[{"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2022-06-01T00:00:00Z","type":"journal_article","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2110.11967"}],"month":"06","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"abstract":[{"text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (fesc=50 per cent, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism.","lang":"eng"}],"doi":"10.1093/mnras/stac801","arxiv":1,"day":"01","external_id":{"arxiv":["2110.11967"]},"date_updated":"2022-08-18T10:42:47Z","year":"2022","citation":{"ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:10.1093/mnras/stac801.","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","ieee":"J. J. Matthee et al., “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2022. https://doi.org/10.1093/mnras/stac801.","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 2022;512(4):5960-5977. doi:10.1093/mnras/stac801","apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stac801"},"extern":"1","volume":512,"acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","intvolume":" 512","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T09:21:30Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"first_name":"Matthew","last_name":"Hayes","full_name":"Hayes, Matthew"},{"first_name":"Dawn","last_name":"Erb","full_name":"Erb, Dawn"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"full_name":"Amorín, Ricardo","first_name":"Ricardo","last_name":"Amorín"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","last_name":"Ana Paulino-Afonso","first_name":"Ana Paulino-Afonso"},{"full_name":"Llerena, Mario","last_name":"Llerena","first_name":"Mario"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"issue":"4","_id":"11521","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"5960-5977","quality_controlled":"1"},{"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2202.10026"}],"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"type":"journal_article","date_published":"2022-05-19T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","magnetohydrodynamics (MHD) / waves / stars","rotation / stars: magnetic field / stars","oscillations / methods"],"language":[{"iso":"eng"}],"article_number":"A133","month":"05","oa_version":"Preprint","publication":"Astronomy & Astrophysics","extern":"1","acknowledgement":"We thank the referee for her/his positive and constructive report, which has allowed us to improve the quality of our article. H.D. and S.M. acknowledge support from the CNES PLATO grant at CEA/DAp. T.V.R. gratefully acknowledges support from the Research Foundation Flanders (FWO) under grant agreement No. 12ZB620N and V414021N. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1748958. C.A. is supported by the KU Leuven Research Council (grant C16/18/005: PARADISE) as well as from the BELgian federal Science Policy Office (BELSPO) through a PLATO PRODEX grant.","volume":661,"abstract":[{"text":"Context. Asteroseismology has revealed small core-to-surface rotation contrasts in stars in the whole Hertzsprung–Russell diagram. This is the signature of strong transport of angular momentum (AM) in stellar interiors. One of the plausible candidates to efficiently carry AM is magnetic fields with various topologies that could be present in stellar radiative zones. Among them, strong axisymmetric azimuthal (toroidal) magnetic fields have received a lot of interest. Indeed, if they are subject to the so-called Tayler instability, the accompanying triggered Maxwell stresses can transport AM efficiently. In addition, the electromotive force induced by the fluctuations of magnetic and velocity fields could potentially sustain a dynamo action that leads to the regeneration of the initial strong axisymmetric azimuthal magnetic field.\r\n\r\nAims. The key question we aim to answer is whether we can detect signatures of these deep strong azimuthal magnetic fields. The only way to answer this question is asteroseismology, and the best laboratories of study are intermediate-mass and massive stars with external radiative envelopes. Most of these are rapid rotators during their main sequence. Therefore, we have to study stellar pulsations propagating in stably stratified, rotating, and potentially strongly magnetised radiative zones, namely magneto-gravito-inertial (MGI) waves.\r\n\r\nMethods. We generalise the traditional approximation of rotation (TAR) by simultaneously taking general axisymmetric differential rotation and azimuthal magnetic fields into account. Both the Coriolis acceleration and the Lorentz force are therefore treated in a non-perturbative way. Using this new formalism, we derive the asymptotic properties of MGI waves and their period spacings.\r\n\r\nResults. We find that toroidal magnetic fields induce a shift in the period spacings of gravity (g) and Rossby (r) modes. An equatorial azimuthal magnetic field with an amplitude of the order of 105 G leads to signatures that are detectable in period spacings for high-radial-order g and r modes in γ Doradus (γ Dor) and slowly pulsating B (SPB) stars. More complex hemispheric configurations are more difficult to observe, particularly when they are localised out of the propagation region of MGI modes, which can be localised in an equatorial belt.\r\n\r\nConclusions. The magnetic TAR, which takes into account toroidal magnetic fields in a non-perturbative way, is derived. This new formalism allows us to assess the effects of the magnetic field in γ Dor and SPB stars on g and r modes. We find that these effects should be detectable for equatorial fields thanks to modern space photometry using observations from Kepler, TESS CVZ, and PLATO.","lang":"eng"}],"day":"19","arxiv":1,"doi":"10.1051/0004-6361/202142956","external_id":{"arxiv":["2202.10026"]},"citation":{"ista":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. 2022. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. Astronomy & Astrophysics. 661, A133.","short":"H. Dhouib, S. Mathis, L.A. Bugnet, T. Van Reeth, C. Aerts, Astronomy & Astrophysics 661 (2022).","mla":"Dhouib, H., et al. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” Astronomy & Astrophysics, vol. 661, A133, EDP Sciences, 2022, doi:10.1051/0004-6361/202142956.","ieee":"H. Dhouib, S. Mathis, L. A. Bugnet, T. Van Reeth, and C. Aerts, “Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field,” Astronomy & Astrophysics, vol. 661. EDP Sciences, 2022.","chicago":"Dhouib, H., S. Mathis, Lisa Annabelle Bugnet, T. Van Reeth, and C. Aerts. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142956.","apa":"Dhouib, H., Mathis, S., Bugnet, L. A., Van Reeth, T., & Aerts, C. (2022). Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142956","ama":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. Astronomy & Astrophysics. 2022;661. doi:10.1051/0004-6361/202142956"},"year":"2022","date_updated":"2022-08-22T07:58:54Z","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","intvolume":" 661","title":"Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field","date_created":"2022-07-19T08:04:15Z","article_processing_charge":"No","publication_status":"published","author":[{"first_name":"H.","last_name":"Dhouib","full_name":"Dhouib, H."},{"full_name":"Mathis, S.","last_name":"Mathis","first_name":"S."},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"T.","last_name":"Van Reeth","full_name":"Van Reeth, T."},{"last_name":"Aerts","first_name":"C.","full_name":"Aerts, C."}],"scopus_import":"1","_id":"11621"},{"extern":"1","acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","volume":508,"abstract":[{"lang":"eng","text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations."}],"arxiv":1,"doi":"10.1093/mnras/stab2762","day":"01","external_id":{"arxiv":["2004.14496"]},"date_updated":"2022-08-18T10:45:56Z","citation":{"ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709.","short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:10.1093/mnras/stab2762.","chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2762.","ieee":"M. Gronke et al., “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” Monthly Notices of the Royal Astronomical Society, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2762","ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 2021;508(3):3697-3709. doi:10.1093/mnras/stab2762"},"year":"2021","article_type":"original","publisher":"Oxford University Press","page":"3697-3709","quality_controlled":"1","title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","intvolume":" 508","publication_status":"published","date_created":"2022-07-07T09:30:21Z","article_processing_charge":"No","author":[{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"first_name":"Pierre","last_name":"Ocvirk","full_name":"Ocvirk, Pierre"},{"full_name":"Mason, Charlotte","last_name":"Mason","first_name":"Charlotte"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Sarah E I","last_name":"Bosman","full_name":"Bosman, Sarah E I"},{"full_name":"Sorce, Jenny G","first_name":"Jenny G","last_name":"Sorce"},{"first_name":"Joseph","last_name":"Lewis","full_name":"Lewis, Joseph"},{"full_name":"Ahn, Kyungjin","last_name":"Ahn","first_name":"Kyungjin"},{"full_name":"Aubert, Dominique","first_name":"Dominique","last_name":"Aubert"},{"last_name":"Dawoodbhoy","first_name":"Taha","full_name":"Dawoodbhoy, Taha"},{"full_name":"Iliev, Ilian T","last_name":"Iliev","first_name":"Ilian T"},{"full_name":"Shapiro, Paul R","last_name":"Shapiro","first_name":"Paul R"},{"full_name":"Yepes, Gustavo","first_name":"Gustavo","last_name":"Yepes"}],"issue":"3","_id":"11522","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2021-12-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"month":"12","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2102.07779","open_access":"1"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2021-07-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","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).","volume":505,"abstract":[{"lang":"eng","text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙."}],"arxiv":1,"doi":"10.1093/mnras/stab1304","day":"01","external_id":{"arxiv":["2102.07779"]},"date_updated":"2022-08-18T10:49:00Z","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.","short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:10.1093/mnras/stab1304.","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.","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 2021;505(1):1382-1412. doi:10.1093/mnras/stab1304","apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1304"},"article_type":"original","publisher":"Oxford University Press","page":"1382-1412","quality_controlled":"1","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","intvolume":" 505","publication_status":"published","date_created":"2022-07-07T09:33:39Z","article_processing_charge":"No","author":[{"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":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Hayes","first_name":"Matthew","full_name":"Hayes, Matthew"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"last_name":"Naidu","first_name":"Rohan P","full_name":"Naidu, Rohan P"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"first_name":"Ricardo","last_name":"Amorín","full_name":"Amorín, Ricardo"}],"issue":"1","_id":"11523","scopus_import":"1"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"language":[{"iso":"eng"}],"oa_version":"Preprint","article_number":"A53","month":"06","publication":"Astronomy & Astrophysics","main_file_link":[{"url":"https://arxiv.org/abs/2102.01216","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"type":"journal_article","date_published":"2021-06-07T00:00:00Z","publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","date_created":"2022-07-18T12:10:59Z","article_processing_charge":"No","publication_status":"published","intvolume":" 650","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","scopus_import":"1","_id":"11605","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"V.","last_name":"Prat","full_name":"Prat, V."},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"full_name":"Astoul, A.","last_name":"Astoul","first_name":"A."},{"full_name":"Augustson, K.","last_name":"Augustson","first_name":"K."},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"first_name":"L.","last_name":"Amard","full_name":"Amard, L."},{"full_name":"Neiner, C.","last_name":"Neiner","first_name":"C."}],"volume":650,"extern":"1","day":"07","arxiv":1,"doi":"10.1051/0004-6361/202039159","abstract":[{"lang":"eng","text":"Context. The discovery of moderate differential rotation between the core and the envelope of evolved solar-like stars could be the signature of a strong magnetic field trapped inside the radiative interior. The population of intermediate-mass red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation modes that behave as acoustic modes in their external envelope and as gravity modes in their core) could also arise from the effect of an internal magnetic field. Indeed, stars more massive than about 1.1 solar masses are known to develop a convective core during their main sequence. The field generated by the dynamo triggered by this convection could be the progenitor of a strong fossil magnetic field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims. Observations of mixed modes can constitute an excellent probe of the deepest layers of evolved solar-like stars, and magnetic fields in those regions can impact their propagation. The magnetic perturbation on mixed modes may therefore be visible in asteroseismic data. To unravel which constraints can be obtained from observations, we theoretically investigate the effects of a plausible mixed axisymmetric magnetic field with various amplitudes on the mixed-mode frequencies of evolved solar-like stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric magnetic field were computed for dipolar and quadrupolar mixed modes. These computations were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions. We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the presence of a dynamo in the convective core during the main sequence, provoke significant asymmetries on mixed-mode frequency multiplets during the red giant branch. We provide constraints and methods for the detectability of such magnetic signatures. We show that these signatures may be detectable in asteroseismic data for field amplitudes small enough for the amplitude of the modes not to be affected by the conversion of gravity into Alfvén waves inside the magnetised interior. Finally, we infer an upper limit for the strength of the field and the associated lower limit for the timescale of its action in order to redistribute angular momentum in stellar interiors."}],"year":"2021","citation":{"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.","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."},"date_updated":"2022-08-19T10:06:33Z","external_id":{"arxiv":["2102.01216"]}},{"external_id":{"arxiv":["2012.11050"]},"date_updated":"2022-08-19T10:11:52Z","citation":{"short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy & Astrophysics 647 (2021).","mla":"Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” Astronomy & Astrophysics, vol. 647, A122, EDP Sciences, 2021, doi:10.1051/0004-6361/202039180.","ista":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy & Astrophysics. 647, A122.","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","chicago":"Mathis, S., Lisa Annabelle Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039180.","ieee":"S. Mathis, L. A. Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia, “Probing the internal magnetism of stars using asymptotic magneto-asteroseismology,” Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021."},"year":"2021","abstract":[{"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.","lang":"eng"}],"doi":"10.1051/0004-6361/202039180","arxiv":1,"day":"18","extern":"1","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.","volume":647,"author":[{"full_name":"Mathis, S.","last_name":"Mathis","first_name":"S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"first_name":"V.","last_name":"Prat","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."}],"_id":"11606","scopus_import":"1","title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","intvolume":" 647","publication_status":"published","date_created":"2022-07-18T12:15:27Z","article_processing_charge":"No","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","date_published":"2021-03-18T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2012.11050"}],"publication":"Astronomy & Astrophysics","month":"03","article_number":"A122","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"]},{"external_id":{"arxiv":["2101.10152"]},"date_updated":"2022-08-22T08:47:47Z","citation":{"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.","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.","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","ista":"Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. 2021. ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy & Astrophysics. 647, A125.","mla":"Breton, S. N., et al. “ROOSTER: A Machine-Learning Analysis Tool for Kepler Stellar Rotation Periods.” Astronomy & Astrophysics, vol. 647, A125, EDP Sciences, 2021, doi:10.1051/0004-6361/202039947.","short":"S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé, Astronomy & Astrophysics 647 (2021)."},"year":"2021","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."}],"arxiv":1,"doi":"10.1051/0004-6361/202039947","day":"19","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,"author":[{"full_name":"Breton, S. N.","first_name":"S. N.","last_name":"Breton"},{"first_name":"A. R. G.","last_name":"Santos","full_name":"Santos, A. R. G."},{"last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"first_name":"P. L.","last_name":"Pallé","full_name":"Pallé, P. L."}],"_id":"11608","scopus_import":"1","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","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","date_published":"2021-03-19T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2101.10152","open_access":"1"}],"publication":"Astronomy & Astrophysics","month":"03","article_number":"A125","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis / stars: solar-type / stars: activity / stars: rotation / starspots"]},{"oa_version":"Preprint","month":"02","article_number":"A64","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","hydrodynamics / turbulence / stars","rotation / stars","evolution"],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"date_published":"2021-02-08T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/2006.10660","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","date_created":"2022-07-18T13:24:32Z","article_processing_charge":"No","title":"Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration","intvolume":" 646","_id":"11609","scopus_import":"1","author":[{"full_name":"Park, J.","last_name":"Park","first_name":"J."},{"first_name":"V.","last_name":"Prat","full_name":"Prat, V."},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000"}],"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","arxiv":1,"doi":"10.1051/0004-6361/202038654","day":"08","abstract":[{"lang":"eng","text":"Context. Stellar interiors are the seat of efficient transport of angular momentum all along their evolution. In this context, understanding the dependence of the turbulent transport triggered by the instabilities of the vertical and horizontal shears of the differential rotation in stellar radiation zones as a function of their rotation, stratification, and thermal diffusivity is mandatory. Indeed, it constitutes one of the cornerstones of the rotational transport and mixing theory, which is implemented in stellar evolution codes to predict the rotational and chemical evolutions of stars.\r\n\r\nAims. We investigate horizontal shear instabilities in rotating stellar radiation zones by considering the full Coriolis acceleration with both the dimensionless horizontal Coriolis component f̃ and the vertical component f.\r\n\r\nMethods. We performed a linear stability analysis using linearized equations derived from the Navier-Stokes and heat transport equations in the rotating nontraditional f-plane. We considered a horizontal shear flow with a hyperbolic tangent profile as the base flow. The linear stability was analyzed numerically in wide ranges of parameters, and we performed an asymptotic analysis for large vertical wavenumbers using the Wentzel-Kramers-Brillouin-Jeffreys (WKBJ) approximation for nondiffusive and highly-diffusive fluids.\r\n\r\nResults. As in the traditional f-plane approximation, we identify two types of instabilities: the inflectional and inertial instabilities. The inflectional instability is destabilized as f̃ increases and its maximum growth rate increases significantly, while the thermal diffusivity stabilizes the inflectional instability similarly to the traditional case. The inertial instability is also strongly affected; for instance, the inertially unstable regime is also extended in the nondiffusive limit as 0 < f < 1 + f̃ 2/N2, where N is the dimensionless Brunt-Väisälä frequency. More strikingly, in the high thermal diffusivity limit, it is always inertially unstable at any colatitude θ except at the poles (i.e., 0° < θ < 180°). We also derived the critical Reynolds numbers for the inertial instability using the asymptotic dispersion relations obtained from the WKBJ analysis. Using the asymptotic and numerical results, we propose a prescription for the effective turbulent viscosities induced by the inertial and inflectional instabilities that can be possibly used in stellar evolution models. The characteristic time of this turbulence is short enough so that it is efficient to redistribute angular momentum and to mix chemicals in stellar radiation zones."}],"date_updated":"2022-08-19T10:18:03Z","year":"2021","citation":{"mla":"Park, J., et al. “Horizontal Shear Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis Acceleration.” Astronomy & Astrophysics, vol. 646, A64, EDP Sciences, 2021, doi:10.1051/0004-6361/202038654.","short":"J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy & Astrophysics 646 (2021).","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.","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."},"external_id":{"arxiv":["2006.10660"]},"acknowledgement":"The authors acknowledge support from the European Research Council through ERC grant SPIRE 647383 and from GOLF and PLATO CNES grants at the Department of Astrophysics at CEA Paris-Saclay. We thank the referee, Prof. A. J. Barker, for his constructive comments that allow us to improve the article.","volume":646,"extern":"1"},{"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"}],"article_number":"A12","month":"06","oa_version":"Published Version","publication":"Astronomy & Astrophysics","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"type":"journal_article","date_published":"2020-06-03T00:00:00Z","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","intvolume":" 638","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","article_processing_charge":"No","date_created":"2022-07-06T09:50:48Z","publication_status":"published","author":[{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"last_name":"Blaizot","first_name":"Jérémy","full_name":"Blaizot, Jérémy"},{"first_name":"Thibault","last_name":"Garel","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","last_name":"Richard","first_name":"Johan"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"full_name":"Conseil, Simon","last_name":"Conseil","first_name":"Simon"},{"full_name":"Guiderdoni, Bruno","last_name":"Guiderdoni","first_name":"Bruno"},{"last_name":"Drake","first_name":"Alyssa B.","full_name":"Drake, Alyssa B."},{"last_name":"Christian Herenz","first_name":"Edmund","full_name":"Christian Herenz, Edmund"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"first_name":"Pascal","last_name":"Oesch","full_name":"Oesch, Pascal"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Anna Marino, Raffaella","first_name":"Raffaella","last_name":"Anna Marino"},{"full_name":"Borello Schmidt, Kasper","first_name":"Kasper","last_name":"Borello Schmidt"},{"full_name":"Pelló, Roser","first_name":"Roser","last_name":"Pelló"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"full_name":"Mahler, Guillaume","last_name":"Mahler","first_name":"Guillaume"}],"scopus_import":"1","_id":"11503","extern":"1","volume":638,"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.","abstract":[{"lang":"eng","text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time."}],"day":"03","doi":"10.1051/0004-6361/201937340","arxiv":1,"external_id":{"arxiv":["2003.12083"]},"citation":{"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.","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).","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.","chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340.","ieee":"H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy & Astrophysics, vol. 638. EDP Sciences, 2020.","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"},"year":"2020","date_updated":"2022-07-19T09:35:20Z"},{"intvolume":" 498","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","article_processing_charge":"No","date_created":"2022-07-07T10:36:01Z","publication_status":"published","issue":"2","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"},{"full_name":"Lilly, Simon","first_name":"Simon","last_name":"Lilly"},{"first_name":"Leindert","last_name":"Boogaard","full_name":"Boogaard, Leindert"},{"first_name":"Raffaella","last_name":"Marino","full_name":"Marino, Raffaella"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"}],"scopus_import":"1","_id":"11529","article_type":"original","publisher":"Oxford University Press","quality_controlled":"1","page":"3043-3059","abstract":[{"text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst.","lang":"eng"}],"day":"01","arxiv":1,"doi":"10.1093/mnras/staa2550","external_id":{"arxiv":["2008.01731"]},"citation":{"apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550","ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550","ieee":"J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020.","chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa2550.","short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:10.1093/mnras/staa2550.","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059."},"year":"2020","date_updated":"2022-08-18T11:04:05Z","extern":"1","volume":498,"month":"10","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"language":[{"iso":"eng"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"type":"journal_article","date_published":"2020-10-01T00:00:00Z","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}]},{"volume":492,"acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and 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. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","extern":"1","day":"01","arxiv":1,"doi":"10.1093/mnras/stz3554","abstract":[{"lang":"eng","text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies."}],"year":"2020","citation":{"apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/stz3554.","ieee":"J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:10.1093/mnras/stz3554.","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790."},"date_updated":"2022-08-18T11:29:53Z","external_id":{"arxiv":["1909.06376"]},"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"1778-1790","article_processing_charge":"No","date_created":"2022-07-07T12:21:36Z","publication_status":"published","intvolume":" 492","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","scopus_import":"1","_id":"11534","issue":"2","author":[{"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":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"full_name":"Darvish, Behnam","first_name":"Behnam","last_name":"Darvish"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1909.06376"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"type":"journal_article","date_published":"2020-02-01T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"language":[{"iso":"eng"}],"oa_version":"Preprint","month":"02","publication":"Monthly Notices of the Royal Astronomical Society"},{"month":"02","article_number":"A51","oa_version":"Published Version","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["stars: massive / stars: emission-line / Be / binaries: spectroscopic / blue stragglers / Magellanic Clouds"],"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_published":"2020-02-05T00:00:00Z","type":"journal_article","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201936743"}],"title":"The young massive SMC cluster NGC 330 seen by MUSE","intvolume":" 634","publication_status":"published","article_processing_charge":"No","date_created":"2023-08-03T10:13:29Z","author":[{"last_name":"Bodensteiner","first_name":"J.","full_name":"Bodensteiner, J."},{"first_name":"H.","last_name":"Sana","full_name":"Sana, H."},{"last_name":"Mahy","first_name":"L.","full_name":"Mahy, L."},{"full_name":"Patrick, L. R.","first_name":"L. R.","last_name":"Patrick"},{"last_name":"de Koter","first_name":"A.","full_name":"de Koter, A."},{"full_name":"de Mink, S. E.","last_name":"de Mink","first_name":"S. E."},{"full_name":"Evans, C. J.","first_name":"C. J.","last_name":"Evans"},{"orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"full_name":"Langer, N.","first_name":"N.","last_name":"Langer"},{"last_name":"Lennon","first_name":"D. J.","full_name":"Lennon, D. J."},{"full_name":"Schneider, F. R. N.","last_name":"Schneider","first_name":"F. R. N."},{"full_name":"Tramper, F.","last_name":"Tramper","first_name":"F."}],"_id":"13466","scopus_import":"1","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","abstract":[{"text":"Context. A majority of massive stars are part of binary systems, a large fraction of which will inevitably interact during their lives. Binary-interaction products (BiPs), that is, stars affected by such interaction, are expected to be commonly present in stellar populations. BiPs are thus a crucial ingredient in the understanding of stellar evolution.\r\nAims. We aim to identify and characterize a statistically significant sample of BiPs by studying clusters of 10 − 40 Myr, an age at which binary population models predict the abundance of BiPs to be highest. One example of such a cluster is NGC 330 in the Small Magellanic Cloud.\r\nMethods. Using MUSE WFM-AO observations of NGC 330, we resolved the dense cluster core for the first time and were able to extract spectra of its entire massive star population. We developed an automated spectral classification scheme based on the equivalent widths of spectral lines in the red part of the spectrum.\r\nResults. We characterize the massive star content of the core of NGC 330, which contains more than 200 B stars, 2 O stars, 6 A-type supergiants, and 11 red supergiants. We find a lower limit on the Be star fraction of 32 ± 3% in the whole sample. It increases to at least 46 ± 10% when we only consider stars brighter than V = 17 mag. We estimate an age of the cluster core between 35 and 40 Myr and a total cluster mass of 88−18+17 × 103 M⊙.\r\nConclusions. We find that the population in the cluster core is different than the population in the outskirts: while the stellar content in the core appears to be older than the stars in the outskirts, the Be star fraction and the observed binary fraction are significantly higher. Furthermore, we detect several BiP candidates that will be subject of future studies.","lang":"eng"}],"doi":"10.1051/0004-6361/201936743","arxiv":1,"day":"05","external_id":{"arxiv":["1911.03477"]},"date_updated":"2023-08-09T12:50:01Z","year":"2020","citation":{"ista":"Bodensteiner J, Sana H, Mahy L, Patrick LR, de Koter A, de Mink SE, Evans CJ, Götberg YLL, Langer N, Lennon DJ, Schneider FRN, Tramper F. 2020. The young massive SMC cluster NGC 330 seen by MUSE. Astronomy & Astrophysics. 634, A51.","short":"J. Bodensteiner, H. Sana, L. Mahy, L.R. Patrick, A. de Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, N. Langer, D.J. Lennon, F.R.N. Schneider, F. Tramper, Astronomy & Astrophysics 634 (2020).","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.” Astronomy & Astrophysics, vol. 634, A51, EDP Sciences, 2020, doi:10.1051/0004-6361/201936743.","ieee":"J. Bodensteiner et al., “The young massive SMC cluster NGC 330 seen by MUSE,” Astronomy & Astrophysics, vol. 634. EDP Sciences, 2020.","chicago":"Bodensteiner, J., H. Sana, L. Mahy, L. R. Patrick, A. de Koter, S. E. de Mink, C. J. Evans, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201936743.","ama":"Bodensteiner J, Sana H, Mahy L, et al. The young massive SMC cluster NGC 330 seen by MUSE. Astronomy & Astrophysics. 2020;634. doi:10.1051/0004-6361/201936743","apa":"Bodensteiner, J., Sana, H., Mahy, L., Patrick, L. R., de Koter, A., de Mink, S. E., … Tramper, F. (2020). The young massive SMC cluster NGC 330 seen by MUSE. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201936743"},"extern":"1","volume":634},{"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","article_processing_charge":"No","date_created":"2022-07-06T10:09:36Z","publication_status":"published","intvolume":" 628","title":"Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE","scopus_import":"1","_id":"11505","author":[{"full_name":"de La Vieuville, G.","first_name":"G.","last_name":"de La Vieuville"},{"last_name":"Bina","first_name":"D.","full_name":"Bina, D."},{"last_name":"Pello","first_name":"R.","full_name":"Pello, R."},{"full_name":"Mahler, G.","last_name":"Mahler","first_name":"G."},{"full_name":"Richard, J.","first_name":"J.","last_name":"Richard"},{"full_name":"Drake, A. B.","first_name":"A. B.","last_name":"Drake"},{"first_name":"E. C.","last_name":"Herenz","full_name":"Herenz, E. C."},{"full_name":"Bauer, F. E.","first_name":"F. E.","last_name":"Bauer"},{"first_name":"B.","last_name":"Clément","full_name":"Clément, B."},{"first_name":"D.","last_name":"Lagattuta","full_name":"Lagattuta, D."},{"full_name":"Laporte, N.","last_name":"Laporte","first_name":"N."},{"full_name":"Martinez, J.","first_name":"J.","last_name":"Martinez"},{"first_name":"V.","last_name":"Patrício","full_name":"Patrício, V."},{"last_name":"Wisotzki","first_name":"L.","full_name":"Wisotzki, L."},{"full_name":"Zabl, J.","last_name":"Zabl","first_name":"J."},{"full_name":"Bouwens, R. J.","first_name":"R. J.","last_name":"Bouwens"},{"full_name":"Contini, T.","first_name":"T.","last_name":"Contini"},{"last_name":"Garel","first_name":"T.","full_name":"Garel, T."},{"first_name":"B.","last_name":"Guiderdoni","full_name":"Guiderdoni, B."},{"first_name":"R. A.","last_name":"Marino","full_name":"Marino, R. A."},{"last_name":"Maseda","first_name":"M. V.","full_name":"Maseda, M. V."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Schaye","first_name":"J.","full_name":"Schaye, J."},{"last_name":"Soucail","first_name":"G.","full_name":"Soucail, G."}],"acknowledgement":"We thank the anonymous referee for their critical review and useful suggestions. This work has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the “Investissements d’Avenir” French government programme managed by the ANR. Partially funded by the ERC starting grant CALENDS (JR, VP, BC, JM), the Agence Nationale de la recherche bearing the reference ANR-13-BS05-0010-02 (FOGHAR), and the “Programme National de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. GdV, RP, JR, GM, JM, BC, and VP also acknowledge support by the Programa de Cooperacion Cientifica – ECOS SUD Program C16U02. NL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 669253), ABD acknowledges support from the ERC advanced grant “Cosmic Gas”. LW acknowledges support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2, and TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE).. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345, 094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also based on observations obtained with the NASA/ESA Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013). All plots in this paper were created using Matplotlib (Hunter 2007).","volume":628,"extern":"1","day":"25","doi":"10.1051/0004-6361/201834471","arxiv":1,"abstract":[{"text":"Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 < z < 6, 7, 2.9 < z < 4.0, 4.0 < z < 5.0, and 5.0 < z < 6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6.","lang":"eng"}],"year":"2019","citation":{"mla":"de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” Astronomy & Astrophysics, vol. 628, A3, EDP Sciences, 2019, doi:10.1051/0004-6361/201834471.","short":"G. de La Vieuville, D. Bina, R. Pello, G. Mahler, J. Richard, A.B. Drake, E.C. Herenz, F.E. Bauer, B. Clément, D. Lagattuta, N. Laporte, J. Martinez, V. Patrício, L. Wisotzki, J. Zabl, R.J. Bouwens, T. Contini, T. Garel, B. Guiderdoni, R.A. Marino, M.V. Maseda, J.J. Matthee, J. Schaye, G. Soucail, Astronomy & Astrophysics 628 (2019).","ista":"de La Vieuville G, Bina D, Pello R, Mahler G, Richard J, Drake AB, Herenz EC, Bauer FE, Clément B, Lagattuta D, Laporte N, Martinez J, Patrício V, Wisotzki L, Zabl J, Bouwens RJ, Contini T, Garel T, Guiderdoni B, Marino RA, Maseda MV, Matthee JJ, Schaye J, Soucail G. 2019. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy & Astrophysics. 628, A3.","apa":"de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., … Soucail, G. (2019). Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834471","ama":"de La Vieuville G, Bina D, Pello R, et al. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy & Astrophysics. 2019;628. doi:10.1051/0004-6361/201834471","chicago":"La Vieuville, G. de, D. Bina, R. Pello, G. Mahler, J. Richard, A. B. Drake, E. C. Herenz, et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” Astronomy & Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201834471.","ieee":"G. de La Vieuville et al., “Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE,” Astronomy & Astrophysics, vol. 628. EDP Sciences, 2019."},"date_updated":"2022-07-19T09:36:31Z","external_id":{"arxiv":["1905.13696"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","gravitational lensing: strong / galaxies: high-redshift / dark ages","reionization","first stars / galaxies: clusters: general / galaxies: luminosity function","mass function"],"language":[{"iso":"eng"}],"oa_version":"Published Version","article_number":"A3","month":"07","publication":"Astronomy & Astrophysics","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1905.13696"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"type":"journal_article","date_published":"2019-07-25T00:00:00Z"},{"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","intvolume":" 482","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-08T10:40:05Z","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"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":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Ferrara, Andrea","first_name":"Andrea","last_name":"Ferrara"},{"full_name":"Alegre, Lara","first_name":"Lara","last_name":"Alegre"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"}],"issue":"2","_id":"11541","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"2422-2441","quality_controlled":"1","abstract":[{"text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/sty2779","day":"01","external_id":{"arxiv":["1710.08422"]},"date_updated":"2022-08-19T06:49:36Z","citation":{"mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:10.1093/mnras/sty2779.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779","chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.","ieee":"D. Sobral et al., “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019."},"year":"2019","extern":"1","volume":482,"acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","month":"01","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: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2019-01-01T00:00:00Z","type":"journal_article","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}]},{"acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","volume":485,"extern":"1","year":"2019","citation":{"ieee":"M. Hon et al., “A search for red giant solar-like oscillations in all Kepler data,” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz622.","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., & Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz622","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 2019;485(4):5616-5630. doi:10.1093/mnras/stz622","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:10.1093/mnras/stz622."},"date_updated":"2022-08-22T07:35:19Z","external_id":{"arxiv":["1903.00115"]},"day":"01","doi":"10.1093/mnras/stz622","arxiv":1,"abstract":[{"lang":"eng","text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars."}],"quality_controlled":"1","page":"5616-5630","publisher":"Oxford University Press","article_type":"original","scopus_import":"1","_id":"11615","issue":"4","author":[{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"full_name":"Stello, Dennis","last_name":"Stello","first_name":"Dennis"},{"full_name":"García, Rafael A","last_name":"García","first_name":"Rafael A"},{"first_name":"Savita","last_name":"Mathur","full_name":"Mathur, Savita"},{"last_name":"Sharma","first_name":"Sanjib","full_name":"Sharma, Sanjib"},{"full_name":"Colman, Isabel L","last_name":"Colman","first_name":"Isabel L"},{"last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501"}],"article_processing_charge":"No","date_created":"2022-07-18T14:26:03Z","publication_status":"published","intvolume":" 485","title":"A search for red giant solar-like oscillations in all Kepler data","main_file_link":[{"url":"https://arxiv.org/abs/1903.00115","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2019-06-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"06"},{"abstract":[{"lang":"eng","text":"Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy Sph using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with Sph being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods."}],"day":"19","arxiv":1,"doi":"10.3847/1538-4365/ab3b56","external_id":{"arxiv":["1908.05222"]},"citation":{"ieee":"A. R. G. Santos et al., “Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars,” The Astrophysical Journal Supplement Series, vol. 244, no. 1. IOP Publishing, 2019.","chicago":"Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L. van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” The Astrophysical Journal Supplement Series. IOP Publishing, 2019. https://doi.org/10.3847/1538-4365/ab3b56.","apa":"Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J. L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. IOP Publishing. https://doi.org/10.3847/1538-4365/ab3b56","ama":"Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 2019;244(1). doi:10.3847/1538-4365/ab3b56","ista":"Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 244(1), 21.","mla":"Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” The Astrophysical Journal Supplement Series, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:10.3847/1538-4365/ab3b56.","short":"A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S. Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement Series 244 (2019)."},"year":"2019","date_updated":"2022-08-22T08:10:38Z","extern":"1","volume":244,"acknowledgement":"The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg, and Isabel L. Colman for helping on the classification of stars. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the National Aeronautics and Space Administration (NASA) Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at the Max Planck Institute for Solar System Research. 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.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy (van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities: MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -","intvolume":" 244","title":"Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars","date_created":"2022-07-19T09:21:58Z","article_processing_charge":"No","publication_status":"published","issue":"1","author":[{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"J. L.","last_name":"van Saders","full_name":"van Saders, J. L."},{"full_name":"Metcalfe, T. S.","first_name":"T. S.","last_name":"Metcalfe"},{"first_name":"G. V. A.","last_name":"Simonian","full_name":"Simonian, G. V. A."},{"last_name":"Pinsonneault","first_name":"M. H.","full_name":"Pinsonneault, M. H."}],"scopus_import":"1","_id":"11623","article_type":"original","publisher":"IOP Publishing","quality_controlled":"1","oa":1,"publication_identifier":{"issn":["0067-0049"]},"type":"journal_article","date_published":"2019-09-19T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1908.05222","open_access":"1"}],"article_number":"21","month":"09","oa_version":"Preprint","publication":"The Astrophysical Journal Supplement Series","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis","stars: activity","stars: low-mass","stars: rotation","starspots","techniques: photometric"],"language":[{"iso":"eng"}]},{"day":"23","arxiv":1,"doi":"10.48550/arXiv.1906.09609","oa":1,"abstract":[{"lang":"eng","text":"For a solar-like star, the surface rotation evolves with time, allowing in principle to estimate the age of a star from its surface rotation period. Here we are interested in measuring surface rotation periods of solar-like stars observed by the NASA mission Kepler. Different methods have been developed to track rotation signals in Kepler photometric light curves: time-frequency analysis based on wavelet techniques, autocorrelation and composite spectrum. We use the learning abilities of random forest classifiers to take decisions during two crucial steps of the analysis. First, given some input parameters, we discriminate the considered Kepler targets between rotating MS stars, non-rotating MS stars, red giants, binaries and pulsators. We then use a second classifier only on the MS rotating targets to decide the best data analysis treatment."}],"year":"2019","citation":{"ista":"Breton SN, Bugnet LA, Santos ARG, Saux AL, Mathur S, Palle PL, Garcia RA. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv, 1906.09609.","mla":"Breton, S. N., et al. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv, 1906.09609, doi:10.48550/arXiv.1906.09609.","short":"S.N. Breton, L.A. Bugnet, A.R.G. Santos, A.L. Saux, S. Mathur, P.L. Palle, R.A. Garcia, ArXiv (n.d.).","ieee":"S. N. Breton et al., “Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques,” arXiv. .","chicago":"Breton, S. N., Lisa Annabelle Bugnet, A. R. G. Santos, A. Le Saux, S. Mathur, P. L. Palle, and R. A. Garcia. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1906.09609.","ama":"Breton SN, Bugnet LA, Santos ARG, et al. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv. doi:10.48550/arXiv.1906.09609","apa":"Breton, S. N., Bugnet, L. A., Santos, A. R. G., Saux, A. L., Mathur, S., Palle, P. L., & Garcia, R. A. (n.d.). Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv. https://doi.org/10.48550/arXiv.1906.09609"},"date_updated":"2022-08-22T08:16:53Z","external_id":{"arxiv":["1906.09609"]},"type":"preprint","date_published":"2019-06-23T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1906.09609","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","extern":"1","article_processing_charge":"No","date_created":"2022-07-20T11:18:53Z","publication_status":"submitted","oa_version":"Preprint","article_number":"1906.09609","month":"06","title":"Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques","publication":"arXiv","_id":"11627","author":[{"full_name":"Breton, S. N.","last_name":"Breton","first_name":"S. N."},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"A. R. G.","last_name":"Santos","full_name":"Santos, A. R. G."},{"full_name":"Saux, A. Le","last_name":"Saux","first_name":"A. Le"},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"Palle, P. L.","last_name":"Palle","first_name":"P. L."},{"full_name":"Garcia, R. A.","last_name":"Garcia","first_name":"R. A."}],"keyword":["asteroseismology","rotation","solar-like stars","kepler","machine learning","random forest"],"language":[{"iso":"eng"}]},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1906.09611"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","extern":"1","citation":{"mla":"Saux, A. Le, et al. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” ArXiv, 1906.09611, doi:10.48550/arXiv.1906.09611.","short":"A.L. Saux, L.A. Bugnet, S. Mathur, S.N. Breton, R.A. Garcia, ArXiv (n.d.).","ista":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. arXiv, 1906.09611.","ama":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. arXiv. doi:10.48550/arXiv.1906.09611","apa":"Saux, A. L., Bugnet, L. A., Mathur, S., Breton, S. N., & Garcia, R. A. (n.d.). Automatic classification of K2 pulsating stars using machine learning techniques. arXiv. https://doi.org/10.48550/arXiv.1906.09611","chicago":"Saux, A. Le, Lisa Annabelle Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1906.09611.","ieee":"A. L. Saux, L. A. Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia, “Automatic classification of K2 pulsating stars using machine learning techniques,” arXiv. ."},"year":"2019","date_updated":"2022-08-22T08:20:29Z","type":"preprint","external_id":{"arxiv":["1906.09611"]},"date_published":"2019-06-23T00:00:00Z","day":"23","arxiv":1,"doi":"10.48550/arXiv.1906.09611","oa":1,"abstract":[{"lang":"eng","text":"The second mission of NASA’s Kepler satellite, K2, has collected hundreds of thousands of lightcurves for stars close to the ecliptic plane. This new sample could increase the number of known pulsating stars and then improve our understanding of those stars. For the moment only a few stars have been properly classified and published. In this work, we present a method to automaticly classify K2 pulsating stars using a Machine Learning technique called Random Forest. The objective is to sort out the stars in four classes: red giant (RG), main-sequence Solar-like stars (SL), classical pulsators (PULS) and Other. To do this we use the effective temperatures and the luminosities of the stars as well as the FliPer features, that measures the amount of power contained in the power spectral density. The classifier now retrieves the right classification for more than 80% of the stars."}],"keyword":["asteroseismology - methods","data analysis - thecniques","machine learning - stars","oscillations"],"language":[{"iso":"eng"}],"publication":"arXiv","_id":"11630","author":[{"full_name":"Saux, A. Le","last_name":"Saux","first_name":"A. Le"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"last_name":"Breton","first_name":"S. N.","full_name":"Breton, S. N."},{"full_name":"Garcia, R. A.","first_name":"R. A.","last_name":"Garcia"}],"article_processing_charge":"No","date_created":"2022-07-21T06:57:10Z","publication_status":"submitted","oa_version":"Preprint","article_number":"1906.09611","title":"Automatic classification of K2 pulsating stars using machine learning techniques","month":"06"},{"publication_status":"published","article_processing_charge":"No","date_created":"2022-07-06T11:14:23Z","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","intvolume":" 619","_id":"11508","scopus_import":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"full_name":"Stefanon, Mauro","first_name":"Mauro","last_name":"Stefanon"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","arxiv":1,"doi":"10.1051/0004-6361/201833528","day":"19","abstract":[{"text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα > 22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z > 6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z < 1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z > 6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z > 5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR.","lang":"eng"}],"date_updated":"2022-07-19T09:32:08Z","citation":{"ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 619, A136.","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics, vol. 619, A136, EDP Sciences, 2018, doi:10.1051/0004-6361/201833528.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy & Astrophysics 619 (2018).","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” Astronomy & Astrophysics, vol. 619. EDP Sciences, 2018.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833528.","ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 2018;619. doi:10.1051/0004-6361/201833528","apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., & Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833528"},"year":"2018","external_id":{"arxiv":["1805.11621"]},"volume":619,"acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","extern":"1","oa_version":"Published Version","month":"11","article_number":"A136","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"date_published":"2018-11-19T00:00:00Z","type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.11621"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"publication":"Astronomy & Astrophysics","month":"12","article_number":"A38","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"date_published":"2018-12-01T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1809.05105","open_access":"1"}],"author":[{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"full_name":"Davies, G. R.","last_name":"Davies","first_name":"G. R."},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"full_name":"Corsaro, E.","first_name":"E.","last_name":"Corsaro"},{"first_name":"O. J.","last_name":"Hall","full_name":"Hall, O. J."},{"full_name":"Rendle, B. M.","last_name":"Rendle","first_name":"B. M."}],"_id":"11618","scopus_import":"1","title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","intvolume":" 620","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-18T14:37:39Z","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","external_id":{"arxiv":["1809.05105"]},"date_updated":"2022-08-22T07:41:07Z","year":"2018","citation":{"short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy & Astrophysics 620 (2018).","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics, vol. 620, A38, EDP Sciences, 2018, doi:10.1051/0004-6361/201833106.","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 620, A38.","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., & Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833106","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 2018;620. doi:10.1051/0004-6361/201833106","ieee":"L. A. Bugnet et al., “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” Astronomy & Astrophysics, vol. 620. EDP Sciences, 2018.","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833106."},"abstract":[{"lang":"eng","text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties."}],"doi":"10.1051/0004-6361/201833106","arxiv":1,"day":"01","extern":"1","volume":620,"acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555."}]