[{"date_published":"2024-02-01T00:00:00Z","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2024","external_id":{"arxiv":["2305.07044"]},"quality_controlled":"1","page":"9853-9871","ddc":["520"],"_id":"14852","date_updated":"2024-01-23T12:33:50Z","type":"journal_article","article_processing_charge":"Yes (in subscription journal)","doi":"10.1093/mnras/stad3853","publisher":"Oxford University Press","citation":{"ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871.","chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>","mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>.","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;527(4):9853-9871. doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>","ieee":"I. Kramarenko <i>et al.</i>, “Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871."},"issue":"4","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"department":[{"_id":"GradSch"},{"_id":"JoMa"}],"file":[{"checksum":"9d02df4035c4951cf63dee0db1e462e9","relation":"main_file","content_type":"application/pdf","access_level":"open_access","file_name":"2024_MNAstronomSoc_Kramarenko.pdf","success":1,"file_id":"14879","date_updated":"2024-01-23T12:30:45Z","creator":"dernst","date_created":"2024-01-23T12:30:45Z","file_size":4521738}],"arxiv":1,"month":"02","file_date_updated":"2024-01-23T12:30:45Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","has_accepted_license":"1","license":"https://creativecommons.org/licenses/by/4.0/","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","short":"CC BY (4.0)"},"intvolume":"       527","abstract":[{"text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &amp;lt; z &amp;lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization.","lang":"eng"}],"volume":527,"date_created":"2024-01-22T08:22:17Z","article_type":"original","day":"01","author":[{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan"},{"full_name":"Kerutt, J","last_name":"Kerutt","first_name":"J"},{"first_name":"A","full_name":"Verhamme, A","last_name":"Verhamme"},{"first_name":"P A","full_name":"Oesch, P A","last_name":"Oesch"},{"last_name":"Barrufet","full_name":"Barrufet, L","first_name":"L"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"H","last_name":"Kusakabe","full_name":"Kusakabe, H"},{"full_name":"Goovaerts, I","last_name":"Goovaerts","first_name":"I"},{"last_name":"Thai","full_name":"Thai, T T","first_name":"T T"}],"title":"Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape","oa_version":"Published Version"},{"volume":952,"date_created":"2023-08-01T14:19:16Z","article_type":"original","day":"01","author":[{"first_name":"Savita","full_name":"Mathur, Savita","last_name":"Mathur"},{"full_name":"Claytor, Zachary R.","last_name":"Claytor","first_name":"Zachary R."},{"first_name":"Ângela R. G.","full_name":"Santos, Ângela R. G.","last_name":"Santos"},{"last_name":"García","full_name":"García, Rafael A.","first_name":"Rafael A."},{"full_name":"Amard, Louis","last_name":"Amard","first_name":"Louis"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"first_name":"Enrico","last_name":"Corsaro","full_name":"Corsaro, Enrico"},{"first_name":"Alfio","last_name":"Bonanno","full_name":"Bonanno, Alfio"},{"last_name":"Breton","full_name":"Breton, Sylvain N.","first_name":"Sylvain N."},{"first_name":"Diego","last_name":"Godoy-Rivera","full_name":"Godoy-Rivera, Diego"},{"first_name":"Marc H.","last_name":"Pinsonneault","full_name":"Pinsonneault, Marc H."},{"last_name":"van Saders","full_name":"van Saders, Jennifer","first_name":"Jennifer"}],"oa_version":"Published Version","title":"Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations","file_date_updated":"2023-08-02T07:42:26Z","publication_status":"published","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"has_accepted_license":"1","abstract":[{"lang":"eng","text":"The ages of solar-like stars have been at the center of many studies such as exoplanet characterization or Galactic-archeology. While ages are usually computed from stellar evolution models, relations linking ages to other stellar properties, such as rotation and magnetic activity, have been investigated. With the large catalog of 55,232 rotation periods, Prot, and photometric magnetic activity index, Sph from Kepler data, we have the opportunity to look for such magneto-gyro-chronology relations. Stellar ages are obtained with two stellar evolution codes that include treatment of angular momentum evolution, hence using Prot as input in addition to classical atmospheric parameters. We explore two different ways of predicting stellar ages on three subsamples with spectroscopic observations: solar analogs, late-F and G dwarfs, and K dwarfs. We first perform a Bayesian analysis to derive relations between Sph and ages between 1 and 5 Gyr, and other stellar properties. For late-F and G dwarfs, and K dwarfs, the multivariate regression favors the model with Prot and Sph with median differences of 0.1% and 0.2%, respectively. We also apply Machine Learning techniques with a Random Forest algorithm to predict ages up to 14 Gyr with the same set of input parameters. For late-F, G and K dwarfs together, predicted ages are on average within 5.3% of the model ages and improve to 3.1% when including Prot. These are very promising results for a quick age estimation for solar-like stars with photometric observations, especially with current and future space missions."}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","short":"CC BY (4.0)"},"intvolume":"       952","department":[{"_id":"LiBu"}],"article_number":"131","file":[{"success":1,"file_name":"2023_AstrophysicalJour_Mathur.pdf","access_level":"open_access","content_type":"application/pdf","relation":"main_file","checksum":"f12452834d7ed6748dbf5ace18af4723","date_created":"2023-08-02T07:42:26Z","file_size":4192386,"creator":"dernst","date_updated":"2023-08-02T07:42:26Z","file_id":"13448"}],"month":"08","citation":{"apa":"Mathur, S., Claytor, Z. R., Santos, Â. R. G., García, R. A., Amard, L., Bugnet, L. A., … van Saders, J. (2023). Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/acd118\">https://doi.org/10.3847/1538-4357/acd118</a>","mla":"Mathur, Savita, et al. “Magnetic Activity Evolution of Solar-like Stars. I. Sph–Age Relation Derived from Kepler Observations.” <i>The Astrophysical Journal</i>, vol. 952, no. 2, 131, American Astronomical Society, 2023, doi:<a href=\"https://doi.org/10.3847/1538-4357/acd118\">10.3847/1538-4357/acd118</a>.","chicago":"Mathur, Savita, Zachary R. Claytor, Ângela R. G. Santos, Rafael A. García, Louis Amard, Lisa Annabelle Bugnet, Enrico Corsaro, et al. “Magnetic Activity Evolution of Solar-like Stars. I. Sph–Age Relation Derived from Kepler Observations.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2023. <a href=\"https://doi.org/10.3847/1538-4357/acd118\">https://doi.org/10.3847/1538-4357/acd118</a>.","ista":"Mathur S, Claytor ZR, Santos ÂRG, García RA, Amard L, Bugnet LA, Corsaro E, Bonanno A, Breton SN, Godoy-Rivera D, Pinsonneault MH, van Saders J. 2023. Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. The Astrophysical Journal. 952(2), 131.","ieee":"S. Mathur <i>et al.</i>, “Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations,” <i>The Astrophysical Journal</i>, vol. 952, no. 2. American Astronomical Society, 2023.","short":"S. Mathur, Z.R. Claytor, Â.R.G. Santos, R.A. García, L. Amard, L.A. Bugnet, E. Corsaro, A. Bonanno, S.N. Breton, D. Godoy-Rivera, M.H. Pinsonneault, J. van Saders, The Astrophysical Journal 952 (2023).","ama":"Mathur S, Claytor ZR, Santos ÂRG, et al. Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. <i>The Astrophysical Journal</i>. 2023;952(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/acd118\">10.3847/1538-4357/acd118</a>"},"issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"_id":"13443","date_updated":"2023-12-13T12:00:15Z","type":"journal_article","article_processing_charge":"Yes","doi":"10.3847/1538-4357/acd118","publisher":"American Astronomical Society","quality_controlled":"1","ddc":["520"],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"isi":1,"year":"2023","external_id":{"isi":["001034185700001"]},"date_published":"2023-08-01T00:00:00Z","acknowledgement":"This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. We acknowledge that this research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958. S.M. acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship No. RYC-2015-17697, the grant No. PID2019-107061GB-C66, and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.M. and D.G.R. acknowledge support from the Spanish Ministry of Science and Innovation (MICINN) with the grant No. PID2019-107187GB-I00. Z.R.C. acknowledges support from National Aeronautics and Space Administration via the TESS Guest Investigator Program (grant No. 80NSSC18K18584). The work presented here was partially supported by the NASA grant NNX17AF27G. A.R.G.S. acknowledges the support by FCT through national funds and by FEDER through COMPETE2020 by the following grants: UIDB/04434/2020 and UIDP/04434/2020. A.R.G.S. is supported by FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001. R.A.G., L.A., and S.N.B. acknowledge the support from PLATO and GOLF CNES grants. S.N.B. acknowledges support from PLATO ASI-INAF agreement No. 2015-019-R.1-2018.","status":"public","publication":"The Astrophysical Journal"},{"_id":"13449","date_updated":"2023-08-21T12:09:14Z","type":"journal_article","article_processing_charge":"No","doi":"10.1088/1538-3873/acb6b5","publisher":"IOP Publishing","main_file_link":[{"url":"https://doi.org/10.1088/1538-3873/acb6b5","open_access":"1"}],"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2023","external_id":{"arxiv":["2301.13611"]},"date_published":"2023-03-09T00:00:00Z","publication":"Publications of the Astronomical Society of the Pacific","extern":"1","status":"public","volume":135,"date_created":"2023-08-03T10:09:57Z","article_type":"original","day":"09","scopus_import":"1","author":[{"last_name":"Geen","full_name":"Geen, Sam","first_name":"Sam"},{"full_name":"Agrawal, Poojan","last_name":"Agrawal","first_name":"Poojan"},{"full_name":"Crowther, Paul A.","last_name":"Crowther","first_name":"Paul A."},{"full_name":"Keller, B. W.","last_name":"Keller","first_name":"B. W."},{"full_name":"de Koter, Alex","last_name":"de Koter","first_name":"Alex"},{"first_name":"Zsolt","last_name":"Keszthelyi","full_name":"Keszthelyi, Zsolt"},{"first_name":"Freeke","full_name":"van de Voort, Freeke","last_name":"van de Voort"},{"first_name":"Ahmad A.","full_name":"Ali, Ahmad A.","last_name":"Ali"},{"last_name":"Backs","full_name":"Backs, Frank","first_name":"Frank"},{"first_name":"Lars","last_name":"Bonne","full_name":"Bonne, Lars"},{"first_name":"Vittoria","full_name":"Brugaletta, Vittoria","last_name":"Brugaletta"},{"full_name":"Derkink, Annelotte","last_name":"Derkink","first_name":"Annelotte"},{"full_name":"Ekström, Sylvia","last_name":"Ekström","first_name":"Sylvia"},{"last_name":"Fichtner","full_name":"Fichtner, Yvonne A.","first_name":"Yvonne A."},{"last_name":"Grassitelli","full_name":"Grassitelli, Luca","first_name":"Luca"},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"first_name":"Erin R.","last_name":"Higgins","full_name":"Higgins, Erin R."},{"first_name":"Eva","last_name":"Laplace","full_name":"Laplace, Eva"},{"last_name":"You Liow","full_name":"You Liow, Kong","first_name":"Kong"},{"first_name":"Marta","last_name":"Lorenzo","full_name":"Lorenzo, Marta"},{"full_name":"McLeod, Anna F.","last_name":"McLeod","first_name":"Anna F."},{"first_name":"Georges","full_name":"Meynet, Georges","last_name":"Meynet"},{"full_name":"Newsome, Megan","last_name":"Newsome","first_name":"Megan"},{"first_name":"G.","last_name":"André Oliva","full_name":"André Oliva, G."},{"first_name":"Varsha","last_name":"Ramachandran","full_name":"Ramachandran, Varsha"},{"full_name":"Rey, Martin P.","last_name":"Rey","first_name":"Martin P."},{"first_name":"Steven","last_name":"Rieder","full_name":"Rieder, Steven"},{"full_name":"Romano-Díaz, Emilio","last_name":"Romano-Díaz","first_name":"Emilio"},{"first_name":"Gautham","full_name":"Sabhahit, Gautham","last_name":"Sabhahit"},{"first_name":"Andreas A. C.","last_name":"Sander","full_name":"Sander, Andreas A. C."},{"full_name":"Sarwar, Rafia","last_name":"Sarwar","first_name":"Rafia"},{"last_name":"Stinshoff","full_name":"Stinshoff, Hanno","first_name":"Hanno"},{"first_name":"Mitchel","full_name":"Stoop, Mitchel","last_name":"Stoop"},{"first_name":"Dorottya","full_name":"Szécsi, Dorottya","last_name":"Szécsi"},{"full_name":"Trebitsch, Maxime","last_name":"Trebitsch","first_name":"Maxime"},{"last_name":"Vink","full_name":"Vink, Jorick S.","first_name":"Jorick S."},{"first_name":"Ethan","last_name":"Winch","full_name":"Winch, Ethan"}],"oa_version":"Published Version","title":"Bringing stellar evolution and feedback together: Summary of proposals from the Lorentz Center workshop","publication_status":"published","publication_identifier":{"eissn":["1538-3873"],"issn":["0004-6280"]},"intvolume":"       135","abstract":[{"text":"Stars strongly impact their environment, and shape structures on all scales throughout the universe, in a process known as \"feedback.\" Due to the complexity of both stellar evolution and the physics of larger astrophysical structures, there remain many unanswered questions about how feedback operates and what we can learn about stars by studying their imprint on the wider universe. In this white paper, we summarize discussions from the Lorentz Center meeting \"Bringing Stellar Evolution and Feedback Together\" in 2022 April and identify key areas where further dialog can bring about radical changes in how we view the relationship between stars and the universe they live in.","lang":"eng"}],"article_number":"021001","arxiv":1,"month":"03","citation":{"chicago":"Geen, Sam, Poojan Agrawal, Paul A. Crowther, B. W. Keller, Alex de Koter, Zsolt Keszthelyi, Freeke van de Voort, et al. “Bringing Stellar Evolution and Feedback Together: Summary of Proposals from the Lorentz Center Workshop.” <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing, 2023. <a href=\"https://doi.org/10.1088/1538-3873/acb6b5\">https://doi.org/10.1088/1538-3873/acb6b5</a>.","ista":"Geen S, Agrawal P, Crowther PA, Keller BW, de Koter A, Keszthelyi Z, van de Voort F, Ali AA, Backs F, Bonne L, Brugaletta V, Derkink A, Ekström S, Fichtner YA, Grassitelli L, Götberg YLL, Higgins ER, Laplace E, You Liow K, Lorenzo M, McLeod AF, Meynet G, Newsome M, André Oliva G, Ramachandran V, Rey MP, Rieder S, Romano-Díaz E, Sabhahit G, Sander AAC, Sarwar R, Stinshoff H, Stoop M, Szécsi D, Trebitsch M, Vink JS, Winch E. 2023. Bringing stellar evolution and feedback together: Summary of proposals from the Lorentz Center workshop. Publications of the Astronomical Society of the Pacific. 135(1044), 021001.","apa":"Geen, S., Agrawal, P., Crowther, P. A., Keller, B. W., de Koter, A., Keszthelyi, Z., … Winch, E. (2023). Bringing stellar evolution and feedback together: Summary of proposals from the Lorentz Center workshop. <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/1538-3873/acb6b5\">https://doi.org/10.1088/1538-3873/acb6b5</a>","mla":"Geen, Sam, et al. “Bringing Stellar Evolution and Feedback Together: Summary of Proposals from the Lorentz Center Workshop.” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 135, no. 1044, 021001, IOP Publishing, 2023, doi:<a href=\"https://doi.org/10.1088/1538-3873/acb6b5\">10.1088/1538-3873/acb6b5</a>.","ama":"Geen S, Agrawal P, Crowther PA, et al. Bringing stellar evolution and feedback together: Summary of proposals from the Lorentz Center workshop. <i>Publications of the Astronomical Society of the Pacific</i>. 2023;135(1044). doi:<a href=\"https://doi.org/10.1088/1538-3873/acb6b5\">10.1088/1538-3873/acb6b5</a>","ieee":"S. Geen <i>et al.</i>, “Bringing stellar evolution and feedback together: Summary of proposals from the Lorentz Center workshop,” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 135, no. 1044. IOP Publishing, 2023.","short":"S. Geen, P. Agrawal, P.A. Crowther, B.W. Keller, A. de Koter, Z. Keszthelyi, F. van de Voort, A.A. Ali, F. Backs, L. Bonne, V. Brugaletta, A. Derkink, S. Ekström, Y.A. Fichtner, L. Grassitelli, Y.L.L. Götberg, E.R. Higgins, E. Laplace, K. You Liow, M. Lorenzo, A.F. McLeod, G. Meynet, M. Newsome, G. André Oliva, V. Ramachandran, M.P. Rey, S. Rieder, E. Romano-Díaz, G. Sabhahit, A.A.C. Sander, R. Sarwar, H. Stinshoff, M. Stoop, D. Szécsi, M. Trebitsch, J.S. Vink, E. Winch, Publications of the Astronomical Society of the Pacific 135 (2023)."},"issue":"1044","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}]},{"publisher":"American Astronomical Society","doi":"10.3847/1538-4357/aca655","article_processing_charge":"No","type":"journal_article","date_updated":"2023-08-21T12:07:05Z","_id":"13450","quality_controlled":"1","main_file_link":[{"url":"https://doi.org/10.3847/1538-4357/aca655","open_access":"1"}],"external_id":{"arxiv":["2211.12438"]},"year":"2023","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","publication":"The Astrophysical Journal","extern":"1","date_published":"2023-01-20T00:00:00Z","oa_version":"Published Version","title":"Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow object and super-AGB star candidates","author":[{"first_name":"Anna J. G.","last_name":"O‘Grady","full_name":"O‘Grady, Anna J. G."},{"first_name":"Maria R.","last_name":"Drout","full_name":"Drout, Maria R."},{"last_name":"Gaensler","full_name":"Gaensler, B. M.","first_name":"B. M."},{"full_name":"Kochanek, C. S.","last_name":"Kochanek","first_name":"C. S."},{"first_name":"Kathryn F.","full_name":"Neugent, Kathryn F.","last_name":"Neugent"},{"full_name":"Doherty, Carolyn L.","last_name":"Doherty","first_name":"Carolyn L."},{"first_name":"Joshua S.","full_name":"Speagle, Joshua S.","last_name":"Speagle"},{"first_name":"B. J.","full_name":"Shappee, B. J.","last_name":"Shappee"},{"first_name":"Michael","last_name":"Rauch","full_name":"Rauch, Michael"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"full_name":"Ludwig, Bethany","last_name":"Ludwig","first_name":"Bethany"},{"first_name":"Todd A.","full_name":"Thompson, Todd A.","last_name":"Thompson"}],"scopus_import":"1","day":"20","article_type":"original","date_created":"2023-08-03T10:10:12Z","volume":943,"abstract":[{"text":"In previous work, we identified a population of 38 cool and luminous variable stars in the Magellanic Clouds and examined 11 in detail in order to classify them as either Thorne–Żytkow objects (TŻOs; red supergiants with a neutron star cores) or super-asymptotic giant branch (sAGB) stars (the most massive stars that will not undergo core collapse). This population includes HV 2112, a peculiar star previously considered in other works to be either a TŻO or high-mass asymptotic giant branch (AGB) star. Here we continue this investigation, using the kinematic and radio environments and local star formation history of these stars to place constraints on the age of the progenitor systems and the presence of past supernovae. These stars are not associated with regions of recent star formation, and we find no evidence of past supernovae at their locations. Finally, we also assess the presence of heavy elements and lithium in their spectra compared to red supergiants. We find strong absorption in Li and s-process elements compared to RSGs in most of the sample, consistent with sAGB nucleosynthesis, while HV 2112 shows additional strong lines associated with TŻO nucleosynthesis. Coupled with our previous mass estimates, the results are consistent with the stars being massive (∼4–6.5 M⊙) or sAGB (∼6.5–12 M⊙) stars in the thermally pulsing phase, providing crucial observations of the transition between low- and high-mass stellar populations. HV 2112 is more ambiguous; it could either be a maximally massive sAGB star, or a TŻO if the minimum mass for stability extends down to ≲13 M⊙.","lang":"eng"}],"intvolume":"       943","publication_status":"published","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"arxiv":1,"month":"01","article_number":"18","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","citation":{"mla":"O‘Grady, Anna J. G., et al. “Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II. Spectroscopic and Environmental Analysis of Thorne–Żytkow Object and Super-AGB Star Candidates.” <i>The Astrophysical Journal</i>, vol. 943, no. 1, 18, American Astronomical Society, 2023, doi:<a href=\"https://doi.org/10.3847/1538-4357/aca655\">10.3847/1538-4357/aca655</a>.","apa":"O‘Grady, A. J. G., Drout, M. R., Gaensler, B. M., Kochanek, C. S., Neugent, K. F., Doherty, C. L., … Thompson, T. A. (2023). Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow object and super-AGB star candidates. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/aca655\">https://doi.org/10.3847/1538-4357/aca655</a>","ista":"O‘Grady AJG, Drout MR, Gaensler BM, Kochanek CS, Neugent KF, Doherty CL, Speagle JS, Shappee BJ, Rauch M, Götberg YLL, Ludwig B, Thompson TA. 2023. Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow object and super-AGB star candidates. The Astrophysical Journal. 943(1), 18.","chicago":"O‘Grady, Anna J. G., Maria R. Drout, B. M. Gaensler, C. S. Kochanek, Kathryn F. Neugent, Carolyn L. Doherty, Joshua S. Speagle, et al. “Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II. Spectroscopic and Environmental Analysis of Thorne–Żytkow Object and Super-AGB Star Candidates.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2023. <a href=\"https://doi.org/10.3847/1538-4357/aca655\">https://doi.org/10.3847/1538-4357/aca655</a>.","short":"A.J.G. O‘Grady, M.R. Drout, B.M. Gaensler, C.S. Kochanek, K.F. Neugent, C.L. Doherty, J.S. Speagle, B.J. Shappee, M. Rauch, Y.L.L. Götberg, B. Ludwig, T.A. Thompson, The Astrophysical Journal 943 (2023).","ieee":"A. J. G. O‘Grady <i>et al.</i>, “Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow object and super-AGB star candidates,” <i>The Astrophysical Journal</i>, vol. 943, no. 1. American Astronomical Society, 2023.","ama":"O‘Grady AJG, Drout MR, Gaensler BM, et al. Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow object and super-AGB star candidates. <i>The Astrophysical Journal</i>. 2023;943(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/aca655\">10.3847/1538-4357/aca655</a>"}},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"external_id":{"arxiv":["2305.06376"]},"year":"2023","date_published":"2023-07-01T00:00:00Z","publication":"Astronomy & Astrophysics","extern":"1","status":"public","type":"journal_article","_id":"14103","date_updated":"2023-08-22T11:01:07Z","publisher":"EDP Sciences","article_processing_charge":"No","doi":"10.1051/0004-6361/202245650","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/202245650"}],"article_number":"A154","arxiv":1,"month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"J.S. Vink, A. Mehner, P.A. Crowther, A. Fullerton, M. Garcia, F. Martins, N. Morrell, L.M. Oskinova, N. St-Louis, A. ud-Doula, A.A.C. Sander, H. Sana, J.-C. Bouret, B. Kubátová, P. Marchant, L.P. Martins, A. Wofford, J.T. van Loon, O. Grace Telford, Y.L.L. Götberg, D.M. Bowman, C. Erba, V.M. Kalari, M. Abdul-Masih, T. Alkousa, F. Backs, C.L. Barbosa, S.R. Berlanas, M. Bernini-Peron, J.M. Bestenlehner, R. Blomme, J. Bodensteiner, S.A. Brands, C.J. Evans, A. David-Uraz, F.A. Driessen, K. Dsilva, S. Geen, V.M.A. Gómez-González, L. Grassitelli, W.-R. Hamann, C. Hawcroft, A. Herrero, E.R. Higgins, D. John Hillier, R. Ignace, A.G. Istrate, L. Kaper, N.D. Kee, C. Kehrig, Z. Keszthelyi, J. Klencki, A. de Koter, R. Kuiper, E. Laplace, C.J.K. Larkin, R.R. Lefever, C. Leitherer, D.J. Lennon, L. Mahy, J. Maíz Apellániz, G. Maravelias, W. Marcolino, A.F. McLeod, S.E. de Mink, F. Najarro, M.S. Oey, T.N. Parsons, D. Pauli, M.G. Pedersen, R.K. Prinja, V. Ramachandran, M.C. Ramírez-Tannus, G.N. Sabhahit, A. Schootemeijer, S. Reyero Serantes, T. Shenar, G.S. Stringfellow, N. Sudnik, F. Tramper, L. Wang, Astronomy &#38; Astrophysics 675 (2023).","ieee":"J. S. Vink <i>et al.</i>, “X-shooting ULLYSES: Massive stars at low metallicity. I. Project description,” <i>Astronomy &#38; Astrophysics</i>, vol. 675. EDP Sciences, 2023.","ama":"Vink JS, Mehner A, Crowther PA, et al. X-shooting ULLYSES: Massive stars at low metallicity. I. Project description. <i>Astronomy &#38; Astrophysics</i>. 2023;675. doi:<a href=\"https://doi.org/10.1051/0004-6361/202245650\">10.1051/0004-6361/202245650</a>","mla":"Vink, Jorick S., et al. “X-Shooting ULLYSES: Massive Stars at Low Metallicity. I. Project Description.” <i>Astronomy &#38; Astrophysics</i>, vol. 675, A154, EDP Sciences, 2023, doi:<a href=\"https://doi.org/10.1051/0004-6361/202245650\">10.1051/0004-6361/202245650</a>.","apa":"Vink, J. S., Mehner, A., Crowther, P. A., Fullerton, A., Garcia, M., Martins, F., … Wang, L. (2023). X-shooting ULLYSES: Massive stars at low metallicity. I. Project description. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202245650\">https://doi.org/10.1051/0004-6361/202245650</a>","ista":"Vink JS, Mehner A, Crowther PA, Fullerton A, Garcia M, Martins F, Morrell N, Oskinova LM, St-Louis N, ud-Doula A, Sander AAC, Sana H, Bouret J-C, Kubátová B, Marchant P, Martins LP, Wofford A, van Loon JT, Grace Telford O, Götberg YLL, Bowman DM, Erba C, Kalari VM, Abdul-Masih M, Alkousa T, Backs F, Barbosa CL, Berlanas SR, Bernini-Peron M, Bestenlehner JM, Blomme R, Bodensteiner J, Brands SA, Evans CJ, David-Uraz A, Driessen FA, Dsilva K, Geen S, Gómez-González VMA, Grassitelli L, Hamann W-R, Hawcroft C, Herrero A, Higgins ER, John Hillier D, Ignace R, Istrate AG, Kaper L, Kee ND, Kehrig C, Keszthelyi Z, Klencki J, de Koter A, Kuiper R, Laplace E, Larkin CJK, Lefever RR, Leitherer C, Lennon DJ, Mahy L, Maíz Apellániz J, Maravelias G, Marcolino W, McLeod AF, de Mink SE, Najarro F, Oey MS, Parsons TN, Pauli D, Pedersen MG, Prinja RK, Ramachandran V, Ramírez-Tannus MC, Sabhahit GN, Schootemeijer A, Reyero Serantes S, Shenar T, Stringfellow GS, Sudnik N, Tramper F, Wang L. 2023. X-shooting ULLYSES: Massive stars at low metallicity. I. Project description. Astronomy &#38; Astrophysics. 675, A154.","chicago":"Vink, Jorick S., A. Mehner, P. A. Crowther, A. Fullerton, M. Garcia, F. Martins, N. Morrell, et al. “X-Shooting ULLYSES: Massive Stars at Low Metallicity. I. Project Description.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2023. <a href=\"https://doi.org/10.1051/0004-6361/202245650\">https://doi.org/10.1051/0004-6361/202245650</a>."},"language":[{"iso":"eng"}],"oa":1,"date_created":"2023-08-21T10:12:35Z","article_type":"original","volume":675,"oa_version":"Published Version","title":"X-shooting ULLYSES: Massive stars at low metallicity. I. Project description","scopus_import":"1","day":"01","author":[{"first_name":"Jorick S.","last_name":"Vink","full_name":"Vink, Jorick S."},{"full_name":"Mehner, A.","last_name":"Mehner","first_name":"A."},{"full_name":"Crowther, P. A.","last_name":"Crowther","first_name":"P. A."},{"last_name":"Fullerton","full_name":"Fullerton, A.","first_name":"A."},{"first_name":"M.","full_name":"Garcia, M.","last_name":"Garcia"},{"first_name":"F.","last_name":"Martins","full_name":"Martins, F."},{"last_name":"Morrell","full_name":"Morrell, N.","first_name":"N."},{"first_name":"L. M.","full_name":"Oskinova, L. M.","last_name":"Oskinova"},{"last_name":"St-Louis","full_name":"St-Louis, N.","first_name":"N."},{"last_name":"ud-Doula","full_name":"ud-Doula, A.","first_name":"A."},{"last_name":"Sander","full_name":"Sander, A. A. C.","first_name":"A. A. C."},{"full_name":"Sana, H.","last_name":"Sana","first_name":"H."},{"first_name":"J.-C.","last_name":"Bouret","full_name":"Bouret, J.-C."},{"first_name":"B.","full_name":"Kubátová, B.","last_name":"Kubátová"},{"full_name":"Marchant, P.","last_name":"Marchant","first_name":"P."},{"last_name":"Martins","full_name":"Martins, L. P.","first_name":"L. P."},{"last_name":"Wofford","full_name":"Wofford, A.","first_name":"A."},{"last_name":"van Loon","full_name":"van Loon, J. Th.","first_name":"J. Th."},{"first_name":"O.","last_name":"Grace Telford","full_name":"Grace Telford, O."},{"first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"first_name":"D. M.","last_name":"Bowman","full_name":"Bowman, D. M."},{"last_name":"Erba","full_name":"Erba, C.","first_name":"C."},{"last_name":"Kalari","full_name":"Kalari, V. M.","first_name":"V. M."},{"first_name":"M.","full_name":"Abdul-Masih, M.","last_name":"Abdul-Masih"},{"full_name":"Alkousa, T.","last_name":"Alkousa","first_name":"T."},{"first_name":"F.","full_name":"Backs, F.","last_name":"Backs"},{"first_name":"C. L.","last_name":"Barbosa","full_name":"Barbosa, C. L."},{"full_name":"Berlanas, S. R.","last_name":"Berlanas","first_name":"S. R."},{"first_name":"M.","last_name":"Bernini-Peron","full_name":"Bernini-Peron, M."},{"last_name":"Bestenlehner","full_name":"Bestenlehner, J. M.","first_name":"J. M."},{"first_name":"R.","last_name":"Blomme","full_name":"Blomme, R."},{"first_name":"J.","last_name":"Bodensteiner","full_name":"Bodensteiner, J."},{"full_name":"Brands, S. A.","last_name":"Brands","first_name":"S. A."},{"first_name":"C. J.","last_name":"Evans","full_name":"Evans, C. J."},{"full_name":"David-Uraz, A.","last_name":"David-Uraz","first_name":"A."},{"first_name":"F. A.","last_name":"Driessen","full_name":"Driessen, F. A."},{"last_name":"Dsilva","full_name":"Dsilva, K.","first_name":"K."},{"first_name":"S.","full_name":"Geen, S.","last_name":"Geen"},{"full_name":"Gómez-González, V. M. A.","last_name":"Gómez-González","first_name":"V. M. A."},{"full_name":"Grassitelli, L.","last_name":"Grassitelli","first_name":"L."},{"first_name":"W.-R.","full_name":"Hamann, W.-R.","last_name":"Hamann"},{"full_name":"Hawcroft, C.","last_name":"Hawcroft","first_name":"C."},{"first_name":"A.","last_name":"Herrero","full_name":"Herrero, A."},{"last_name":"Higgins","full_name":"Higgins, E. R.","first_name":"E. R."},{"last_name":"John Hillier","full_name":"John Hillier, D.","first_name":"D."},{"full_name":"Ignace, R.","last_name":"Ignace","first_name":"R."},{"first_name":"A. G.","last_name":"Istrate","full_name":"Istrate, A. G."},{"last_name":"Kaper","full_name":"Kaper, L.","first_name":"L."},{"full_name":"Kee, N. D.","last_name":"Kee","first_name":"N. D."},{"last_name":"Kehrig","full_name":"Kehrig, C.","first_name":"C."},{"full_name":"Keszthelyi, Z.","last_name":"Keszthelyi","first_name":"Z."},{"first_name":"J.","full_name":"Klencki, J.","last_name":"Klencki"},{"full_name":"de Koter, A.","last_name":"de Koter","first_name":"A."},{"first_name":"R.","full_name":"Kuiper, R.","last_name":"Kuiper"},{"full_name":"Laplace, E.","last_name":"Laplace","first_name":"E."},{"last_name":"Larkin","full_name":"Larkin, C. J. K.","first_name":"C. J. K."},{"full_name":"Lefever, R. R.","last_name":"Lefever","first_name":"R. R."},{"first_name":"C.","full_name":"Leitherer, C.","last_name":"Leitherer"},{"last_name":"Lennon","full_name":"Lennon, D. J.","first_name":"D. J."},{"full_name":"Mahy, L.","last_name":"Mahy","first_name":"L."},{"first_name":"J.","full_name":"Maíz Apellániz, J.","last_name":"Maíz Apellániz"},{"full_name":"Maravelias, G.","last_name":"Maravelias","first_name":"G."},{"first_name":"W.","full_name":"Marcolino, W.","last_name":"Marcolino"},{"last_name":"McLeod","full_name":"McLeod, A. F.","first_name":"A. F."},{"first_name":"S. E.","full_name":"de Mink, S. E.","last_name":"de Mink"},{"first_name":"F.","last_name":"Najarro","full_name":"Najarro, F."},{"full_name":"Oey, M. S.","last_name":"Oey","first_name":"M. S."},{"first_name":"T. N.","full_name":"Parsons, T. N.","last_name":"Parsons"},{"first_name":"D.","last_name":"Pauli","full_name":"Pauli, D."},{"first_name":"M. G.","last_name":"Pedersen","full_name":"Pedersen, M. G."},{"first_name":"R. K.","full_name":"Prinja, R. K.","last_name":"Prinja"},{"last_name":"Ramachandran","full_name":"Ramachandran, V.","first_name":"V."},{"full_name":"Ramírez-Tannus, M. C.","last_name":"Ramírez-Tannus","first_name":"M. C."},{"full_name":"Sabhahit, G. N.","last_name":"Sabhahit","first_name":"G. N."},{"full_name":"Schootemeijer, A.","last_name":"Schootemeijer","first_name":"A."},{"last_name":"Reyero Serantes","full_name":"Reyero Serantes, S.","first_name":"S."},{"full_name":"Shenar, T.","last_name":"Shenar","first_name":"T."},{"last_name":"Stringfellow","full_name":"Stringfellow, G. S.","first_name":"G. S."},{"full_name":"Sudnik, N.","last_name":"Sudnik","first_name":"N."},{"full_name":"Tramper, F.","last_name":"Tramper","first_name":"F."},{"last_name":"Wang","full_name":"Wang, L.","first_name":"L."}],"publication_status":"published","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"intvolume":"       675","abstract":[{"text":"Observations of individual massive stars, super-luminous supernovae, gamma-ray bursts, and gravitational wave events involving spectacular black hole mergers indicate that the low-metallicity Universe is fundamentally different from our own Galaxy. Many transient phenomena will remain enigmatic until we achieve a firm understanding of the physics and evolution of massive stars at low metallicity (Z). The Hubble Space Telescope has devoted 500 orbits to observing ∼250 massive stars at low Z in the ultraviolet (UV) with the COS and STIS spectrographs under the ULLYSES programme. The complementary X-Shooting ULLYSES (XShootU) project provides an enhanced legacy value with high-quality optical and near-infrared spectra obtained with the wide-wavelength coverage X-shooter spectrograph at ESO’s Very Large Telescope. We present an overview of the XShootU project, showing that combining ULLYSES UV and XShootU optical spectra is critical for the uniform determination of stellar parameters such as effective temperature, surface gravity, luminosity, and abundances, as well as wind properties such as mass-loss rates as a function of Z. As uncertainties in stellar and wind parameters percolate into many adjacent areas of astrophysics, the data and modelling of the XShootU project is expected to be a game changer for our physical understanding of massive stars at low Z. To be able to confidently interpret James Webb Space Telescope spectra of the first stellar generations, the individual spectra of low-Z stars need to be understood, which is exactly where XShootU can deliver.","lang":"eng"}]},{"page":"1692-1709","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2305.07337"}],"quality_controlled":"1","doi":"10.1093/mnras/stad1977","article_processing_charge":"No","publisher":"Oxford University Press","date_updated":"2023-08-21T12:12:48Z","_id":"14104","type":"journal_article","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","date_published":"2023-09-01T00:00:00Z","year":"2023","external_id":{"arxiv":["2305.07337"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       524","abstract":[{"text":"Thorne–Żytkow objects (TŻO) are potential end products of the merger of a neutron star with a non-degenerate star. In this work, we have computed the first grid of evolutionary models of TŻOs with the MESA stellar evolution code. With these models, we predict several observational properties of TŻOs, including their surface temperatures and luminosities, pulsation periods, and nucleosynthetic products. We expand the range of possible TŻO solutions to cover 3.45≲log(Teff/K)≲3.65 and 4.85≲log(L/L⊙)≲5.5⁠. Due to the much higher densities our TŻOs reach compared to previous models, if TŻOs form we expect them to be stable over a larger mass range than previously predicted, without exhibiting a gap in their mass distribution. Using the GYRE stellar pulsation code we show that TŻOs should have fundamental pulsation periods of 1000–2000 d, and period ratios of ≈0.2–0.3. Models computed with a large 399 isotope fully coupled nuclear network show a nucleosynthetic signal that is different to previously predicted. We propose a new nucleosynthetic signal to determine a star’s status as a TŻO: the isotopologues 44TiO2 and 44TiO⁠, which will have a shift in their spectral features as compared to stable titanium-containing molecules. We find that in the local Universe (∼SMC metallicities and above) TŻOs show little heavy metal enrichment, potentially explaining the difficulty in finding TŻOs to-date.","lang":"eng"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","author":[{"first_name":"R","full_name":"Farmer, R","last_name":"Farmer"},{"full_name":"Renzo, M","last_name":"Renzo","first_name":"M"},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"last_name":"Bellinger","full_name":"Bellinger, E","first_name":"E"},{"first_name":"S","full_name":"Justham, S","last_name":"Justham"},{"first_name":"S E","last_name":"de Mink","full_name":"de Mink, S E"}],"scopus_import":"1","day":"01","title":"Observational predictions for Thorne–Żytkow objects","oa_version":"Preprint","volume":524,"article_type":"original","date_created":"2023-08-21T10:13:56Z","oa":1,"language":[{"iso":"eng"}],"issue":"2","citation":{"short":"R. Farmer, M. Renzo, Y.L.L. Götberg, E. Bellinger, S. Justham, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 524 (2023) 1692–1709.","ieee":"R. Farmer, M. Renzo, Y. L. L. Götberg, E. Bellinger, S. Justham, and S. E. de Mink, “Observational predictions for Thorne–Żytkow objects,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2. Oxford University Press, pp. 1692–1709, 2023.","ama":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;524(2):1692-1709. doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>","mla":"Farmer, R., et al. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2, Oxford University Press, 2023, pp. 1692–709, doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>.","apa":"Farmer, R., Renzo, M., Götberg, Y. L. L., Bellinger, E., Justham, S., &#38; de Mink, S. E. (2023). Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>","chicago":"Farmer, R, M Renzo, Ylva Louise Linsdotter Götberg, E Bellinger, S Justham, and S E de Mink. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>.","ista":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. 2023. Observational predictions for Thorne–Żytkow objects. Monthly Notices of the Royal Astronomical Society. 524(2), 1692–1709."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"month":"09"},{"year":"2022","external_id":{"arxiv":["2201.07257"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"publication":"Astronomy & Astrophysics","status":"public","extern":"1","date_published":"2022-04-07T00:00:00Z","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard, Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges support from Swiss Government Excellence Scholarships and Japan Society for the Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC Starting Grant 757258“TRIPLE”. This work was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy, which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), and other software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).","article_processing_charge":"No","doi":"10.1051/0004-6361/202142302","publisher":"EDP Sciences","_id":"11488","date_updated":"2022-07-19T09:33:24Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/2201.07257","open_access":"1"}],"quality_controlled":"1","month":"04","arxiv":1,"article_number":"A44","oa":1,"language":[{"iso":"eng"}],"citation":{"ista":"Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. Astronomy &#38; Astrophysics. 660, A44.","chicago":"Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field: Individual Detections of Ly<i>α</i> Haloes around Rest-Frame UV-Selected Galaxies at <i>z</i> ≃ 2.9–4.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142302\">https://doi.org/10.1051/0004-6361/202142302</a>.","mla":"Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections of Ly<i>α</i> Haloes around Rest-Frame UV-Selected Galaxies at <i>z</i> ≃ 2.9–4.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 660, A44, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142302\">10.1051/0004-6361/202142302</a>.","apa":"Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq, F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142302\">https://doi.org/10.1051/0004-6361/202142302</a>","ama":"Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. <i>Astronomy &#38; Astrophysics</i>. 2022;660. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142302\">10.1051/0004-6361/202142302</a>","short":"H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq, R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara, R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy &#38; Astrophysics 660 (2022).","ieee":"H. Kusakabe <i>et al.</i>, “The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 660. EDP Sciences, 2022."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","day":"07","author":[{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"last_name":"Blaizot","full_name":"Blaizot, Jérémy","first_name":"Jérémy"},{"last_name":"Garel","full_name":"Garel, Thibault","first_name":"Thibault"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"full_name":"Gallego, Sofia G.","last_name":"Gallego","first_name":"Sofia G."},{"first_name":"Josephine","last_name":"Kerutt","full_name":"Kerutt, Josephine"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"full_name":"Pelló, Roser","last_name":"Pelló","first_name":"Roser"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"last_name":"Tresse","full_name":"Tresse, Laurence","first_name":"Laurence"},{"first_name":"Tanya","last_name":"Urrutia","full_name":"Urrutia, Tanya"},{"full_name":"Vitte, Eloïse","last_name":"Vitte","first_name":"Eloïse"}],"oa_version":"Published Version","title":"The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4","volume":660,"date_created":"2022-07-05T14:27:26Z","article_type":"original","intvolume":"       660","abstract":[{"lang":"eng","text":"Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic medium (CGM) at high redshifts. In this work, we aim to explore the existence of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters (LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5, and spectroscopic redshifts were assigned or constrained for all the sources thanks to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes 21 galaxies that are purely F775W-magnitude selected within the redshift range z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs and four non-LAHs. We report the first individual detections of extended Lyα emission around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected galaxies generally have a large amount of hydrogen in their CGM. We derived the mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz, is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7. Assuming that Lyα emission and absorption arise in the same gas, this suggests, based on abundance matching, that LAHs trace the same gas as damped Lyα systems (DLAs) and sub-DLAs."}],"publication_status":"published","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"status":"public","extern":"1","publication":"Astronomy & Astrophysics","acknowledgement":"We thank the referee for thoughtful and constructive comments that have improved the quality of this manuscript. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060.","date_published":"2022-03-30T00:00:00Z","year":"2022","external_id":{"arxiv":["2111.14855"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / techniques: spectroscopic / galaxies: stellar content / galaxies: formation"],"main_file_link":[{"url":"https://arxiv.org/abs/2111.14855","open_access":"1"}],"quality_controlled":"1","article_processing_charge":"No","doi":"10.1051/0004-6361/202142187","publisher":"EDP Sciences","_id":"11490","date_updated":"2022-07-19T09:33:46Z","type":"journal_article","oa":1,"language":[{"iso":"eng"}],"citation":{"chicago":"Matthee, Jorryt J, Anna Feltre, Michael Maseda, Themiya Nanayakkara, Leindert Boogaard, Roland Bacon, Anne Verhamme, et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142187\">https://doi.org/10.1051/0004-6361/202142187</a>.","ista":"Matthee JJ, Feltre A, Maseda M, Nanayakkara T, Boogaard L, Bacon R, Verhamme A, Leclercq F, Kusakabe H, Urrutia T, Wisotzki L. 2022. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy &#38; Astrophysics. 660, A10.","apa":"Matthee, J. J., Feltre, A., Maseda, M., Nanayakkara, T., Boogaard, L., Bacon, R., … Wisotzki, L. (2022). Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142187\">https://doi.org/10.1051/0004-6361/202142187</a>","mla":"Matthee, Jorryt J., et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 660, A10, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142187\">10.1051/0004-6361/202142187</a>.","ama":"Matthee JJ, Feltre A, Maseda M, et al. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. <i>Astronomy &#38; Astrophysics</i>. 2022;660. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142187\">10.1051/0004-6361/202142187</a>","ieee":"J. J. Matthee <i>et al.</i>, “Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field,” <i>Astronomy &#38; Astrophysics</i>, vol. 660. EDP Sciences, 2022.","short":"J.J. Matthee, A. Feltre, M. Maseda, T. Nanayakkara, L. Boogaard, R. Bacon, A. Verhamme, F. Leclercq, H. Kusakabe, T. Urrutia, L. Wisotzki, Astronomy &#38; Astrophysics 660 (2022)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"month":"03","article_number":"A10","intvolume":"       660","abstract":[{"lang":"eng","text":"Directly characterising the first generations of stars in distant galaxies is a key quest of observational cosmology. We present a case study of ID53 at z = 4.77, the UV-brightest (but L⋆) star-forming galaxy at z > 3 in the MUSE eXtremely Deep Field with a mass of ≈109 M⊙. In addition to very strong Lyman-α (Lyα) emission, we clearly detect the (stellar) continuum and an N V P Cygni feature, interstellar absorption, fine-structure emission and nebular C IV emission lines in the 140 h spectrum. Continuum emission from two spatially resolved components in Hubble Space Telescope data are blended in the MUSE data, but we show that the nebular C IV emission originates from a subcomponent of the galaxy. The UV spectrum can be fit with recent BPASS stellar population models combined with single-burst or continuous star formation histories (SFHs), a standard initial mass function, and an attenuation law. Models with a young age and low metallicity (log10(age/yr) = 6.5–7.6 and [Z/H] = −2.15 to −1.15) are preferred, but the details depend on the assumed SFH. The intrinsic Hα luminosity of the best-fit models is an order of magnitude higher than the Hα luminosity inferred from Spitzer/IRAC data, which either suggests a high escape fraction of ionising photons, a high relative attenuation of nebular to stellar dust, or a complex SFH. The metallicity appears lower than the metallicity in more massive galaxies at z = 3 − 5, consistent with the scenario according to which younger galaxies have lower metallicities. This chemical immaturity likely facilitates Lyα escape, explaining why the Lyα equivalent width is anti-correlated with stellar metallicity. Finally, we stress that uncertainties in SFHs impose a challenge for future inferences of the stellar metallicity of young galaxies. This highlights the need for joint (spatially resolved) analyses of stellar spectra and photo-ionisation models."}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"publication_status":"published","scopus_import":"1","day":"30","author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Feltre, Anna","last_name":"Feltre","first_name":"Anna"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"first_name":"Leindert","full_name":"Boogaard, Leindert","last_name":"Boogaard"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"},{"first_name":"Floriane","full_name":"Leclercq, Floriane","last_name":"Leclercq"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"first_name":"Tanya","full_name":"Urrutia, Tanya","last_name":"Urrutia"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"}],"title":"Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field","oa_version":"Published Version","volume":660,"date_created":"2022-07-05T15:25:35Z","article_type":"original"},{"article_type":"original","date_created":"2022-07-06T08:17:27Z","volume":659,"oa_version":"Published Version","title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","author":[{"first_name":"J.","full_name":"Kerutt, J.","last_name":"Kerutt"},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"last_name":"Verhamme","full_name":"Verhamme, A.","first_name":"A."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"full_name":"Herenz, E. C.","last_name":"Herenz","first_name":"E. C."},{"first_name":"T.","last_name":"Urrutia","full_name":"Urrutia, T."},{"last_name":"Garel","full_name":"Garel, T.","first_name":"T."},{"last_name":"Hashimoto","full_name":"Hashimoto, T.","first_name":"T."},{"last_name":"Maseda","full_name":"Maseda, M.","first_name":"M."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"H.","full_name":"Kusakabe, H.","last_name":"Kusakabe"},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."},{"last_name":"Richard","full_name":"Richard, J.","first_name":"J."},{"first_name":"B.","last_name":"Guiderdoni","full_name":"Guiderdoni, B."},{"full_name":"Mauerhofer, V.","last_name":"Mauerhofer","first_name":"V."},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"first_name":"E.","full_name":"Vitte, E.","last_name":"Vitte"}],"day":"25","scopus_import":"1","publication_status":"published","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"intvolume":"       659","abstract":[{"lang":"eng","text":"Context. The hydrogen Lyman α line is often the only measurable feature in optical spectra of high-redshift galaxies. Its shape and strength are influenced by radiative transfer processes and the properties of the underlying stellar population. High equivalent widths of several hundred Å are especially hard to explain by models and could point towards unusual stellar populations, for example with low metallicities, young stellar ages, and a top-heavy initial mass function. Other aspects influencing equivalent widths are the morphology of the galaxy and its gas properties.\r\nAims. The aim of this study is to better understand the connection between the Lyman α rest-frame equivalent width (EW0) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths.\r\nMethods. We used integral field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the Galfit software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults. The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16% for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW0. The object with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman α spectral or UV continuum morphological properties.\r\nConclusions. The survey depth has to be taken into account when studying EW0 distributions. We find that in general, high EW0 objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW0 values are equally varied."}],"article_number":"183","arxiv":1,"month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. <i>Astronomy &#38; Astrophysics</i>. 2022;659. doi:<a href=\"https://doi.org/10.1051/0004-6361/202141900\">10.1051/0004-6361/202141900</a>","ieee":"J. Kerutt <i>et al.</i>, “Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep,” <i>Astronomy &#38; Astrophysics</i>, vol. 659. EDP Sciences, 2022.","short":"J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz, T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye, J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy &#38; Astrophysics 659 (2022).","chicago":"Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C. Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202141900\">https://doi.org/10.1051/0004-6361/202141900</a>.","ista":"Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J, Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy &#38; Astrophysics. 659, 183.","apa":"Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz, E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202141900\">https://doi.org/10.1051/0004-6361/202141900</a>","mla":"Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” <i>Astronomy &#38; Astrophysics</i>, vol. 659, 183, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202141900\">10.1051/0004-6361/202141900</a>."},"language":[{"iso":"eng"}],"oa":1,"type":"journal_article","date_updated":"2022-07-19T09:47:16Z","_id":"11497","publisher":"EDP Sciences","doi":"10.1051/0004-6361/202141900","article_processing_charge":"No","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2202.06642"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"external_id":{"arxiv":["2202.06642"]},"year":"2022","date_published":"2022-03-25T00:00:00Z","acknowledgement":"We thank the referee for thoughtful and constructive comments that have improved the quality of this manuscript. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060.","publication":"Astronomy & Astrophysics","status":"public","extern":"1"},{"oa":1,"language":[{"iso":"eng"}],"issue":"2","citation":{"mla":"Isobe, Yuki, et al. “EMPRESS. IV. Extremely Metal-Poor Galaxies Including Very Low-Mass Primordial Systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability Supernovae.” <i>The Astrophysical Journal</i>, vol. 925, no. 2, 111, IOP Publishing, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac3509\">10.3847/1538-4357/ac3509</a>.","apa":"Isobe, Y., Ouchi, M., Suzuki, A., Moriya, T. J., Nakajima, K., Nomoto, K., … Xu, Y. (2022). EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac3509\">https://doi.org/10.3847/1538-4357/ac3509</a>","chicago":"Isobe, Yuki, Masami Ouchi, Akihiro Suzuki, Takashi J. Moriya, Kimihiko Nakajima, Ken’ichi Nomoto, Michael Rauch, et al. “EMPRESS. IV. Extremely Metal-Poor Galaxies Including Very Low-Mass Primordial Systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability Supernovae.” <i>The Astrophysical Journal</i>. IOP Publishing, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac3509\">https://doi.org/10.3847/1538-4357/ac3509</a>.","ista":"Isobe Y, Ouchi M, Suzuki A, Moriya TJ, Nakajima K, Nomoto K, Rauch M, Harikane Y, Kojima T, Ono Y, Fujimoto S, Inoue AK, Kim JH, Komiyama Y, Kusakabe H, Lee C-H, Maseda M, Matthee JJ, Michel-Dansac L, Nagao T, Nanayakkara T, Nishigaki M, Onodera M, Sugahara Y, Xu Y. 2022. EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. The Astrophysical Journal. 925(2), 111.","short":"Y. Isobe, M. Ouchi, A. Suzuki, T.J. Moriya, K. Nakajima, K. Nomoto, M. Rauch, Y. Harikane, T. Kojima, Y. Ono, S. Fujimoto, A.K. Inoue, J.H. Kim, Y. Komiyama, H. Kusakabe, C.-H. Lee, M. Maseda, J.J. Matthee, L. Michel-Dansac, T. Nagao, T. Nanayakkara, M. Nishigaki, M. Onodera, Y. Sugahara, Y. Xu, The Astrophysical Journal 925 (2022).","ieee":"Y. Isobe <i>et al.</i>, “EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae,” <i>The Astrophysical Journal</i>, vol. 925, no. 2. IOP Publishing, 2022.","ama":"Isobe Y, Ouchi M, Suzuki A, et al. EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10<sup>4</sup>-10<sup>5</sup>⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. <i>The Astrophysical Journal</i>. 2022;925(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac3509\">10.3847/1538-4357/ac3509</a>"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"01","arxiv":1,"article_number":"111","intvolume":"       925","abstract":[{"lang":"eng","text":"We present Keck/LRIS follow-up spectroscopy for 13 photometric candidates of extremely metal-poor galaxies (EMPGs) selected by a machine-learning technique applied to the deep (∼26 AB mag) optical and wide-area (∼500 deg2) Subaru imaging data in the EMPRESS survey. Nine out of the 13 candidates are EMPGs with an oxygen abundance (O/H) less than ∼10% solar value (O/H)⊙, and four sources are contaminants of moderately metal-rich galaxies or no emission-line objects. Notably, two out of the nine EMPGs have extremely low stellar masses and oxygen abundances of 5 × 10⁴x–7 × -10⁵ M⊙ and 2%–3% (O/H)⊙, respectively. With a sample of five EMPGs with (Fe/O) measurements, two (three) of which are taken from this study (the literature), we confirm that two EMPGs with the lowest (O/H) ratios of ∼2% (O/H)⊙ show high (Fe/O) ratios of ∼0.1, close to the solar abundance ratio. Comparing galaxy chemical enrichment models, we find that the two EMPGs cannot be explained by a scenario of metal-poor gas accretion/episodic star formation history due to their low (N/O) ratios. We conclude that the two EMPGs can be reproduced by the inclusion of bright hypernovae and/or hypothetical pair-instability supernovae (SNe) preferentially produced in a metal-poor environment. This conclusion implies that primordial galaxies at z ∼ 10 could have a high abundance of Fe that did not originate from Type Ia SNe with delays and that Fe may not serve as a cosmic clock for primordial galaxies."}],"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication_status":"published","author":[{"first_name":"Yuki","full_name":"Isobe, Yuki","last_name":"Isobe"},{"first_name":"Masami","last_name":"Ouchi","full_name":"Ouchi, Masami"},{"full_name":"Suzuki, Akihiro","last_name":"Suzuki","first_name":"Akihiro"},{"first_name":"Takashi J.","full_name":"Moriya, Takashi J.","last_name":"Moriya"},{"last_name":"Nakajima","full_name":"Nakajima, Kimihiko","first_name":"Kimihiko"},{"first_name":"Ken’ichi","full_name":"Nomoto, Ken’ichi","last_name":"Nomoto"},{"full_name":"Rauch, Michael","last_name":"Rauch","first_name":"Michael"},{"first_name":"Yuichi","last_name":"Harikane","full_name":"Harikane, Yuichi"},{"first_name":"Takashi","full_name":"Kojima, Takashi","last_name":"Kojima"},{"last_name":"Ono","full_name":"Ono, Yoshiaki","first_name":"Yoshiaki"},{"full_name":"Fujimoto, Seiji","last_name":"Fujimoto","first_name":"Seiji"},{"first_name":"Akio K.","full_name":"Inoue, Akio K.","last_name":"Inoue"},{"last_name":"Kim","full_name":"Kim, Ji Hoon","first_name":"Ji Hoon"},{"last_name":"Komiyama","full_name":"Komiyama, Yutaka","first_name":"Yutaka"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Lee","full_name":"Lee, Chien-Hsiu","first_name":"Chien-Hsiu"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Michel-Dansac, Leo","last_name":"Michel-Dansac","first_name":"Leo"},{"first_name":"Tohru","full_name":"Nagao, Tohru","last_name":"Nagao"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"first_name":"Moka","full_name":"Nishigaki, Moka","last_name":"Nishigaki"},{"last_name":"Onodera","full_name":"Onodera, Masato","first_name":"Masato"},{"last_name":"Sugahara","full_name":"Sugahara, Yuma","first_name":"Yuma"},{"first_name":"Yi","last_name":"Xu","full_name":"Xu, Yi"}],"day":"31","scopus_import":"1","title":"EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10⁴-10⁵⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae","oa_version":"Published Version","volume":925,"article_type":"original","date_created":"2022-07-06T12:01:48Z","publication":"The Astrophysical Journal","extern":"1","status":"public","acknowledgement":"We thank the referee for the valuable comments. We are also grateful to Koh Takahashi, Nozomu Tominaga, Chiaki Kobayashi, Yutaka Hirai, and Daichi Kashino for having useful discussions. This paper includes data gathered with the 10 m Keck Telescope located at W. M. Keck Observatory, Hawaii. We thank the staff of Keck Observatory for their help with the observations. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Based on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at NAOJ. This work was supported by the joint research program of the Institute for Cosmic Ray Research (ICRR), University of Tokyo. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. S.F. acknowledges support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). This project has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.” This work is supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, as well as the KAKENHI Grant-in-Aid for Scientific Research (A; 15H02064, 17H01110, 17H01114, 20H00180, and 21H04467) through the Japan Society for the Promotion of Science (JSPS). This work has been supported in part by JSPS KAKENHI grant Nos. JP17K05382, JP20K04024, and JP21H04499 (K.N.). Yuki Isobe, Kimihiko Nakajima, Yuichi Harikane, Takashi Kojima, and Masato Onodera are supported by JSPS KAKENHI grant Nos. 21J20785, 20K22373,19J01222, 18J12840, and 17K14257, respectively.","date_published":"2022-01-31T00:00:00Z","year":"2022","external_id":{"arxiv":["2108.03850"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"main_file_link":[{"url":"https://arxiv.org/abs/2108.03850","open_access":"1"}],"quality_controlled":"1","doi":"10.3847/1538-4357/ac3509","article_processing_charge":"No","publisher":"IOP Publishing","date_updated":"2022-07-21T05:51:25Z","_id":"11509","type":"journal_article"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","citation":{"mla":"Sobral, David, et al. “The LEGA-C of Nature and Nurture in Stellar Populations at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly Histories for Quiescent Galaxies in Different Environments.” <i>The Astrophysical Journal</i>, vol. 926, no. 2, 117, IOP Publishing, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac4419\">10.3847/1538-4357/ac4419</a>.","apa":"Sobral, D., van der Wel, A., Bezanson, R., Bell, E., Muzzin, A., D’Eugenio, F., … van Dokkum, P. G. (2022). The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac4419\">https://doi.org/10.3847/1538-4357/ac4419</a>","ista":"Sobral D, van der Wel A, Bezanson R, Bell E, Muzzin A, D’Eugenio F, Darvish B, Gallazzi A, Wu P-F, Maseda M, Matthee JJ, Paulino-Afonso A, Straatman C, van Dokkum PG. 2022. The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. The Astrophysical Journal. 926(2), 117.","chicago":"Sobral, David, Arjen van der Wel, Rachel Bezanson, Eric Bell, Adam Muzzin, Francesco D’Eugenio, Behnam Darvish, et al. “The LEGA-C of Nature and Nurture in Stellar Populations at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly Histories for Quiescent Galaxies in Different Environments.” <i>The Astrophysical Journal</i>. IOP Publishing, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac4419\">https://doi.org/10.3847/1538-4357/ac4419</a>.","short":"D. Sobral, A. van der Wel, R. Bezanson, E. Bell, A. Muzzin, F. D’Eugenio, B. Darvish, A. Gallazzi, P.-F. Wu, M. Maseda, J.J. Matthee, A. Paulino-Afonso, C. Straatman, P.G. van Dokkum, The Astrophysical Journal 926 (2022).","ieee":"D. Sobral <i>et al.</i>, “The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments,” <i>The Astrophysical Journal</i>, vol. 926, no. 2. IOP Publishing, 2022.","ama":"Sobral D, van der Wel A, Bezanson R, et al. The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. <i>The Astrophysical Journal</i>. 2022;926(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac4419\">10.3847/1538-4357/ac4419</a>"},"language":[{"iso":"eng"}],"oa":1,"article_number":"117","arxiv":1,"month":"02","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication_status":"published","abstract":[{"text":"Galaxy evolution is driven by a variety of physical processes that are predicted to proceed at different rates for different dark matter haloes and environments across cosmic times. A record of this evolution is preserved in galaxy stellar populations, which we can access using absorption-line spectroscopy. Here we explore the large LEGA-C survey (DR3) to investigate the role of the environment and stellar mass on stellar populations at z ∼ 0.6–1 in the COSMOS field. Leveraging the statistical power and depth of LEGA-C, we reveal significant gradients in Dn4000 and Hδ equivalent widths (EWs) distributions over the stellar mass versus environment 2D spaces for the massive galaxy population (M > 1010 M⊙) at z ∼ 0.6–1.0. Dn4000 and Hδ EWs primarily depend on stellar mass, but they also depend on environment at fixed stellar mass. By splitting the sample into centrals and satellites, and in terms of star-forming galaxies and quiescent galaxies, we reveal that the significant environmental trends of Dn4000 and Hδ EW, when controlling for stellar mass, are driven by quiescent galaxies. Regardless of being centrals or satellites, star-forming galaxies reveal Dn4000 and Hδ EWs, which depend strongly on their stellar mass and are completely independent of the environment at 0.6 < z < 1.0. The environmental trends seen for satellite galaxies are fully driven by the trends that hold only for quiescent galaxies, combined with the strong environmental dependency of the quiescent fraction at fixed stellar mass. Our results are consistent with recent predictions from simulations that point toward massive galaxies forming first in overdensities or the most compact dark matter haloes.","lang":"eng"}],"intvolume":"       926","article_type":"original","date_created":"2022-07-06T12:38:42Z","volume":926,"oa_version":"Published Version","title":"The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Arjen","full_name":"van der Wel, Arjen","last_name":"van der Wel"},{"last_name":"Bezanson","full_name":"Bezanson, Rachel","first_name":"Rachel"},{"full_name":"Bell, Eric","last_name":"Bell","first_name":"Eric"},{"first_name":"Adam","last_name":"Muzzin","full_name":"Muzzin, Adam"},{"first_name":"Francesco","last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Anna","last_name":"Gallazzi","full_name":"Gallazzi, Anna"},{"first_name":"Po-Feng","last_name":"Wu","full_name":"Wu, Po-Feng"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"first_name":"Caroline","last_name":"Straatman","full_name":"Straatman, Caroline"},{"full_name":"van Dokkum, Pieter G.","last_name":"van Dokkum","first_name":"Pieter G."}],"day":"17","scopus_import":"1","date_published":"2022-02-17T00:00:00Z","acknowledgement":"We thank the reviewer for several valuable comments that improved the clarity of the manuscript. P.F.W. acknowledges the support of the fellowship by the East Asian Core Observatories Association. This work is based on observations made with ESO VLT Telescopes at the La Silla Paranal Observatory under programmes ID 194-A.2005 and 1100.A-0949 (The LEGA-C Public Spectroscopy Survey). This project has received funding from the European Research Council (ERC) under the European Union—Horizon 2020 research and innovation program (grant agreement No. 683184).","extern":"1","status":"public","publication":"The Astrophysical Journal","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"external_id":{"arxiv":["2112.08372"]},"year":"2022","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/2112.08372","open_access":"1"}],"type":"journal_article","date_updated":"2022-07-19T09:37:42Z","_id":"11510","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ac4419","article_processing_charge":"No"},{"main_file_link":[{"url":"https://arxiv.org/abs/2102.04561","open_access":"1"}],"quality_controlled":"1","doi":"10.3847/1538-4357/ac350b","article_processing_charge":"No","publisher":"IOP Publishing","date_updated":"2022-07-19T09:38:03Z","_id":"11511","type":"journal_article","publication":"The Astrophysical Journal","extern":"1","status":"public","acknowledgement":"We thank our anonymous referee for the constructive feedback. We extend our gratitude to Maarten Baes, Simon Lilly, Rafael Ottersberg, Gabriele Pezzulli, Alvio Renzini, and Andrea Weibel for insightful discussions. A.G. gratefully acknowledges financial support from the Fund for Scientific Research Flanders (FWO-Vlaanderen, project G.0G04.16N). This work used the DiRAC Data Centric system at Durham University, operated by the ICC on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.\r\n\r\nWe have benefited from the data analysis tool Topcat (Taylor 2013) and the programming language Python, including the numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and scipy (Virtanen et al. 2020) packages.","date_published":"2022-01-13T00:00:00Z","year":"2022","external_id":{"arxiv":["2102.04561"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"abstract":[{"text":"The ratio of α-elements to iron in galaxies holds valuable information about the star formation history (SFH) since their enrichment occurs on different timescales. The fossil record of stars in galaxies has mostly been excavated for passive galaxies, since the light of star-forming galaxies is dominated by young stars, which have much weaker atmospheric absorption features. Here we use the largest reference cosmological simulation of the EAGLE project to investigate the origin of variations in stellar α-enhancement among star-forming galaxies at z = 0, and their impact on integrated spectra. The definition of α-enhancement in a composite stellar population is ambiguous. We elucidate two definitions—termed “mean” and “galactic” α-enhancement—in more detail. While a star-forming galaxy has a high “mean” α-enhancement when its stars formed rapidly, a galaxy with a large “galactic” α-enhancement generally had a delayed SFH. We find that absorption-line strengths of Mg and Fe correlate with variations in α-enhancement. These correlations are strongest for the “galactic” α-enhancement. However, we show that these are mostly caused by other effects that are cross-correlated with α-enhancement, such as variations in the light-weighted age. This severely complicates the retrieval of α-enhancements in star-forming galaxies. The ambiguity is not severe for passive galaxies, and we confirm that spectral variations in these galaxies are caused by measurable variations in α-enhancements. We suggest that this more complex coupling between α-enhancement and SFHs can guide the interpretation of new observations of star-forming galaxies.","lang":"eng"}],"intvolume":"       924","publication_status":"published","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"author":[{"last_name":"Gebek","full_name":"Gebek, Andrea","first_name":"Andrea"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"}],"day":"13","scopus_import":"1","oa_version":"Published Version","title":"On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation","volume":924,"article_type":"original","date_created":"2022-07-06T12:48:32Z","oa":1,"language":[{"iso":"eng"}],"issue":"2","citation":{"ama":"Gebek A, Matthee JJ. On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. <i>The Astrophysical Journal</i>. 2022;924(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac350b\">10.3847/1538-4357/ac350b</a>","ieee":"A. Gebek and J. J. Matthee, “On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation,” <i>The Astrophysical Journal</i>, vol. 924, no. 2. IOP Publishing, 2022.","short":"A. Gebek, J.J. Matthee, The Astrophysical Journal 924 (2022).","ista":"Gebek A, Matthee JJ. 2022. On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. The Astrophysical Journal. 924(2), 73.","chicago":"Gebek, Andrea, and Jorryt J Matthee. “On the Variation in Stellar α-Enhancements of Star-Forming Galaxies in the EAGLE Simulation.” <i>The Astrophysical Journal</i>. IOP Publishing, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac350b\">https://doi.org/10.3847/1538-4357/ac350b</a>.","apa":"Gebek, A., &#38; Matthee, J. J. (2022). On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac350b\">https://doi.org/10.3847/1538-4357/ac350b</a>","mla":"Gebek, Andrea, and Jorryt J. Matthee. “On the Variation in Stellar α-Enhancements of Star-Forming Galaxies in the EAGLE Simulation.” <i>The Astrophysical Journal</i>, vol. 924, no. 2, 73, IOP Publishing, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac350b\">10.3847/1538-4357/ac350b</a>."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"month":"01","article_number":"73"},{"page":"631-632","intvolume":"         6","abstract":[{"text":"The Sun’s surface hosts varying magnetic activities and rotation rates (from equator to pole), and unique solar weather. Now, a combination of ground and space observations has unveiled a previously undetected magnetized plasma current.","lang":"eng"}],"publication_status":"published","publication_identifier":{"eissn":["2397-3366"]},"quality_controlled":"1","scopus_import":"1","day":"18","article_processing_charge":"No","doi":"10.1038/s41550-022-01683-2","author":[{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"}],"publisher":"Springer Nature","oa_version":"None","title":"Hidden currents at the Sun’s surface","volume":6,"_id":"11600","date_updated":"2022-08-19T09:52:21Z","date_created":"2022-07-18T09:34:37Z","type":"journal_article","article_type":"letter_note","publication":"Nature Astronomy","language":[{"iso":"eng"}],"extern":"1","status":"public","citation":{"chicago":"Bugnet, Lisa Annabelle. “Hidden Currents at the Sun’s Surface.” <i>Nature Astronomy</i>. Springer Nature, 2022. <a href=\"https://doi.org/10.1038/s41550-022-01683-2\">https://doi.org/10.1038/s41550-022-01683-2</a>.","ista":"Bugnet LA. 2022. Hidden currents at the Sun’s surface. Nature Astronomy. 6, 631–632.","apa":"Bugnet, L. A. (2022). Hidden currents at the Sun’s surface. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-022-01683-2\">https://doi.org/10.1038/s41550-022-01683-2</a>","mla":"Bugnet, Lisa Annabelle. “Hidden Currents at the Sun’s Surface.” <i>Nature Astronomy</i>, vol. 6, Springer Nature, 2022, pp. 631–32, doi:<a href=\"https://doi.org/10.1038/s41550-022-01683-2\">10.1038/s41550-022-01683-2</a>.","ama":"Bugnet LA. Hidden currents at the Sun’s surface. <i>Nature Astronomy</i>. 2022;6:631-632. doi:<a href=\"https://doi.org/10.1038/s41550-022-01683-2\">10.1038/s41550-022-01683-2</a>","ieee":"L. A. Bugnet, “Hidden currents at the Sun’s surface,” <i>Nature Astronomy</i>, vol. 6. Springer Nature, pp. 631–632, 2022.","short":"L.A. Bugnet, Nature Astronomy 6 (2022) 631–632."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2022-05-18T00:00:00Z","year":"2022","month":"05","keyword":["Astronomy and Astrophysics"]},{"month":"02","arxiv":1,"article_number":"191","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ieee":"J. C. Zinn <i>et al.</i>, “The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18,” <i>The Astrophysical Journal</i>, vol. 926, no. 2. IOP Publishing, 2022.","short":"J.C. Zinn, D. Stello, Y. Elsworth, R.A. García, T. Kallinger, S. Mathur, B. Mosser, M. Hon, L.A. Bugnet, C. Jones, C. Reyes, S. Sharma, R. Schönrich, J.T. Warfield, R. Luger, A. Vanderburg, C. Kobayashi, M.H. Pinsonneault, J.A. Johnson, D. Huber, S. Buder, M. Joyce, J. Bland-Hawthorn, L. Casagrande, G.F. Lewis, A. Miglio, T. Nordlander, G.R. Davies, G.D. Silva, W.J. Chaplin, V. Silva Aguirre, The Astrophysical Journal 926 (2022).","ama":"Zinn JC, Stello D, Elsworth Y, et al. The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. <i>The Astrophysical Journal</i>. 2022;926(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">10.3847/1538-4357/ac2c83</a>","apa":"Zinn, J. C., Stello, D., Elsworth, Y., García, R. A., Kallinger, T., Mathur, S., … Silva Aguirre, V. (2022). The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">https://doi.org/10.3847/1538-4357/ac2c83</a>","mla":"Zinn, Joel C., et al. “The K2 Galactic Archaeology Program Data Release 3: Age-Abundance Patterns in C1–C8 and C10–C18.” <i>The Astrophysical Journal</i>, vol. 926, no. 2, 191, IOP Publishing, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">10.3847/1538-4357/ac2c83</a>.","ista":"Zinn JC, Stello D, Elsworth Y, García RA, Kallinger T, Mathur S, Mosser B, Hon M, Bugnet LA, Jones C, Reyes C, Sharma S, Schönrich R, Warfield JT, Luger R, Vanderburg A, Kobayashi C, Pinsonneault MH, Johnson JA, Huber D, Buder S, Joyce M, Bland-Hawthorn J, Casagrande L, Lewis GF, Miglio A, Nordlander T, Davies GR, Silva GD, Chaplin WJ, Silva Aguirre V. 2022. The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. The Astrophysical Journal. 926(2), 191.","chicago":"Zinn, Joel C., Dennis Stello, Yvonne Elsworth, Rafael A. García, Thomas Kallinger, Savita Mathur, Benoît Mosser, et al. “The K2 Galactic Archaeology Program Data Release 3: Age-Abundance Patterns in C1–C8 and C10–C18.” <i>The Astrophysical Journal</i>. IOP Publishing, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">https://doi.org/10.3847/1538-4357/ac2c83</a>."},"issue":"2","oa_version":"Preprint","title":"The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18","scopus_import":"1","day":"24","author":[{"first_name":"Joel C.","full_name":"Zinn, Joel C.","last_name":"Zinn"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"first_name":"Yvonne","full_name":"Elsworth, Yvonne","last_name":"Elsworth"},{"full_name":"García, Rafael A.","last_name":"García","first_name":"Rafael A."},{"first_name":"Thomas","full_name":"Kallinger, Thomas","last_name":"Kallinger"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"first_name":"Benoît","last_name":"Mosser","full_name":"Mosser, Benoît"},{"first_name":"Marc","full_name":"Hon, Marc","last_name":"Hon"},{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet"},{"first_name":"Caitlin","last_name":"Jones","full_name":"Jones, Caitlin"},{"first_name":"Claudia","full_name":"Reyes, Claudia","last_name":"Reyes"},{"full_name":"Sharma, Sanjib","last_name":"Sharma","first_name":"Sanjib"},{"last_name":"Schönrich","full_name":"Schönrich, Ralph","first_name":"Ralph"},{"full_name":"Warfield, Jack T.","last_name":"Warfield","first_name":"Jack T."},{"first_name":"Rodrigo","full_name":"Luger, Rodrigo","last_name":"Luger"},{"first_name":"Andrew","full_name":"Vanderburg, Andrew","last_name":"Vanderburg"},{"first_name":"Chiaki","last_name":"Kobayashi","full_name":"Kobayashi, Chiaki"},{"first_name":"Marc H.","full_name":"Pinsonneault, Marc H.","last_name":"Pinsonneault"},{"full_name":"Johnson, Jennifer A.","last_name":"Johnson","first_name":"Jennifer A."},{"first_name":"Daniel","full_name":"Huber, Daniel","last_name":"Huber"},{"last_name":"Buder","full_name":"Buder, Sven","first_name":"Sven"},{"last_name":"Joyce","full_name":"Joyce, Meridith","first_name":"Meridith"},{"first_name":"Joss","last_name":"Bland-Hawthorn","full_name":"Bland-Hawthorn, Joss"},{"full_name":"Casagrande, Luca","last_name":"Casagrande","first_name":"Luca"},{"full_name":"Lewis, Geraint F.","last_name":"Lewis","first_name":"Geraint F."},{"full_name":"Miglio, Andrea","last_name":"Miglio","first_name":"Andrea"},{"first_name":"Thomas","last_name":"Nordlander","full_name":"Nordlander, Thomas"},{"full_name":"Davies, Guy R.","last_name":"Davies","first_name":"Guy R."},{"first_name":"Gayandhi De","full_name":"Silva, Gayandhi De","last_name":"Silva"},{"full_name":"Chaplin, William J.","last_name":"Chaplin","first_name":"William J."},{"full_name":"Silva Aguirre, Victor","last_name":"Silva Aguirre","first_name":"Victor"}],"date_created":"2022-07-18T10:57:30Z","article_type":"original","volume":926,"abstract":[{"text":"We present the third and final data release of the K2 Galactic Archaeology Program (K2 GAP) for Campaigns C1–C8 and C10–C18. We provide asteroseismic radius and mass coefficients, κR and κM, for ∼19,000 red giant stars, which translate directly to radius and mass given a temperature. As such, K2 GAP DR3 represents the largest asteroseismic sample in the literature to date. K2 GAP DR3 stellar parameters are calibrated to be on an absolute parallactic scale based on Gaia DR2, with red giant branch and red clump evolutionary state classifications provided via a machine-learning approach. Combining these stellar parameters with GALAH DR3 spectroscopy, we determine asteroseismic ages with precisions of ∼20%–30% and compare age-abundance relations to Galactic chemical evolution models among both low- and high-α populations for α, light, iron-peak, and neutron-capture elements. We confirm recent indications in the literature of both increased Ba production at late Galactic times as well as significant contributions to r-process enrichment from prompt sources associated with, e.g., core-collapse supernovae. With an eye toward other Galactic archeology applications, we characterize K2 GAP DR3 uncertainties and completeness using injection tests, suggesting that K2 GAP DR3 is largely unbiased in mass/age, with uncertainties of 2.9% (stat.) ± 0.1% (syst.) and 6.7% (stat.) ± 0.3% (syst.) in κR and κM for red giant branch stars and 4.7% (stat.) ± 0.3% (syst.) and 11% (stat.) ± 0.9% (syst.) for red clump stars. We also identify percent-level asteroseismic systematics, which are likely related to the time baseline of the underlying data, and which therefore should be considered in TESS asteroseismic analysis.","lang":"eng"}],"intvolume":"       926","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication_status":"published","external_id":{"arxiv":["2108.05455"]},"year":"2022","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication":"The Astrophysical Journal","status":"public","extern":"1","acknowledgement":"We would like to thank the anonymous referee whose comments significantly improved the manuscript. J.C.Z. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001869. J.C.Z. and M.H.P. acknowledge support from NASA grants 80NSSC18K0391 and NNX17AJ40G. Y.E. and C.J. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S.M. acknowledges support from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697 and the grant number PID2019-107187GB-I00. R.A.G. acknowledges funding received from the PLATO CNES grant. C.K. acknowledges funding from the UK Science and Technology Facilities Council (STFC) through grants ST/M000958/1, ST/R000905/1, and ST/V000632/1.\r\n\r\nFunding for the Stellar Astrophysics Centre (SAC) is provided by the Danish National Research Foundation (grant agreement No. DNRF106).\r\n\r\nThe K2 Galactic Archaeology Program is supported by the National Aeronautics and Space Administration under grant NNX16AJ17G issued through the K2 Guest Observer Program. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\r\n\r\nThis paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.\r\n\r\nParts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013.\r\n\r\nThis research was partially conducted during the Exostar19 program at the Kavli Institute for Theoretical Physics at UC Santa Barbara, which was supported in part by the National Science Foundation under grant No. NSF PHY-1748958.\r\n\r\nBased in part on data obtained at Siding Spring Observatory via GALAH. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present.\r\n\r\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.\r\n\r\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah (www.sdss.org).\r\n\r\nSoftware: asfgrid (Sharma & Stello 2016), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), NumPy (Walt 2011), pandas (McKinney 2010), Matplotlib (Hunter 2007), IPython (Pérez & Granger 2007), SciPy (Virtanen et al.2020).","date_published":"2022-02-24T00:00:00Z","publisher":"IOP Publishing","article_processing_charge":"No","doi":"10.3847/1538-4357/ac2c83","type":"journal_article","_id":"11601","date_updated":"2022-08-19T09:52:08Z","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/2108.05455","open_access":"1"}]},{"month":"01","arxiv":1,"article_number":"A31","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Mathur S, García RA, Breton S, et al. Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data. <i>Astronomy &#38; Astrophysics</i>. 2022;657. doi:<a href=\"https://doi.org/10.1051/0004-6361/202141168\">10.1051/0004-6361/202141168</a>","short":"S. Mathur, R.A. García, S. Breton, A.R.G. Santos, B. Mosser, D. Huber, M. Sayeed, L.A. Bugnet, A. Chontos, Astronomy &#38; Astrophysics 657 (2022).","ieee":"S. Mathur <i>et al.</i>, “Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data,” <i>Astronomy &#38; Astrophysics</i>, vol. 657. EDP Sciences, 2022.","chicago":"Mathur, S., R. A. García, S. Breton, A. R. G. Santos, B. Mosser, D. Huber, M. Sayeed, Lisa Annabelle Bugnet, and A. Chontos. “Detections of Solar-like Oscillations in Dwarfs and Subgiants with Kepler DR25 Short-Cadence Data.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202141168\">https://doi.org/10.1051/0004-6361/202141168</a>.","ista":"Mathur S, García RA, Breton S, Santos ARG, Mosser B, Huber D, Sayeed M, Bugnet LA, Chontos A. 2022. Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data. Astronomy &#38; Astrophysics. 657, A31.","mla":"Mathur, S., et al. “Detections of Solar-like Oscillations in Dwarfs and Subgiants with Kepler DR25 Short-Cadence Data.” <i>Astronomy &#38; Astrophysics</i>, vol. 657, A31, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202141168\">10.1051/0004-6361/202141168</a>.","apa":"Mathur, S., García, R. A., Breton, S., Santos, A. R. G., Mosser, B., Huber, D., … Chontos, A. (2022). Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202141168\">https://doi.org/10.1051/0004-6361/202141168</a>"},"oa_version":"Preprint","title":"Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data","day":"01","scopus_import":"1","author":[{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"first_name":"R. A.","full_name":"García, R. A.","last_name":"García"},{"first_name":"S.","last_name":"Breton","full_name":"Breton, S."},{"full_name":"Santos, A. R. G.","last_name":"Santos","first_name":"A. R. G."},{"full_name":"Mosser, B.","last_name":"Mosser","first_name":"B."},{"first_name":"D.","full_name":"Huber, D.","last_name":"Huber"},{"full_name":"Sayeed, M.","last_name":"Sayeed","first_name":"M."},{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"},{"first_name":"A.","last_name":"Chontos","full_name":"Chontos, A."}],"date_created":"2022-07-18T11:41:59Z","article_type":"original","volume":657,"intvolume":"       657","abstract":[{"lang":"eng","text":"During the survey phase of the Kepler mission, several thousand stars were observed in short cadence, allowing for the detection of solar-like oscillations in more than 500 main-sequence and subgiant stars. These detections showed the power of asteroseismology in determining fundamental stellar parameters. However, the Kepler Science Office discovered an issue in the calibration that affected half of the store of short-cadence data, leading to a new data release (DR25) with corrections on the light curves. In this work, we re-analyzed the one-month time series of the Kepler survey phase to search for solar-like oscillations that might have been missed when using the previous data release. We studied the seismic parameters of 99 stars, among which there are 46 targets with new reported solar-like oscillations, increasing, by around 8%, the known sample of solar-like stars with an asteroseismic analysis of the short-cadence data from this mission. The majority of these stars have mid- to high-resolution spectroscopy publicly available with the LAMOST and APOGEE surveys, respectively, as well as precise Gaia parallaxes. We computed the masses and radii using seismic scaling relations and we find that this new sample features massive stars (above 1.2 M⊙ and up to 2 M⊙) and subgiants. We determined the granulation parameters and amplitude of the modes, which agree with the scaling relations derived for dwarfs and subgiants. The stars studied here are slightly fainter than the previously known sample of main-sequence and subgiants with asteroseismic detections. We also studied the surface rotation and magnetic activity levels of those stars. Our sample of 99 stars has similar levels of activity compared to the previously known sample and is in the same range as the Sun between the minimum and maximum of its activity cycle. We find that for seven stars, a possible blend could be the reason for the non-detection with the early data release. Finally, we compared the radii obtained from the scaling relations with the Gaia ones and we find that the Gaia radii are overestimated by 4.4%, on average, compared to the seismic radii, with a scatter of 12.3% and a decreasing trend according to the evolutionary stage. In addition, for homogeneity purposes, we re-analyzed the DR25 of the main-sequence and subgiant stars with solar-like oscillations that were previously detected and, as a result, we provide the global seismic parameters for a total of 525 stars."}],"publication_status":"published","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"external_id":{"arxiv":["2109.14058"]},"year":"2022","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","extern":"1","publication":"Astronomy & Astrophysics","acknowledgement":"This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. S. M. acknowledges support by the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697 and the grant number PID2019-107187GB-I00. R. A. G. and S. N. B acknowledge the support from PLATO and GOLF CNES grants. A. R. G. S. acknowledges the support from National Aeronautics and Space Administration under Grant NNX17AF27G and STFC consolidated grant ST/T000252/1. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC19K0597), and the National Science Foundation (AST-1717000). M.S. is supported by the Research Corporation for Science Advancement through Scialog award #26080. Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences.","date_published":"2022-01-01T00:00:00Z","publisher":"EDP Sciences","article_processing_charge":"No","doi":"10.1051/0004-6361/202141168","type":"journal_article","_id":"11602","date_updated":"2022-08-19T09:56:58Z","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2109.14058"}]},{"year":"2022","external_id":{"arxiv":["2202.10026"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","magnetohydrodynamics (MHD) / waves / stars","rotation / stars: magnetic field / stars","oscillations / methods"],"extern":"1","publication":"Astronomy & Astrophysics","status":"public","acknowledgement":"We thank the referee for her/his positive and constructive report, which has allowed us to improve the quality of our article. H.D. and S.M. acknowledge support from the CNES PLATO grant at CEA/DAp. T.V.R. gratefully acknowledges support from the Research Foundation Flanders (FWO) under grant agreement No. 12ZB620N and V414021N. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1748958. C.A. is supported by the KU Leuven Research Council (grant C16/18/005: PARADISE) as well as from the BELgian federal Science Policy Office (BELSPO) through a PLATO PRODEX grant.","date_published":"2022-05-19T00:00:00Z","doi":"10.1051/0004-6361/202142956","article_processing_charge":"No","publisher":"EDP Sciences","date_updated":"2022-08-22T07:58:54Z","_id":"11621","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/2202.10026","open_access":"1"}],"quality_controlled":"1","month":"05","arxiv":1,"article_number":"A133","oa":1,"language":[{"iso":"eng"}],"citation":{"ista":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. 2022. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. Astronomy &#38; Astrophysics. 661, A133.","chicago":"Dhouib, H., S. Mathis, Lisa Annabelle Bugnet, T. Van Reeth, and C. Aerts. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142956\">https://doi.org/10.1051/0004-6361/202142956</a>.","mla":"Dhouib, H., et al. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 661, A133, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142956\">10.1051/0004-6361/202142956</a>.","apa":"Dhouib, H., Mathis, S., Bugnet, L. A., Van Reeth, T., &#38; Aerts, C. (2022). Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142956\">https://doi.org/10.1051/0004-6361/202142956</a>","ama":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. <i>Astronomy &#38; Astrophysics</i>. 2022;661. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142956\">10.1051/0004-6361/202142956</a>","short":"H. Dhouib, S. Mathis, L.A. Bugnet, T. Van Reeth, C. Aerts, Astronomy &#38; Astrophysics 661 (2022).","ieee":"H. Dhouib, S. Mathis, L. A. Bugnet, T. Van Reeth, and C. Aerts, “Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field,” <i>Astronomy &#38; Astrophysics</i>, vol. 661. EDP Sciences, 2022."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"H.","last_name":"Dhouib","full_name":"Dhouib, H."},{"full_name":"Mathis, S.","last_name":"Mathis","first_name":"S."},{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"T.","full_name":"Van Reeth, T.","last_name":"Van Reeth"},{"full_name":"Aerts, C.","last_name":"Aerts","first_name":"C."}],"scopus_import":"1","day":"19","title":"Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field","oa_version":"Preprint","volume":661,"article_type":"original","date_created":"2022-07-19T08:04:15Z","intvolume":"       661","abstract":[{"lang":"eng","text":"Context. Asteroseismology has revealed small core-to-surface rotation contrasts in stars in the whole Hertzsprung–Russell diagram. This is the signature of strong transport of angular momentum (AM) in stellar interiors. One of the plausible candidates to efficiently carry AM is magnetic fields with various topologies that could be present in stellar radiative zones. Among them, strong axisymmetric azimuthal (toroidal) magnetic fields have received a lot of interest. Indeed, if they are subject to the so-called Tayler instability, the accompanying triggered Maxwell stresses can transport AM efficiently. In addition, the electromotive force induced by the fluctuations of magnetic and velocity fields could potentially sustain a dynamo action that leads to the regeneration of the initial strong axisymmetric azimuthal magnetic field.\r\n\r\nAims. The key question we aim to answer is whether we can detect signatures of these deep strong azimuthal magnetic fields. The only way to answer this question is asteroseismology, and the best laboratories of study are intermediate-mass and massive stars with external radiative envelopes. Most of these are rapid rotators during their main sequence. Therefore, we have to study stellar pulsations propagating in stably stratified, rotating, and potentially strongly magnetised radiative zones, namely magneto-gravito-inertial (MGI) waves.\r\n\r\nMethods. We generalise the traditional approximation of rotation (TAR) by simultaneously taking general axisymmetric differential rotation and azimuthal magnetic fields into account. Both the Coriolis acceleration and the Lorentz force are therefore treated in a non-perturbative way. Using this new formalism, we derive the asymptotic properties of MGI waves and their period spacings.\r\n\r\nResults. We find that toroidal magnetic fields induce a shift in the period spacings of gravity (g) and Rossby (r) modes. An equatorial azimuthal magnetic field with an amplitude of the order of 105 G leads to signatures that are detectable in period spacings for high-radial-order g and r modes in γ Doradus (γ Dor) and slowly pulsating B (SPB) stars. More complex hemispheric configurations are more difficult to observe, particularly when they are localised out of the propagation region of MGI modes, which can be localised in an equatorial belt.\r\n\r\nConclusions. The magnetic TAR, which takes into account toroidal magnetic fields in a non-perturbative way, is derived. This new formalism allows us to assess the effects of the magnetic field in γ Dor and SPB stars on g and r modes. We find that these effects should be detectable for equatorial fields thanks to modern space photometry using observations from Kepler, TESS CVZ, and PLATO."}],"publication_status":"published","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]}},{"date_published":"2022-11-16T00:00:00Z","extern":"1","publication":"The Astrophysical Journal","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2022","external_id":{"arxiv":["2210.01928"]},"main_file_link":[{"url":"https://arxiv.org/abs/2210.01928","open_access":"1"}],"quality_controlled":"1","_id":"13445","date_updated":"2023-09-06T07:27:45Z","type":"journal_article","article_processing_charge":"No","doi":"10.3847/1538-4357/ac97e7","publisher":"American Astronomical Society","citation":{"apa":"Ong, J. M. J., Bugnet, L. A., &#38; Basu, S. (2022). Mode mixing and rotational splittings. I. Near-degeneracy effects revisited. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ac97e7\">https://doi.org/10.3847/1538-4357/ac97e7</a>","mla":"Ong, J. M. Joel, et al. “Mode Mixing and Rotational Splittings. I. Near-Degeneracy Effects Revisited.” <i>The Astrophysical Journal</i>, vol. 940, no. 1, 18, American Astronomical Society, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac97e7\">10.3847/1538-4357/ac97e7</a>.","chicago":"Ong, J. M. Joel, Lisa Annabelle Bugnet, and Sarbani Basu. “Mode Mixing and Rotational Splittings. I. Near-Degeneracy Effects Revisited.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac97e7\">https://doi.org/10.3847/1538-4357/ac97e7</a>.","ista":"Ong JMJ, Bugnet LA, Basu S. 2022. Mode mixing and rotational splittings. I. Near-degeneracy effects revisited. The Astrophysical Journal. 940(1), 18.","ieee":"J. M. J. Ong, L. A. Bugnet, and S. Basu, “Mode mixing and rotational splittings. I. Near-degeneracy effects revisited,” <i>The Astrophysical Journal</i>, vol. 940, no. 1. American Astronomical Society, 2022.","short":"J.M.J. Ong, L.A. Bugnet, S. Basu, The Astrophysical Journal 940 (2022).","ama":"Ong JMJ, Bugnet LA, Basu S. Mode mixing and rotational splittings. I. Near-degeneracy effects revisited. <i>The Astrophysical Journal</i>. 2022;940(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac97e7\">10.3847/1538-4357/ac97e7</a>"},"issue":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"article_number":"18","arxiv":1,"month":"11","publication_status":"published","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"intvolume":"       940","abstract":[{"text":"Rotation is typically assumed to induce strictly symmetric rotational splitting into the rotational multiplets of pure p- and g-modes. However, for evolved stars exhibiting mixed modes, avoided crossings between different multiplet components are known to yield asymmetric rotational splitting, in particular for near-degenerate mixed-mode pairs, where notional pure p-modes are fortuitously in resonance with pure g-modes. These near-degeneracy effects have been described in subgiants, but their consequences for the characterization of internal rotation in red giants have not previously been investigated in detail, in part owing to theoretical intractability. We employ new developments in the analytic theory of mixed-mode coupling to study these near-resonance phenomena. In the vicinity of the most p-dominated mixed modes, the near-degenerate intrinsic asymmetry from pure rotational splitting increases dramatically over the course of stellar evolution, and it depends strongly on the mode-mixing fraction ζ. We also find that a linear treatment of rotation remains viable for describing the underlying p- and g-modes, even when it does not for the resulting mixed modes undergoing these avoided crossings. We explore observational consequences for potential measurements of asymmetric mixed-mode splitting, which has been proposed as a magnetic-field diagnostic. Finally, we propose improved measurement techniques for rotational characterization, exploiting the linearity of rotational effects on the underlying p/g-modes, while still accounting for these mixed-mode coupling effects.","lang":"eng"}],"volume":940,"date_created":"2023-08-01T14:20:41Z","article_type":"original","day":"16","scopus_import":"1","author":[{"last_name":"Ong","full_name":"Ong, J. M. Joel","first_name":"J. M. Joel"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"full_name":"Basu, Sarbani","last_name":"Basu","first_name":"Sarbani"}],"oa_version":"Published Version","title":"Mode mixing and rotational splittings. I. Near-degeneracy effects revisited"},{"abstract":[{"text":"We characterize massive stars (M > 8 M⊙) in the nearby (D ∼ 0.8 Mpc) extremely metal-poor (Z ∼ 5% Z⊙) galaxy Leo A using Hubble Space Telescope ultraviolet (UV), optical, and near-infrared (NIR) imaging along with Keck/Low-Resolution Imaging Spectrograph and MMT/Binospec optical spectroscopy for 18 main-sequence OB stars. We find that: (a) 12 of our 18 stars show emission lines, despite not being associated with an H ii region, suggestive of stellar activity (e.g., mass loss, accretion, binary star interaction), which is consistent with previous predictions of enhanced activity at low metallicity; (b) six are Be stars, which are the first to be spectroscopically studied at such low metallicity—these Be stars have unusual panchromatic SEDs; (c) for stars well fit by the TLUSTY nonlocal thermodynamic equilibrium models, the photometric and spectroscopic values of $\\mathrm{log}({T}_{\\mathrm{eff}})$ and $\\mathrm{log}(g)$ agree to within ∼0.01 dex and ∼0.18 dex, respectively, indicating that near-UV/optical/NIR imaging can be used to reliably characterize massive (M ∼ 8–30 M⊙) main-sequence star properties relative to optical spectroscopy; (d) the properties of the most-massive stars in H II regions are consistent with constraints from previous nebular emission line studies; and (e) 13 stars with M > 8M⊙ are >40 pc from a known star cluster or H II region. Our sample comprises ∼50% of all known massive stars at Z ≲ 10% Z⊙with derived stellar parameters, high-quality optical spectra, and panchromatic photometry.","lang":"eng"}],"intvolume":"       941","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication_status":"published","day":"27","scopus_import":"1","author":[{"full_name":"Gull, Maude","last_name":"Gull","first_name":"Maude"},{"first_name":"Daniel R.","full_name":"Weisz, Daniel R.","last_name":"Weisz"},{"first_name":"Peter","last_name":"Senchyna","full_name":"Senchyna, Peter"},{"full_name":"Sandford, Nathan R.","last_name":"Sandford","first_name":"Nathan R."},{"full_name":"Choi, Yumi","last_name":"Choi","first_name":"Yumi"},{"first_name":"Anna F.","full_name":"McLeod, Anna F.","last_name":"McLeod"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"first_name":"Karoline M.","last_name":"Gilbert","full_name":"Gilbert, Karoline M."},{"first_name":"Martha","last_name":"Boyer","full_name":"Boyer, Martha"},{"first_name":"Julianne J.","full_name":"Dalcanton, Julianne J.","last_name":"Dalcanton"},{"first_name":"Puragra","last_name":"GuhaThakurta","full_name":"GuhaThakurta, Puragra"},{"full_name":"Goldman, Steven","last_name":"Goldman","first_name":"Steven"},{"last_name":"Marigo","full_name":"Marigo, Paola","first_name":"Paola"},{"last_name":"McQuinn","full_name":"McQuinn, Kristen B. W.","first_name":"Kristen B. W."},{"first_name":"Giada","last_name":"Pastorelli","full_name":"Pastorelli, Giada"},{"last_name":"Stark","full_name":"Stark, Daniel P.","first_name":"Daniel P."},{"last_name":"Skillman","full_name":"Skillman, Evan","first_name":"Evan"},{"first_name":"Yuan-sen","full_name":"Ting, Yuan-sen","last_name":"Ting"},{"first_name":"Benjamin F.","full_name":"Williams, Benjamin F.","last_name":"Williams"}],"oa_version":"Published Version","title":"A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A","volume":941,"date_created":"2023-08-03T10:10:25Z","article_type":"original","oa":1,"language":[{"iso":"eng"}],"citation":{"short":"M. Gull, D.R. Weisz, P. Senchyna, N.R. Sandford, Y. Choi, A.F. McLeod, K. El-Badry, Y.L.L. Götberg, K.M. Gilbert, M. Boyer, J.J. Dalcanton, P. GuhaThakurta, S. Goldman, P. Marigo, K.B.W. McQuinn, G. Pastorelli, D.P. Stark, E. Skillman, Y. Ting, B.F. Williams, The Astrophysical Journal 941 (2022).","ieee":"M. Gull <i>et al.</i>, “A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A,” <i>The Astrophysical Journal</i>, vol. 941, no. 2. American Astronomical Society, 2022.","ama":"Gull M, Weisz DR, Senchyna P, et al. A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A. <i>The Astrophysical Journal</i>. 2022;941(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/aca295\">10.3847/1538-4357/aca295</a>","mla":"Gull, Maude, et al. “A Panchromatic Study of Massive Stars in the Extremely Metal-Poor Local Group Dwarf Galaxy Leo A.” <i>The Astrophysical Journal</i>, vol. 941, no. 2, 206, American Astronomical Society, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/aca295\">10.3847/1538-4357/aca295</a>.","apa":"Gull, M., Weisz, D. R., Senchyna, P., Sandford, N. R., Choi, Y., McLeod, A. F., … Williams, B. F. (2022). A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/aca295\">https://doi.org/10.3847/1538-4357/aca295</a>","chicago":"Gull, Maude, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, et al. “A Panchromatic Study of Massive Stars in the Extremely Metal-Poor Local Group Dwarf Galaxy Leo A.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2022. <a href=\"https://doi.org/10.3847/1538-4357/aca295\">https://doi.org/10.3847/1538-4357/aca295</a>.","ista":"Gull M, Weisz DR, Senchyna P, Sandford NR, Choi Y, McLeod AF, El-Badry K, Götberg YLL, Gilbert KM, Boyer M, Dalcanton JJ, GuhaThakurta P, Goldman S, Marigo P, McQuinn KBW, Pastorelli G, Stark DP, Skillman E, Ting Y, Williams BF. 2022. A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A. The Astrophysical Journal. 941(2), 206."},"issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"12","arxiv":1,"article_number":"206","main_file_link":[{"url":"https://doi.org/10.3847/1538-4357/aca295","open_access":"1"}],"quality_controlled":"1","article_processing_charge":"No","doi":"10.3847/1538-4357/aca295","publisher":"American Astronomical Society","_id":"13451","date_updated":"2023-08-21T12:04:58Z","type":"journal_article","status":"public","publication":"The Astrophysical Journal","extern":"1","date_published":"2022-12-27T00:00:00Z","year":"2022","external_id":{"arxiv":["2211.14349"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"]},{"date_published":"2022-12-01T00:00:00Z","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2022","external_id":{"arxiv":["2209.06350"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2209.06350"}],"quality_controlled":"1","page":"2028-2055","_id":"13452","date_updated":"2023-08-21T12:02:17Z","type":"journal_article","article_processing_charge":"No","doi":"10.1093/mnras/stac2598","publisher":"Oxford University Press","citation":{"ieee":"Z. Keszthelyi <i>et al.</i>, “The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2. Oxford University Press, pp. 2028–2055, 2022.","short":"Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit, M. Carrington, A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J. Ramalatswa, M.E. Shultz, A. ud-Doula, Monthly Notices of the Royal Astronomical Society 517 (2022) 2028–2055.","ama":"Keszthelyi Z, de Koter A, Götberg YLL, et al. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(2):2028-2055. doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>","apa":"Keszthelyi, Z., de Koter, A., Götberg, Y. L. L., Meynet, G., Brands, S. A., Petit, V., … ud-Doula, A. (2022). The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>","mla":"Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2, Oxford University Press, 2022, pp. 2028–55, doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>.","ista":"Keszthelyi Z, de Koter A, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington M, David-Uraz A, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME, ud-Doula A. 2022. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.","chicago":"Keszthelyi, Z, A de Koter, Ylva Louise Linsdotter Götberg, G Meynet, S A Brands, V Petit, M Carrington, et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>."},"issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"month":"12","arxiv":1,"publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"intvolume":"       517","abstract":[{"lang":"eng","text":"Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes."}],"volume":517,"date_created":"2023-08-03T10:10:37Z","article_type":"original","day":"01","scopus_import":"1","author":[{"full_name":"Keszthelyi, Z","last_name":"Keszthelyi","first_name":"Z"},{"first_name":"A","last_name":"de Koter","full_name":"de Koter, A"},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg"},{"first_name":"G","last_name":"Meynet","full_name":"Meynet, G"},{"last_name":"Brands","full_name":"Brands, S A","first_name":"S A"},{"first_name":"V","full_name":"Petit, V","last_name":"Petit"},{"first_name":"M","last_name":"Carrington","full_name":"Carrington, M"},{"last_name":"David-Uraz","full_name":"David-Uraz, A","first_name":"A"},{"first_name":"S T","last_name":"Geen","full_name":"Geen, S T"},{"full_name":"Georgy, C","last_name":"Georgy","first_name":"C"},{"first_name":"R","full_name":"Hirschi, R","last_name":"Hirschi"},{"full_name":"Puls, J","last_name":"Puls","first_name":"J"},{"last_name":"Ramalatswa","full_name":"Ramalatswa, K J","first_name":"K J"},{"last_name":"Shultz","full_name":"Shultz, M E","first_name":"M E"},{"first_name":"A","last_name":"ud-Doula","full_name":"ud-Doula, A"}],"title":"The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities","oa_version":"Preprint"},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.01713"}],"quality_controlled":"1","_id":"11498","date_updated":"2022-07-19T09:34:36Z","type":"journal_article","article_processing_charge":"No","doi":"10.1051/0004-6361/202140876","publisher":"EDP Sciences","date_published":"2021-10-15T00:00:00Z","acknowledgement":"We would like to thank Charlotte Mason for useful discussions and for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing the observational data for the comparison sample studied by Steidel et al. (2014), also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and we acknowledge support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research Council (NWO). GM received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS – DLV-896778. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. This paper also makes use of observations made with the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of the following programs and open-source packages for Python and we are thankful to their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013, 2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).","status":"public","publication":"Astronomy & Astrophysics","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"year":"2021","external_id":{"arxiv":["2108.01713"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","intvolume":"       654","abstract":[{"lang":"eng","text":"Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The strongest main UV emission line, Lyα, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Lyα emission becomes increasingly challenging at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies’ physical properties and their Lyα emission. The sample of 2052 emission line sources with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Lyα) UV emission lines increases with survey depth, and that the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and [Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 + C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III] λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548 + C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range of 250−500 km s−1 which is in agreement with previous results from the literature. The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III] λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization Model Probability Density Functions” to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper."}],"volume":654,"date_created":"2022-07-06T08:49:03Z","article_type":"original","day":"15","scopus_import":"1","author":[{"last_name":"Schmidt","full_name":"Schmidt, K. B.","first_name":"K. B."},{"last_name":"Kerutt","full_name":"Kerutt, J.","first_name":"J."},{"last_name":"Wisotzki","full_name":"Wisotzki, L.","first_name":"L."},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"first_name":"A.","full_name":"Feltre, A.","last_name":"Feltre"},{"first_name":"M. V.","last_name":"Maseda","full_name":"Maseda, M. V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"full_name":"Bacon, R.","last_name":"Bacon","first_name":"R."},{"first_name":"L. A.","last_name":"Boogaard","full_name":"Boogaard, L. A."},{"first_name":"S.","full_name":"Conseil, S.","last_name":"Conseil"},{"first_name":"T.","last_name":"Contini","full_name":"Contini, T."},{"first_name":"E. C.","last_name":"Herenz","full_name":"Herenz, E. C."},{"last_name":"Kollatschny","full_name":"Kollatschny, W.","first_name":"W."},{"full_name":"Krumpe, M.","last_name":"Krumpe","first_name":"M."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"last_name":"Mahler","full_name":"Mahler, G.","first_name":"G."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Mauerhofer, V.","last_name":"Mauerhofer","first_name":"V."},{"first_name":"J.","full_name":"Richard, J.","last_name":"Richard"},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."}],"oa_version":"Published Version","title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","citation":{"ista":"Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. Astronomy &#38; Astrophysics. 654, A80.","chicago":"Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>.","apa":"Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda, M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>","mla":"Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 654, A80, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>.","ama":"Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. 2021;654. doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>","ieee":"K. B. Schmidt <i>et al.</i>, “Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 654. EDP Sciences, 2021.","short":"K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda, T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz, W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer, J. Richard, J. Schaye, Astronomy &#38; Astrophysics 654 (2021)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"article_number":"A80","month":"10","arxiv":1}]