[{"issue":"5","quality_controlled":"1","day":"04","month":"05","status":"public","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"extern":"1","date_published":"2021-05-04T00:00:00Z","external_id":{"arxiv":["2103.13642"]},"type":"journal_article","publisher":"American Astronomical Society","_id":"13459","date_created":"2023-08-03T10:11:57Z","year":"2021","article_number":"248","citation":{"short":"L. Wang, D.R. Gies, G.J. Peters, Y.L.L. Götberg, S.D. Chojnowski, K.V. Lester, S.B. Howell, The Astronomical Journal 161 (2021).","chicago":"Wang, Luqian, Douglas R. Gies, Geraldine J. Peters, Ylva Louise Linsdotter Götberg, S. Drew Chojnowski, Kathryn V. Lester, and Steve B. Howell. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” <i>The Astronomical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-3881/abf144\">https://doi.org/10.3847/1538-3881/abf144</a>.","apa":"Wang, L., Gies, D. R., Peters, G. J., Götberg, Y. L. L., Chojnowski, S. D., Lester, K. V., &#38; Howell, S. B. (2021). The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-3881/abf144\">https://doi.org/10.3847/1538-3881/abf144</a>","mla":"Wang, Luqian, et al. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” <i>The Astronomical Journal</i>, vol. 161, no. 5, 248, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/abf144\">10.3847/1538-3881/abf144</a>.","ama":"Wang L, Gies DR, Peters GJ, et al. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. <i>The Astronomical Journal</i>. 2021;161(5). doi:<a href=\"https://doi.org/10.3847/1538-3881/abf144\">10.3847/1538-3881/abf144</a>","ista":"Wang L, Gies DR, Peters GJ, Götberg YLL, Chojnowski SD, Lester KV, Howell SB. 2021. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. The Astronomical Journal. 161(5), 248.","ieee":"L. Wang <i>et al.</i>, “The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy,” <i>The Astronomical Journal</i>, vol. 161, no. 5. American Astronomical Society, 2021."},"abstract":[{"lang":"eng","text":"The B emission-line stars are rapid rotators that were probably spun up by mass and angular momentum accretion through mass transfer in an interacting binary. Mass transfer will strip the donor star of its envelope to create a small and hot subdwarf remnant. Here we report on Hubble Space Telescope/STIS far-ultraviolet spectroscopy of a sample of Be stars that reveals the presence of the hot sdO companion through the calculation of cross-correlation functions of the observed and model spectra. We clearly detect the spectral signature of the sdO star in 10 of the 13 stars in the sample, and the spectral signals indicate that the sdO stars are hot, relatively faint, and slowly rotating as predicted by models. A comparison of their temperatures and radii with evolutionary tracks indicates that the sdO stars occupy the relatively long-lived, He-core burning stage. Only 1 of the 10 detections was a known binary prior to this investigation, which emphasizes the difficulty of finding such Be+sdO binaries through optical spectroscopy. However, these results and others indicate that many Be stars probably host hot subdwarf companions."}],"title":"The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy","publication_status":"published","article_processing_charge":"No","oa_version":"Preprint","main_file_link":[{"url":"https://arxiv.org/abs/2103.13642","open_access":"1"}],"doi":"10.3847/1538-3881/abf144","scopus_import":"1","article_type":"original","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"publication":"The Astronomical Journal","date_updated":"2023-08-21T11:35:50Z","arxiv":1,"intvolume":"       161","oa":1,"volume":161,"author":[{"full_name":"Wang, Luqian","first_name":"Luqian","last_name":"Wang"},{"full_name":"Gies, Douglas R.","first_name":"Douglas R.","last_name":"Gies"},{"full_name":"Peters, Geraldine J.","last_name":"Peters","first_name":"Geraldine J."},{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Chojnowski, S. Drew","first_name":"S. Drew","last_name":"Chojnowski"},{"last_name":"Lester","first_name":"Kathryn V.","full_name":"Lester, Kathryn V."},{"first_name":"Steve B.","last_name":"Howell","full_name":"Howell, Steve B."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"arxiv":1,"intvolume":"       162","publication":"The Astronomical Journal","date_updated":"2022-08-19T10:01:56Z","author":[{"full_name":"Audenaert, J.","last_name":"Audenaert","first_name":"J."},{"first_name":"J. S.","last_name":"Kuszlewicz","full_name":"Kuszlewicz, J. S."},{"first_name":"R.","last_name":"Handberg","full_name":"Handberg, R."},{"first_name":"A.","last_name":"Tkachenko","full_name":"Tkachenko, A."},{"full_name":"Armstrong, D. J.","last_name":"Armstrong","first_name":"D. J."},{"first_name":"M.","last_name":"Hon","full_name":"Hon, M."},{"first_name":"R.","last_name":"Kgoadi","full_name":"Kgoadi, R."},{"full_name":"Lund, M. N.","last_name":"Lund","first_name":"M. N."},{"first_name":"K. J.","last_name":"Bell","full_name":"Bell, K. J."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"full_name":"Bowman, D. M.","last_name":"Bowman","first_name":"D. M."},{"full_name":"Johnston, C.","first_name":"C.","last_name":"Johnston"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"first_name":"D.","last_name":"Stello","full_name":"Stello, D."},{"last_name":"Molnár","first_name":"L.","full_name":"Molnár, L."},{"full_name":"Plachy, E.","last_name":"Plachy","first_name":"E."},{"full_name":"Buzasi, D.","first_name":"D.","last_name":"Buzasi"},{"last_name":"Aerts","first_name":"C.","full_name":"Aerts, C."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"volume":162,"article_number":"209","year":"2021","citation":{"chicago":"Audenaert, J., J. S. Kuszlewicz, R. Handberg, A. Tkachenko, D. J. Armstrong, M. Hon, R. Kgoadi, et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>. IOP Publishing, 2021. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>.","short":"J. Audenaert, J.S. Kuszlewicz, R. Handberg, A. Tkachenko, D.J. Armstrong, M. Hon, R. Kgoadi, M.N. Lund, K.J. Bell, L.A. Bugnet, D.M. Bowman, C. Johnston, R.A. García, D. Stello, L. Molnár, E. Plachy, D. Buzasi, C. Aerts, The Astronomical Journal 162 (2021).","apa":"Audenaert, J., Kuszlewicz, J. S., Handberg, R., Tkachenko, A., Armstrong, D. J., Hon, M., … Aerts, C. (2021). TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>","mla":"Audenaert, J., et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>, vol. 162, no. 5, 209, IOP Publishing, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>.","ieee":"J. Audenaert <i>et al.</i>, “TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data,” <i>The Astronomical Journal</i>, vol. 162, no. 5. IOP Publishing, 2021.","ista":"Audenaert J, Kuszlewicz JS, Handberg R, Tkachenko A, Armstrong DJ, Hon M, Kgoadi R, Lund MN, Bell KJ, Bugnet LA, Bowman DM, Johnston C, García RA, Stello D, Molnár L, Plachy E, Buzasi D, Aerts C. 2021. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. The Astronomical Journal. 162(5), 209.","ama":"Audenaert J, Kuszlewicz JS, Handberg R, et al. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. 2021;162(5). doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>"},"abstract":[{"text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of millions of stars with time spans ranging from ∼27 days to about 1 yr of continuous observations. This vast amount of data contains a wealth of information for variability, exoplanet, and stellar astrophysics studies but requires a number of processing steps before it can be fully utilized. In order to efficiently process all the TESS data and make it available to the wider scientific community, the TESS Data for Asteroseismology working group, as part of the TESS Asteroseismic Science Consortium, has created an automated open-source processing pipeline to produce light curves corrected for systematics from the short- and long-cadence raw photometry data and to classify these according to stellar variability type. We will process all stars down to a TESS magnitude of 15. This paper is the next in a series detailing how the pipeline works. Here, we present our methodology for the automatic variability classification of TESS photometry using an ensemble of supervised learners that are combined into a metaclassifier. We successfully validate our method using a carefully constructed labeled sample of Kepler Q9 light curves with a 27.4 days time span mimicking single-sector TESS observations, on which we obtain an overall accuracy of 94.9%. We demonstrate that our methodology can successfully classify stars outside of our labeled sample by applying it to all ∼167,000 stars observed in Q9 of the Kepler space mission.","lang":"eng"}],"_id":"11604","date_created":"2022-07-18T11:54:55Z","main_file_link":[{"url":"https://arxiv.org/abs/2107.06301","open_access":"1"}],"doi":"10.3847/1538-3881/ac166a","scopus_import":"1","article_type":"original","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"acknowledgement":"The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 670519: MAMSIE), from the KU Leuven Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. D.J.A acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). R.H. and M.N.L. acknowledge the ESA PRODEX program. This research was supported by the National Aeronautics and Space Administration (80NSSC18K1585 and 80NSSC19K0379) awarded through the TESS Guest Investigator Program. K.J.B. is supported by the National Science Foundation under Award AST-1903828. J.S.K and K.J.B. were supported by funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). D.M.B. gratefully acknowledges funding from a senior postdoctoral fellowship from the Research Foundation Flanders (FWO) with grant agreement No. 1286521N. The research leading to these results has received funding from the Research Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM). R.A.G. acknowledges support from the GOLF and PLATO CNES grants. L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has been supported by the Hungarian National Research, Development, and Innovation Office (NKFIH) grant KH_18 130405 and the Lendület LP2014-17 and LP2018-7/2020 grants of the Hungarian Academy of Sciences. D.B. acknowledges support from the NASA TESS Guest Investigator Program under award 80NSSC19K0385.\r\n\r\nThis paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. This research has made use of NASA's Astrophysics Data System as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and the Stellar Astrophysics Centre (SAC) at Aarhus University. We thank the TESS team and staff and TASC/TASOC for their support of the present work.\r\n\r\nThis paper includes data collected by the Kepler mission. Funding for the Kepler and K2 mission was provided by NASA's Science Mission Directorate. The authors acknowledge the efforts of the Kepler Mission team in obtaining the light-curve data and data validation products used in this publication. These data were generated by the Kepler Mission science pipeline through the efforts of the Kepler Science Operations Center and Science Office. The Kepler light curves are archived at the Mikulski Archive for Space Telescopes.\r\n\r\nThe numerical results presented in this work were obtained at the Centre for Scientific Computing, Aarhus. 37 This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018).\r\n\r\nSoftware: Scikit-learn (Pedregosa et al. 2011), Numpy (Harris et al. 2020), Astropy (Astropy Collaboration et al. 2013, 2018), Scipy (Virtanen et al. 2020), Pandas (McKinney 2010; Pandas Development Team 2020), Lightkurve (Lightkurve Collaboration et al. 2018), XGBoost (Chen & Guestrin 2016), Tensorflow (Abadi et al. 2015).","title":"TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data","publication_status":"published","oa_version":"Preprint","article_processing_charge":"No","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"extern":"1","month":"10","status":"public","publisher":"IOP Publishing","date_published":"2021-10-21T00:00:00Z","external_id":{"arxiv":["2107.06301"]},"type":"journal_article","issue":"5","day":"21","quality_controlled":"1"},{"arxiv":1,"intvolume":"       157","publication":"The Astronomical Journal","date_updated":"2022-08-22T07:38:34Z","author":[{"full_name":"Huber, Daniel","first_name":"Daniel","last_name":"Huber"},{"first_name":"William J.","last_name":"Chaplin","full_name":"Chaplin, William J."},{"full_name":"Chontos, Ashley","first_name":"Ashley","last_name":"Chontos"},{"first_name":"Hans","last_name":"Kjeldsen","full_name":"Kjeldsen, Hans"},{"first_name":"Jørgen","last_name":"Christensen-Dalsgaard","full_name":"Christensen-Dalsgaard, Jørgen"},{"last_name":"Bedding","first_name":"Timothy R.","full_name":"Bedding, Timothy R."},{"full_name":"Ball, Warrick","last_name":"Ball","first_name":"Warrick"},{"full_name":"Brahm, Rafael","last_name":"Brahm","first_name":"Rafael"},{"full_name":"Espinoza, Nestor","first_name":"Nestor","last_name":"Espinoza"},{"first_name":"Thomas","last_name":"Henning","full_name":"Henning, Thomas"},{"full_name":"Jordán, Andrés","first_name":"Andrés","last_name":"Jordán"},{"full_name":"Sarkis, Paula","last_name":"Sarkis","first_name":"Paula"},{"full_name":"Knudstrup, Emil","first_name":"Emil","last_name":"Knudstrup"},{"last_name":"Albrecht","first_name":"Simon","full_name":"Albrecht, Simon"},{"full_name":"Grundahl, Frank","last_name":"Grundahl","first_name":"Frank"},{"full_name":"Andersen, Mads Fredslund","first_name":"Mads Fredslund","last_name":"Andersen"},{"first_name":"Pere L.","last_name":"Pallé","full_name":"Pallé, Pere L."},{"full_name":"Crossfield, Ian","last_name":"Crossfield","first_name":"Ian"},{"last_name":"Fulton","first_name":"Benjamin","full_name":"Fulton, Benjamin"},{"first_name":"Andrew W.","last_name":"Howard","full_name":"Howard, Andrew W."},{"last_name":"Isaacson","first_name":"Howard T.","full_name":"Isaacson, Howard T."},{"first_name":"Lauren M.","last_name":"Weiss","full_name":"Weiss, Lauren M."},{"full_name":"Handberg, Rasmus","first_name":"Rasmus","last_name":"Handberg"},{"last_name":"Lund","first_name":"Mikkel N.","full_name":"Lund, Mikkel N."},{"first_name":"Aldo M.","last_name":"Serenelli","full_name":"Serenelli, Aldo M."},{"full_name":"Rørsted Mosumgaard, Jakob","first_name":"Jakob","last_name":"Rørsted Mosumgaard"},{"first_name":"Amalie","last_name":"Stokholm","full_name":"Stokholm, Amalie"},{"last_name":"Bieryla","first_name":"Allyson","full_name":"Bieryla, Allyson"},{"first_name":"Lars A.","last_name":"Buchhave","full_name":"Buchhave, Lars A."},{"first_name":"David W.","last_name":"Latham","full_name":"Latham, David W."},{"full_name":"Quinn, Samuel N.","last_name":"Quinn","first_name":"Samuel N."},{"first_name":"Eric","last_name":"Gaidos","full_name":"Gaidos, Eric"},{"full_name":"Hirano, Teruyuki","last_name":"Hirano","first_name":"Teruyuki"},{"last_name":"Ricker","first_name":"George R.","full_name":"Ricker, George R."},{"last_name":"Vanderspek","first_name":"Roland K.","full_name":"Vanderspek, Roland K."},{"full_name":"Seager, Sara","last_name":"Seager","first_name":"Sara"},{"full_name":"Jenkins, Jon M.","first_name":"Jon M.","last_name":"Jenkins"},{"last_name":"Winn","first_name":"Joshua N.","full_name":"Winn, Joshua N."},{"full_name":"Antia, H. M.","first_name":"H. M.","last_name":"Antia"},{"full_name":"Appourchaux, Thierry","last_name":"Appourchaux","first_name":"Thierry"},{"full_name":"Basu, Sarbani","last_name":"Basu","first_name":"Sarbani"},{"last_name":"Bell","first_name":"Keaton J.","full_name":"Bell, Keaton J."},{"full_name":"Benomar, Othman","first_name":"Othman","last_name":"Benomar"},{"full_name":"Bonanno, Alfio","first_name":"Alfio","last_name":"Bonanno"},{"full_name":"Buzasi, Derek L.","first_name":"Derek L.","last_name":"Buzasi"},{"last_name":"Campante","first_name":"Tiago L.","full_name":"Campante, Tiago L."},{"last_name":"Çelik Orhan","first_name":"Z.","full_name":"Çelik Orhan, Z."},{"full_name":"Corsaro, Enrico","first_name":"Enrico","last_name":"Corsaro"},{"full_name":"Cunha, Margarida S.","first_name":"Margarida S.","last_name":"Cunha"},{"full_name":"Davies, Guy R.","first_name":"Guy R.","last_name":"Davies"},{"first_name":"Sebastien","last_name":"Deheuvels","full_name":"Deheuvels, Sebastien"},{"full_name":"Grunblatt, Samuel K.","first_name":"Samuel K.","last_name":"Grunblatt"},{"full_name":"Hasanzadeh, Amir","last_name":"Hasanzadeh","first_name":"Amir"},{"last_name":"Di Mauro","first_name":"Maria Pia","full_name":"Di Mauro, Maria Pia"},{"full_name":"A. García, Rafael","first_name":"Rafael","last_name":"A. 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G.","full_name":"Tinney, C. G."},{"full_name":"Teske, Johanna","last_name":"Teske","first_name":"Johanna"},{"full_name":"Thomas, Alexandra","first_name":"Alexandra","last_name":"Thomas"},{"full_name":"Trampedach, Regner","last_name":"Trampedach","first_name":"Regner"},{"last_name":"Wright","first_name":"Duncan","full_name":"Wright, Duncan"},{"full_name":"Yuan, Thomas T.","last_name":"Yuan","first_name":"Thomas T."},{"full_name":"Zohrabi, Farzaneh","last_name":"Zohrabi","first_name":"Farzaneh"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"volume":157,"article_number":"245","year":"2019","citation":{"ama":"Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. 2019;157(6). doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>","ieee":"D. Huber <i>et al.</i>, “A hot Saturn orbiting an oscillating late subgiant discovered by TESS,” <i>The Astronomical Journal</i>, vol. 157, no. 6. IOP Publishing, 2019.","ista":"Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 157(6), 245.","mla":"Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>, vol. 157, no. 6, 245, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>.","short":"D. Huber, W.J. Chaplin, A. Chontos, H. Kjeldsen, J. Christensen-Dalsgaard, T.R. Bedding, W. Ball, R. Brahm, N. Espinoza, T. Henning, A. Jordán, P. Sarkis, E. Knudstrup, S. Albrecht, F. Grundahl, M.F. Andersen, P.L. Pallé, I. Crossfield, B. Fulton, A.W. Howard, H.T. Isaacson, L.M. Weiss, R. Handberg, M.N. Lund, A.M. Serenelli, J. Rørsted Mosumgaard, A. Stokholm, A. Bieryla, L.A. Buchhave, D.W. Latham, S.N. Quinn, E. Gaidos, T. Hirano, G.R. Ricker, R.K. Vanderspek, S. Seager, J.M. Jenkins, J.N. Winn, H.M. Antia, T. Appourchaux, S. Basu, K.J. Bell, O. Benomar, A. Bonanno, D.L. Buzasi, T.L. Campante, Z. Çelik Orhan, E. Corsaro, M.S. Cunha, G.R. Davies, S. Deheuvels, S.K. Grunblatt, A. Hasanzadeh, M.P. Di Mauro, R. A. García, P. Gaulme, L. Girardi, J.A. Guzik, M. Hon, C. Jiang, T. Kallinger, S.D. Kawaler, J.S. Kuszlewicz, Y. Lebreton, T. Li, M. Lucas, M.S. Lundkvist, A.W. Mann, S. Mathis, S. Mathur, A. Mazumdar, T.S. Metcalfe, A. Miglio, M.J.P. F. G. Monteiro, B. Mosser, A. Noll, B. Nsamba, J.M. Joel Ong, S. Örtel, F. Pereira, P. Ranadive, C. Régulo, T.S. Rodrigues, I.W. Roxburgh, V.S. Aguirre, B. Smalley, M. Schofield, S.G. Sousa, K.G. Stassun, D. Stello, J. Tayar, T.R. White, K. Verma, M. Vrard, M. Yıldız, D. Baker, M. Bazot, C. Beichmann, C. Bergmann, L.A. Bugnet, B. Cale, R. Carlino, S.M. Cartwright, J.L. Christiansen, D.R. Ciardi, O. Creevey, J.A. Dittmann, J.-D.D. Nascimento, V.V. Eylen, G. Fürész, J. Gagné, P. Gao, K. Gazeas, F. Giddens, O.J. Hall, S. Hekker, M.J. Ireland, N. Latouf, D. LeBrun, A.M. Levine, W. Matzko, E. Natinsky, E. Page, P. Plavchan, M. Mansouri-Samani, S. McCauliff, S.E. Mullally, B. Orenstein, A.G. Soto, M. Paegert, J.L. van Saders, C. Schnaible, D.R. Soderblom, R. Szabó, A. Tanner, C.G. Tinney, J. Teske, A. Thomas, R. Trampedach, D. Wright, T.T. Yuan, F. Zohrabi, The Astronomical Journal 157 (2019).","apa":"Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard, J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>","chicago":"Huber, Daniel, William J. Chaplin, Ashley Chontos, Hans Kjeldsen, Jørgen Christensen-Dalsgaard, Timothy R. Bedding, Warrick Ball, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>."},"abstract":[{"text":"We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064 R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a \"hot Saturn\" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology.","lang":"eng"}],"_id":"11616","date_created":"2022-07-18T14:29:07Z","main_file_link":[{"url":"https://arxiv.org/abs/1901.01643","open_access":"1"}],"doi":"10.3847/1538-3881/ab1488","scopus_import":"1","article_type":"original","acknowledgement":"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 Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank Andrei Tokovinin for helpful information on the Speckle observations obtained with SOAR. D.H. acknowledges support by the National Aeronautics and Space Administration through the TESS Guest Investigator Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). A.C. acknowledges support by the National Science Foundation under the Graduate Research Fellowship Program. W.J.C., W.H.B., A.M., O.J.H., and G.R.D. acknowledge support from the Science and Technology Facilities Council and UK Space Agency. H.K. and F.G. acknowledge support from the European Social Fund via the Lithuanian Science Council grant No. 09.3.3-LMT-K-712-01-0103. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). A.J. acknowledges support from FONDECYT project 1171208, CONICYT project BASAL AFB-170002, and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.M.S. is supported by grants ESP2017-82674-R (MINECO) and SGR2017-1131 (AGAUR). R.A.G. and L.B. acknowledge the support of the PLATO grant from the CNES. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP72007-2013)ERC grant agreement No. 338251 (StellarAges). S.M. acknowledges support from the European Research Council through the SPIRE grant 647383. This work was also supported by FCT (Portugal) through national funds and by FEDER through COMPETE2020 by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. 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). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.S. acknowledges support from the Australian Research Council. S.B. acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. T.R.W. acknowledges support from the Australian Research Council through grant DP150100250. A.M. acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. n. 772293). S.M. acknowledges support from the Ramon y Cajal fellowship number RYC-2015-17697. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). A.M. and P.R. acknowledge support from the HBCSE-NIUS programme. J.K.T. and J.T. acknowledge that support for this work was provided by NASA through Hubble Fellowship grants HST-HF2-51399.001 and HST-HF2-51424.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). This project has been supported by the NKFIH K-115709 grant and the Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018.\r\n\r\nBased on observations made with the Hertzsprung SONG telescope operated on the Spanish Observatorio del Teide on the island of Tenerife by the Aarhus and Copenhagen Universities and by the Instituto de Astrofísica de Canarias. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2018), Matplotlib (Hunter 2007), DIAMONDS (Corsaro & De Ridder 2014), isoclassify (Huber et al. 2017), EXOFASTv2 (Eastman 2017), ktransit (Barclay 2018).","publication_identifier":{"issn":["0004-6256"]},"publication_status":"published","title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","oa_version":"Preprint","article_processing_charge":"No","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"extern":"1","month":"05","status":"public","publisher":"IOP Publishing","date_published":"2019-05-30T00:00:00Z","external_id":{"arxiv":["1901.01643"]},"type":"journal_article","issue":"6","day":"30","quality_controlled":"1"}]