[{"isi":1,"volume":952,"article_type":"original","month":"08","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","file_date_updated":"2023-08-02T07:42:26Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"Yes","ddc":["520"],"intvolume":"       952","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_created":"2023-08-01T14:19:16Z","article_number":"131","department":[{"_id":"LiBu"}],"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.","date_published":"2023-08-01T00:00:00Z","author":[{"first_name":"Savita","full_name":"Mathur, Savita","last_name":"Mathur"},{"last_name":"Claytor","first_name":"Zachary R.","full_name":"Claytor, Zachary R."},{"full_name":"Santos, Ângela R. G.","first_name":"Ângela R. G.","last_name":"Santos"},{"first_name":"Rafael A.","full_name":"García, Rafael A.","last_name":"García"},{"last_name":"Amard","first_name":"Louis","full_name":"Amard, Louis"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Corsaro","first_name":"Enrico","full_name":"Corsaro, Enrico"},{"last_name":"Bonanno","first_name":"Alfio","full_name":"Bonanno, Alfio"},{"first_name":"Sylvain N.","full_name":"Breton, Sylvain N.","last_name":"Breton"},{"first_name":"Diego","full_name":"Godoy-Rivera, Diego","last_name":"Godoy-Rivera"},{"last_name":"Pinsonneault","first_name":"Marc H.","full_name":"Pinsonneault, Marc H."},{"full_name":"van Saders, Jennifer","first_name":"Jennifer","last_name":"van Saders"}],"_id":"13443","oa":1,"type":"journal_article","doi":"10.3847/1538-4357/acd118","language":[{"iso":"eng"}],"year":"2023","publisher":"American Astronomical Society","publication":"The Astrophysical Journal","file":[{"file_name":"2023_AstrophysicalJour_Mathur.pdf","file_size":4192386,"checksum":"f12452834d7ed6748dbf5ace18af4723","date_created":"2023-08-02T07:42:26Z","file_id":"13448","success":1,"date_updated":"2023-08-02T07:42:26Z","creator":"dernst","access_level":"open_access","content_type":"application/pdf","relation":"main_file"}],"title":"Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations","external_id":{"isi":["001034185700001"]},"issue":"2","has_accepted_license":"1","citation":{"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>.","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.","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>.","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).","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.","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>"},"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)"},"day":"01","oa_version":"Published Version","publication_status":"published","abstract":[{"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.","lang":"eng"}],"status":"public","date_updated":"2023-12-13T12:00:15Z"},{"issue":"1","scopus_import":"1","citation":{"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>","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.","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.","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>."},"arxiv":1,"external_id":{"arxiv":["2211.12438"]},"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","publication":"The Astrophysical Journal","main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/1538-4357/aca655"}],"status":"public","date_updated":"2023-08-21T12:07:05Z","abstract":[{"lang":"eng","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⊙."}],"publication_status":"published","oa_version":"Published Version","day":"20","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       943","extern":"1","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"18","date_created":"2023-08-03T10:10:12Z","article_type":"original","volume":943,"quality_controlled":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"month":"01","type":"journal_article","publisher":"American Astronomical Society","year":"2023","language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/aca655","date_published":"2023-01-20T00:00:00Z","oa":1,"_id":"13450","author":[{"last_name":"O‘Grady","first_name":"Anna J. G.","full_name":"O‘Grady, Anna J. G."},{"first_name":"Maria R.","full_name":"Drout, Maria R.","last_name":"Drout"},{"first_name":"B. M.","full_name":"Gaensler, B. M.","last_name":"Gaensler"},{"first_name":"C. S.","full_name":"Kochanek, C. S.","last_name":"Kochanek"},{"last_name":"Neugent","full_name":"Neugent, Kathryn F.","first_name":"Kathryn F."},{"last_name":"Doherty","full_name":"Doherty, Carolyn L.","first_name":"Carolyn L."},{"last_name":"Speagle","full_name":"Speagle, Joshua S.","first_name":"Joshua S."},{"last_name":"Shappee","full_name":"Shappee, B. J.","first_name":"B. J."},{"first_name":"Michael","full_name":"Rauch, Michael","last_name":"Rauch"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Ludwig, Bethany","first_name":"Bethany","last_name":"Ludwig"},{"full_name":"Thompson, Todd A.","first_name":"Todd A.","last_name":"Thompson"}]},{"author":[{"last_name":"Isobe","full_name":"Isobe, Yuki","first_name":"Yuki"},{"full_name":"Ouchi, Masami","first_name":"Masami","last_name":"Ouchi"},{"last_name":"Suzuki","first_name":"Akihiro","full_name":"Suzuki, Akihiro"},{"first_name":"Takashi J.","full_name":"Moriya, Takashi J.","last_name":"Moriya"},{"last_name":"Nakajima","full_name":"Nakajima, Kimihiko","first_name":"Kimihiko"},{"full_name":"Nomoto, Ken’ichi","first_name":"Ken’ichi","last_name":"Nomoto"},{"last_name":"Rauch","first_name":"Michael","full_name":"Rauch, Michael"},{"full_name":"Harikane, Yuichi","first_name":"Yuichi","last_name":"Harikane"},{"last_name":"Kojima","first_name":"Takashi","full_name":"Kojima, Takashi"},{"full_name":"Ono, Yoshiaki","first_name":"Yoshiaki","last_name":"Ono"},{"full_name":"Fujimoto, Seiji","first_name":"Seiji","last_name":"Fujimoto"},{"full_name":"Inoue, Akio K.","first_name":"Akio K.","last_name":"Inoue"},{"last_name":"Kim","first_name":"Ji Hoon","full_name":"Kim, Ji Hoon"},{"last_name":"Komiyama","first_name":"Yutaka","full_name":"Komiyama, Yutaka"},{"first_name":"Haruka","full_name":"Kusakabe, Haruka","last_name":"Kusakabe"},{"last_name":"Lee","first_name":"Chien-Hsiu","full_name":"Lee, Chien-Hsiu"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"last_name":"Michel-Dansac","full_name":"Michel-Dansac, Leo","first_name":"Leo"},{"first_name":"Tohru","full_name":"Nagao, Tohru","last_name":"Nagao"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"first_name":"Moka","full_name":"Nishigaki, Moka","last_name":"Nishigaki"},{"last_name":"Onodera","first_name":"Masato","full_name":"Onodera, Masato"},{"full_name":"Sugahara, Yuma","first_name":"Yuma","last_name":"Sugahara"},{"last_name":"Xu","first_name":"Yi","full_name":"Xu, Yi"}],"oa":1,"_id":"11509","date_published":"2022-01-31T00:00:00Z","language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ac3509","publisher":"IOP Publishing","year":"2022","type":"journal_article","month":"01","quality_controlled":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"volume":925,"article_type":"original","date_created":"2022-07-06T12:01:48Z","article_number":"111","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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       925","publication_status":"published","oa_version":"Published Version","day":"31","abstract":[{"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.","lang":"eng"}],"date_updated":"2022-07-21T05:51:25Z","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.03850"}],"publication":"The Astrophysical Journal","external_id":{"arxiv":["2108.03850"]},"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","arxiv":1,"citation":{"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>.","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.","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).","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.","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>","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>"},"issue":"2","scopus_import":"1"},{"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","external_id":{"arxiv":["2112.08372"]},"publication":"The Astrophysical Journal","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2112.08372"}],"scopus_import":"1","issue":"2","arxiv":1,"citation":{"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>","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).","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.","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>.","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.","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>."},"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"}],"day":"17","oa_version":"Published Version","publication_status":"published","status":"public","date_updated":"2022-07-19T09:37:42Z","article_type":"original","volume":926,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","month":"02","intvolume":"       926","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","extern":"1","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).","article_number":"117","date_created":"2022-07-06T12:38:42Z","date_published":"2022-02-17T00:00:00Z","_id":"11510","oa":1,"author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"van der Wel","full_name":"van der Wel, Arjen","first_name":"Arjen"},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"last_name":"Bell","first_name":"Eric","full_name":"Bell, Eric"},{"last_name":"Muzzin","full_name":"Muzzin, Adam","first_name":"Adam"},{"last_name":"D’Eugenio","first_name":"Francesco","full_name":"D’Eugenio, Francesco"},{"full_name":"Darvish, Behnam","first_name":"Behnam","last_name":"Darvish"},{"last_name":"Gallazzi","full_name":"Gallazzi, Anna","first_name":"Anna"},{"first_name":"Po-Feng","full_name":"Wu, Po-Feng","last_name":"Wu"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"last_name":"Straatman","first_name":"Caroline","full_name":"Straatman, Caroline"},{"full_name":"van Dokkum, Pieter G.","first_name":"Pieter G.","last_name":"van Dokkum"}],"type":"journal_article","year":"2022","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ac4419","language":[{"iso":"eng"}]},{"date_published":"2022-01-13T00:00:00Z","oa":1,"_id":"11511","author":[{"full_name":"Gebek, Andrea","first_name":"Andrea","last_name":"Gebek"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"}],"type":"journal_article","publisher":"IOP Publishing","year":"2022","language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ac350b","volume":924,"article_type":"original","quality_controlled":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"month":"01","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       924","extern":"1","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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_created":"2022-07-06T12:48:32Z","article_number":"73","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"}],"oa_version":"Published Version","publication_status":"published","day":"13","status":"public","date_updated":"2022-07-19T09:38:03Z","external_id":{"arxiv":["2102.04561"]},"title":"On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation","publication":"The Astrophysical Journal","main_file_link":[{"url":"https://arxiv.org/abs/2102.04561","open_access":"1"}],"issue":"2","scopus_import":"1","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>","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.","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>.","short":"A. Gebek, J.J. Matthee, The Astrophysical Journal 924 (2022).","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>","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.","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>."},"arxiv":1},{"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"}],"day":"24","publication_status":"published","oa_version":"Preprint","status":"public","date_updated":"2022-08-19T09:52:08Z","title":"The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18","external_id":{"arxiv":["2108.05455"]},"publication":"The Astrophysical Journal","main_file_link":[{"url":"https://arxiv.org/abs/2108.05455","open_access":"1"}],"scopus_import":"1","issue":"2","arxiv":1,"citation":{"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>.","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).","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.","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>","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>","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>.","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."},"date_published":"2022-02-24T00:00:00Z","_id":"11601","oa":1,"author":[{"last_name":"Zinn","full_name":"Zinn, Joel C.","first_name":"Joel C."},{"last_name":"Stello","first_name":"Dennis","full_name":"Stello, Dennis"},{"last_name":"Elsworth","full_name":"Elsworth, Yvonne","first_name":"Yvonne"},{"last_name":"García","first_name":"Rafael A.","full_name":"García, Rafael A."},{"full_name":"Kallinger, Thomas","first_name":"Thomas","last_name":"Kallinger"},{"first_name":"Savita","full_name":"Mathur, Savita","last_name":"Mathur"},{"last_name":"Mosser","full_name":"Mosser, Benoît","first_name":"Benoît"},{"first_name":"Marc","full_name":"Hon, Marc","last_name":"Hon"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"Caitlin","full_name":"Jones, Caitlin","last_name":"Jones"},{"last_name":"Reyes","first_name":"Claudia","full_name":"Reyes, Claudia"},{"first_name":"Sanjib","full_name":"Sharma, Sanjib","last_name":"Sharma"},{"full_name":"Schönrich, Ralph","first_name":"Ralph","last_name":"Schönrich"},{"full_name":"Warfield, Jack T.","first_name":"Jack T.","last_name":"Warfield"},{"last_name":"Luger","first_name":"Rodrigo","full_name":"Luger, Rodrigo"},{"first_name":"Andrew","full_name":"Vanderburg, Andrew","last_name":"Vanderburg"},{"last_name":"Kobayashi","full_name":"Kobayashi, Chiaki","first_name":"Chiaki"},{"last_name":"Pinsonneault","first_name":"Marc H.","full_name":"Pinsonneault, Marc H."},{"last_name":"Johnson","first_name":"Jennifer A.","full_name":"Johnson, Jennifer A."},{"last_name":"Huber","first_name":"Daniel","full_name":"Huber, Daniel"},{"first_name":"Sven","full_name":"Buder, Sven","last_name":"Buder"},{"last_name":"Joyce","full_name":"Joyce, Meridith","first_name":"Meridith"},{"full_name":"Bland-Hawthorn, Joss","first_name":"Joss","last_name":"Bland-Hawthorn"},{"first_name":"Luca","full_name":"Casagrande, Luca","last_name":"Casagrande"},{"first_name":"Geraint F.","full_name":"Lewis, Geraint F.","last_name":"Lewis"},{"last_name":"Miglio","full_name":"Miglio, Andrea","first_name":"Andrea"},{"last_name":"Nordlander","full_name":"Nordlander, Thomas","first_name":"Thomas"},{"last_name":"Davies","first_name":"Guy R.","full_name":"Davies, Guy R."},{"last_name":"Silva","full_name":"Silva, Gayandhi De","first_name":"Gayandhi De"},{"last_name":"Chaplin","full_name":"Chaplin, William J.","first_name":"William J."},{"full_name":"Silva Aguirre, Victor","first_name":"Victor","last_name":"Silva Aguirre"}],"type":"journal_article","year":"2022","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ac2c83","language":[{"iso":"eng"}],"article_type":"original","volume":926,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","month":"02","intvolume":"       926","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","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_created":"2022-07-18T10:57:30Z","article_number":"191"},{"arxiv":1,"citation":{"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>.","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).","ista":"Ong JMJ, Bugnet LA, Basu S. 2022. Mode mixing and rotational splittings. I. Near-degeneracy effects revisited. The Astrophysical Journal. 940(1), 18.","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>.","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>","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>"},"scopus_import":"1","issue":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2210.01928"}],"publication":"The Astrophysical Journal","title":"Mode mixing and rotational splittings. I. Near-degeneracy effects revisited","external_id":{"arxiv":["2210.01928"]},"date_updated":"2023-09-06T07:27:45Z","status":"public","day":"16","publication_status":"published","oa_version":"Published Version","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"}],"date_created":"2023-08-01T14:20:41Z","article_number":"18","article_processing_charge":"No","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       940","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"month":"11","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","article_type":"original","volume":940,"doi":"10.3847/1538-4357/ac97e7","language":[{"iso":"eng"}],"year":"2022","publisher":"American Astronomical Society","type":"journal_article","author":[{"last_name":"Ong","first_name":"J. M. Joel","full_name":"Ong, J. M. Joel"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Basu, Sarbani","first_name":"Sarbani","last_name":"Basu"}],"_id":"13445","oa":1,"date_published":"2022-11-16T00:00:00Z"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","article_processing_charge":"No","intvolume":"       941","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_number":"206","date_created":"2023-08-03T10:10:25Z","article_type":"original","volume":941,"month":"12","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","type":"journal_article","doi":"10.3847/1538-4357/aca295","language":[{"iso":"eng"}],"year":"2022","publisher":"American Astronomical Society","date_published":"2022-12-27T00:00:00Z","author":[{"last_name":"Gull","full_name":"Gull, Maude","first_name":"Maude"},{"last_name":"Weisz","first_name":"Daniel R.","full_name":"Weisz, Daniel R."},{"last_name":"Senchyna","full_name":"Senchyna, Peter","first_name":"Peter"},{"last_name":"Sandford","first_name":"Nathan R.","full_name":"Sandford, Nathan R."},{"last_name":"Choi","first_name":"Yumi","full_name":"Choi, Yumi"},{"last_name":"McLeod","first_name":"Anna F.","full_name":"McLeod, Anna F."},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"},{"full_name":"Gilbert, Karoline M.","first_name":"Karoline M.","last_name":"Gilbert"},{"full_name":"Boyer, Martha","first_name":"Martha","last_name":"Boyer"},{"first_name":"Julianne J.","full_name":"Dalcanton, Julianne J.","last_name":"Dalcanton"},{"last_name":"GuhaThakurta","full_name":"GuhaThakurta, Puragra","first_name":"Puragra"},{"last_name":"Goldman","full_name":"Goldman, Steven","first_name":"Steven"},{"first_name":"Paola","full_name":"Marigo, Paola","last_name":"Marigo"},{"first_name":"Kristen B. W.","full_name":"McQuinn, Kristen B. W.","last_name":"McQuinn"},{"last_name":"Pastorelli","first_name":"Giada","full_name":"Pastorelli, Giada"},{"first_name":"Daniel P.","full_name":"Stark, Daniel P.","last_name":"Stark"},{"full_name":"Skillman, Evan","first_name":"Evan","last_name":"Skillman"},{"last_name":"Ting","full_name":"Ting, Yuan-sen","first_name":"Yuan-sen"},{"full_name":"Williams, Benjamin F.","first_name":"Benjamin F.","last_name":"Williams"}],"_id":"13451","oa":1,"scopus_import":"1","issue":"2","citation":{"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.","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>.","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>","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>","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>.","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).","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."},"arxiv":1,"publication":"The Astrophysical Journal","title":"A panchromatic study of massive stars in the extremely metal-poor local group dwarf galaxy Leo A","external_id":{"arxiv":["2211.14349"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/1538-4357/aca295"}],"status":"public","date_updated":"2023-08-21T12:04:58Z","day":"27","oa_version":"Published Version","publication_status":"published","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"}]},{"month":"07","quality_controlled":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_type":"original","volume":916,"article_number":"12","date_created":"2022-07-06T13:05:50Z","acknowledgement":"We would like to thank the referee for a constructive and helpful report. L.A.B. is grateful to Corentin Schreiber for assisting with the near-infrared spectroscopy during the early stages of this work. L.A.B. acknowledges support from the Leids Kerkhoven-Bosscha Fonds under subsidy numbers 18.2.074 and 19.1.147. D.R. acknowledges support from the National Science Foundation under grant numbers AST-1614213 and AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.F. acknowledges the support from grant PRIN MIUR 201720173ML3WW_001. J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020. H.I. acknowledges support from JSPS KAKENHI grant No. JP19K23462. This work is based on observations collected at the European Southern Observatory under ESO programs 094.A-2089(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 099.A-0858(A), and 0101.A-0725(A). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       916","author":[{"first_name":"Leindert A.","full_name":"Boogaard, Leindert A.","last_name":"Boogaard"},{"last_name":"Bouwens","first_name":"Rychard J.","full_name":"Bouwens, Rychard J."},{"first_name":"Dominik","full_name":"Riechers, Dominik","last_name":"Riechers"},{"last_name":"van der Werf","full_name":"van der Werf, Paul","first_name":"Paul"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"last_name":"Stefanon","full_name":"Stefanon, Mauro","first_name":"Mauro"},{"last_name":"Feltre","full_name":"Feltre, Anna","first_name":"Anna"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"first_name":"Hanae","full_name":"Inami, Hanae","last_name":"Inami"},{"last_name":"Aravena","first_name":"Manuel","full_name":"Aravena, Manuel"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Carilli","full_name":"Carilli, Chris","first_name":"Chris"},{"last_name":"Contini","full_name":"Contini, Thierry","first_name":"Thierry"},{"last_name":"Decarli","full_name":"Decarli, Roberto","first_name":"Roberto"},{"last_name":"González-López","full_name":"González-López, Jorge","first_name":"Jorge"},{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"}],"oa":1,"_id":"11512","date_published":"2021-07-20T00:00:00Z","language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ac01d7","publisher":"IOP Publishing","year":"2021","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/2105.12489","open_access":"1"}],"publication":"The Astrophysical Journal","external_id":{"arxiv":["2105.12489"]},"title":"Measuring the average molecular gas content of star-forming galaxies at z = 3–4","arxiv":1,"citation":{"ieee":"L. A. Boogaard <i>et al.</i>, “Measuring the average molecular gas content of star-forming galaxies at z = 3–4,” <i>The Astrophysical Journal</i>, vol. 916, no. 1. IOP Publishing, 2021.","chicago":"Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” <i>The Astrophysical Journal</i>. IOP Publishing, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">https://doi.org/10.3847/1538-4357/ac01d7</a>.","ama":"Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. <i>The Astrophysical Journal</i>. 2021;916(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">10.3847/1538-4357/ac01d7</a>","mla":"Boogaard, Leindert A., et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” <i>The Astrophysical Journal</i>, vol. 916, no. 1, 12, IOP Publishing, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">10.3847/1538-4357/ac01d7</a>.","short":"L.A. Boogaard, R.J. Bouwens, D. Riechers, P. van der Werf, R. Bacon, J.J. Matthee, M. Stefanon, A. Feltre, M. Maseda, H. Inami, M. Aravena, J. Brinchmann, C. Carilli, T. Contini, R. Decarli, J. González-López, T. Nanayakkara, F. Walter, The Astrophysical Journal 916 (2021).","apa":"Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R., Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content of star-forming galaxies at z = 3–4. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">https://doi.org/10.3847/1538-4357/ac01d7</a>","ista":"Boogaard LA, Bouwens RJ, Riechers D, van der Werf P, Bacon R, Matthee JJ, Stefanon M, Feltre A, Maseda M, Inami H, Aravena M, Brinchmann J, Carilli C, Contini T, Decarli R, González-López J, Nanayakkara T, Walter F. 2021. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. 916(1), 12."},"issue":"1","scopus_import":"1","oa_version":"Preprint","publication_status":"published","day":"20","abstract":[{"lang":"eng","text":"We study the molecular gas content of 24 star-forming galaxies at z = 3–4, with a median stellar mass of 109.1 M⊙, from the MUSE Hubble Ultra Deep Field (HUDF) Survey. Selected by their Lyα λ1216 emission and HF160W-band magnitude, the galaxies show an average $\\langle {\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\rangle \\approx 20$ Å, below the typical selection threshold for Lyα emitters (${\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\gt 25$ Å), and a rest-frame UV spectrum similar to Lyman-break galaxies. We use rest-frame optical spectroscopy from KMOS and MOSFIRE, and the UV features observed with MUSE, to determine the systemic redshifts, which are offset from Lyα by 〈Δv(Lyα)〉 = 346 km s−1, with a 100 to 600 km s−1 range. Stacking 12CO J = 4 → 3 and [C i]3P1 → 3P0 (and higher-J CO lines) from the ALMA Spectroscopic Survey of the HUDF, we determine 3σ upper limits on the line luminosities of 4.0 × 108 K km s−1pc2 and 5.6 × 108 K km s−1pc2, respectively (for a 300 km s−1 line width). Stacking the 1.2 mm and 3 mm dust-continuum flux densities, we find a 3σ upper limits of 9 μJy and 1.2 μJy, respectively. The inferred gas fractions, under the assumption of a \"Galactic\" CO-to-H2 conversion factor and gas-to-dust ratio, are in tension with previously determined scaling relations. This implies a substantially higher αCO ≥ 10 and δGDR ≥ 1200, consistent with the subsolar metallicity estimated for these galaxies ($12+\\mathrm{log}({\\rm{O}}/{\\rm{H}})\\approx 7.8\\pm 0.2$). The low metallicity of z ≥ 3 star-forming galaxies may thus make it very challenging to unveil their cold gas through CO or dust emission, warranting further exploration of alternative tracers, such as [C ii]."}],"date_updated":"2022-07-19T09:32:48Z","status":"public"},{"language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ac29c5","publisher":"American Astronomical Society","year":"2021","type":"journal_article","author":[{"last_name":"Renzo","full_name":"Renzo, M.","first_name":"M."},{"full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","orcid":"0000-0002-6960-6911"}],"oa":1,"_id":"13453","date_published":"2021-12-29T00:00:00Z","date_created":"2023-08-03T10:10:48Z","article_number":"277","article_processing_charge":"No","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       923","month":"12","quality_controlled":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"volume":923,"article_type":"original","date_updated":"2023-08-21T11:59:34Z","status":"public","oa_version":"Preprint","publication_status":"published","day":"29","abstract":[{"lang":"eng","text":"Most massive stars are born in binaries close enough for mass transfer episodes. These modify the appearance, structure, and future evolution of both stars. We compute the evolution of a 100-day-period binary, consisting initially of a 25 M⊙ star and a 17 M⊙ star, which experiences stable mass transfer. We focus on the impact of mass accretion on the surface composition, internal rotation, and structure of the accretor. To anchor our models, we show that our accretor broadly reproduces the properties of ζ Ophiuchi, which has long been proposed to have accreted mass before being ejected as a runaway star when the companion exploded. We compare our accretor to models of single rotating stars and find that the later and stronger spin-up provided by mass accretion produces significant differences. Specifically, the core of the accretor retains higher spin at the end of the main sequence, and a convective layer develops that changes its density profile. Moreover, the surface of the accretor star is polluted by CNO-processed material donated by the companion. Our models show effects of mass accretion in binaries that are not captured in single rotating stellar models. This possibly impacts the further evolution (either in a binary or as single stars), the final collapse, and the resulting spin of the compact object."}],"citation":{"ieee":"M. Renzo and Y. L. L. Götberg, “Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi,” <i>The Astrophysical Journal</i>, vol. 923, no. 2. American Astronomical Society, 2021.","chicago":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac29c5\">https://doi.org/10.3847/1538-4357/ac29c5</a>.","ama":"Renzo M, Götberg YLL. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. <i>The Astrophysical Journal</i>. 2021;923(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac29c5\">10.3847/1538-4357/ac29c5</a>","short":"M. Renzo, Y.L.L. Götberg, The Astrophysical Journal 923 (2021).","ista":"Renzo M, Götberg YLL. 2021. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 923(2), 277.","mla":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” <i>The Astrophysical Journal</i>, vol. 923, no. 2, 277, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac29c5\">10.3847/1538-4357/ac29c5</a>.","apa":"Renzo, M., &#38; Götberg, Y. L. L. (2021). Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ac29c5\">https://doi.org/10.3847/1538-4357/ac29c5</a>"},"arxiv":1,"issue":"2","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2107.10933"}],"publication":"The Astrophysical Journal","external_id":{"arxiv":["2107.10933"]},"title":"Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi"},{"date_created":"2023-08-03T10:10:58Z","article_number":"241","intvolume":"       922","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","article_processing_charge":"No","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","month":"12","article_type":"original","volume":922,"year":"2021","publisher":"American Astronomical Society","doi":"10.3847/1538-4357/ac27ae","language":[{"iso":"eng"}],"type":"journal_article","_id":"13454","oa":1,"author":[{"full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny","last_name":"Wong"},{"last_name":"Schwab","first_name":"Josiah","full_name":"Schwab, Josiah"},{"orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"}],"date_published":"2021-12-03T00:00:00Z","citation":{"chicago":"Wong, Tin Long Sunny, Josiah Schwab, and Ylva Louise Linsdotter Götberg. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">https://doi.org/10.3847/1538-4357/ac27ae</a>.","ieee":"T. L. S. Wong, J. Schwab, and Y. L. L. Götberg, “Pre-explosion properties of Helium star donors to thermonuclear supernovae,” <i>The Astrophysical Journal</i>, vol. 922, no. 2. American Astronomical Society, 2021.","ista":"Wong TLS, Schwab J, Götberg YLL. 2021. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 922(2), 241.","apa":"Wong, T. L. S., Schwab, J., &#38; Götberg, Y. L. L. (2021). Pre-explosion properties of Helium star donors to thermonuclear supernovae. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">https://doi.org/10.3847/1538-4357/ac27ae</a>","mla":"Wong, Tin Long Sunny, et al. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” <i>The Astrophysical Journal</i>, vol. 922, no. 2, 241, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">10.3847/1538-4357/ac27ae</a>.","short":"T.L.S. Wong, J. Schwab, Y.L.L. Götberg, The Astrophysical Journal 922 (2021).","ama":"Wong TLS, Schwab J, Götberg YLL. Pre-explosion properties of Helium star donors to thermonuclear supernovae. <i>The Astrophysical Journal</i>. 2021;922(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">10.3847/1538-4357/ac27ae</a>"},"arxiv":1,"scopus_import":"1","issue":"2","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2109.14817"}],"title":"Pre-explosion properties of Helium star donors to thermonuclear supernovae","external_id":{"arxiv":["2109.14817"]},"publication":"The Astrophysical Journal","date_updated":"2023-08-21T11:52:05Z","status":"public","abstract":[{"text":"Helium star–carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code MESA, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to near-UV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultra-massive WD in a multiday orbit. However, extending our binary models to initial CO WD masses of up to 1.2 M⊙, we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star–WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition.","lang":"eng"}],"day":"03","publication_status":"published","oa_version":"Preprint"},{"scopus_import":"1","issue":"1","citation":{"chicago":"Berzin, Elizabeth, Amy Secunda, Renyue Cen, Alexander Menegas, and Ylva Louise Linsdotter Götberg. “Spectral Signatures of Population III and Envelope-Stripped Stars in Galaxies at the Epoch of Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac0af6\">https://doi.org/10.3847/1538-4357/ac0af6</a>.","ieee":"E. Berzin, A. Secunda, R. Cen, A. Menegas, and Y. L. L. Götberg, “Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization,” <i>The Astrophysical Journal</i>, vol. 918, no. 1. American Astronomical Society, 2021.","apa":"Berzin, E., Secunda, A., Cen, R., Menegas, A., &#38; Götberg, Y. L. L. (2021). Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ac0af6\">https://doi.org/10.3847/1538-4357/ac0af6</a>","mla":"Berzin, Elizabeth, et al. “Spectral Signatures of Population III and Envelope-Stripped Stars in Galaxies at the Epoch of Reionization.” <i>The Astrophysical Journal</i>, vol. 918, no. 1, 5, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac0af6\">10.3847/1538-4357/ac0af6</a>.","short":"E. Berzin, A. Secunda, R. Cen, A. Menegas, Y.L.L. Götberg, The Astrophysical Journal 918 (2021).","ista":"Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. 2021. Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. The Astrophysical Journal. 918(1), 5.","ama":"Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization. <i>The Astrophysical Journal</i>. 2021;918(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac0af6\">10.3847/1538-4357/ac0af6</a>"},"arxiv":1,"publication":"The Astrophysical Journal","title":"Spectral signatures of population III and envelope-stripped stars in galaxies at the epoch of reionization","external_id":{"arxiv":["2102.08408"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/1538-4357/ac0af6"}],"status":"public","date_updated":"2023-08-21T11:44:50Z","day":"27","oa_version":"Published Version","publication_status":"published","abstract":[{"text":"While most simulations of the epoch of reionization have focused on single-stellar populations in star-forming dwarf galaxies, products of binary evolution are expected to significantly contribute to emissions of hydrogen-ionizing photons. Among these products are stripped stars (or helium stars), which have their envelopes stripped from interactions with binary companions, leaving an exposed helium core. Previous work has suggested these stripped stars can dominate the Lyman Continuum (LyC) photon output of high-redshift, low-luminosity galaxies post-starburst. Other sources of hard radiation in the early universe include zero-metallicity Population iii stars, which may have similar spectral energy distribution (SED) properties to galaxies with radiation dominated by stripped-star emissions. Here, we use four metrics (the power-law exponent over wavelength intervals 240–500 Å, 600–900 Å, and 1200–2000 Å, and the ratio of total luminosity in FUV wavelengths to LyC wavelengths) to compare the SEDs of simulated galaxies with only single-stellar evolution, galaxies containing stripped stars, and galaxies containing Population iii stars, with four different initial mass functions (IMFs). We find that stripped stars significantly alter SEDs in the LyC range of galaxies at the epoch of reionization. SEDs in galaxies with stripped stars have lower power-law indices in the LyC range and lower FUV to LyC luminosity ratios. These differences in SEDs are present at all considered luminosities (${M}_{\\mathrm{UV}}\\gt -15$, AB system), and are most pronounced for lower-luminosity galaxies. Intrinsic SEDs as well as those with interstellar medium absorption of galaxies with stripped stars and Population iii stars are found to be distinct for all tested Population iii IMFs.","lang":"eng"}],"article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","intvolume":"       918","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_number":"5","date_created":"2023-08-03T10:11:24Z","article_type":"original","volume":918,"month":"08","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","type":"journal_article","doi":"10.3847/1538-4357/ac0af6","language":[{"iso":"eng"}],"year":"2021","publisher":"American Astronomical Society","date_published":"2021-08-27T00:00:00Z","author":[{"first_name":"Elizabeth","full_name":"Berzin, Elizabeth","last_name":"Berzin"},{"last_name":"Secunda","first_name":"Amy","full_name":"Secunda, Amy"},{"full_name":"Cen, Renyue","first_name":"Renyue","last_name":"Cen"},{"last_name":"Menegas","first_name":"Alexander","full_name":"Menegas, Alexander"},{"full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg"}],"_id":"13456","oa":1},{"scopus_import":"1","issue":"1","arxiv":1,"citation":{"ama":"Darvish B, Scoville NZ, Martin C, et al. Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. <i>The Astrophysical Journal</i>. 2020;892(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab75c3\">10.3847/1538-4357/ab75c3</a>","apa":"Darvish, B., Scoville, N. Z., Martin, C., Sobral, D., Mobasher, B., Rettura, A., … Cucciati, O. (2020). Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab75c3\">https://doi.org/10.3847/1538-4357/ab75c3</a>","mla":"Darvish, Behnam, et al. “Spectroscopic Confirmation of a Coma Cluster Progenitor at z ∼ 2.2.” <i>The Astrophysical Journal</i>, vol. 892, no. 1, 8, IOP Publishing, 2020, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab75c3\">10.3847/1538-4357/ab75c3</a>.","ista":"Darvish B, Scoville NZ, Martin C, Sobral D, Mobasher B, Rettura A, Matthee JJ, Capak P, Chartab N, Hemmati S, Masters D, Nayyeri H, O’Sullivan D, Paulino-Afonso A, Sattari Z, Shahidi A, Salvato M, Lemaux BC, Fèvre OL, Cucciati O. 2020. Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. The Astrophysical Journal. 892(1), 8.","short":"B. Darvish, N.Z. Scoville, C. Martin, D. Sobral, B. Mobasher, A. Rettura, J.J. Matthee, P. Capak, N. Chartab, S. Hemmati, D. Masters, H. Nayyeri, D. O’Sullivan, A. Paulino-Afonso, Z. Sattari, A. Shahidi, M. Salvato, B.C. Lemaux, O.L. Fèvre, O. Cucciati, The Astrophysical Journal 892 (2020).","ieee":"B. Darvish <i>et al.</i>, “Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2,” <i>The Astrophysical Journal</i>, vol. 892, no. 1. IOP Publishing, 2020.","chicago":"Darvish, Behnam, Nick Z. Scoville, Christopher Martin, David Sobral, Bahram Mobasher, Alessandro Rettura, Jorryt J Matthee, et al. “Spectroscopic Confirmation of a Coma Cluster Progenitor at z ∼ 2.2.” <i>The Astrophysical Journal</i>. IOP Publishing, 2020. <a href=\"https://doi.org/10.3847/1538-4357/ab75c3\">https://doi.org/10.3847/1538-4357/ab75c3</a>."},"title":"Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2","external_id":{"arxiv":["2002.06207"]},"publication":"The Astrophysical Journal","main_file_link":[{"url":"https://arxiv.org/abs/2002.06207","open_access":"1"}],"status":"public","date_updated":"2022-07-19T09:31:35Z","abstract":[{"lang":"eng","text":"We report the spectroscopic confirmation of a new protocluster in the COSMOS field at z ∼ 2.2, COSMOS Cluster 2.2 (CC2.2), originally identified as an overdensity of narrowband selected Hα emitting candidates. With only two masks of Keck/MOSFIRE near-IR spectroscopy in both H (∼1.47–1.81 μm) and K (∼1.92–2.40 μm) bands (∼1.5 hr each), we confirm 35 unique protocluster members with at least two emission lines detected with S/N > 3. Combined with 12 extra members from the zCOSMOS-deep spectroscopic survey (47 in total), we estimate a mean redshift and a line-of-sight velocity dispersion of zmean = 2.23224 ± 0.00101 and σlos = 645 ± 69 km s−1 for this protocluster, respectively. Assuming virialization and spherical symmetry for the system, we estimate a total mass of Mvir ∼ (1–2) ×1014M⊙ for the structure. We evaluate a number density enhancement of δg ∼ 7 for this system and we argue that the structure is likely not fully virialized at z ∼ 2.2. However, in a spherical collapse model, δg is expected to grow to a linear matter enhancement of ∼1.9 by z = 0, exceeding the collapse threshold of 1.69, and leading to a fully collapsed and virialized Coma-type structure with a total mass of Mdyn(z = 0) ∼ 9.2 × 1014M⊙ by now. This observationally efficient confirmation suggests that large narrowband emission-line galaxy surveys, when combined with ancillary photometric data, can be used to effectively trace the large-scale structure and protoclusters at a time when they are mostly dominated by star-forming galaxies."}],"day":"19","publication_status":"published","oa_version":"Preprint","intvolume":"       892","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","acknowledgement":"We are thankful to the anonymous referee for useful comments and suggestions that improved the quality of this paper. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. B.D. is thankful to Andreas Faisst, Laura Danly, and Matthew Burlando for their companionship during the observing run. B.D. is grateful to the COSMOS team for their useful comments during the team meeting in New York City 2019 May 14–17. A.R. research was made possible by Friends of W. M. Keck Observatory who philanthropically support the Keck Science Collaborative (KSC) fund. The observations presented herein were obtained at the W. M. Keck Observatory (program C236, PI Scoville), which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors would like to recognize and acknowledge the very prominent cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are fortunate to have the opportunity to perform observations from this mountain.","date_created":"2022-07-06T13:10:51Z","article_number":"8","volume":892,"article_type":"original","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","month":"03","type":"journal_article","year":"2020","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ab75c3","language":[{"iso":"eng"}],"date_published":"2020-03-19T00:00:00Z","_id":"11513","oa":1,"author":[{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Scoville","full_name":"Scoville, Nick Z.","first_name":"Nick Z."},{"first_name":"Christopher","full_name":"Martin, Christopher","last_name":"Martin"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"last_name":"Rettura","full_name":"Rettura, Alessandro","first_name":"Alessandro"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Capak","full_name":"Capak, Peter","first_name":"Peter"},{"first_name":"Nima","full_name":"Chartab, Nima","last_name":"Chartab"},{"first_name":"Shoubaneh","full_name":"Hemmati, Shoubaneh","last_name":"Hemmati"},{"full_name":"Masters, Daniel","first_name":"Daniel","last_name":"Masters"},{"last_name":"Nayyeri","first_name":"Hooshang","full_name":"Nayyeri, Hooshang"},{"last_name":"O’Sullivan","first_name":"Donal","full_name":"O’Sullivan, Donal"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"last_name":"Sattari","full_name":"Sattari, Zahra","first_name":"Zahra"},{"last_name":"Shahidi","full_name":"Shahidi, Abtin","first_name":"Abtin"},{"first_name":"Mara","full_name":"Salvato, Mara","last_name":"Salvato"},{"last_name":"Lemaux","first_name":"Brian C.","full_name":"Lemaux, Brian C."},{"first_name":"Olivier Le","full_name":"Fèvre, Olivier Le","last_name":"Fèvre"},{"last_name":"Cucciati","full_name":"Cucciati, Olga","first_name":"Olga"}]},{"arxiv":1,"citation":{"chicago":"Aguirre, Víctor Silva, Dennis Stello, Amalie Stokholm, Jakob R. Mosumgaard, Warrick H. Ball, Sarbani Basu, Diego Bossini, et al. “Detection and Characterization of Oscillating Red Giants: First Results from the TESS Satellite.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2020. <a href=\"https://doi.org/10.3847/2041-8213/ab6443\">https://doi.org/10.3847/2041-8213/ab6443</a>.","ieee":"V. S. Aguirre <i>et al.</i>, “Detection and characterization of oscillating red giants: First results from the TESS satellite,” <i>The Astrophysical Journal Letters</i>, vol. 889, no. 2. IOP Publishing, 2020.","ista":"Aguirre VS, Stello D, Stokholm A, Mosumgaard JR, Ball WH, Basu S, Bossini D, Bugnet LA, Buzasi D, Campante TL, Carboneau L, Chaplin WJ, Corsaro E, Davies GR, Elsworth Y, García RA, Gaulme P, Hall OJ, Handberg R, Hon M, Kallinger T, Kang L, Lund MN, Mathur S, Mints A, Mosser B, Çelik Orhan Z, Rodrigues TS, Vrard M, Yıldız M, Zinn JC, Örtel S, Beck PG, Bell KJ, Guo Z, Jiang C, Kuszlewicz JS, Kuehn CA, Li T, Lundkvist MS, Pinsonneault M, Tayar J, Cunha MS, Hekker S, Huber D, Miglio A, F. G. Monteiro MJP, Slumstrup D, Winther ML, Angelou G, Benomar O, Bódi A, De Moura BL, Deheuvels S, Derekas A, Di Mauro MP, Dupret M-A, Jiménez A, Lebreton Y, Matthews J, Nardetto N, do Nascimento JD, Pereira F, Rodríguez Díaz LF, Serenelli AM, Spitoni E, Stonkutė E, Suárez JC, Szabó R, Van Eylen V, Ventura R, Verma K, Weiss A, Wu T, Barclay T, Christensen-Dalsgaard J, Jenkins JM, Kjeldsen H, Ricker GR, Seager S, Vanderspek R. 2020. Detection and characterization of oscillating red giants: First results from the TESS satellite. The Astrophysical Journal Letters. 889(2), L34.","mla":"Aguirre, Víctor Silva, et al. “Detection and Characterization of Oscillating Red Giants: First Results from the TESS Satellite.” <i>The Astrophysical Journal Letters</i>, vol. 889, no. 2, L34, IOP Publishing, 2020, doi:<a href=\"https://doi.org/10.3847/2041-8213/ab6443\">10.3847/2041-8213/ab6443</a>.","short":"V.S. Aguirre, D. Stello, A. Stokholm, J.R. Mosumgaard, W.H. Ball, S. Basu, D. Bossini, L.A. Bugnet, D. Buzasi, T.L. Campante, L. Carboneau, W.J. Chaplin, E. Corsaro, G.R. Davies, Y. Elsworth, R.A. García, P. Gaulme, O.J. Hall, R. Handberg, M. Hon, T. Kallinger, L. Kang, M.N. Lund, S. Mathur, A. Mints, B. Mosser, Z. Çelik Orhan, T.S. Rodrigues, M. Vrard, M. Yıldız, J.C. Zinn, S. Örtel, P.G. Beck, K.J. Bell, Z. Guo, C. Jiang, J.S. Kuszlewicz, C.A. Kuehn, T. Li, M.S. Lundkvist, M. Pinsonneault, J. Tayar, M.S. Cunha, S. Hekker, D. Huber, A. Miglio, M.J.P. F. G. Monteiro, D. Slumstrup, M.L. Winther, G. Angelou, O. Benomar, A. Bódi, B.L. De Moura, S. Deheuvels, A. Derekas, M.P. Di Mauro, M.-A. Dupret, A. Jiménez, Y. Lebreton, J. Matthews, N. Nardetto, J.D. do Nascimento, F. Pereira, L.F. Rodríguez Díaz, A.M. Serenelli, E. Spitoni, E. Stonkutė, J.C. Suárez, R. Szabó, V. Van Eylen, R. Ventura, K. Verma, A. Weiss, T. Wu, T. Barclay, J. Christensen-Dalsgaard, J.M. Jenkins, H. Kjeldsen, G.R. Ricker, S. Seager, R. Vanderspek, The Astrophysical Journal Letters 889 (2020).","apa":"Aguirre, V. S., Stello, D., Stokholm, A., Mosumgaard, J. R., Ball, W. H., Basu, S., … Vanderspek, R. (2020). Detection and characterization of oscillating red giants: First results from the TESS satellite. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ab6443\">https://doi.org/10.3847/2041-8213/ab6443</a>","ama":"Aguirre VS, Stello D, Stokholm A, et al. Detection and characterization of oscillating red giants: First results from the TESS satellite. <i>The Astrophysical Journal Letters</i>. 2020;889(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ab6443\">10.3847/2041-8213/ab6443</a>"},"issue":"2","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1912.07604"}],"publication":"The Astrophysical Journal Letters","external_id":{"arxiv":["1912.07604"]},"title":"Detection and characterization of oscillating red giants: First results from the TESS satellite","date_updated":"2022-08-22T07:25:51Z","status":"public","publication_status":"published","oa_version":"Preprint","day":"01","abstract":[{"text":"Since the onset of the \"space revolution\" of high-precision high-cadence photometry, asteroseismology has been demonstrated as a powerful tool for informing Galactic archeology investigations. The launch of the NASA Transiting Exoplanet Survey Satellite (TESS) mission has enabled seismic-based inferences to go full sky—providing a clear advantage for large ensemble studies of the different Milky Way components. Here we demonstrate its potential for investigating the Galaxy by carrying out the first asteroseismic ensemble study of red giant stars observed by TESS. We use a sample of 25 stars for which we measure their global asteroseimic observables and estimate their fundamental stellar properties, such as radius, mass, and age. Significant improvements are seen in the uncertainties of our estimates when combining seismic observables from TESS with astrometric measurements from the Gaia mission compared to when the seismology and astrometry are applied separately. Specifically, when combined we show that stellar radii can be determined to a precision of a few percent, masses to 5%–10%, and ages to the 20% level. This is comparable to the precision typically obtained using end-of-mission Kepler data.","lang":"eng"}],"article_number":"L34","date_created":"2022-07-18T13:52:54Z","acknowledgement":"This Letter includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (grant agreement No. DNRF106), ESA PRODEX (PEA 4000119301), and Stellar Astrophysics Centre (SAC) at Aarhus University. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.B. is supported in the form of work contract FCT/MCTES through national funds and by FEDER through COMPETE2020 in connection to these grants: UID/FIS/04434/2019; PTDC/FIS-AST/30389/2017 & POCI-01-0145-FEDER-030389. L.B., R.A.G., and B.M. acknowledge the support from the CNES/PLATO grant. D.B. acknowledges NASA grant NNX16AB76G. T.L.C. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). This work was supported by FCT/MCTES through national funds (UID/FIS/04434/2019). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 664931. R.H. and M.N.L. acknowledge the support of the ESA PRODEX programme. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). K.J.B. is supported by the National Science Foundation under Award AST-1903828. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). M.C. is funded by FCT//MCTES through national funds and by FEDER through COMPETE2020 through these grants: UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017 & POCI-01-0145-FEDER-030389, CEECIND/02619/2017. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no 338251 (StellarAges). A.M. acknowledges support from the European Research Council Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement No. 772293, http://www.asterochronometry.eu). A.M.S. is partially supported by MINECO grant ESP2017-82674-R. J.C.S. acknowledges funding support from Spanish public funds for research under projects ESP2017-87676-2-2, and from project RYC-2012-09913 under the 'Ramón y Cajal' program of the Spanish Ministry of Science and Education. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.","extern":"1","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       889","month":"02","quality_controlled":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"volume":889,"article_type":"original","language":[{"iso":"eng"}],"doi":"10.3847/2041-8213/ab6443","publisher":"IOP Publishing","year":"2020","type":"journal_article","author":[{"last_name":"Aguirre","full_name":"Aguirre, Víctor Silva","first_name":"Víctor Silva"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"last_name":"Stokholm","full_name":"Stokholm, Amalie","first_name":"Amalie"},{"last_name":"Mosumgaard","full_name":"Mosumgaard, Jakob R.","first_name":"Jakob R."},{"full_name":"Ball, Warrick H.","first_name":"Warrick H.","last_name":"Ball"},{"last_name":"Basu","full_name":"Basu, Sarbani","first_name":"Sarbani"},{"last_name":"Bossini","full_name":"Bossini, Diego","first_name":"Diego"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle"},{"first_name":"Derek","full_name":"Buzasi, Derek","last_name":"Buzasi"},{"full_name":"Campante, Tiago L.","first_name":"Tiago L.","last_name":"Campante"},{"last_name":"Carboneau","full_name":"Carboneau, Lindsey","first_name":"Lindsey"},{"last_name":"Chaplin","first_name":"William J.","full_name":"Chaplin, William J."},{"full_name":"Corsaro, Enrico","first_name":"Enrico","last_name":"Corsaro"},{"first_name":"Guy R.","full_name":"Davies, Guy R.","last_name":"Davies"},{"full_name":"Elsworth, Yvonne","first_name":"Yvonne","last_name":"Elsworth"},{"full_name":"García, Rafael A.","first_name":"Rafael A.","last_name":"García"},{"last_name":"Gaulme","first_name":"Patrick","full_name":"Gaulme, Patrick"},{"full_name":"Hall, Oliver J.","first_name":"Oliver J.","last_name":"Hall"},{"last_name":"Handberg","full_name":"Handberg, Rasmus","first_name":"Rasmus"},{"last_name":"Hon","full_name":"Hon, Marc","first_name":"Marc"},{"last_name":"Kallinger","first_name":"Thomas","full_name":"Kallinger, Thomas"},{"full_name":"Kang, Liu","first_name":"Liu","last_name":"Kang"},{"first_name":"Mikkel N.","full_name":"Lund, Mikkel N.","last_name":"Lund"},{"full_name":"Mathur, Savita","first_name":"Savita","last_name":"Mathur"},{"first_name":"Alexey","full_name":"Mints, Alexey","last_name":"Mints"},{"last_name":"Mosser","first_name":"Benoit","full_name":"Mosser, Benoit"},{"first_name":"Zeynep","full_name":"Çelik Orhan, Zeynep","last_name":"Çelik Orhan"},{"first_name":"Thaíse S.","full_name":"Rodrigues, Thaíse S.","last_name":"Rodrigues"},{"first_name":"Mathieu","full_name":"Vrard, Mathieu","last_name":"Vrard"},{"last_name":"Yıldız","full_name":"Yıldız, Mutlu","first_name":"Mutlu"},{"last_name":"Zinn","full_name":"Zinn, Joel C.","first_name":"Joel C."},{"full_name":"Örtel, Sibel","first_name":"Sibel","last_name":"Örtel"},{"full_name":"Beck, Paul G.","first_name":"Paul G.","last_name":"Beck"},{"last_name":"Bell","first_name":"Keaton J.","full_name":"Bell, Keaton J."},{"last_name":"Guo","full_name":"Guo, Zhao","first_name":"Zhao"},{"first_name":"Chen","full_name":"Jiang, Chen","last_name":"Jiang"},{"last_name":"Kuszlewicz","first_name":"James S.","full_name":"Kuszlewicz, James S."},{"last_name":"Kuehn","full_name":"Kuehn, Charles A.","first_name":"Charles A."},{"full_name":"Li, Tanda","first_name":"Tanda","last_name":"Li"},{"first_name":"Mia S.","full_name":"Lundkvist, Mia S.","last_name":"Lundkvist"},{"last_name":"Pinsonneault","full_name":"Pinsonneault, Marc","first_name":"Marc"},{"last_name":"Tayar","full_name":"Tayar, Jamie","first_name":"Jamie"},{"first_name":"Margarida S.","full_name":"Cunha, Margarida S.","last_name":"Cunha"},{"first_name":"Saskia","full_name":"Hekker, Saskia","last_name":"Hekker"},{"full_name":"Huber, Daniel","first_name":"Daniel","last_name":"Huber"},{"last_name":"Miglio","first_name":"Andrea","full_name":"Miglio, Andrea"},{"first_name":"Mario J. P.","full_name":"F. G. Monteiro, Mario J. P.","last_name":"F. G. Monteiro"},{"first_name":"Ditte","full_name":"Slumstrup, Ditte","last_name":"Slumstrup"},{"last_name":"Winther","first_name":"Mark L.","full_name":"Winther, Mark L."},{"first_name":"George","full_name":"Angelou, George","last_name":"Angelou"},{"full_name":"Benomar, Othman","first_name":"Othman","last_name":"Benomar"},{"full_name":"Bódi, Attila","first_name":"Attila","last_name":"Bódi"},{"last_name":"De Moura","first_name":"Bruno L.","full_name":"De Moura, Bruno L."},{"full_name":"Deheuvels, Sébastien","first_name":"Sébastien","last_name":"Deheuvels"},{"last_name":"Derekas","full_name":"Derekas, Aliz","first_name":"Aliz"},{"last_name":"Di Mauro","full_name":"Di Mauro, Maria Pia","first_name":"Maria Pia"},{"full_name":"Dupret, Marc-Antoine","first_name":"Marc-Antoine","last_name":"Dupret"},{"last_name":"Jiménez","first_name":"Antonio","full_name":"Jiménez, Antonio"},{"full_name":"Lebreton, Yveline","first_name":"Yveline","last_name":"Lebreton"},{"last_name":"Matthews","full_name":"Matthews, Jaymie","first_name":"Jaymie"},{"last_name":"Nardetto","full_name":"Nardetto, Nicolas","first_name":"Nicolas"},{"last_name":"do Nascimento","full_name":"do Nascimento, Jose D.","first_name":"Jose D."},{"last_name":"Pereira","full_name":"Pereira, Filipe","first_name":"Filipe"},{"last_name":"Rodríguez Díaz","full_name":"Rodríguez Díaz, Luisa F.","first_name":"Luisa F."},{"last_name":"Serenelli","first_name":"Aldo M.","full_name":"Serenelli, Aldo M."},{"last_name":"Spitoni","full_name":"Spitoni, Emanuele","first_name":"Emanuele"},{"last_name":"Stonkutė","first_name":"Edita","full_name":"Stonkutė, Edita"},{"last_name":"Suárez","first_name":"Juan Carlos","full_name":"Suárez, Juan Carlos"},{"last_name":"Szabó","first_name":"Robert","full_name":"Szabó, Robert"},{"first_name":"Vincent","full_name":"Van Eylen, Vincent","last_name":"Van Eylen"},{"first_name":"Rita","full_name":"Ventura, Rita","last_name":"Ventura"},{"last_name":"Verma","first_name":"Kuldeep","full_name":"Verma, Kuldeep"},{"first_name":"Achim","full_name":"Weiss, Achim","last_name":"Weiss"},{"last_name":"Wu","full_name":"Wu, Tao","first_name":"Tao"},{"full_name":"Barclay, Thomas","first_name":"Thomas","last_name":"Barclay"},{"full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen","last_name":"Christensen-Dalsgaard"},{"first_name":"Jon M.","full_name":"Jenkins, Jon M.","last_name":"Jenkins"},{"full_name":"Kjeldsen, Hans","first_name":"Hans","last_name":"Kjeldsen"},{"first_name":"George R.","full_name":"Ricker, George R.","last_name":"Ricker"},{"first_name":"Sara","full_name":"Seager, Sara","last_name":"Seager"},{"first_name":"Roland","full_name":"Vanderspek, Roland","last_name":"Vanderspek"}],"oa":1,"_id":"11612","date_published":"2020-02-01T00:00:00Z"},{"scopus_import":"1","issue":"1","citation":{"chicago":"Götberg, Ylva Louise Linsdotter, V. Korol, A. Lamberts, T. Kupfer, K. Breivik, B. Ludwig, and M. R. Drout. “Stars Stripped in Binaries: The Living Gravitational-Wave Sources.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2020. <a href=\"https://doi.org/10.3847/1538-4357/abbda5\">https://doi.org/10.3847/1538-4357/abbda5</a>.","ieee":"Y. L. L. Götberg <i>et al.</i>, “Stars stripped in binaries: The living gravitational-wave sources,” <i>The Astrophysical Journal</i>, vol. 904, no. 1. American Astronomical Society, 2020.","apa":"Götberg, Y. L. L., Korol, V., Lamberts, A., Kupfer, T., Breivik, K., Ludwig, B., &#38; Drout, M. R. (2020). Stars stripped in binaries: The living gravitational-wave sources. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/abbda5\">https://doi.org/10.3847/1538-4357/abbda5</a>","ista":"Götberg YLL, Korol V, Lamberts A, Kupfer T, Breivik K, Ludwig B, Drout MR. 2020. Stars stripped in binaries: The living gravitational-wave sources. The Astrophysical Journal. 904(1), 56.","mla":"Götberg, Ylva Louise Linsdotter, et al. “Stars Stripped in Binaries: The Living Gravitational-Wave Sources.” <i>The Astrophysical Journal</i>, vol. 904, no. 1, 56, American Astronomical Society, 2020, doi:<a href=\"https://doi.org/10.3847/1538-4357/abbda5\">10.3847/1538-4357/abbda5</a>.","short":"Y.L.L. Götberg, V. Korol, A. Lamberts, T. Kupfer, K. Breivik, B. Ludwig, M.R. Drout, The Astrophysical Journal 904 (2020).","ama":"Götberg YLL, Korol V, Lamberts A, et al. Stars stripped in binaries: The living gravitational-wave sources. <i>The Astrophysical Journal</i>. 2020;904(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/abbda5\">10.3847/1538-4357/abbda5</a>"},"arxiv":1,"title":"Stars stripped in binaries: The living gravitational-wave sources","external_id":{"arxiv":["2006.07382"]},"publication":"The Astrophysical Journal","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2006.07382"}],"status":"public","date_updated":"2023-08-21T11:32:40Z","abstract":[{"text":"Binary interaction can cause stellar envelopes to be stripped, which significantly reduces the radius of the star. The orbit of a binary composed of a stripped star and a compact object can therefore be so tight that the gravitational radiation the system produces reaches frequencies accessible to the Laser Interferometer Space Antenna (LISA). Two such stripped stars in tight orbits with white dwarfs are known so far (ZTF J2130+4420 and CD−30°11223), but many more are expected to exist. These binaries provide important constraints for binary evolution models and may be used as LISA verification sources. We develop a Monte Carlo code that uses detailed evolutionary models to simulate the Galactic population of stripped stars in tight orbits with either neutron star or white dwarf companions. We predict 0–100 stripped star + white dwarf binaries and 0–4 stripped star + neutron star binaries with a signal-to-noise ratio >5 after 10 yr of observations with LISA. More than 90% of these binaries are expected to show large radial velocity shifts of ≳200 $\\,\\mathrm{km}\\,{{\\rm{s}}}^{-1}$, which are spectroscopically detectable. Photometric variability due to tidal deformation of the stripped star is also expected and has been observed in ZTF J2130+4420 and CD−30°11223. In addition, the stripped star + neutron star binaries are expected to be X-ray bright with LX ≳ 1033–1036 $\\,\\mathrm{erg}\\,{{\\rm{s}}}^{-1}$. Our results show that stripped star binaries are promising multimessenger sources for the upcoming electromagnetic and gravitational wave facilities.","lang":"eng"}],"day":"20","publication_status":"published","oa_version":"Preprint","intvolume":"       904","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2023-08-03T10:12:07Z","article_number":"56","article_type":"original","volume":904,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","month":"11","type":"journal_article","year":"2020","publisher":"American Astronomical Society","doi":"10.3847/1538-4357/abbda5","language":[{"iso":"eng"}],"date_published":"2020-11-20T00:00:00Z","_id":"13460","oa":1,"author":[{"orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter"},{"first_name":"V.","full_name":"Korol, V.","last_name":"Korol"},{"first_name":"A.","full_name":"Lamberts, A.","last_name":"Lamberts"},{"last_name":"Kupfer","first_name":"T.","full_name":"Kupfer, T."},{"last_name":"Breivik","full_name":"Breivik, K.","first_name":"K."},{"full_name":"Ludwig, B.","first_name":"B.","last_name":"Ludwig"},{"last_name":"Drout","first_name":"M. R.","full_name":"Drout, M. R."}]},{"type":"journal_article","year":"2020","publisher":"American Astronomical Society","doi":"10.3847/1538-4357/abaefa","language":[{"iso":"eng"}],"date_published":"2020-09-23T00:00:00Z","_id":"13461","oa":1,"author":[{"last_name":"Secunda","full_name":"Secunda, Amy","first_name":"Amy"},{"last_name":"Cen","first_name":"Renyue","full_name":"Cen, Renyue"},{"last_name":"Kimm","first_name":"Taysun","full_name":"Kimm, Taysun"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"},{"first_name":"Selma E.","full_name":"de Mink, Selma E.","last_name":"de Mink"}],"intvolume":"       901","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"extern":"1","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2023-08-03T10:12:16Z","article_number":"72","volume":901,"article_type":"original","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","month":"09","status":"public","date_updated":"2023-08-09T13:01:45Z","abstract":[{"text":"High-resolution numerical simulations including feedback and aimed at calculating the escape fraction (fesc) of hydrogen-ionizing photons often assume stellar radiation based on single-stellar population synthesis models. However, strong evidence suggests the binary fraction of massive stars is ≳70%. Moreover, simulations so far have yielded values of fesc falling only on the lower end of the ∼10%–20% range, the amount presumed necessary to reionize the universe. Analyzing a high-resolution (4 pc) cosmological radiation-hydrodynamic simulation, we study how fesc changes when we include two different products of binary stellar evolution—stars stripped of their hydrogen envelopes and massive blue stragglers. Both produce significant amounts of ionizing photons 10–200 Myr after each starburst. We find the relative importance of these photons to be amplified with respect to escaped ionizing photons, because peaks in star formation rates (SFRs) and fesc are often out of phase by this 10–200 Myr. Additionally, low-mass, bursty galaxies emit Lyman continuum radiation primarily from binary products when SFRs are low. Observations of these galaxies by the James Webb Space Telescope could provide crucial information on the evolution of binary stars as a function of redshift. Overall, including stripped stars and massive blue stragglers increases our photon-weighted mean escape fraction ($\\langle {f}_{\\mathrm{esc}}\\rangle $) by ∼13% and ∼10%, respectively, resulting in $\\langle {f}_{\\mathrm{esc}}\\rangle =17 \\% $. Our results emphasize that using updated stellar population synthesis models with binary stellar evolution provides a more sound physical basis for stellar reionization.","lang":"eng"}],"day":"23","publication_status":"published","oa_version":"Published Version","scopus_import":"1","issue":"1","citation":{"ama":"Secunda A, Cen R, Kimm T, Götberg YLL, de Mink SE. Delayed photons from binary evolution help reionize the universe. <i>The Astrophysical Journal</i>. 2020;901(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/abaefa\">10.3847/1538-4357/abaefa</a>","ista":"Secunda A, Cen R, Kimm T, Götberg YLL, de Mink SE. 2020. Delayed photons from binary evolution help reionize the universe. The Astrophysical Journal. 901(1), 72.","short":"A. Secunda, R. Cen, T. Kimm, Y.L.L. Götberg, S.E. de Mink, The Astrophysical Journal 901 (2020).","mla":"Secunda, Amy, et al. “Delayed Photons from Binary Evolution Help Reionize the Universe.” <i>The Astrophysical Journal</i>, vol. 901, no. 1, 72, American Astronomical Society, 2020, doi:<a href=\"https://doi.org/10.3847/1538-4357/abaefa\">10.3847/1538-4357/abaefa</a>.","apa":"Secunda, A., Cen, R., Kimm, T., Götberg, Y. L. L., &#38; de Mink, S. E. (2020). Delayed photons from binary evolution help reionize the universe. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/abaefa\">https://doi.org/10.3847/1538-4357/abaefa</a>","ieee":"A. Secunda, R. Cen, T. Kimm, Y. L. L. Götberg, and S. E. de Mink, “Delayed photons from binary evolution help reionize the universe,” <i>The Astrophysical Journal</i>, vol. 901, no. 1. American Astronomical Society, 2020.","chicago":"Secunda, Amy, Renyue Cen, Taysun Kimm, Ylva Louise Linsdotter Götberg, and Selma E. de Mink. “Delayed Photons from Binary Evolution Help Reionize the Universe.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2020. <a href=\"https://doi.org/10.3847/1538-4357/abaefa\">https://doi.org/10.3847/1538-4357/abaefa</a>."},"arxiv":1,"title":"Delayed photons from binary evolution help reionize the universe","external_id":{"arxiv":["2007.15012"]},"publication":"The Astrophysical Journal","main_file_link":[{"url":"https://doi.org/10.3847/1538-4357/abaefa","open_access":"1"}]},{"publication_status":"published","oa_version":"Preprint","day":"11","abstract":[{"lang":"eng","text":"We discuss the nature and physical properties of gas-mass selected galaxies in the ALMA spectroscopic survey (ASPECS) of the Hubble Ultra Deep Field (HUDF). We capitalize on the deep optical integral-field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) HUDF Survey and multiwavelength data to uniquely associate all 16 line emitters, detected in the ALMA data without preselection, with rotational transitions of carbon monoxide (CO). We identify 10 as CO(2–1) at 1 < z < 2, 5 as CO(3–2) at 2 < z < 3, and 1 as CO(4–3) at z = 3.6. Using the MUSE data as a prior, we identify two additional CO(2–1) emitters, increasing the total sample size to 18. We infer metallicities consistent with (super-)solar for the CO-detected galaxies at z ≤ 1.5, motivating our choice of a Galactic conversion factor between CO luminosity and molecular gas mass for these galaxies. Using deep Chandra imaging of the HUDF, we determine an X-ray AGN fraction of 20% and 60% among the CO emitters at z ∼ 1.4 and z ∼ 2.6, respectively. Being a CO-flux-limited survey, ASPECS-LP detects molecular gas in galaxies on, above, and below the main sequence (MS) at z ∼ 1.4. For stellar masses ≥1010 (1010.5) ${M}_{\\odot }$, we detect about 40% (50%) of all galaxies in the HUDF at 1 < z < 2 (2 < z < 3). The combination of ALMA and MUSE integral-field spectroscopy thus enables an unprecedented view of MS galaxies during the peak of galaxy formation."}],"status":"public","date_updated":"2022-07-19T09:50:55Z","publication":"The Astrophysical Journal","external_id":{"arxiv":["1903.09167"]},"title":"The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy","main_file_link":[{"url":"https://arxiv.org/abs/1903.09167","open_access":"1"}],"issue":"2","scopus_import":"1","citation":{"ieee":"L. A. Boogaard <i>et al.</i>, “The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy,” <i>The Astrophysical Journal</i>, vol. 882, no. 2. IOP Publishing, 2019.","chicago":"Boogaard, Leindert A., Roberto Decarli, Jorge González-López, Paul van der Werf, Fabian Walter, Rychard Bouwens, Manuel Aravena, et al. “The ALMA Spectroscopic Survey in the HUDF: Nature and Physical Properties of Gas-Mass Selected Galaxies Using MUSE Spectroscopy.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab3102\">https://doi.org/10.3847/1538-4357/ab3102</a>.","ama":"Boogaard LA, Decarli R, González-López J, et al. The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. <i>The Astrophysical Journal</i>. 2019;882(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab3102\">10.3847/1538-4357/ab3102</a>","mla":"Boogaard, Leindert A., et al. “The ALMA Spectroscopic Survey in the HUDF: Nature and Physical Properties of Gas-Mass Selected Galaxies Using MUSE Spectroscopy.” <i>The Astrophysical Journal</i>, vol. 882, no. 2, 140, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab3102\">10.3847/1538-4357/ab3102</a>.","ista":"Boogaard LA, Decarli R, González-López J, van der Werf P, Walter F, Bouwens R, Aravena M, Carilli C, Bauer FE, Brinchmann J, Contini T, Cox P, da Cunha E, Daddi E, Díaz-Santos T, Hodge J, Inami H, Ivison R, Maseda M, Matthee JJ, Oesch P, Popping G, Riechers D, Schaye J, Schouws S, Smail I, Weiss A, Wisotzki L, Bacon R, Cortes PC, Rix H-W, Somerville RS, Swinbank M, Wagg J. 2019. The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. The Astrophysical Journal. 882(2), 140.","short":"L.A. Boogaard, R. Decarli, J. González-López, P. van der Werf, F. Walter, R. Bouwens, M. Aravena, C. Carilli, F.E. Bauer, J. Brinchmann, T. Contini, P. Cox, E. da Cunha, E. Daddi, T. Díaz-Santos, J. Hodge, H. Inami, R. Ivison, M. Maseda, J.J. Matthee, P. Oesch, G. Popping, D. Riechers, J. Schaye, S. Schouws, I. Smail, A. Weiss, L. Wisotzki, R. Bacon, P.C. Cortes, H.-W. Rix, R.S. Somerville, M. Swinbank, J. Wagg, The Astrophysical Journal 882 (2019).","apa":"Boogaard, L. A., Decarli, R., González-López, J., van der Werf, P., Walter, F., Bouwens, R., … Wagg, J. (2019). The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab3102\">https://doi.org/10.3847/1538-4357/ab3102</a>"},"arxiv":1,"date_published":"2019-09-11T00:00:00Z","author":[{"last_name":"Boogaard","full_name":"Boogaard, Leindert A.","first_name":"Leindert A."},{"last_name":"Decarli","full_name":"Decarli, Roberto","first_name":"Roberto"},{"full_name":"González-López, Jorge","first_name":"Jorge","last_name":"González-López"},{"last_name":"van der Werf","full_name":"van der Werf, Paul","first_name":"Paul"},{"first_name":"Fabian","full_name":"Walter, Fabian","last_name":"Walter"},{"last_name":"Bouwens","full_name":"Bouwens, Rychard","first_name":"Rychard"},{"last_name":"Aravena","full_name":"Aravena, Manuel","first_name":"Manuel"},{"last_name":"Carilli","full_name":"Carilli, Chris","first_name":"Chris"},{"last_name":"Bauer","first_name":"Franz Erik","full_name":"Bauer, Franz Erik"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Contini","full_name":"Contini, Thierry","first_name":"Thierry"},{"last_name":"Cox","full_name":"Cox, Pierre","first_name":"Pierre"},{"first_name":"Elisabete","full_name":"da Cunha, Elisabete","last_name":"da Cunha"},{"last_name":"Daddi","first_name":"Emanuele","full_name":"Daddi, Emanuele"},{"last_name":"Díaz-Santos","full_name":"Díaz-Santos, Tanio","first_name":"Tanio"},{"first_name":"Jacqueline","full_name":"Hodge, Jacqueline","last_name":"Hodge"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"last_name":"Ivison","full_name":"Ivison, Rob","first_name":"Rob"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"first_name":"Gergö","full_name":"Popping, Gergö","last_name":"Popping"},{"last_name":"Riechers","full_name":"Riechers, Dominik","first_name":"Dominik"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"first_name":"Sander","full_name":"Schouws, Sander","last_name":"Schouws"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"last_name":"Weiss","first_name":"Axel","full_name":"Weiss, Axel"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"last_name":"Cortes","full_name":"Cortes, Paulo C.","first_name":"Paulo C."},{"full_name":"Rix, Hans-Walter","first_name":"Hans-Walter","last_name":"Rix"},{"first_name":"Rachel S.","full_name":"Somerville, Rachel S.","last_name":"Somerville"},{"first_name":"Mark","full_name":"Swinbank, Mark","last_name":"Swinbank"},{"first_name":"Jeff","full_name":"Wagg, Jeff","last_name":"Wagg"}],"oa":1,"_id":"11514","type":"journal_article","language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ab3102","publisher":"IOP Publishing","year":"2019","article_type":"original","volume":882,"month":"09","quality_controlled":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"article_processing_charge":"No","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       882","article_number":"140","date_created":"2022-07-06T13:31:35Z","acknowledgement":"We are grateful to the referee for providing a constructive report. L.A.B. wants to thank Madusha L.P. Gunawardhana for her help with platefit. Based on observations collected at the European Southern Observatory under ESO programme(s): 094.A-2089(B), 095.A-0010(A), 096.A-0045(A), and 096.A-0045(B). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\r\n\r\n\"Este trabajo contó con el apoyo de CONICYT+Programa de Astronomía+ Fondo CHINA-CONICYT\" J.G-L. acknowledges partial support from ALMA-CONICYT project 31160033. F.E.B. acknowledges support from CONICYT grant Basal AFB-170002 (FEB), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003., and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). T.D-S. acknowledges support from ALMA-CONYCIT project 31130005 and FONDECYT project 1151239. J.H. acknowledges support of the VIDI research programme with project number 639.042.611, which is (partly) financed by the Netherlands Organization for Scientific Research (NWO). D.R. acknowledges support from the National Science Foundation under grant No. AST-1614213. I.R.S. acknowledges support from the ERC Advanced Grant DUSTYGAL (321334) and STFC (ST/P000541/1)\r\n\r\nWork on Gnuastro has been funded by the Japanese MEXT scholarship and its Grant-in-Aid for Scientific Research (21244012, 24253003), the ERC advanced grant 339659-MUSICOS, European Union's Horizon 2020 research and innovation programme under Marie Sklodowska-Curie grant agreement No. 721463 to the SUNDIAL ITN, and from the Spanish MINECO under grant No. AYA2016-76219-P."},{"scopus_import":"1","issue":"2","arxiv":1,"citation":{"short":"J.J. Matthee, D. Sobral, L.A. Boogaard, H. Röttgering, L. Vallini, A. Ferrara, A. Paulino-Afonso, F. Boone, D. Schaerer, B. Mobasher, The Astrophysical Journal 881 (2019).","mla":"Matthee, Jorryt J., et al. “Resolved UV and [C Ii] Structures of Luminous Galaxies within the Epoch of Reionization.” <i>The Astrophysical Journal</i>, vol. 881, no. 2, 124, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2f81\">10.3847/1538-4357/ab2f81</a>.","apa":"Matthee, J. J., Sobral, D., Boogaard, L. A., Röttgering, H., Vallini, L., Ferrara, A., … Mobasher, B. (2019). Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab2f81\">https://doi.org/10.3847/1538-4357/ab2f81</a>","ista":"Matthee JJ, Sobral D, Boogaard LA, Röttgering H, Vallini L, Ferrara A, Paulino-Afonso A, Boone F, Schaerer D, Mobasher B. 2019. Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. The Astrophysical Journal. 881(2), 124.","ama":"Matthee JJ, Sobral D, Boogaard LA, et al. Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. <i>The Astrophysical Journal</i>. 2019;881(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2f81\">10.3847/1538-4357/ab2f81</a>","chicago":"Matthee, Jorryt J, D. Sobral, L. A. Boogaard, H. Röttgering, L. Vallini, A. Ferrara, A. Paulino-Afonso, F. Boone, D. Schaerer, and B. Mobasher. “Resolved UV and [C Ii] Structures of Luminous Galaxies within the Epoch of Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab2f81\">https://doi.org/10.3847/1538-4357/ab2f81</a>.","ieee":"J. J. Matthee <i>et al.</i>, “Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization,” <i>The Astrophysical Journal</i>, vol. 881, no. 2. IOP Publishing, 2019."},"title":"Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization","external_id":{"arxiv":["1903.08171"]},"publication":"The Astrophysical Journal","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.08171"}],"status":"public","date_updated":"2022-08-18T10:19:48Z","abstract":[{"lang":"eng","text":"We present new deep ALMA and Hubble Space Telescope (HST)/WFC3 observations of MASOSA and VR7, two luminous Lyα emitters (LAEs) at z = 6.5, for which the UV continuum levels differ by a factor of four. No IR dust continuum emission is detected in either, indicating little amounts of obscured star formation and/or high dust temperatures. MASOSA, with a UV luminosity M1500 = −20.9, compact size, and very high Lyα ${\\mathrm{EW}}_{0}\\approx 145\\,\\mathring{\\rm A} $, is undetected in [C ii] to a limit of L[C ii] < 2.2 × 107 L⊙, implying a metallicity Z ≲ 0.07 Z⊙. Intriguingly, our HST data indicate a red UV slope β = −1.1 ± 0.7, at odds with the low dust content. VR7, which is a bright (M1500 = −22.4) galaxy with moderate color (β = −1.4 ± 0.3) and Lyα EW0 = 34 Å, is clearly detected in [C ii] emission (S/N = 15). VR7's rest-frame UV morphology can be described by two components separated by ≈1.5 kpc and is globally more compact than the [C ii] emission. The global [C ii]/UV ratio indicates Z ≈ 0.2 Z⊙, but there are large variations in the UV/[C ii] ratio on kiloparsec scales. We also identify diffuse, possibly outflowing, [C ii]-emitting gas at ≈100 km s−1 with respect to the peak. VR7 appears to be assembling its components at a slightly more evolved stage than other luminous LAEs, with outflows already shaping its direct environment at z ∼ 7. Our results further indicate that the global [C ii]−UV relation steepens at SFR < 30 M⊙ yr−1, naturally explaining why the [C ii]/UV ratio is anticorrelated with Lyα EW in many, but not all, observed LAEs."}],"day":"21","oa_version":"Preprint","publication_status":"published","intvolume":"       881","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We thank Max Gronke for comments on an earlier version of this paper. L.V. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 746119. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. Based on observations obtained with the Very Large Telescope, programs 294.A-5018, 097.A-0943, and 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program No. 14699.","article_number":"124","date_created":"2022-07-06T13:38:15Z","volume":881,"article_type":"original","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","month":"08","type":"journal_article","year":"2019","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ab2f81","language":[{"iso":"eng"}],"date_published":"2019-08-21T00:00:00Z","_id":"11515","oa":1,"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Sobral","first_name":"D.","full_name":"Sobral, D."},{"last_name":"Boogaard","first_name":"L. A.","full_name":"Boogaard, L. A."},{"last_name":"Röttgering","first_name":"H.","full_name":"Röttgering, H."},{"last_name":"Vallini","full_name":"Vallini, L.","first_name":"L."},{"last_name":"Ferrara","first_name":"A.","full_name":"Ferrara, A."},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A.","first_name":"A."},{"full_name":"Boone, F.","first_name":"F.","last_name":"Boone"},{"full_name":"Schaerer, D.","first_name":"D.","last_name":"Schaerer"},{"last_name":"Mobasher","full_name":"Mobasher, B.","first_name":"B."}]},{"month":"07","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1","volume":880,"article_type":"original","date_created":"2022-07-06T13:50:33Z","article_number":"47","acknowledgement":"We thank Lutz Wisotzki for stimulating discussions. This work is based on observations taken at ESO/VLT in Paranal and we would like to thank the ESO staff for their assistance and support during the MUSE GTO campaigns. This work was supported by the Swiss National Science Foundation. This research made use of Astropy, a community-developed core PYTHON package for astronomy (Astropy Collaboration et al. 2013), NumPy and SciPy (Oliphant 2007), Matplotlib (Hunter 2007), IPython (Perez & Granger 2007), and of the NASA Astrophysics Data System Bibliographic Services. S.C. and G.P. gratefully acknowledge support from Swiss National Science Foundation grant PP00P2−163824. A.F. acknowledges support from the ERC via Advanced Grant under grants agreement no. 339659-MUSICOS. J.B. acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. S.D.J. is supported by a NASA Hubble Fellowship (HST-HF2-51375.001-A). T.N. acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","intvolume":"       880","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna","last_name":"Marino"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Lilly","full_name":"Lilly, Simon J.","first_name":"Simon J."},{"first_name":"Sofia","full_name":"Gallego, Sofia","last_name":"Gallego"},{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Bouché","first_name":"Nicolas","full_name":"Bouché, Nicolas"},{"last_name":"Feltre","first_name":"Anna","full_name":"Feltre, Anna"},{"last_name":"Muzahid","first_name":"Sowgat","full_name":"Muzahid, Sowgat"},{"last_name":"Schroetter","first_name":"Ilane","full_name":"Schroetter, Ilane"},{"last_name":"Johnson","first_name":"Sean D.","full_name":"Johnson, Sean D."},{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"}],"_id":"11516","oa":1,"date_published":"2019-07-24T00:00:00Z","doi":"10.3847/1538-4357/ab2881","language":[{"iso":"eng"}],"year":"2019","publisher":"IOP Publishing","type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1906.06347"}],"publication":"The Astrophysical Journal","title":"A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE","external_id":{"arxiv":["1906.06347"]},"citation":{"apa":"Marino, R. A., Cantalupo, S., Pezzulli, G., Lilly, S. J., Gallego, S., Mackenzie, R., … Nanayakkara, T. (2019). A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab2881\">https://doi.org/10.3847/1538-4357/ab2881</a>","mla":"Marino, Raffaella Anna, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” <i>The Astrophysical Journal</i>, vol. 880, no. 1, 47, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2881\">10.3847/1538-4357/ab2881</a>.","ista":"Marino RA, Cantalupo S, Pezzulli G, Lilly SJ, Gallego S, Mackenzie R, Matthee JJ, Brinchmann J, Bouché N, Feltre A, Muzahid S, Schroetter I, Johnson SD, Nanayakkara T. 2019. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. 880(1), 47.","short":"R.A. Marino, S. Cantalupo, G. Pezzulli, S.J. Lilly, S. Gallego, R. Mackenzie, J.J. Matthee, J. Brinchmann, N. Bouché, A. Feltre, S. Muzahid, I. Schroetter, S.D. Johnson, T. Nanayakkara, The Astrophysical Journal 880 (2019).","ama":"Marino RA, Cantalupo S, Pezzulli G, et al. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. <i>The Astrophysical Journal</i>. 2019;880(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2881\">10.3847/1538-4357/ab2881</a>","chicago":"Marino, Raffaella Anna, Sebastiano Cantalupo, Gabriele Pezzulli, Simon J. Lilly, Sofia Gallego, Ruari Mackenzie, Jorryt J Matthee, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab2881\">https://doi.org/10.3847/1538-4357/ab2881</a>.","ieee":"R. A. Marino <i>et al.</i>, “A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE,” <i>The Astrophysical Journal</i>, vol. 880, no. 1. IOP Publishing, 2019."},"arxiv":1,"scopus_import":"1","issue":"1","day":"24","oa_version":"Preprint","publication_status":"published","abstract":[{"text":"The well-known quasar SDSS J095253.83+011421.9 (J0952+0114) at z = 3.02 has one of the most peculiar spectra discovered so far, showing the presence of narrow Lyα and broad metal emission lines. Although recent studies have suggested that a proximate damped Lyα absorption (PDLA) system causes this peculiar spectrum, the origin of the gas associated with the PDLA is unknown. Here we report the results of observations with the Multi Unit Spectroscopic Explorer (MUSE) that reveal a new giant (≈100 physical kpc) Lyα nebula. The detailed analysis of the Lyα velocity, velocity dispersion, and surface brightness profiles suggests that the J0952+0114 Lyα nebula shares similar properties with other QSO nebulae previously detected with MUSE, implying that the PDLA in J0952+0144 is covering only a small fraction of the solid angle of the QSO emission. We also detected bright and spectrally narrow C iv λ1550 and He ii λ1640 extended emission around J0952+0114 with velocity centroids similar to the peak of the extended and central narrow Lyα emission. The presence of a peculiarly bright, unresolved, and relatively broad He ii λ1640 emission in the central region at exactly the same PDLA redshift hints at the possibility that the PDLA originates in a clumpy outflow with a bulk velocity of about 500 km s−1. The smaller velocity dispersion of the large-scale Lyα emission suggests that the high-speed outflow is confined to the central region. Lastly, the derived spatially resolved He ii/Lyα and C iv/Lyα maps show a positive gradient with the distance to the QSO, hinting at a non-homogeneous distribution of the ionization parameter.","lang":"eng"}],"date_updated":"2022-08-18T10:20:18Z","status":"public"},{"status":"public","date_updated":"2022-08-18T10:19:08Z","day":"04","publication_status":"published","oa_version":"Preprint","abstract":[{"text":"To understand star formation in galaxies, we investigate the star formation rate (SFR) surface density (ΣSFR) profiles for galaxies, based on a well-defined sample of 976 star-forming MaNGA galaxies. We find that the typical ΣSFR profiles within 1.5Re of normal SF galaxies can be well described by an exponential function for different stellar mass intervals, while the sSFR profile shows positive gradients, especially for more massive SF galaxies. This is due to the more pronounced central cores or bulges rather than the onset of a `quenching' process. While galaxies that lie significantly above (or below) the star formation main sequence (SFMS) show overall an elevation (or suppression) of ΣSFR at all radii, this central elevation (or suppression) is more pronounced in more massive galaxies. The degree of central enhancement and suppression is quite symmetric, suggesting that both the elevation and suppression of star formation are following the same physical processes. Furthermore, we find that the dispersion in ΣSFR within and across the population is found to be tightly correlated with the inferred gas depletion time, whether based on the stellar surface mass density or the orbital dynamical time. This suggests that we are seeing the response of a simple gas-regulator system to variations in the accretion rate. This is explored using a heuristic model that can quantitatively explain the dependence of σ(ΣSFR) on gas depletion timescale. Variations in accretion rate are progressively more damped out in regions of low star-formation efficiency leading to a reduced amplitude of variations in star-formation.","lang":"eng"}],"scopus_import":"1","issue":"2","citation":{"ama":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. On the elevation and suppression of star formation within galaxies. <i>The Astrophysical Journal</i>. 2019;877(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">10.3847/1538-4357/ab1c5b</a>","apa":"Wang, E., Lilly, S. J., Pezzulli, G., &#38; Matthee, J. J. (2019). On the elevation and suppression of star formation within galaxies. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">https://doi.org/10.3847/1538-4357/ab1c5b</a>","ista":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. 2019. On the elevation and suppression of star formation within galaxies. The Astrophysical Journal. 877(2), 132.","mla":"Wang, Enci, et al. “On the Elevation and Suppression of Star Formation within Galaxies.” <i>The Astrophysical Journal</i>, vol. 877, no. 2, 132, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">10.3847/1538-4357/ab1c5b</a>.","short":"E. Wang, S.J. Lilly, G. Pezzulli, J.J. Matthee, The Astrophysical Journal 877 (2019).","ieee":"E. Wang, S. J. Lilly, G. Pezzulli, and J. J. Matthee, “On the elevation and suppression of star formation within galaxies,” <i>The Astrophysical Journal</i>, vol. 877, no. 2. IOP Publishing, 2019.","chicago":"Wang, Enci, Simon J. Lilly, Gabriele Pezzulli, and Jorryt J Matthee. “On the Elevation and Suppression of Star Formation within Galaxies.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">https://doi.org/10.3847/1538-4357/ab1c5b</a>."},"arxiv":1,"publication":"The Astrophysical Journal","title":"On the elevation and suppression of star formation within galaxies","external_id":{"arxiv":["1901.10276"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1901.10276"}],"type":"journal_article","doi":"10.3847/1538-4357/ab1c5b","language":[{"iso":"eng"}],"year":"2019","publisher":"IOP Publishing","date_published":"2019-06-04T00:00:00Z","author":[{"first_name":"Enci","full_name":"Wang, Enci","last_name":"Wang"},{"last_name":"Lilly","first_name":"Simon J.","full_name":"Lilly, Simon J."},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"}],"_id":"11517","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","extern":"1","intvolume":"       877","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_number":"132","date_created":"2022-07-07T08:38:24Z","acknowledgement":"We are grateful to the anonymous referee for their thoughtful and constructive review of the paper and their several suggestions (including the analysis of Section 3.4), which have improved the paper. This research has been supported by the Swiss National Science Foundation.\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. The SDSS website is www.sdss.org.\r\n\r\nSDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, the Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, the Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University","volume":877,"article_type":"original","month":"06","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"quality_controlled":"1"}]