurence","last_name":"Tresse"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"full_name":"Weilbacher, Peter M.","last_name":"Weilbacher","first_name":"Peter M."}],"_id":"11501","scopus_import":"1","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","abstract":[{"text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z > 2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.","lang":"eng"}],"arxiv":1,"doi":"10.1051/0004-6361/202038133","day":"18","external_id":{"arxiv":["2007.01878"]},"date_updated":"2022-07-19T09:35:43Z","citation":{"chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202038133.","ieee":"A. Feltre et al., “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3,” Astronomy & Astrophysics, vol. 641. EDP Sciences, 2020.","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 2020;641. doi:10.1051/0004-6361/202038133","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038133","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 641, A118.","mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics, vol. 641, A118, EDP Sciences, 2020, doi:10.1051/0004-6361/202038133.","short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy & Astrophysics 641 (2020)."},"year":"2020","extern":"1","acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","volume":641,"month":"09","article_number":"A118","oa_version":"Published Version","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_published":"2020-09-18T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2007.01878"}]},{"extern":"1","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima, Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy (http://www.astropy.org), which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE. This work was supported by the project FOGHAR (Agence Nationale de la Recherche, ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid for Scientic Research 19J01620.","volume":638,"external_id":{"arxiv":["2003.12083"]},"citation":{"ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340","apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937340","ieee":"H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy & Astrophysics, vol. 638. EDP Sciences, 2020.","chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340.","mla":"Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics, vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.","short":"H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T. Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz, J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló, M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy & Astrophysics 638 (2020).","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 638, A12."},"year":"2020","date_updated":"2022-07-19T09:35:20Z","abstract":[{"text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time.","lang":"eng"}],"day":"03","arxiv":1,"doi":"10.1051/0004-6361/201937340","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","author":[{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"last_name":"Blaizot","first_name":"Jérémy","full_name":"Blaizot, Jérémy"},{"last_name":"Garel","first_name":"Thibault","full_name":"Garel, Thibault"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"last_name":"Hashimoto","first_name":"Takuya","full_name":"Hashimoto, Takuya"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"first_name":"Simon","last_name":"Conseil","full_name":"Conseil, Simon"},{"last_name":"Guiderdoni","first_name":"Bruno","full_name":"Guiderdoni, Bruno"},{"first_name":"Alyssa B.","last_name":"Drake","full_name":"Drake, Alyssa B."},{"full_name":"Christian Herenz, Edmund","first_name":"Edmund","last_name":"Christian Herenz"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"last_name":"Oesch","first_name":"Pascal","full_name":"Oesch, Pascal"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Anna Marino, Raffaella","first_name":"Raffaella","last_name":"Anna Marino"},{"last_name":"Borello Schmidt","first_name":"Kasper","full_name":"Borello Schmidt, Kasper"},{"full_name":"Pelló, Roser","first_name":"Roser","last_name":"Pelló"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Kerutt, Josephine","first_name":"Josephine","last_name":"Kerutt"},{"full_name":"Mahler, Guillaume","first_name":"Guillaume","last_name":"Mahler"}],"scopus_import":"1","_id":"11503","intvolume":" 638","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","date_created":"2022-07-06T09:50:48Z","article_processing_charge":"No","publication_status":"published","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2003.12083"}],"type":"journal_article","date_published":"2020-06-03T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"A12","month":"06","oa_version":"Published Version"}]