[{"year":"2021","doi":"10.1051/0004-6361/202039887","author":[{"full_name":"Bacon, R.","first_name":"R.","last_name":"Bacon"},{"full_name":"Mary, D.","first_name":"D.","last_name":"Mary"},{"full_name":"Garel, T.","last_name":"Garel","first_name":"T."},{"full_name":"Blaizot, J.","first_name":"J.","last_name":"Blaizot"},{"full_name":"Maseda, M.","last_name":"Maseda","first_name":"M."},{"full_name":"Schaye, J.","last_name":"Schaye","first_name":"J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"last_name":"Conseil","first_name":"S.","full_name":"Conseil, S."},{"first_name":"J.","last_name":"Brinchmann","full_name":"Brinchmann, J."},{"full_name":"Leclercq, F.","first_name":"F.","last_name":"Leclercq"},{"first_name":"V.","last_name":"Abril-Melgarejo","full_name":"Abril-Melgarejo, V."},{"last_name":"Boogaard","first_name":"L.","full_name":"Boogaard, L."},{"first_name":"N. F.","last_name":"Bouché","full_name":"Bouché, N. F."},{"full_name":"Contini, T.","first_name":"T.","last_name":"Contini"},{"last_name":"Feltre","first_name":"A.","full_name":"Feltre, A."},{"last_name":"Guiderdoni","first_name":"B.","full_name":"Guiderdoni, B."},{"full_name":"Herenz, C.","last_name":"Herenz","first_name":"C."},{"first_name":"W.","last_name":"Kollatschny","full_name":"Kollatschny, W."},{"full_name":"Kusakabe, H.","last_name":"Kusakabe","first_name":"H."},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"L.","last_name":"Michel-Dansac","full_name":"Michel-Dansac, L."},{"full_name":"Nanayakkara, T.","first_name":"T.","last_name":"Nanayakkara"},{"full_name":"Richard, J.","first_name":"J.","last_name":"Richard"},{"first_name":"M.","last_name":"Roth","full_name":"Roth, M."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"M.","last_name":"Steinmetz","full_name":"Steinmetz, M."},{"full_name":"Tresse, L.","first_name":"L.","last_name":"Tresse"},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"full_name":"Verhamme, A.","last_name":"Verhamme","first_name":"A."},{"full_name":"Weilbacher, P. M.","first_name":"P. M.","last_name":"Weilbacher"},{"last_name":"Zabl","first_name":"J.","full_name":"Zabl, J."},{"first_name":"S. L.","last_name":"Zoutendijk","full_name":"Zoutendijk, S. L."}],"scopus_import":"1","day":"18","article_number":"A107","article_type":"original","month":"03","title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","main_file_link":[{"url":"https://arxiv.org/abs/2102.05516","open_access":"1"}],"abstract":[{"lang":"eng","text":"We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift."}],"date_created":"2022-07-06T09:31:50Z","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"type":"journal_article","arxiv":1,"quality_controlled":"1","status":"public","external_id":{"arxiv":["2102.05516"]},"citation":{"ieee":"R. Bacon <i>et al.</i>, “The MUSE Extremely Deep Field: The cosmic web in emission at high redshift,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","chicago":"Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>.","apa":"Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk, S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>","short":"R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F. Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe, J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt, M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L. Zoutendijk, Astronomy &#38; Astrophysics 647 (2021).","ista":"Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy &#38; Astrophysics. 647, A107.","mla":"Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A107, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>.","ama":"Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>"},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"language":[{"iso":"eng"}],"extern":"1","article_processing_charge":"No","date_updated":"2022-07-19T09:34:57Z","_id":"11500","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       647","acknowledgement":"We warmly thank ESO Paranal staff for their great professional support during all MXDF GTO observing runs. We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We also thank Matthew Lehnert for fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support from the GDR ISIS through the Projets exploratoires program (project TASTY). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges support by The Netherlands Organisation for Scientific Research (NWO) through a TOP Grant Module 1 under project number 614.001.652. This research made use of the following open-source software and we are thankful to the developers of these: GNU Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).","publisher":"EDP Sciences","publication_status":"published","oa_version":"Published Version","date_published":"2021-03-18T00:00:00Z","volume":647},{"_id":"11605","date_updated":"2024-10-14T11:39:01Z","article_processing_charge":"No","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"ama":"Bugnet LA, Prat V, Mathis S, et al. Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. 2021;650. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>","mla":"Bugnet, Lisa Annabelle, et al. “Magnetic Signatures on Mixed-Mode Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 650, A53, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>.","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 &#38; Astrophysics. 650, A53.","short":"L.A. Bugnet, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.A. García, S. Mathur, L. Amard, C. Neiner, Astronomy &#38; Astrophysics 650 (2021).","apa":"Bugnet, L. A., Prat, V., Mathis, S., Astoul, A., Augustson, K., García, R. A., … Neiner, C. (2021). Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>.","ieee":"L. A. Bugnet <i>et al.</i>, “Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 650. EDP Sciences, 2021."},"external_id":{"arxiv":["2102.01216"]},"extern":"1","language":[{"iso":"eng"}],"publication_status":"published","publisher":"EDP Sciences","volume":650,"date_published":"2021-06-07T00:00:00Z","oa_version":"Preprint","intvolume":"       650","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","month":"06","day":"07","scopus_import":"1","author":[{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"first_name":"V.","last_name":"Prat","full_name":"Prat, V."},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"last_name":"Astoul","first_name":"A.","full_name":"Astoul, A."},{"first_name":"K.","last_name":"Augustson","full_name":"Augustson, K."},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"full_name":"Amard, L.","last_name":"Amard","first_name":"L."},{"full_name":"Neiner, C.","last_name":"Neiner","first_name":"C."}],"year":"2021","doi":"10.1051/0004-6361/202039159","article_type":"original","article_number":"A53","status":"public","arxiv":1,"quality_controlled":"1","date_created":"2022-07-18T12:10:59Z","abstract":[{"text":"Context. The discovery of moderate differential rotation between the core and the envelope of evolved solar-like stars could be the signature of a strong magnetic field trapped inside the radiative interior. The population of intermediate-mass red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation modes that behave as acoustic modes in their external envelope and as gravity modes in their core) could also arise from the effect of an internal magnetic field. Indeed, stars more massive than about 1.1 solar masses are known to develop a convective core during their main sequence. The field generated by the dynamo triggered by this convection could be the progenitor of a strong fossil magnetic field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims. Observations of mixed modes can constitute an excellent probe of the deepest layers of evolved solar-like stars, and magnetic fields in those regions can impact their propagation. The magnetic perturbation on mixed modes may therefore be visible in asteroseismic data. To unravel which constraints can be obtained from observations, we theoretically investigate the effects of a plausible mixed axisymmetric magnetic field with various amplitudes on the mixed-mode frequencies of evolved solar-like stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric magnetic field were computed for dipolar and quadrupolar mixed modes. These computations were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions. We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the presence of a dynamo in the convective core during the main sequence, provoke significant asymmetries on mixed-mode frequency multiplets during the red giant branch. We provide constraints and methods for the detectability of such magnetic signatures. We show that these signatures may be detectable in asteroseismic data for field amplitudes small enough for the amplitude of the modes not to be affected by the conversion of gravity into Alfvén waves inside the magnetised interior. Finally, we infer an upper limit for the strength of the field and the associated lower limit for the timescale of its action in order to redistribute angular momentum in stellar interiors.","lang":"eng"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.01216"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"oa":1},{"title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","month":"03","day":"18","scopus_import":"1","author":[{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Prat, V.","last_name":"Prat","first_name":"V."},{"full_name":"Augustson, K.","first_name":"K.","last_name":"Augustson"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"last_name":"Garcia","first_name":"R. A.","full_name":"Garcia, R. A."}],"year":"2021","doi":"10.1051/0004-6361/202039180","article_type":"original","article_number":"A122","status":"public","quality_controlled":"1","arxiv":1,"date_created":"2022-07-18T12:15:27Z","abstract":[{"lang":"eng","text":"Context. Our knowledge of the dynamics of stars has undergone a revolution through the simultaneous large amount of high-quality photometric observations collected by space-based asteroseismology and ground-based high-precision spectropolarimetry. They allowed us to probe the internal rotation of stars and their surface magnetism in the whole Hertzsprung-Russell diagram. However, new methods should still be developed to probe the deep magnetic fields in these stars.\r\n\r\nAims. Our goal is to provide seismic diagnoses that allow us to probe the internal magnetism of stars.\r\n\r\nMethods. We focused on asymptotic low-frequency gravity modes and high-frequency acoustic modes. Using a first-order perturbative theory, we derived magnetic splittings of their frequencies as explicit functions of stellar parameters.\r\n\r\nResults. As in the case of rotation, we show that asymptotic gravity and acoustic modes can allow us to probe the different components of the magnetic field in the cavities in which they propagate. This again demonstrates the high potential of using mixed-modes when this is possible."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2012.11050"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"],"oa":1,"_id":"11606","date_updated":"2024-10-14T11:39:21Z","article_processing_charge":"No","citation":{"apa":"Mathis, S., Bugnet, L. A., Prat, V., Augustson, K., Mathur, S., &#38; Garcia, R. A. (2021). Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>","mla":"Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A122, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>.","ama":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>","short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy &#38; Astrophysics 647 (2021).","ista":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy &#38; Astrophysics. 647, A122.","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>.","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,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021."},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"external_id":{"arxiv":["2012.11050"]},"extern":"1","language":[{"iso":"eng"}],"publication_status":"published","publisher":"EDP Sciences","volume":647,"date_published":"2021-03-18T00:00:00Z","oa_version":"Preprint","intvolume":"       647","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","acknowledgement":"The authors thank the referee and Pr. J. Christensen-Dalsgaard for their very constructive comments and remarks that allowed us to improve the article. St. M., L. B., V. P., and K. A. acknowledge support from the European Research Council through ERC grant SPIRE 647383. All the members from CEA acknowledge support from GOLF and PLATO CNES grants of the Astrophysics Division at CEA. S. Mathur acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. We made great use of the megyr python package for interfacing MESA and GYRE codes."},{"article_number":"A125","article_type":"original","author":[{"first_name":"S. N.","last_name":"Breton","full_name":"Breton, S. N."},{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"full_name":"Pallé, P. L.","first_name":"P. L.","last_name":"Pallé"}],"year":"2021","doi":"10.1051/0004-6361/202039947","day":"19","scopus_import":"1","month":"03","title":"ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis / stars: solar-type / stars: activity / stars: rotation / starspots"],"oa":1,"type":"journal_article","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."}],"main_file_link":[{"url":"https://arxiv.org/abs/2101.10152","open_access":"1"}],"date_created":"2022-07-18T12:21:32Z","arxiv":1,"quality_controlled":"1","status":"public","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["2101.10152"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039947\">https://doi.org/10.1051/0004-6361/202039947</a>.","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,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","apa":"Breton, S. N., Santos, A. R. G., Bugnet, L. A., Mathur, S., García, R. A., &#38; Pallé, P. L. (2021). ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039947\">https://doi.org/10.1051/0004-6361/202039947</a>","mla":"Breton, S. N., et al. “ROOSTER: A Machine-Learning Analysis Tool for Kepler Stellar Rotation Periods.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A125, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039947\">10.1051/0004-6361/202039947</a>.","ama":"Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039947\">10.1051/0004-6361/202039947</a>","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 &#38; Astrophysics. 647, A125.","short":"S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé, Astronomy &#38; Astrophysics 647 (2021)."},"date_updated":"2022-08-22T08:47:47Z","article_processing_charge":"No","_id":"11608","acknowledgement":"We thank Suzanne Aigrain and Joe Llama for providing us with the simulated data used in Aigrain et al. (2015). S. N. B., L. B. and R. A. G. acknowledge the support from PLATO and GOLF CNES grants. A. R. G. S. acknowledges the support from NASA under grant NNX17AF27G. S. M. acknowledges the support from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697. P. L. P. and S. M. acknowledge support from the Spanish Ministry of Science and Innovation with the grant number PID2019-107187GB-I00. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Software: Python (Van Rossum & Drake 2009), numpy (Oliphant 2006), pandas (The pandas development team 2020; McKinney 2010), matplotlib (Hunter 2007), scikit-learn (Pedregosa et al. 2011). The source code used to obtain the present results can be found at: https://gitlab.com/sybreton/pushkin ; https://gitlab.com/sybreton/ml_surface_rotation_paper .","publication":"Astronomy & Astrophysics","intvolume":"       647","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","date_published":"2021-03-19T00:00:00Z","volume":647,"publication_status":"published","publisher":"EDP Sciences"},{"day":"08","scopus_import":"1","author":[{"first_name":"J.","last_name":"Park","full_name":"Park, J."},{"full_name":"Prat, V.","last_name":"Prat","first_name":"V."},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"}],"doi":"10.1051/0004-6361/202038654","year":"2021","article_type":"original","article_number":"A64","title":"Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration","month":"02","date_created":"2022-07-18T13:24:32Z","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."}],"main_file_link":[{"url":"https://arxiv.org/abs/2006.10660","open_access":"1"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","hydrodynamics / turbulence / stars","rotation / stars","evolution"],"oa":1,"status":"public","quality_controlled":"1","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"apa":"Park, J., Prat, V., Mathis, S., &#38; Bugnet, L. A. (2021). Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202038654\">https://doi.org/10.1051/0004-6361/202038654</a>","ama":"Park J, Prat V, Mathis S, Bugnet LA. Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration. <i>Astronomy &#38; Astrophysics</i>. 2021;646. doi:<a href=\"https://doi.org/10.1051/0004-6361/202038654\">10.1051/0004-6361/202038654</a>","mla":"Park, J., et al. “Horizontal Shear Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis Acceleration.” <i>Astronomy &#38; Astrophysics</i>, vol. 646, A64, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202038654\">10.1051/0004-6361/202038654</a>.","short":"J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy &#38; 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 &#38; Astrophysics. 646, A64.","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202038654\">https://doi.org/10.1051/0004-6361/202038654</a>.","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,” <i>Astronomy &#38; Astrophysics</i>, vol. 646. EDP Sciences, 2021."},"external_id":{"arxiv":["2006.10660"]},"extern":"1","language":[{"iso":"eng"}],"_id":"11609","date_updated":"2022-08-19T10:18:03Z","article_processing_charge":"No","intvolume":"       646","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","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.","publication_status":"published","publisher":"EDP Sciences","volume":646,"date_published":"2021-02-08T00:00:00Z","oa_version":"Preprint"},{"article_number":"A58","article_type":"original","doi":"10.1051/0004-6361/202140506","year":"2021","author":[{"first_name":"E.","last_name":"Laplace","full_name":"Laplace, E."},{"first_name":"S.","last_name":"Justham","full_name":"Justham, S."},{"full_name":"Renzo, M.","first_name":"M.","last_name":"Renzo"},{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Farmer, R.","first_name":"R.","last_name":"Farmer"},{"first_name":"D.","last_name":"Vartanyan","full_name":"Vartanyan, D."},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"}],"scopus_import":"1","day":"02","month":"12","title":"Different to the core: The pre-supernova structures of massive single and binary-stripped stars","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"type":"journal_article","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/202140506"}],"abstract":[{"lang":"eng","text":"The majority of massive stars live in binary or multiple systems and will interact with a companion during their lifetimes, which helps to explain the observed diversity of core-collapse supernovae. Donor stars in binary systems can lose most of their hydrogen-rich envelopes through mass transfer. As a result, not only are the surface properties affected, but so is the core structure. However, most calculations of the core-collapse properties of massive stars rely on single-star models. We present a systematic study of the difference between the pre-supernova structures of single stars and stars of the same initial mass (11–21 M⊙) that have been stripped due to stable post-main-sequence mass transfer at solar metallicity. We present the pre-supernova core composition with novel diagrams that give an intuitive representation of the isotope distribution. As shown in previous studies, at the edge of the carbon-oxygen core, the binary-stripped star models contain an extended gradient of carbon, oxygen, and neon. This layer remains until core collapse and is more extended in mass for higher initial stellar masses. It originates from the receding of the convective helium core during core helium burning in binary-stripped stars, which does not occur in single-star models. We find that this same evolutionary phase leads to systematic differences in the final density and nuclear energy generation profiles. Binary-stripped star models have systematically higher total masses of carbon at the moment of core collapse compared to single-star models, which likely results in systematically different supernova yields. In about half of our models, the silicon-burning and oxygen-rich layers merge after core silicon burning. We discuss the implications of our findings for the “explodability”, supernova observations, and nucleosynthesis of these stars. Our models are publicly available and can be readily used as input for detailed supernova simulations."}],"date_created":"2023-08-03T10:11:09Z","arxiv":1,"quality_controlled":"1","status":"public","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["2102.05036"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"chicago":"Laplace, E., S. Justham, M. Renzo, Ylva Louise Linsdotter Götberg, R. Farmer, D. Vartanyan, and S. E. de Mink. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202140506\">https://doi.org/10.1051/0004-6361/202140506</a>.","ieee":"E. Laplace <i>et al.</i>, “Different to the core: The pre-supernova structures of massive single and binary-stripped stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 656. EDP Sciences, 2021.","apa":"Laplace, E., Justham, S., Renzo, M., Götberg, Y. L. L., Farmer, R., Vartanyan, D., &#38; de Mink, S. E. (2021). Different to the core: The pre-supernova structures of massive single and binary-stripped stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202140506\">https://doi.org/10.1051/0004-6361/202140506</a>","ama":"Laplace E, Justham S, Renzo M, et al. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. <i>Astronomy &#38; Astrophysics</i>. 2021;656. doi:<a href=\"https://doi.org/10.1051/0004-6361/202140506\">10.1051/0004-6361/202140506</a>","mla":"Laplace, E., et al. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 656, A58, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202140506\">10.1051/0004-6361/202140506</a>.","short":"E. Laplace, S. Justham, M. Renzo, Y.L.L. Götberg, R. Farmer, D. Vartanyan, S.E. de Mink, Astronomy &#38; Astrophysics 656 (2021).","ista":"Laplace E, Justham S, Renzo M, Götberg YLL, Farmer R, Vartanyan D, de Mink SE. 2021. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy &#38; Astrophysics. 656, A58."},"article_processing_charge":"No","date_updated":"2025-01-14T14:11:32Z","_id":"13455","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       656","oa_version":"Published Version","volume":656,"date_published":"2021-12-02T00:00:00Z","publisher":"EDP Sciences","publication_status":"published"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa":1,"type":"journal_article","abstract":[{"lang":"eng","text":"Context. Observations of massive stars in open clusters younger than ∼8 Myr have shown that a majority of them are in binary systems, most of which will interact during their life. While these can be used as a proxy of the initial multiplicity properties, studying populations of massive stars older than ∼20 Myr allows us to probe the outcome of these interactions after a significant number of systems have experienced mass and angular momentum transfer and may even have merged.\r\n\r\nAims. Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity properties of the massive-star population in the dense core of the ∼40 Myr old cluster NGC 330 in the Small Magellanic Cloud in order to search for possible imprints of stellar evolution on the multiplicity properties.\r\n\r\nMethods. We obtained six epochs of VLT/MUSE observations operated in wide-field mode with the extended wavelength setup and supported by adaptive optics. We extracted spectra and measured radial velocities for stars brighter than mF814W = 19. We identified single-lined spectroscopic binaries through significant RV variability with a peak-to-peak amplitude larger than 20 km s−1. We also identified double-lined spectroscopic binaries, and quantified the observational biases for binary detection. In particular, we took into account that binary systems with similar line strengths are difficult to detect in our data set.\r\n\r\nResults. The observed spectroscopic binary fraction among stars brighter than mF814W = 19 (approximately 5.5 M⊙ on the main sequence) is fSBobs = 13.2 ± 2.0%. Considering period and mass ratio ranges from log(P) = 0.15−3.5 (about 1.4 to 3160 d), q = 0.1−1.0, and a representative set of orbital parameter distributions, we find a bias-corrected close binary fraction of fcl = 34−7+8%. This fraction seems to decline for the fainter stars, which indicates either that the close binary fraction drops in the B-type domain, or that the period distribution becomes more heavily weighted toward longer orbital periods. We further find that both fractions vary strongly in different regions of the color-magnitude diagram, which corresponds to different evolutionary stages. This probably reveals the imprint of the binary history of different groups of stars. In particular, we find that the observed spectroscopic binary fraction of Be stars (fSBobs = 2 ± 2%) is significantly lower than that of B-type stars (fSBobs = 9 ± 2%).\r\n\r\nConclusions. We provide the first homogeneous radial velocity study of a large sample of B-type stars at a low metallicity ([Fe/H] ≲ −1.0). The overall bias-corrected close binary fraction (log(P) < 3.5 d) of the B-star population in NGC 330 is lower than the fraction reported for younger Galactic and Large Magellanic Cloud clusters in previous works. More data are needed, however, to establish whether the observed differences are caused by an age or a metallicity effect."}],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/202140507","open_access":"1"}],"date_created":"2023-08-03T10:11:34Z","quality_controlled":"1","arxiv":1,"status":"public","article_number":"A70","article_type":"original","author":[{"last_name":"Bodensteiner","first_name":"J.","full_name":"Bodensteiner, J."},{"first_name":"H.","last_name":"Sana","full_name":"Sana, H."},{"full_name":"Wang, C.","first_name":"C.","last_name":"Wang"},{"full_name":"Langer, N.","first_name":"N.","last_name":"Langer"},{"full_name":"Mahy, L.","first_name":"L.","last_name":"Mahy"},{"full_name":"Banyard, G.","first_name":"G.","last_name":"Banyard"},{"full_name":"de Koter, A.","first_name":"A.","last_name":"de Koter"},{"first_name":"S. E.","last_name":"de Mink","full_name":"de Mink, S. E."},{"first_name":"C. J.","last_name":"Evans","full_name":"Evans, C. J."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter"},{"last_name":"Patrick","first_name":"L. R.","full_name":"Patrick, L. R."},{"full_name":"Schneider, F. R. N.","last_name":"Schneider","first_name":"F. R. N."},{"last_name":"Tramper","first_name":"F.","full_name":"Tramper, F."}],"doi":"10.1051/0004-6361/202140507","year":"2021","day":"12","scopus_import":"1","month":"08","title":"The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population","publication":"Astronomy & Astrophysics","intvolume":"       652","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Published Version","volume":652,"date_published":"2021-08-12T00:00:00Z","publication_status":"published","publisher":"EDP Sciences","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["2104.13409"]},"citation":{"ama":"Bodensteiner J, Sana H, Wang C, et al. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. <i>Astronomy &#38; Astrophysics</i>. 2021;652. doi:<a href=\"https://doi.org/10.1051/0004-6361/202140507\">10.1051/0004-6361/202140507</a>","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” <i>Astronomy &#38; Astrophysics</i>, vol. 652, A70, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202140507\">10.1051/0004-6361/202140507</a>.","short":"J. Bodensteiner, H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, L.R. Patrick, F.R.N. Schneider, F. Tramper, Astronomy &#38; Astrophysics 652 (2021).","ista":"Bodensteiner J, Sana H, Wang C, Langer N, Mahy L, Banyard G, de Koter A, de Mink SE, Evans CJ, Götberg YLL, Patrick LR, Schneider FRN, Tramper F. 2021. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy &#38; Astrophysics. 652, A70.","apa":"Bodensteiner, J., Sana, H., Wang, C., Langer, N., Mahy, L., Banyard, G., … Tramper, F. (2021). The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202140507\">https://doi.org/10.1051/0004-6361/202140507</a>","chicago":"Bodensteiner, J., H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202140507\">https://doi.org/10.1051/0004-6361/202140507</a>.","ieee":"J. Bodensteiner <i>et al.</i>, “The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population,” <i>Astronomy &#38; Astrophysics</i>, vol. 652. EDP Sciences, 2021."},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2023-08-21T11:49:36Z","article_processing_charge":"No","_id":"13457"},{"_id":"11501","date_updated":"2022-07-19T09:35:43Z","article_processing_charge":"No","citation":{"chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/202038133\">https://doi.org/10.1051/0004-6361/202038133</a>.","ieee":"A. Feltre <i>et al.</i>, “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3,” <i>Astronomy &#38; Astrophysics</i>, vol. 641. EDP Sciences, 2020.","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202038133\">https://doi.org/10.1051/0004-6361/202038133</a>","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. 2020;641. doi:<a href=\"https://doi.org/10.1051/0004-6361/202038133\">10.1051/0004-6361/202038133</a>","mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>, vol. 641, A118, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/202038133\">10.1051/0004-6361/202038133</a>.","short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy &#38; Astrophysics 641 (2020).","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. Astronomy &#38; Astrophysics. 641, A118."},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"external_id":{"arxiv":["2007.01878"]},"extern":"1","language":[{"iso":"eng"}],"publication_status":"published","publisher":"EDP Sciences","volume":641,"date_published":"2020-09-18T00:00:00Z","oa_version":"Published Version","intvolume":"       641","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","month":"09","day":"18","scopus_import":"1","author":[{"full_name":"Feltre, Anna","last_name":"Feltre","first_name":"Anna"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"first_name":"Jayadev","last_name":"Pradeep","full_name":"Pradeep, Jayadev"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"},{"first_name":"Takuya","last_name":"Hashimoto","full_name":"Hashimoto, Takuya"},{"full_name":"Schmidt, Kasper B.","first_name":"Kasper B.","last_name":"Schmidt"},{"first_name":"Jeremy","last_name":"Blaizot","full_name":"Blaizot, Jeremy"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"last_name":"Boogaard","first_name":"Leindert","full_name":"Boogaard, Leindert"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"full_name":"Carton, David","first_name":"David","last_name":"Carton"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"full_name":"Kollatschny, Wolfram","first_name":"Wolfram","last_name":"Kollatschny"},{"last_name":"Marino","first_name":"Raffaella A.","full_name":"Marino, Raffaella A."},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"first_name":"Laurence","last_name":"Tresse","full_name":"Tresse, Laurence"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"first_name":"Peter M.","last_name":"Weilbacher","full_name":"Weilbacher, Peter M."}],"doi":"10.1051/0004-6361/202038133","year":"2020","article_type":"original","article_number":"A118","status":"public","quality_controlled":"1","arxiv":1,"date_created":"2022-07-06T09:38:16Z","abstract":[{"lang":"eng","text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z >  2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2007.01878"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"oa":1},{"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"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. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>","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.” <i>Astronomy &#38; Astrophysics</i>, vol. 638, A12, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>.","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. <i>Astronomy &#38; Astrophysics</i>. 2020;638. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>","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 &#38; Astrophysics 638 (2020).","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy &#38; Astrophysics. 638, A12.","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>.","ieee":"H. Kusakabe <i>et al.</i>, “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” <i>Astronomy &#38; Astrophysics</i>, vol. 638. EDP Sciences, 2020."},"external_id":{"arxiv":["2003.12083"]},"extern":"1","language":[{"iso":"eng"}],"_id":"11503","date_updated":"2022-07-19T09:35:20Z","article_processing_charge":"No","intvolume":"       638","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","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.","publication_status":"published","publisher":"EDP Sciences","volume":638,"date_published":"2020-06-03T00:00:00Z","oa_version":"Published Version","day":"03","scopus_import":"1","author":[{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"last_name":"Blaizot","first_name":"Jérémy","full_name":"Blaizot, Jérémy"},{"full_name":"Garel, Thibault","last_name":"Garel","first_name":"Thibault"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"full_name":"Conseil, Simon","first_name":"Simon","last_name":"Conseil"},{"full_name":"Guiderdoni, Bruno","last_name":"Guiderdoni","first_name":"Bruno"},{"full_name":"Drake, Alyssa B.","last_name":"Drake","first_name":"Alyssa B."},{"last_name":"Christian Herenz","first_name":"Edmund","full_name":"Christian Herenz, Edmund"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Anna Marino","first_name":"Raffaella","full_name":"Anna Marino, Raffaella"},{"last_name":"Borello Schmidt","first_name":"Kasper","full_name":"Borello Schmidt, Kasper"},{"full_name":"Pelló, Roser","last_name":"Pelló","first_name":"Roser"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"first_name":"Josephine","last_name":"Kerutt","full_name":"Kerutt, Josephine"},{"full_name":"Mahler, Guillaume","first_name":"Guillaume","last_name":"Mahler"}],"doi":"10.1051/0004-6361/201937340","year":"2020","article_type":"original","article_number":"A12","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","month":"06","date_created":"2022-07-06T09:50:48Z","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."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2003.12083"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"oa":1,"status":"public","quality_controlled":"1","arxiv":1},{"publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       635","acknowledgement":"F.L., R.B., and S.C. acknowledge support from the ERC advanced grant 339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds (PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan.","publisher":"EDP Sciences","publication_status":"published","oa_version":"Published Version","date_published":"2020-03-11T00:00:00Z","volume":635,"external_id":{"arxiv":["2002.05731"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"chicago":"Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>.","ieee":"F. Leclercq <i>et al.</i>, “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3,” <i>Astronomy &#38; Astrophysics</i>, vol. 635. EDP Sciences, 2020.","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>","mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>, vol. 635, A82, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>.","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. 2020;635. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy &#38; Astrophysics 635 (2020).","ista":"Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. Astronomy &#38; Astrophysics. 635, A82."},"language":[{"iso":"eng"}],"extern":"1","article_processing_charge":"No","date_updated":"2022-07-19T09:36:58Z","_id":"11504","main_file_link":[{"url":"https://arxiv.org/abs/2002.05731","open_access":"1"}],"abstract":[{"text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >  MUV >  −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV <  −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs.","lang":"eng"}],"date_created":"2022-07-06T09:56:20Z","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"type":"journal_article","arxiv":1,"quality_controlled":"1","status":"public","year":"2020","doi":"10.1051/0004-6361/201937339","author":[{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"full_name":"Blaizot, Jérémy","first_name":"Jérémy","last_name":"Blaizot"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"last_name":"Claeyssens","first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde"},{"first_name":"Simon","last_name":"Conseil","full_name":"Conseil, Simon"},{"last_name":"Contini","first_name":"Thierry","full_name":"Contini, Thierry"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"last_name":"Herenz","first_name":"Edmund Christian","full_name":"Herenz, Edmund Christian"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Mitchell","first_name":"Peter","full_name":"Mitchell, Peter"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"first_name":"Kasper Borello","last_name":"Schmidt","full_name":"Schmidt, Kasper Borello"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"scopus_import":"1","day":"11","article_number":"A82","article_type":"original","month":"03","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3"},{"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"chicago":"Renzo, M., R. Farmer, S. Justham, Ylva Louise Linsdotter Götberg, S. E. de Mink, E. Zapartas, P. Marchant, and N. Smith. “Predictions for the Hydrogen-Free Ejecta of Pulsational Pair-Instability Supernovae.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/202037710\">https://doi.org/10.1051/0004-6361/202037710</a>.","ieee":"M. Renzo <i>et al.</i>, “Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae,” <i>Astronomy &#38; Astrophysics</i>, vol. 640. EDP Sciences, 2020.","apa":"Renzo, M., Farmer, R., Justham, S., Götberg, Y. L. L., de Mink, S. E., Zapartas, E., … Smith, N. (2020). Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202037710\">https://doi.org/10.1051/0004-6361/202037710</a>","mla":"Renzo, M., et al. “Predictions for the Hydrogen-Free Ejecta of Pulsational Pair-Instability Supernovae.” <i>Astronomy &#38; Astrophysics</i>, vol. 640, A56, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/202037710\">10.1051/0004-6361/202037710</a>.","ama":"Renzo M, Farmer R, Justham S, et al. Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae. <i>Astronomy &#38; Astrophysics</i>. 2020;640. doi:<a href=\"https://doi.org/10.1051/0004-6361/202037710\">10.1051/0004-6361/202037710</a>","short":"M. Renzo, R. Farmer, S. Justham, Y.L.L. Götberg, S.E. de Mink, E. Zapartas, P. Marchant, N. Smith, Astronomy &#38; Astrophysics 640 (2020).","ista":"Renzo M, Farmer R, Justham S, Götberg YLL, de Mink SE, Zapartas E, Marchant P, Smith N. 2020. Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae. Astronomy &#38; Astrophysics. 640, A56."},"external_id":{"arxiv":["2002.05077"]},"extern":"1","language":[{"iso":"eng"}],"_id":"13463","article_processing_charge":"No","date_updated":"2023-08-09T12:58:41Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       640","publication":"Astronomy & Astrophysics","publisher":"EDP Sciences","publication_status":"published","date_published":"2020-08-12T00:00:00Z","volume":640,"oa_version":"Published Version","scopus_import":"1","day":"12","doi":"10.1051/0004-6361/202037710","year":"2020","author":[{"first_name":"M.","last_name":"Renzo","full_name":"Renzo, M."},{"last_name":"Farmer","first_name":"R.","full_name":"Farmer, R."},{"full_name":"Justham, S.","last_name":"Justham","first_name":"S."},{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"de Mink, S. E.","last_name":"de Mink","first_name":"S. E."},{"last_name":"Zapartas","first_name":"E.","full_name":"Zapartas, E."},{"full_name":"Marchant, P.","first_name":"P.","last_name":"Marchant"},{"last_name":"Smith","first_name":"N.","full_name":"Smith, N."}],"article_type":"original","article_number":"A56","title":"Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae","month":"08","date_created":"2023-08-03T10:12:58Z","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/202037710"}],"abstract":[{"lang":"eng","text":"Present and upcoming time-domain astronomy efforts, in part driven by gravitational-wave follow-up campaigns, will unveil a variety of rare explosive transients in the sky. Here, we focus on pulsational pair-instability evolution, which can result in signatures that are observable with electromagnetic and gravitational waves. We simulated grids of bare helium stars to characterize the resulting black hole (BH) masses together with the ejecta composition, velocity, and thermal state. We find that the stars do not react “elastically” to the thermonuclear ignition in the core: there is not a one-to-one correspondence between pair-instability driven ignition and mass ejections, which causes ambiguity as to what is an observable pulse. In agreement with previous studies, we find that for initial helium core masses of 37.5 M⊙ ≲ MHe, init ≲ 41 M⊙, corresponding to carbon-oxygen core masses 27.5 M⊙ ≲ MCO ≲ 30.1 M⊙, the explosions are not strong enough to affect the surface. With increasing initial helium core mass, they become progressively stronger causing first large radial expansion (41 M⊙ ≲ MHe, init ≲ 42 M⊙, corresponding to 30.1 M⊙ ≲ MCO ≲ 30.8 M⊙) and, finally, also mass ejection episodes (for MHe, init ≳ 42 M⊙, or MCO ≳ 30.8 M⊙). The lowest mass helium core to be fully disrupted in a pair-instability supernova is MHe, init ≃ 80 M⊙, corresponding to MCO ≃ 55 M⊙. Models with MHe, init ≳ 200 M⊙ (MCO ≳ 114 M⊙) reach the photodisintegration regime, resulting in BHs with masses of MBH ≳ 125 M⊙. Although this is currently considered unlikely, if BHs from these models form via (weak) explosions, the previously-ejected material might be hit by the blast wave and convert kinetic energy into observable electromagnetic radiation. We characterize the hydrogen-free circumstellar material from the pulsational pair-instability of helium cores by simply assuming that the ejecta maintain a constant velocity after ejection. We find that our models produce helium-rich ejecta with mass of 10−3 M⊙ ≲ MCSM ≲ 40 M⊙, the larger values corresponding to the more massive progenitor stars. These ejecta are typically launched at a few thousand km s−1 and reach distances of ∼1012 − 1015 cm before the core-collapse of the star. The delays between mass ejection events and the final collapse span a wide and mass-dependent range (from subhour to 104 years), and the shells ejected can also collide with each other, powering supernova impostor events before the final core-collapse. The range of properties we find suggests a possible connection with (some) type Ibn supernovae."}],"type":"journal_article","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","arxiv":1,"quality_controlled":"1"},{"publication":"Astronomy & Astrophysics","intvolume":"       637","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","publisher":"EDP Sciences","oa_version":"Published Version","date_published":"2020-05-01T00:00:00Z","volume":637,"external_id":{"arxiv":["2003.01120"]},"citation":{"apa":"Laplace, E., Götberg, Y. L. L., de Mink, S. E., Justham, S., &#38; Farmer, R. (2020). The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937300\">https://doi.org/10.1051/0004-6361/201937300</a>","mla":"Laplace, E., et al. “The Expansion of Stripped-Envelope Stars: Consequences for Supernovae and Gravitational-Wave Progenitors.” <i>Astronomy &#38; Astrophysics</i>, vol. 637, A6, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937300\">10.1051/0004-6361/201937300</a>.","ama":"Laplace E, Götberg YLL, de Mink SE, Justham S, Farmer R. The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors. <i>Astronomy &#38; Astrophysics</i>. 2020;637. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937300\">10.1051/0004-6361/201937300</a>","short":"E. Laplace, Y.L.L. Götberg, S.E. de Mink, S. Justham, R. Farmer, Astronomy &#38; Astrophysics 637 (2020).","ista":"Laplace E, Götberg YLL, de Mink SE, Justham S, Farmer R. 2020. The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors. Astronomy &#38; Astrophysics. 637, A6.","chicago":"Laplace, E., Ylva Louise Linsdotter Götberg, S. E. de Mink, S. Justham, and R. Farmer. “The Expansion of Stripped-Envelope Stars: Consequences for Supernovae and Gravitational-Wave Progenitors.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937300\">https://doi.org/10.1051/0004-6361/201937300</a>.","ieee":"E. Laplace, Y. L. L. Götberg, S. E. de Mink, S. Justham, and R. Farmer, “The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors,” <i>Astronomy &#38; Astrophysics</i>, vol. 637. EDP Sciences, 2020."},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"language":[{"iso":"eng"}],"extern":"1","date_updated":"2023-08-09T12:56:32Z","article_processing_charge":"No","_id":"13464","abstract":[{"lang":"eng","text":"Massive binaries that merge as compact objects are the progenitors of gravitational-wave sources. Most of these binaries experience one or more phases of mass transfer, during which one of the stars loses all or part of its outer envelope and becomes a stripped-envelope star. The evolution of the size of these stripped stars is crucial in determining whether they experience further interactions and understanding their ultimate fate. We present new calculations of stripped-envelope stars based on binary evolution models computed with MESA. We use these to investigate their radius evolution as a function of mass and metallicity. We further discuss their pre-supernova observable characteristics and potential consequences of their evolution on the properties of supernovae from stripped stars. At high metallicity, we find that practically all of the hydrogen-rich envelope is removed, which is in agreement with earlier findings. Only progenitors with initial masses below 10 M⊙ expand to large radii (up to 100 R⊙), while more massive progenitors remain compact. At low metallicity, a substantial amount of hydrogen remains and the progenitors can, in principle, expand to giant sizes (> 400 R⊙) for all masses we consider. This implies that they can fill their Roche lobe anew. We show that the prescriptions commonly used in population synthesis models underestimate the stellar radii by up to two orders of magnitude. We expect that this has consequences for the predictions for gravitational-wave sources from double neutron star mergers, particularly with regard to their metallicity dependence."}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201937300"}],"date_created":"2023-08-03T10:13:10Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa":1,"type":"journal_article","quality_controlled":"1","arxiv":1,"status":"public","author":[{"last_name":"Laplace","first_name":"E.","full_name":"Laplace, E."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"full_name":"Justham, S.","last_name":"Justham","first_name":"S."},{"full_name":"Farmer, R.","first_name":"R.","last_name":"Farmer"}],"year":"2020","doi":"10.1051/0004-6361/201937300","day":"01","scopus_import":"1","article_number":"A6","article_type":"original","month":"05","title":"The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors"},{"date_published":"2020-02-05T00:00:00Z","volume":634,"oa_version":"Published Version","publication_status":"published","publisher":"EDP Sciences","intvolume":"       634","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","_id":"13466","date_updated":"2023-08-09T12:50:01Z","article_processing_charge":"No","extern":"1","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"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. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201936743\">https://doi.org/10.1051/0004-6361/201936743</a>","ama":"Bodensteiner J, Sana H, Mahy L, et al. The young massive SMC cluster NGC 330 seen by MUSE. <i>Astronomy &#38; Astrophysics</i>. 2020;634. doi:<a href=\"https://doi.org/10.1051/0004-6361/201936743\">10.1051/0004-6361/201936743</a>","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.” <i>Astronomy &#38; Astrophysics</i>, vol. 634, A51, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201936743\">10.1051/0004-6361/201936743</a>.","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 &#38; 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 &#38; Astrophysics 634 (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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201936743\">https://doi.org/10.1051/0004-6361/201936743</a>.","ieee":"J. Bodensteiner <i>et al.</i>, “The young massive SMC cluster NGC 330 seen by MUSE,” <i>Astronomy &#38; Astrophysics</i>, vol. 634. EDP Sciences, 2020."},"external_id":{"arxiv":["1911.03477"]},"status":"public","quality_controlled":"1","arxiv":1,"type":"journal_article","keyword":["stars: massive / stars: emission-line / Be / binaries: spectroscopic / blue stragglers / Magellanic Clouds"],"oa":1,"date_created":"2023-08-03T10:13:29Z","abstract":[{"lang":"eng","text":"Context. A majority of massive stars are part of binary systems, a large fraction of which will inevitably interact during their lives. Binary-interaction products (BiPs), that is, stars affected by such interaction, are expected to be commonly present in stellar populations. BiPs are thus a crucial ingredient in the understanding of stellar evolution.\r\nAims. We aim to identify and characterize a statistically significant sample of BiPs by studying clusters of 10 − 40 Myr, an age at which binary population models predict the abundance of BiPs to be highest. One example of such a cluster is NGC 330 in the Small Magellanic Cloud.\r\nMethods. Using MUSE WFM-AO observations of NGC 330, we resolved the dense cluster core for the first time and were able to extract spectra of its entire massive star population. We developed an automated spectral classification scheme based on the equivalent widths of spectral lines in the red part of the spectrum.\r\nResults. We characterize the massive star content of the core of NGC 330, which contains more than 200 B stars, 2 O stars, 6 A-type supergiants, and 11 red supergiants. We find a lower limit on the Be star fraction of 32 ± 3% in the whole sample. It increases to at least 46 ± 10% when we only consider stars brighter than V = 17 mag. We estimate an age of the cluster core between 35 and 40 Myr and a total cluster mass of 88−18+17 × 103 M⊙.\r\nConclusions. We find that the population in the cluster core is different than the population in the outskirts: while the stellar content in the core appears to be older than the stars in the outskirts, the Be star fraction and the observed binary fraction are significantly higher. Furthermore, we detect several BiP candidates that will be subject of future studies."}],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201936743","open_access":"1"}],"title":"The young massive SMC cluster NGC 330 seen by MUSE","month":"02","article_type":"original","article_number":"A51","day":"05","scopus_import":"1","author":[{"last_name":"Bodensteiner","first_name":"J.","full_name":"Bodensteiner, J."},{"full_name":"Sana, H.","first_name":"H.","last_name":"Sana"},{"last_name":"Mahy","first_name":"L.","full_name":"Mahy, L."},{"full_name":"Patrick, L. R.","first_name":"L. R.","last_name":"Patrick"},{"full_name":"de Koter, A.","last_name":"de Koter","first_name":"A."},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"last_name":"Evans","first_name":"C. J.","full_name":"Evans, C. J."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"full_name":"Langer, N.","last_name":"Langer","first_name":"N."},{"first_name":"D. J.","last_name":"Lennon","full_name":"Lennon, D. J."},{"last_name":"Schneider","first_name":"F. R. N.","full_name":"Schneider, F. R. N."},{"full_name":"Tramper, F.","last_name":"Tramper","first_name":"F."}],"doi":"10.1051/0004-6361/201936743","year":"2020"},{"day":"25","scopus_import":"1","author":[{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter"},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"first_name":"M.","last_name":"McQuinn","full_name":"McQuinn, M."},{"last_name":"Zapartas","first_name":"E.","full_name":"Zapartas, E."},{"full_name":"Groh, J. H.","last_name":"Groh","first_name":"J. H."},{"full_name":"Norman, C.","first_name":"C.","last_name":"Norman"}],"year":"2020","doi":"10.1051/0004-6361/201936669","article_type":"original","article_number":"A134","title":"Contribution from stars stripped in binaries to cosmic reionization of hydrogen and helium","month":"02","date_created":"2023-08-03T10:13:43Z","abstract":[{"text":"Massive stars are often found in binary systems, and it has been argued that binary products boost the ionizing radiation of stellar populations. Accurate predictions for binary products are needed to understand and quantify their contribution to cosmic reionization. We investigate the contribution of stars stripped in binaries because (1) they are, arguably, the best-understood products of binary evolution, (2) we recently produced the first radiative transfer calculations for the atmospheres of these stripped stars that predict their ionizing spectra, and (3) they are very promising sources because they boost the ionizing emission of stellar populations at late times. This allows stellar feedback to clear the surroundings such that a higher fraction of their photons can escape and ionize the intergalactic medium. Combining our detailed predictions for the ionizing spectra with a simple cosmic reionization model, we estimate that stripped stars contributed tens of percent of the photons that caused cosmic reionization of hydrogen, depending on the assumed escape fractions. More importantly, stripped stars harden the ionizing emission. We estimate that the spectral index for the ionizing part of the spectrum can increase to −1 compared to ≲ − 2 for single stars. At high redshift, stripped stars and massive single stars combined dominate the He II-ionizing emission, but we expect that active galactic nuclei drive cosmic helium reionization. Further observational consequences we expect are (1) high ionization states for the intergalactic gas surrounding stellar systems, such as C IV and Si IV, and (2) additional heating of the intergalactic medium of up to a few thousand Kelvin. Quantifying these warrants the inclusion of accurate models for stripped stars and other binary products in full cosmological simulations.","lang":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201936669","open_access":"1"}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa":1,"status":"public","arxiv":1,"quality_controlled":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"apa":"Götberg, Y. L. L., de Mink, S. E., McQuinn, M., Zapartas, E., Groh, J. H., &#38; Norman, C. (2020). Contribution from stars stripped in binaries to cosmic reionization of hydrogen and helium. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201936669\">https://doi.org/10.1051/0004-6361/201936669</a>","ista":"Götberg YLL, de Mink SE, McQuinn M, Zapartas E, Groh JH, Norman C. 2020. Contribution from stars stripped in binaries to cosmic reionization of hydrogen and helium. Astronomy &#38; Astrophysics. 634, A134.","short":"Y.L.L. Götberg, S.E. de Mink, M. McQuinn, E. Zapartas, J.H. Groh, C. Norman, Astronomy &#38; Astrophysics 634 (2020).","ama":"Götberg YLL, de Mink SE, McQuinn M, Zapartas E, Groh JH, Norman C. Contribution from stars stripped in binaries to cosmic reionization of hydrogen and helium. <i>Astronomy &#38; Astrophysics</i>. 2020;634. doi:<a href=\"https://doi.org/10.1051/0004-6361/201936669\">10.1051/0004-6361/201936669</a>","mla":"Götberg, Ylva Louise Linsdotter, et al. “Contribution from Stars Stripped in Binaries to Cosmic Reionization of Hydrogen and Helium.” <i>Astronomy &#38; Astrophysics</i>, vol. 634, A134, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201936669\">10.1051/0004-6361/201936669</a>.","ieee":"Y. L. L. Götberg, S. E. de Mink, M. McQuinn, E. Zapartas, J. H. Groh, and C. Norman, “Contribution from stars stripped in binaries to cosmic reionization of hydrogen and helium,” <i>Astronomy &#38; Astrophysics</i>, vol. 634. EDP Sciences, 2020.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, M. McQuinn, E. Zapartas, J. H. Groh, and C. Norman. “Contribution from Stars Stripped in Binaries to Cosmic Reionization of Hydrogen and Helium.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201936669\">https://doi.org/10.1051/0004-6361/201936669</a>."},"external_id":{"arxiv":["1911.00543"]},"extern":"1","language":[{"iso":"eng"}],"_id":"13467","date_updated":"2024-10-14T12:22:53Z","article_processing_charge":"No","intvolume":"       634","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","publication_status":"published","publisher":"EDP Sciences","volume":634,"date_published":"2020-02-25T00:00:00Z","oa_version":"Published Version"},{"arxiv":1,"quality_controlled":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift"],"oa":1,"type":"journal_article","abstract":[{"text":"Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys. Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II λ1640 equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models to match the observed He II λ1640 properties.","lang":"eng"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.05960"}],"date_created":"2022-07-06T09:07:06Z","month":"04","title":"Exploring He II λ1640 emission line properties at z ∼2−4","related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1051/0004-6361/201834565e"}]},"article_number":"A89","article_type":"original","author":[{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Brinchmann, Jarle","last_name":"Brinchmann","first_name":"Jarle"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Feltre, Anna","last_name":"Feltre","first_name":"Anna"},{"full_name":"Kollatschny, Wolfram","last_name":"Kollatschny","first_name":"Wolfram"},{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Paalvast, Mieke","last_name":"Paalvast","first_name":"Mieke"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"}],"doi":"10.1051/0004-6361/201834565","year":"2019","day":"16","scopus_import":"1","oa_version":"Published Version","date_published":"2019-04-16T00:00:00Z","volume":648,"publication_status":"published","publisher":"EDP Sciences","acknowledgement":"The authors wish to thank the referee for constructive comments that improved the paper substantially. We thank the BPASS team for making the stellar population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz Centre and the scientific organizers of the Characterizing galaxies with spectroscopy with a view for JWST workshop held at the Lorentz Centre in 2017 October, which promoted useful discussions in the wider community. TN, JB, and RB acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057. AF acknowledges support from the ERC via an Advanced Grant under grant agreement no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research made use of astropy (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org). Facilities: VLT (MUSE).","publication":"Astronomy & Astrophysics","intvolume":"       648","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-07-19T09:36:08Z","article_processing_charge":"No","_id":"11499","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["1902.05960"]},"citation":{"apa":"Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S., Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834565\">https://doi.org/10.1051/0004-6361/201834565</a>","ista":"Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A, Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &#38; Astrophysics. 648, A89.","short":"T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A. Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J. Richard, A. Verhamme, Astronomy &#38; Astrophysics 648 (2019).","ama":"Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. 2019;648. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834565\">10.1051/0004-6361/201834565</a>","mla":"Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>, vol. 648, A89, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834565\">10.1051/0004-6361/201834565</a>.","ieee":"T. Nanayakkara <i>et al.</i>, “Exploring He II λ1640 emission line properties at z ∼2−4,” <i>Astronomy &#38; Astrophysics</i>, vol. 648. EDP Sciences, 2019.","chicago":"Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens, Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834565\">https://doi.org/10.1051/0004-6361/201834565</a>."},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"volume":628,"date_published":"2019-07-25T00:00:00Z","oa_version":"Published Version","publication_status":"published","publisher":"EDP Sciences","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).","intvolume":"       628","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","_id":"11505","date_updated":"2022-07-19T09:36:31Z","article_processing_charge":"No","extern":"1","language":[{"iso":"eng"}],"citation":{"ieee":"G. de La Vieuville <i>et al.</i>, “Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE,” <i>Astronomy &#38; Astrophysics</i>, vol. 628. EDP Sciences, 2019.","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>.","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 &#38; 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 &#38; Astrophysics. 628, A3.","mla":"de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>, vol. 628, A3, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>.","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. <i>Astronomy &#38; Astrophysics</i>. 2019;628. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>","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. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>"},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"external_id":{"arxiv":["1905.13696"]},"status":"public","arxiv":1,"quality_controlled":"1","type":"journal_article","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"],"oa":1,"date_created":"2022-07-06T10:09:36Z","abstract":[{"lang":"eng","text":"Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 <  z <  6, 7, 2.9 <  z <  4.0, 4.0 <  z <  5.0, and 5.0 <  z <  6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1905.13696"}],"title":"Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE","month":"07","article_type":"original","article_number":"A3","day":"25","scopus_import":"1","author":[{"last_name":"de La Vieuville","first_name":"G.","full_name":"de La Vieuville, G."},{"last_name":"Bina","first_name":"D.","full_name":"Bina, D."},{"full_name":"Pello, R.","first_name":"R.","last_name":"Pello"},{"first_name":"G.","last_name":"Mahler","full_name":"Mahler, G."},{"last_name":"Richard","first_name":"J.","full_name":"Richard, J."},{"last_name":"Drake","first_name":"A. B.","full_name":"Drake, A. B."},{"full_name":"Herenz, E. C.","last_name":"Herenz","first_name":"E. C."},{"first_name":"F. E.","last_name":"Bauer","full_name":"Bauer, F. E."},{"full_name":"Clément, B.","last_name":"Clément","first_name":"B."},{"full_name":"Lagattuta, D.","last_name":"Lagattuta","first_name":"D."},{"first_name":"N.","last_name":"Laporte","full_name":"Laporte, N."},{"last_name":"Martinez","first_name":"J.","full_name":"Martinez, J."},{"full_name":"Patrício, V.","last_name":"Patrício","first_name":"V."},{"full_name":"Wisotzki, L.","first_name":"L.","last_name":"Wisotzki"},{"full_name":"Zabl, J.","first_name":"J.","last_name":"Zabl"},{"first_name":"R. J.","last_name":"Bouwens","full_name":"Bouwens, R. J."},{"last_name":"Contini","first_name":"T.","full_name":"Contini, T."},{"full_name":"Garel, T.","last_name":"Garel","first_name":"T."},{"full_name":"Guiderdoni, B.","last_name":"Guiderdoni","first_name":"B."},{"first_name":"R. A.","last_name":"Marino","full_name":"Marino, R. A."},{"full_name":"Maseda, M. V.","last_name":"Maseda","first_name":"M. V."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Schaye","first_name":"J.","full_name":"Schaye, J."},{"full_name":"Soucail, G.","first_name":"G.","last_name":"Soucail"}],"year":"2019","doi":"10.1051/0004-6361/201834471"},{"oa_version":"Published Version","volume":623,"date_published":"2019-03-26T00:00:00Z","publisher":"EDP Sciences","publication_status":"published","acknowledgement":"We thank the anonymous referees for multiple comments and suggestions which have improved the manuscript. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017, 2018a) and we also provide the toy model used as a PYTHON script.","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       623","article_processing_charge":"No","date_updated":"2022-07-19T09:37:20Z","_id":"11507","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["1803.08923"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"ieee":"D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator,” <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.","chicago":"Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>.","short":"D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).","ista":"Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy &#38; Astrophysics. 623, A157.","mla":"Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A157, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>.","ama":"Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. 2019;623. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>","apa":"Sobral, D., &#38; Matthee, J. J. (2019). Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>"},"quality_controlled":"1","arxiv":1,"status":"public","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1803.08923"}],"abstract":[{"text":"Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies. While it originates from many physical processes, for star-forming galaxies the intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star formation rate (SFR) indicator. However, its resonant nature and susceptibility to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs) at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and we show that it constrains a well-defined anti-correlation between ionisation efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0 are easy measurable quantities at high redshift, thus making our relation a practical tool to estimate intrinsic Lyα and LyC luminosities under well controlled and simple assumptions. Our results allow observed Lyα luminosities to be used to compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs. We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6 to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1 and that our calibration might be even applicable for the most luminous LAEs within the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1] = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily tested with future observations with JWST which can obtain Hα and Hβ measurements for high-redshift LAEs.","lang":"eng"}],"date_created":"2022-07-06T11:08:16Z","month":"03","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","article_number":"A157","article_type":"original","doi":"10.1051/0004-6361/201833075","year":"2019","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"scopus_import":"1","day":"26"},{"extern":"1","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"chicago":"Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall, M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” <i>Astronomy &#38; Astrophysics</i>. EDP Science, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834780\">https://doi.org/10.1051/0004-6361/201834780</a>.","ieee":"L. A. Bugnet <i>et al.</i>, “FliPerClass: In search of solar-like pulsators among TESS targets,” <i>Astronomy &#38; Astrophysics</i>, vol. 624. EDP Science, 2019.","apa":"Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund, M. N., &#38; Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators among TESS targets. <i>Astronomy &#38; Astrophysics</i>. EDP Science. <a href=\"https://doi.org/10.1051/0004-6361/201834780\">https://doi.org/10.1051/0004-6361/201834780</a>","mla":"Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” <i>Astronomy &#38; Astrophysics</i>, vol. 624, A79, EDP Science, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834780\">10.1051/0004-6361/201834780</a>.","ama":"Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like pulsators among TESS targets. <i>Astronomy &#38; Astrophysics</i>. 2019;624. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834780\">10.1051/0004-6361/201834780</a>","short":"L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M. Rendle, Astronomy &#38; Astrophysics 624 (2019).","ista":"Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy &#38; Astrophysics. 624, A79."},"external_id":{"arxiv":["1902.09854"]},"_id":"11614","date_updated":"2024-10-14T11:39:57Z","article_processing_charge":"No","acknowledgement":"We thank the enitre T’DA team for useful comments and discussions, in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106).","intvolume":"       624","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","date_published":"2019-04-19T00:00:00Z","volume":624,"oa_version":"Preprint","publication_status":"published","publisher":"EDP Science","article_type":"original","article_number":"A79","day":"19","scopus_import":"1","author":[{"orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"last_name":"Davies","first_name":"G. R.","full_name":"Davies, G. R."},{"last_name":"Hall","first_name":"O. J.","full_name":"Hall, O. J."},{"last_name":"Lund","first_name":"M. N.","full_name":"Lund, M. N."},{"full_name":"Rendle, B. M.","first_name":"B. M.","last_name":"Rendle"}],"doi":"10.1051/0004-6361/201834780","year":"2019","title":"FliPerClass: In search of solar-like pulsators among TESS targets","month":"04","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa":1,"date_created":"2022-07-18T14:13:34Z","abstract":[{"lang":"eng","text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide full-frame images of almost the entire sky. The amount of stellar data to be analysed represents hundreds of millions stars, which is several orders of magnitude more than the number of stars observed by the Convection, Rotation and planetary Transits satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying the newly observed stars with near real-time algorithms to better guide the subsequent detailed studies. In this paper, we present a classification algorithm built to recognise solar-like pulsators among classical pulsators. This algorithm relies on the global amount of power contained in the power spectral density (PSD), also known as the flicker in spectral power density (FliPer). Because each type of pulsating star has a characteristic background or pulsation pattern, the shape of the PSD at different frequencies can be used to characterise the type of pulsating star. The FliPer classifier (FliPerClass) uses different FliPer parameters along with the effective temperature as input parameters to feed a ML algorithm in order to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators with a 98% accuracy. Among them, solar-like pulsating stars are recognised with a 99% accuracy, which is of great interest for a further seismic analysis of these stars, which are like our Sun. Similar results are obtained when we trained our classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is part of the large TASC classification pipeline developed by the TESS Data for Asteroseismology (T’DA) classification working group."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.09854"}],"status":"public","arxiv":1,"quality_controlled":"1"},{"month":"11","title":"The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction","article_number":"A5","article_type":"original","doi":"10.1051/0004-6361/201935854","year":"2019","author":[{"full_name":"Zapartas, Emmanouil","last_name":"Zapartas","first_name":"Emmanouil"},{"last_name":"de Mink","first_name":"Selma E.","full_name":"de Mink, Selma E."},{"last_name":"Justham","first_name":"Stephen","full_name":"Justham, Stephen"},{"full_name":"Smith, Nathan","last_name":"Smith","first_name":"Nathan"},{"full_name":"de Koter, Alex","first_name":"Alex","last_name":"de Koter"},{"last_name":"Renzo","first_name":"Mathieu","full_name":"Renzo, Mathieu"},{"last_name":"Arcavi","first_name":"Iair","full_name":"Arcavi, Iair"},{"last_name":"Farmer","first_name":"Rob","full_name":"Farmer, Rob"},{"orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Toonen, Silvia","last_name":"Toonen","first_name":"Silvia"}],"scopus_import":"1","day":"20","arxiv":1,"quality_controlled":"1","status":"public","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"type":"journal_article","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201935854"}],"abstract":[{"lang":"eng","text":"Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class of explosions observed following the collapse of the core of massive stars. We used analytical estimates and population synthesis simulations to assess the fraction of SNe II progenitors that are expected to have exchanged mass with a companion prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history of mass exchange with a binary companion before exploding. The dominant binary channels leading to SN II progenitors involve the merger of binary stars. Mergers are expected to produce a diversity of SN II progenitor characteristics, depending on the evolutionary timing and properties of the merger. Alternatively, SN II progenitors from interacting binaries may have accreted mass from their companion, and subsequently been ejected from the binary system after their companion exploded. We show that the overall fraction of SN II progenitors that are predicted to have experienced binary interaction is robust against the main physical uncertainties in our models. However, the relative importance of different binary evolutionary channels is affected by changing physical assumptions. We further discuss ways in which binarity might contribute to the observed diversity of SNe II by considering potential observational signatures arising from each binary channel. For supernovae which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb SNe), a surviving non-compact companion would typically indicate that the supernova progenitor star was in a wide, non-interacting binary. We argue that a significant fraction of even Type II-P SNe are expected to have gained mass from a companion prior to explosion."}],"date_created":"2023-08-03T10:13:52Z","article_processing_charge":"No","date_updated":"2023-08-09T12:36:09Z","_id":"13468","language":[{"iso":"eng"}],"extern":"1","external_id":{"arxiv":["1907.06687"]},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"chicago":"Zapartas, Emmanouil, Selma E. de Mink, Stephen Justham, Nathan Smith, Alex de Koter, Mathieu Renzo, Iair Arcavi, Rob Farmer, Ylva Louise Linsdotter Götberg, and Silvia Toonen. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>.","ieee":"E. Zapartas <i>et al.</i>, “The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction,” <i>Astronomy &#38; Astrophysics</i>, vol. 631. EDP Sciences, 2019.","apa":"Zapartas, E., de Mink, S. E., Justham, S., Smith, N., de Koter, A., Renzo, M., … Toonen, S. (2019). The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>","ama":"Zapartas E, de Mink SE, Justham S, et al. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. 2019;631. doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>","mla":"Zapartas, Emmanouil, et al. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>, vol. 631, A5, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>.","short":"E. Zapartas, S.E. de Mink, S. Justham, N. Smith, A. de Koter, M. Renzo, I. Arcavi, R. Farmer, Y.L.L. Götberg, S. Toonen, Astronomy &#38; Astrophysics 631 (2019).","ista":"Zapartas E, de Mink SE, Justham S, Smith N, de Koter A, Renzo M, Arcavi I, Farmer R, Götberg YLL, Toonen S. 2019. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. Astronomy &#38; Astrophysics. 631, A5."},"oa_version":"Published Version","date_published":"2019-11-20T00:00:00Z","volume":631,"publisher":"EDP Sciences","publication_status":"published","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       631"},{"_id":"13469","article_processing_charge":"No","date_updated":"2024-10-14T12:22:42Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"apa":"Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Leitherer, C., &#38; Norman, C. (2019). The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>","short":"Y.L.L. Götberg, S.E. de Mink, J.H. Groh, C. Leitherer, C. Norman, Astronomy &#38; Astrophysics 629 (2019).","ista":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. 2019. The impact of stars stripped in binaries on the integrated spectra of stellar populations. Astronomy &#38; Astrophysics. 629, A134.","mla":"Götberg, Ylva Louise Linsdotter, et al. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>, vol. 629, A134, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>.","ama":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. 2019;629. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>","ieee":"Y. L. L. Götberg, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman, “The impact of stars stripped in binaries on the integrated spectra of stellar populations,” <i>Astronomy &#38; Astrophysics</i>, vol. 629. EDP Sciences, 2019.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>."},"external_id":{"arxiv":["1908.06102"]},"extern":"1","language":[{"iso":"eng"}],"publisher":"EDP Sciences","publication_status":"published","date_published":"2019-09-17T00:00:00Z","volume":629,"oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       629","publication":"Astronomy & Astrophysics","title":"The impact of stars stripped in binaries on the integrated spectra of stellar populations","month":"09","scopus_import":"1","day":"17","year":"2019","doi":"10.1051/0004-6361/201834525","author":[{"orcid":"0000-0002-6960-6911","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"S. E.","last_name":"de Mink","full_name":"de Mink, S. E."},{"last_name":"Groh","first_name":"J. H.","full_name":"Groh, J. H."},{"full_name":"Leitherer, C.","last_name":"Leitherer","first_name":"C."},{"full_name":"Norman, C.","first_name":"C.","last_name":"Norman"}],"article_type":"original","article_number":"A134","status":"public","arxiv":1,"quality_controlled":"1","date_created":"2023-08-03T10:14:00Z","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201834525"}],"abstract":[{"text":"Stars stripped of their envelopes from interaction with a binary companion emit a significant fraction of their radiation as ionizing photons. They are potentially important stellar sources of ionizing radiation, however, they are still often neglected in spectral synthesis simulations or simulations of stellar feedback. In anticipating the large datasets of galaxy spectra from the upcoming James Webb Space Telescope, we modeled the radiative contribution from stripped stars by using detailed evolutionary and spectral models. We estimated their impact on the integrated spectra and specifically on the emission rates of H I-, He I-, and He II-ionizing photons from stellar populations. We find that stripped stars have the largest impact on the ionizing spectrum of a population in which star formation halted several Myr ago. In such stellar populations, stripped stars dominate the emission of ionizing photons, mimicking a younger stellar population in which massive stars are still present. Our models also suggest that stripped stars have harder ionizing spectra than massive stars. The additional ionizing radiation, with which stripped stars contribute affects observable properties that are related to the emission of ionizing photons from stellar populations. In co-eval stellar populations, the ionizing radiation from stripped stars increases the ionization parameter and the production efficiency of hydrogen ionizing photons. They also cause high values for these parameters for about ten times longer than what is predicted for massive stars. The effect on properties related to non-ionizing wavelengths is less pronounced, such as on the ultraviolet continuum slope or stellar contribution to emission lines. However, the hard ionizing radiation from stripped stars likely introduces a characteristic ionization structure of the nebula, which leads to the emission of highly ionized elements such as O2+ and C3+. We, therefore, expect that the presence of stripped stars affects the location in the BPT diagram and the diagnostic ratio of O III to O II nebular emission lines. Our models are publicly available through CDS database and on the STARBURST99 website.","lang":"eng"}],"type":"journal_article","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"]}]