[{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1901.01643"}],"language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"245","year":"2019","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"last_name":"Huber","full_name":"Huber, Daniel","first_name":"Daniel"},{"last_name":"Chaplin","full_name":"Chaplin, William J.","first_name":"William J."},{"first_name":"Ashley","last_name":"Chontos","full_name":"Chontos, Ashley"},{"first_name":"Hans","last_name":"Kjeldsen","full_name":"Kjeldsen, Hans"},{"last_name":"Christensen-Dalsgaard","full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen"},{"last_name":"Bedding","full_name":"Bedding, Timothy R.","first_name":"Timothy R."},{"full_name":"Ball, Warrick","last_name":"Ball","first_name":"Warrick"},{"last_name":"Brahm","full_name":"Brahm, Rafael","first_name":"Rafael"},{"last_name":"Espinoza","full_name":"Espinoza, Nestor","first_name":"Nestor"},{"full_name":"Henning, Thomas","last_name":"Henning","first_name":"Thomas"},{"first_name":"Andrés","last_name":"Jordán","full_name":"Jordán, Andrés"},{"last_name":"Sarkis","full_name":"Sarkis, Paula","first_name":"Paula"},{"full_name":"Knudstrup, Emil","last_name":"Knudstrup","first_name":"Emil"},{"last_name":"Albrecht","full_name":"Albrecht, Simon","first_name":"Simon"},{"last_name":"Grundahl","full_name":"Grundahl, Frank","first_name":"Frank"},{"full_name":"Andersen, Mads Fredslund","last_name":"Andersen","first_name":"Mads Fredslund"},{"first_name":"Pere L.","last_name":"Pallé","full_name":"Pallé, Pere L."},{"first_name":"Ian","last_name":"Crossfield","full_name":"Crossfield, Ian"},{"full_name":"Fulton, Benjamin","last_name":"Fulton","first_name":"Benjamin"},{"full_name":"Howard, Andrew W.","last_name":"Howard","first_name":"Andrew W."},{"full_name":"Isaacson, Howard T.","last_name":"Isaacson","first_name":"Howard T."},{"full_name":"Weiss, Lauren M.","last_name":"Weiss","first_name":"Lauren M."},{"last_name":"Handberg","full_name":"Handberg, Rasmus","first_name":"Rasmus"},{"first_name":"Mikkel N.","last_name":"Lund","full_name":"Lund, Mikkel N."},{"first_name":"Aldo M.","full_name":"Serenelli, Aldo M.","last_name":"Serenelli"},{"first_name":"Jakob","last_name":"Rørsted Mosumgaard","full_name":"Rørsted Mosumgaard, Jakob"},{"full_name":"Stokholm, Amalie","last_name":"Stokholm","first_name":"Amalie"},{"last_name":"Bieryla","full_name":"Bieryla, Allyson","first_name":"Allyson"},{"last_name":"Buchhave","full_name":"Buchhave, Lars A.","first_name":"Lars A."},{"full_name":"Latham, David W.","last_name":"Latham","first_name":"David W."},{"last_name":"Quinn","full_name":"Quinn, Samuel N.","first_name":"Samuel N."},{"first_name":"Eric","full_name":"Gaidos, Eric","last_name":"Gaidos"},{"last_name":"Hirano","full_name":"Hirano, Teruyuki","first_name":"Teruyuki"},{"full_name":"Ricker, George R.","last_name":"Ricker","first_name":"George R."},{"first_name":"Roland K.","last_name":"Vanderspek","full_name":"Vanderspek, Roland K."},{"last_name":"Seager","full_name":"Seager, Sara","first_name":"Sara"},{"first_name":"Jon M.","last_name":"Jenkins","full_name":"Jenkins, Jon M."},{"full_name":"Winn, Joshua N.","last_name":"Winn","first_name":"Joshua N."},{"first_name":"H. M.","full_name":"Antia, H. M.","last_name":"Antia"},{"first_name":"Thierry","full_name":"Appourchaux, Thierry","last_name":"Appourchaux"},{"first_name":"Sarbani","last_name":"Basu","full_name":"Basu, Sarbani"},{"first_name":"Keaton J.","full_name":"Bell, Keaton J.","last_name":"Bell"},{"first_name":"Othman","last_name":"Benomar","full_name":"Benomar, Othman"},{"full_name":"Bonanno, Alfio","last_name":"Bonanno","first_name":"Alfio"},{"first_name":"Derek L.","last_name":"Buzasi","full_name":"Buzasi, Derek L."},{"first_name":"Tiago L.","full_name":"Campante, Tiago L.","last_name":"Campante"},{"last_name":"Çelik Orhan","full_name":"Çelik Orhan, Z.","first_name":"Z."},{"first_name":"Enrico","full_name":"Corsaro, Enrico","last_name":"Corsaro"},{"first_name":"Margarida S.","last_name":"Cunha","full_name":"Cunha, Margarida S."},{"last_name":"Davies","full_name":"Davies, Guy R.","first_name":"Guy R."},{"first_name":"Sebastien","full_name":"Deheuvels, Sebastien","last_name":"Deheuvels"},{"full_name":"Grunblatt, Samuel K.","last_name":"Grunblatt","first_name":"Samuel K."},{"first_name":"Amir","last_name":"Hasanzadeh","full_name":"Hasanzadeh, Amir"},{"first_name":"Maria Pia","full_name":"Di Mauro, Maria Pia","last_name":"Di Mauro"},{"first_name":"Rafael","full_name":"A. García, Rafael","last_name":"A. 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G. Monteiro, Mário J. P.","last_name":"F. G. Monteiro","first_name":"Mário J. P."},{"last_name":"Mosser","full_name":"Mosser, Benoit","first_name":"Benoit"},{"full_name":"Noll, Anthony","last_name":"Noll","first_name":"Anthony"},{"full_name":"Nsamba, Benard","last_name":"Nsamba","first_name":"Benard"},{"first_name":"Jia Mian","full_name":"Joel Ong, Jia Mian","last_name":"Joel Ong"},{"first_name":"S.","last_name":"Örtel","full_name":"Örtel, S."},{"last_name":"Pereira","full_name":"Pereira, Filipe","first_name":"Filipe"},{"first_name":"Pritesh","full_name":"Ranadive, Pritesh","last_name":"Ranadive"},{"first_name":"Clara","last_name":"Régulo","full_name":"Régulo, Clara"},{"full_name":"Rodrigues, Thaíse S.","last_name":"Rodrigues","first_name":"Thaíse S."},{"first_name":"Ian W.","full_name":"Roxburgh, Ian W.","last_name":"Roxburgh"},{"last_name":"Aguirre","full_name":"Aguirre, Victor Silva","first_name":"Victor Silva"},{"first_name":"Barry","last_name":"Smalley","full_name":"Smalley, Barry"},{"last_name":"Schofield","full_name":"Schofield, Mathew","first_name":"Mathew"},{"full_name":"Sousa, Sérgio G.","last_name":"Sousa","first_name":"Sérgio G."},{"first_name":"Keivan G.","last_name":"Stassun","full_name":"Stassun, Keivan G."},{"last_name":"Stello","full_name":"Stello, Dennis","first_name":"Dennis"},{"last_name":"Tayar","full_name":"Tayar, Jamie","first_name":"Jamie"},{"last_name":"White","full_name":"White, Timothy R.","first_name":"Timothy R."},{"last_name":"Verma","full_name":"Verma, Kuldeep","first_name":"Kuldeep"},{"first_name":"Mathieu","full_name":"Vrard, Mathieu","last_name":"Vrard"},{"last_name":"Yıldız","full_name":"Yıldız, M.","first_name":"M."},{"full_name":"Baker, David","last_name":"Baker","first_name":"David"},{"full_name":"Bazot, Michaël","last_name":"Bazot","first_name":"Michaël"},{"full_name":"Beichmann, Charles","last_name":"Beichmann","first_name":"Charles"},{"first_name":"Christoph","full_name":"Bergmann, Christoph","last_name":"Bergmann"},{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Cale","full_name":"Cale, Bryson","first_name":"Bryson"},{"full_name":"Carlino, Roberto","last_name":"Carlino","first_name":"Roberto"},{"full_name":"Cartwright, Scott M.","last_name":"Cartwright","first_name":"Scott M."},{"last_name":"Christiansen","full_name":"Christiansen, Jessie L.","first_name":"Jessie L."},{"full_name":"Ciardi, David R.","last_name":"Ciardi","first_name":"David R."},{"first_name":"Orlagh","last_name":"Creevey","full_name":"Creevey, Orlagh"},{"full_name":"Dittmann, Jason A.","last_name":"Dittmann","first_name":"Jason A."},{"full_name":"Nascimento, Jose-Dias Do","last_name":"Nascimento","first_name":"Jose-Dias Do"},{"last_name":"Eylen","full_name":"Eylen, Vincent Van","first_name":"Vincent Van"},{"full_name":"Fürész, Gabor","last_name":"Fürész","first_name":"Gabor"},{"first_name":"Jonathan","full_name":"Gagné, Jonathan","last_name":"Gagné"},{"full_name":"Gao, Peter","last_name":"Gao","first_name":"Peter"},{"full_name":"Gazeas, Kosmas","last_name":"Gazeas","first_name":"Kosmas"},{"last_name":"Giddens","full_name":"Giddens, Frank","first_name":"Frank"},{"first_name":"Oliver J.","full_name":"Hall, Oliver J.","last_name":"Hall"},{"last_name":"Hekker","full_name":"Hekker, Saskia","first_name":"Saskia"},{"last_name":"Ireland","full_name":"Ireland, Michael J.","first_name":"Michael J."},{"last_name":"Latouf","full_name":"Latouf, Natasha","first_name":"Natasha"},{"first_name":"Danny","full_name":"LeBrun, Danny","last_name":"LeBrun"},{"full_name":"Levine, Alan M.","last_name":"Levine","first_name":"Alan M."},{"full_name":"Matzko, William","last_name":"Matzko","first_name":"William"},{"first_name":"Eva","last_name":"Natinsky","full_name":"Natinsky, Eva"},{"last_name":"Page","full_name":"Page, Emma","first_name":"Emma"},{"full_name":"Plavchan, Peter","last_name":"Plavchan","first_name":"Peter"},{"first_name":"Masoud","last_name":"Mansouri-Samani","full_name":"Mansouri-Samani, Masoud"},{"first_name":"Sean","full_name":"McCauliff, Sean","last_name":"McCauliff"},{"first_name":"Susan E.","full_name":"Mullally, Susan E.","last_name":"Mullally"},{"full_name":"Orenstein, Brendan","last_name":"Orenstein","first_name":"Brendan"},{"last_name":"Soto","full_name":"Soto, Aylin Garcia","first_name":"Aylin Garcia"},{"full_name":"Paegert, Martin","last_name":"Paegert","first_name":"Martin"},{"first_name":"Jennifer L.","last_name":"van Saders","full_name":"van Saders, Jennifer L."},{"first_name":"Chloe","full_name":"Schnaible, Chloe","last_name":"Schnaible"},{"first_name":"David R.","full_name":"Soderblom, David R.","last_name":"Soderblom"},{"last_name":"Szabó","full_name":"Szabó, Róbert","first_name":"Róbert"},{"last_name":"Tanner","full_name":"Tanner, Angelle","first_name":"Angelle"},{"first_name":"C. G.","full_name":"Tinney, C. G.","last_name":"Tinney"},{"full_name":"Teske, Johanna","last_name":"Teske","first_name":"Johanna"},{"full_name":"Thomas, Alexandra","last_name":"Thomas","first_name":"Alexandra"},{"full_name":"Trampedach, Regner","last_name":"Trampedach","first_name":"Regner"},{"full_name":"Wright, Duncan","last_name":"Wright","first_name":"Duncan"},{"first_name":"Thomas T.","last_name":"Yuan","full_name":"Yuan, Thomas T."},{"first_name":"Farzaneh","last_name":"Zohrabi","full_name":"Zohrabi, Farzaneh"}],"date_created":"2022-07-18T14:29:07Z","_id":"11616","doi":"10.3847/1538-3881/ab1488","issue":"6","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).","scopus_import":"1","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"}],"arxiv":1,"title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","oa_version":"Preprint","day":"30","date_updated":"2022-08-22T07:38:34Z","article_processing_charge":"No","date_published":"2019-05-30T00:00:00Z","publication_status":"published","status":"public","publication":"The Astronomical Journal","quality_controlled":"1","extern":"1","external_id":{"arxiv":["1901.01643"]},"type":"journal_article","month":"05","oa":1,"publisher":"IOP Publishing","volume":157,"publication_identifier":{"issn":["0004-6256"]},"intvolume":"       157","article_type":"original","citation":{"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.","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>.","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).","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>","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>"}},{"abstract":[{"lang":"eng","text":"Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy Sph using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with Sph being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods."}],"arxiv":1,"title":"Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars","oa_version":"Preprint","date_updated":"2022-08-22T08:10:38Z","day":"19","article_processing_charge":"No","date_published":"2019-09-19T00:00:00Z","publication_status":"published","status":"public","publication":"The Astrophysical Journal Supplement Series","quality_controlled":"1","extern":"1","external_id":{"arxiv":["1908.05222"]},"month":"09","type":"journal_article","publisher":"IOP Publishing","oa":1,"volume":244,"publication_identifier":{"issn":["0067-0049"]},"intvolume":"       244","article_type":"original","citation":{"ama":"Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. 2019;244(1). doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>","apa":"Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J. L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>","ieee":"A. R. G. Santos <i>et al.</i>, “Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars,” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1. IOP Publishing, 2019.","ista":"Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 244(1), 21.","chicago":"Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L. van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>.","mla":"Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>.","short":"A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S. Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement Series 244 (2019)."},"language":[{"iso":"eng"}],"main_file_link":[{"url":"https://arxiv.org/abs/1908.05222","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"21","year":"2019","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis","stars: activity","stars: low-mass","stars: rotation","starspots","techniques: photometric"],"author":[{"first_name":"A. R. G.","full_name":"Santos, A. R. G.","last_name":"Santos"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"first_name":"S.","full_name":"Mathur, S.","last_name":"Mathur"},{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"van Saders, J. L.","last_name":"van Saders","first_name":"J. L."},{"last_name":"Metcalfe","full_name":"Metcalfe, T. S.","first_name":"T. S."},{"first_name":"G. V. A.","full_name":"Simonian, G. V. A.","last_name":"Simonian"},{"first_name":"M. H.","full_name":"Pinsonneault, M. H.","last_name":"Pinsonneault"}],"date_created":"2022-07-19T09:21:58Z","_id":"11623","doi":"10.3847/1538-4365/ab3b56","issue":"1","acknowledgement":"The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg, and Isabel L. Colman for helping on the classification of stars. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the National Aeronautics and Space Administration (NASA) Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at the Max Planck Institute for Solar System Research. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy (van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities: MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -","scopus_import":"1"},{"author":[{"first_name":"Emmanouil","full_name":"Zapartas, Emmanouil","last_name":"Zapartas"},{"full_name":"de Mink, Selma E.","last_name":"de Mink","first_name":"Selma E."},{"first_name":"Stephen","full_name":"Justham, Stephen","last_name":"Justham"},{"last_name":"Smith","full_name":"Smith, Nathan","first_name":"Nathan"},{"first_name":"Alex","last_name":"de Koter","full_name":"de Koter, Alex"},{"full_name":"Renzo, Mathieu","last_name":"Renzo","first_name":"Mathieu"},{"first_name":"Iair","last_name":"Arcavi","full_name":"Arcavi, Iair"},{"full_name":"Farmer, Rob","last_name":"Farmer","first_name":"Rob"},{"full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"last_name":"Toonen","full_name":"Toonen, Silvia","first_name":"Silvia"}],"date_created":"2023-08-03T10:13:52Z","scopus_import":"1","_id":"13468","doi":"10.1051/0004-6361/201935854","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201935854"}],"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_number":"A5","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2019","oa":1,"volume":631,"publisher":"EDP Sciences","intvolume":"       631","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"extern":"1","quality_controlled":"1","month":"11","type":"journal_article","external_id":{"arxiv":["1907.06687"]},"citation":{"apa":"Zapartas, E., de Mink, S. E., Justham, S., Smith, N., de Koter, A., Renzo, M., … Toonen, S. (2019). The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>","ama":"Zapartas E, de Mink SE, Justham S, et al. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. 2019;631. doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>","mla":"Zapartas, Emmanouil, et al. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>, vol. 631, A5, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>.","short":"E. Zapartas, S.E. de Mink, S. Justham, N. Smith, A. de Koter, M. Renzo, I. Arcavi, R. Farmer, Y.L.L. Götberg, S. Toonen, Astronomy &#38; Astrophysics 631 (2019).","ieee":"E. Zapartas <i>et al.</i>, “The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction,” <i>Astronomy &#38; Astrophysics</i>, vol. 631. EDP Sciences, 2019.","ista":"Zapartas E, de Mink SE, Justham S, Smith N, de Koter A, Renzo M, Arcavi I, Farmer R, Götberg YLL, Toonen S. 2019. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. Astronomy &#38; Astrophysics. 631, A5.","chicago":"Zapartas, Emmanouil, Selma E. de Mink, Stephen Justham, Nathan Smith, Alex de Koter, Mathieu Renzo, Iair Arcavi, Rob Farmer, Ylva Louise Linsdotter Götberg, and Silvia Toonen. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>."},"article_type":"original","title":"The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction","arxiv":1,"abstract":[{"text":"Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class of explosions observed following the collapse of the core of massive stars. We used analytical estimates and population synthesis simulations to assess the fraction of SNe II progenitors that are expected to have exchanged mass with a companion prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history of mass exchange with a binary companion before exploding. The dominant binary channels leading to SN II progenitors involve the merger of binary stars. Mergers are expected to produce a diversity of SN II progenitor characteristics, depending on the evolutionary timing and properties of the merger. Alternatively, SN II progenitors from interacting binaries may have accreted mass from their companion, and subsequently been ejected from the binary system after their companion exploded. We show that the overall fraction of SN II progenitors that are predicted to have experienced binary interaction is robust against the main physical uncertainties in our models. However, the relative importance of different binary evolutionary channels is affected by changing physical assumptions. We further discuss ways in which binarity might contribute to the observed diversity of SNe II by considering potential observational signatures arising from each binary channel. For supernovae which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb SNe), a surviving non-compact companion would typically indicate that the supernova progenitor star was in a wide, non-interacting binary. We argue that a significant fraction of even Type II-P SNe are expected to have gained mass from a companion prior to explosion.","lang":"eng"}],"publication":"Astronomy & Astrophysics","publication_status":"published","status":"public","date_updated":"2023-08-09T12:36:09Z","day":"20","oa_version":"Published Version","article_processing_charge":"No","date_published":"2019-11-20T00:00:00Z"},{"article_type":"original","citation":{"short":"Y.L.L. Götberg, S.E. de Mink, J.H. Groh, C. Leitherer, C. Norman, Astronomy &#38; Astrophysics 629 (2019).","mla":"Götberg, Ylva Louise Linsdotter, et al. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>, vol. 629, A134, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>.","ista":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. 2019. The impact of stars stripped in binaries on the integrated spectra of stellar populations. Astronomy &#38; Astrophysics. 629, A134.","ieee":"Y. L. L. Götberg, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman, “The impact of stars stripped in binaries on the integrated spectra of stellar populations,” <i>Astronomy &#38; Astrophysics</i>, vol. 629. EDP Sciences, 2019.","apa":"Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Leitherer, C., &#38; Norman, C. (2019). The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>","ama":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. 2019;629. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>"},"quality_controlled":"1","extern":"1","month":"09","external_id":{"arxiv":["1908.06102"]},"type":"journal_article","oa":1,"publisher":"EDP Sciences","volume":629,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"intvolume":"       629","oa_version":"Published Version","date_updated":"2024-10-14T12:22:42Z","day":"17","article_processing_charge":"No","date_published":"2019-09-17T00:00:00Z","publication_status":"published","status":"public","publication":"Astronomy & Astrophysics","abstract":[{"text":"Stars stripped of their envelopes from interaction with a binary companion emit a significant fraction of their radiation as ionizing photons. They are potentially important stellar sources of ionizing radiation, however, they are still often neglected in spectral synthesis simulations or simulations of stellar feedback. In anticipating the large datasets of galaxy spectra from the upcoming James Webb Space Telescope, we modeled the radiative contribution from stripped stars by using detailed evolutionary and spectral models. We estimated their impact on the integrated spectra and specifically on the emission rates of H I-, He I-, and He II-ionizing photons from stellar populations. We find that stripped stars have the largest impact on the ionizing spectrum of a population in which star formation halted several Myr ago. In such stellar populations, stripped stars dominate the emission of ionizing photons, mimicking a younger stellar population in which massive stars are still present. Our models also suggest that stripped stars have harder ionizing spectra than massive stars. The additional ionizing radiation, with which stripped stars contribute affects observable properties that are related to the emission of ionizing photons from stellar populations. In co-eval stellar populations, the ionizing radiation from stripped stars increases the ionization parameter and the production efficiency of hydrogen ionizing photons. They also cause high values for these parameters for about ten times longer than what is predicted for massive stars. The effect on properties related to non-ionizing wavelengths is less pronounced, such as on the ultraviolet continuum slope or stellar contribution to emission lines. However, the hard ionizing radiation from stripped stars likely introduces a characteristic ionization structure of the nebula, which leads to the emission of highly ionized elements such as O2+ and C3+. We, therefore, expect that the presence of stripped stars affects the location in the BPT diagram and the diagnostic ratio of O III to O II nebular emission lines. Our models are publicly available through CDS database and on the STARBURST99 website.","lang":"eng"}],"arxiv":1,"title":"The impact of stars stripped in binaries on the integrated spectra of stellar populations","_id":"13469","doi":"10.1051/0004-6361/201834525","scopus_import":"1","author":[{"first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter"},{"first_name":"S. E.","last_name":"de Mink","full_name":"de Mink, S. E."},{"full_name":"Groh, J. H.","last_name":"Groh","first_name":"J. H."},{"last_name":"Leitherer","full_name":"Leitherer, C.","first_name":"C."},{"first_name":"C.","last_name":"Norman","full_name":"Norman, C."}],"date_created":"2023-08-03T10:14:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A134","year":"2019","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201834525","open_access":"1"}]},{"article_type":"original","citation":{"ista":"Shenar T, Sablowski DP, Hainich R, Todt H, Moffat AFJ, Oskinova LM, Ramachandran V, Sana H, Sander AAC, Schnurr O, St-Louis N, Vanbeveren D, Götberg YLL, Hamann W-R. 2019. The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. Astronomy &#38; Astrophysics. 627, A151.","chicago":"Shenar, T., D. P. Sablowski, R. Hainich, H. Todt, A. F. J. Moffat, L. M. Oskinova, V. Ramachandran, et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence in the Large Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201935684\">https://doi.org/10.1051/0004-6361/201935684</a>.","ieee":"T. Shenar <i>et al.</i>, “The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud,” <i>Astronomy &#38; Astrophysics</i>, vol. 627. EDP Sciences, 2019.","short":"T. Shenar, D.P. Sablowski, R. Hainich, H. Todt, A.F.J. Moffat, L.M. Oskinova, V. Ramachandran, H. Sana, A.A.C. Sander, O. Schnurr, N. St-Louis, D. Vanbeveren, Y.L.L. Götberg, W.-R. Hamann, Astronomy &#38; Astrophysics 627 (2019).","mla":"Shenar, T., et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence in the Large Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>, vol. 627, A151, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201935684\">10.1051/0004-6361/201935684</a>.","ama":"Shenar T, Sablowski DP, Hainich R, et al. The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. 2019;627. doi:<a href=\"https://doi.org/10.1051/0004-6361/201935684\">10.1051/0004-6361/201935684</a>","apa":"Shenar, T., Sablowski, D. P., Hainich, R., Todt, H., Moffat, A. F. J., Oskinova, L. M., … Hamann, W.-R. (2019). The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201935684\">https://doi.org/10.1051/0004-6361/201935684</a>"},"extern":"1","quality_controlled":"1","month":"07","type":"journal_article","publisher":"EDP Sciences","oa":1,"volume":627,"intvolume":"       627","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2023-08-09T12:29:58Z","day":"16","oa_version":"Published Version","article_processing_charge":"No","date_published":"2019-07-16T00:00:00Z","publication":"Astronomy & Astrophysics","status":"public","publication_status":"published","abstract":[{"text":"Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z ≈ 0.5 Z⊙), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities.\r\n\r\nAims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars.\r\n\r\nMethods. Spectroscopy was performed using the Potsdam Wolf–Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution.\r\n\r\nResults. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45  ±  30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only ≈12  ±  7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises ≈4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L ≈ 5.2 [L⊙], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (veq ≲ 250 km s−1) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor.\r\n\r\nConclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models.","lang":"eng"}],"title":"The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud","_id":"13470","doi":"10.1051/0004-6361/201935684","scopus_import":"1","author":[{"first_name":"T.","full_name":"Shenar, T.","last_name":"Shenar"},{"full_name":"Sablowski, D. P.","last_name":"Sablowski","first_name":"D. P."},{"full_name":"Hainich, R.","last_name":"Hainich","first_name":"R."},{"full_name":"Todt, H.","last_name":"Todt","first_name":"H."},{"last_name":"Moffat","full_name":"Moffat, A. F. J.","first_name":"A. F. J."},{"first_name":"L. M.","last_name":"Oskinova","full_name":"Oskinova, L. M."},{"last_name":"Ramachandran","full_name":"Ramachandran, V.","first_name":"V."},{"last_name":"Sana","full_name":"Sana, H.","first_name":"H."},{"last_name":"Sander","full_name":"Sander, A. A. C.","first_name":"A. A. C."},{"last_name":"Schnurr","full_name":"Schnurr, O.","first_name":"O."},{"last_name":"St-Louis","full_name":"St-Louis, N.","first_name":"N."},{"full_name":"Vanbeveren, D.","last_name":"Vanbeveren","first_name":"D."},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"last_name":"Hamann","full_name":"Hamann, W.-R.","first_name":"W.-R."}],"date_created":"2023-08-03T10:14:09Z","article_number":"A151","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2019","related_material":{"link":[{"url":"https://doi.org/10.1051/0004-6361/201935684e","relation":"erratum"}]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201935684","open_access":"1"}],"language":[{"iso":"eng"}]},{"scopus_import":"1","doi":"10.1051/0004-6361/201833297","_id":"13471","date_created":"2023-08-03T10:14:18Z","author":[{"first_name":"M.","full_name":"Renzo, M.","last_name":"Renzo"},{"first_name":"E.","last_name":"Zapartas","full_name":"Zapartas, E."},{"last_name":"de Mink","full_name":"de Mink, S. E.","first_name":"S. E."},{"full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"full_name":"Justham, S.","last_name":"Justham","first_name":"S."},{"full_name":"Farmer, R. J.","last_name":"Farmer","first_name":"R. J."},{"first_name":"R. G.","full_name":"Izzard, R. G.","last_name":"Izzard"},{"last_name":"Toonen","full_name":"Toonen, S.","first_name":"S."},{"first_name":"H.","last_name":"Sana","full_name":"Sana, H."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2019","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A66","language":[{"iso":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201833297","open_access":"1"}],"citation":{"ieee":"M. Renzo <i>et al.</i>, “Massive runaway and walkaway stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 624. EDP Sciences, 2019.","ista":"Renzo M, Zapartas E, de Mink SE, Götberg YLL, Justham S, Farmer RJ, Izzard RG, Toonen S, Sana H. 2019. Massive runaway and walkaway stars. Astronomy &#38; Astrophysics. 624, A66.","chicago":"Renzo, M., E. Zapartas, S. E. de Mink, Ylva Louise Linsdotter Götberg, S. Justham, R. J. Farmer, R. G. Izzard, S. Toonen, and H. Sana. “Massive Runaway and Walkaway Stars.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201833297\">https://doi.org/10.1051/0004-6361/201833297</a>.","mla":"Renzo, M., et al. “Massive Runaway and Walkaway Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 624, A66, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833297\">10.1051/0004-6361/201833297</a>.","short":"M. Renzo, E. Zapartas, S.E. de Mink, Y.L.L. Götberg, S. Justham, R.J. Farmer, R.G. Izzard, S. Toonen, H. Sana, Astronomy &#38; Astrophysics 624 (2019).","ama":"Renzo M, Zapartas E, de Mink SE, et al. Massive runaway and walkaway stars. <i>Astronomy &#38; Astrophysics</i>. 2019;624. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833297\">10.1051/0004-6361/201833297</a>","apa":"Renzo, M., Zapartas, E., de Mink, S. E., Götberg, Y. L. L., Justham, S., Farmer, R. J., … Sana, H. (2019). Massive runaway and walkaway stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833297\">https://doi.org/10.1051/0004-6361/201833297</a>"},"article_type":"original","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"intvolume":"       624","volume":624,"publisher":"EDP Sciences","oa":1,"external_id":{"arxiv":["1804.09164"]},"month":"04","type":"journal_article","quality_controlled":"1","extern":"1","publication_status":"published","status":"public","publication":"Astronomy & Astrophysics","date_published":"2019-04-11T00:00:00Z","article_processing_charge":"No","oa_version":"Published Version","day":"11","date_updated":"2023-08-09T12:26:08Z","title":"Massive runaway and walkaway stars","abstract":[{"lang":"eng","text":"We perform an extensive numerical study of the evolution of massive binary systems to predict the peculiar velocities that stars obtain when their companion collapses and disrupts the system. Our aim is to (i) identify which predictions are robust against model uncertainties and assess their implications, (ii) investigate which physical processes leave a clear imprint and may therefore be constrained observationally, and (iii) provide a suite of publicly available model predictions to allow for the use of kinematic constraints from the Gaia mission. We find that 22+26−8% of all massive binary systems merge prior to the first core-collapse in the system. Of the remainder, 86+11−9% become unbound because of the core-collapse. Remarkably, this rarely produces runaway stars (observationally defined as stars with velocities above 30 km s−1). These are outnumbered by more than an order of magnitude by slower unbound companions, or “walkaway stars”. This is a robust outcome of our simulations and is due to the reversal of the mass ratio prior to the explosion and widening of the orbit, as we show analytically and numerically. For stars more massive than 15 M⊙, we estimate that 10+5−8% are walkaways and only 0.5+1.0−0.4% are runaways, nearly all of which have accreted mass from their companion. Our findings are consistent with earlier studies; however, the low runaway fraction we find is in tension with observed fractions of about 10%. Thus, astrometric data on presently single massive stars can potentially constrain the physics of massive binary evolution. Finally, we show that the high end of the mass distributions of runaway stars is very sensitive to the assumed black hole natal kicks, and we propose this as a potentially stringent test for the explosion mechanism. We also discuss companions remaining bound that can evolve into X-ray and gravitational wave sources."}],"arxiv":1},{"day":"27","date_updated":"2023-08-09T12:28:17Z","oa_version":"Published Version","article_processing_charge":"No","date_published":"2019-03-27T00:00:00Z","publication":"Astronomy & Astrophysics","publication_status":"published","status":"public","arxiv":1,"abstract":[{"lang":"eng","text":"Massive stars in binaries can give rise to extreme phenomena such as X-ray binaries and gravitational wave sources after one or both stars end their lives as core-collapse supernovae. Stars in close orbit around a stellar or compact companion are expected to explode as “stripped-envelope supernovae”, showing no (Type Ib/c) or little (Type IIb) signs of hydrogen in the spectra, because hydrogen-rich progenitors are too large to fit. The physical processes responsible for the stripping process and the fate of the companion are still very poorly understood. Aiming to find new clues, we investigate Cas A, which is a very young (∼340 yr) and near (∼3.4 kpc) remnant of a core-collapse supernova. Cas A has been subject to several searches for possible companions, all unsuccessfully. We present new measurements of the proper motions and photometry of stars in the vicinity based on deep HST ACS/WFC and WFC3-IR data. We identify stellar sources that are close enough in projection but using their proper motions we show that none are compatible with being at the location of center at the time of explosion, in agreement with earlier findings. Our photometric measurements allow us to place much deeper (order-of-magnitude) upper limits on the brightness of possible undetected companions. We systematically compare them with model predictions for a wide variety of scenarios. We can confidently rule out the presence of any stellar companion of any reasonable mass and age (main sequence, pre main sequence or stripped) ruling out what many considered to be likely evolutionary scenarios for Type IIb supernova (SN IIb). More exotic scenarios that predict the presence of a compact companion (white dwarf, neutron star or black hole) are still possible as well as scenarios where the progenitor of Cas A was single at the moment of explosion (either because it was truly single, or resulted from a binary that was disrupted, or from a binary merger). The presence of a compact companion would imply that Cas A is of interest to study exotic outcomes of binary evolution. The single-at-death solution would still require fine-tuning of the process that removed most of the envelope through a mass-loss mechanism yet to be identified. We discuss how future constraints from Gaia and even deeper photometric studies may help to place further constraints."}],"title":"No surviving non-compact stellar companion to Cassiopeia A","article_type":"original","citation":{"ieee":"W. E. Kerzendorf <i>et al.</i>, “No surviving non-compact stellar companion to Cassiopeia A,” <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.","chicago":"Kerzendorf, Wolfgang E., Tuan Do, Selma E. de Mink, Ylva Louise Linsdotter Götberg, Dan Milisavljevic, Emmanouil Zapartas, Mathieu Renzo, Stephen Justham, Philipp Podsiadlowski, and Robert A. Fesen. “No Surviving Non-Compact Stellar Companion to Cassiopeia A.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201732206\">https://doi.org/10.1051/0004-6361/201732206</a>.","ista":"Kerzendorf WE, Do T, de Mink SE, Götberg YLL, Milisavljevic D, Zapartas E, Renzo M, Justham S, Podsiadlowski P, Fesen RA. 2019. No surviving non-compact stellar companion to Cassiopeia A. Astronomy &#38; Astrophysics. 623, A34.","mla":"Kerzendorf, Wolfgang E., et al. “No Surviving Non-Compact Stellar Companion to Cassiopeia A.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A34, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201732206\">10.1051/0004-6361/201732206</a>.","short":"W.E. Kerzendorf, T. Do, S.E. de Mink, Y.L.L. Götberg, D. Milisavljevic, E. Zapartas, M. Renzo, S. Justham, P. Podsiadlowski, R.A. Fesen, Astronomy &#38; Astrophysics 623 (2019).","ama":"Kerzendorf WE, Do T, de Mink SE, et al. No surviving non-compact stellar companion to Cassiopeia A. <i>Astronomy &#38; Astrophysics</i>. 2019;623. doi:<a href=\"https://doi.org/10.1051/0004-6361/201732206\">10.1051/0004-6361/201732206</a>","apa":"Kerzendorf, W. E., Do, T., de Mink, S. E., Götberg, Y. L. L., Milisavljevic, D., Zapartas, E., … Fesen, R. A. (2019). No surviving non-compact stellar companion to Cassiopeia A. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201732206\">https://doi.org/10.1051/0004-6361/201732206</a>"},"extern":"1","quality_controlled":"1","type":"journal_article","external_id":{"arxiv":["1711.00055"]},"month":"03","oa":1,"volume":623,"publisher":"EDP Sciences","intvolume":"       623","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_number":"A34","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2019","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201732206"}],"language":[{"iso":"eng"}],"_id":"13472","doi":"10.1051/0004-6361/201732206","scopus_import":"1","author":[{"first_name":"Wolfgang E.","last_name":"Kerzendorf","full_name":"Kerzendorf, Wolfgang E."},{"first_name":"Tuan","full_name":"Do, Tuan","last_name":"Do"},{"first_name":"Selma E.","last_name":"de Mink","full_name":"de Mink, Selma E."},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"Dan","last_name":"Milisavljevic","full_name":"Milisavljevic, Dan"},{"first_name":"Emmanouil","full_name":"Zapartas, Emmanouil","last_name":"Zapartas"},{"last_name":"Renzo","full_name":"Renzo, Mathieu","first_name":"Mathieu"},{"last_name":"Justham","full_name":"Justham, Stephen","first_name":"Stephen"},{"full_name":"Podsiadlowski, Philipp","last_name":"Podsiadlowski","first_name":"Philipp"},{"first_name":"Robert A.","last_name":"Fesen","full_name":"Fesen, Robert A."}],"date_created":"2023-08-03T10:14:27Z"},{"month":"07","type":"journal_article","external_id":{"arxiv":["1906.04727"]},"quality_controlled":"1","extern":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"intvolume":"       880","volume":880,"publisher":"American Astronomical Society","oa":1,"article_type":"original","citation":{"ieee":"H. B. Richer <i>et al.</i>, “A massive magnetic helium atmosphere white dwarf binary in a young star cluster,” <i>The Astrophysical Journal</i>, vol. 880, no. 2. American Astronomical Society, 2019.","ista":"Richer HB, Kerr R, Heyl J, Caiazzo I, Cummings J, Bergeron P, Dufour P. 2019. A massive magnetic helium atmosphere white dwarf binary in a young star cluster. The Astrophysical Journal. 880(2), 75.","chicago":"Richer, Harvey B., Ronan Kerr, Jeremy Heyl, Ilaria Caiazzo, Jeffrey Cummings, Pierre Bergeron, and Patrick Dufour. “A Massive Magnetic Helium Atmosphere White Dwarf Binary in a Young Star Cluster.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab2874\">https://doi.org/10.3847/1538-4357/ab2874</a>.","mla":"Richer, Harvey B., et al. “A Massive Magnetic Helium Atmosphere White Dwarf Binary in a Young Star Cluster.” <i>The Astrophysical Journal</i>, vol. 880, no. 2, 75, American Astronomical Society, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2874\">10.3847/1538-4357/ab2874</a>.","short":"H.B. Richer, R. Kerr, J. Heyl, I. Caiazzo, J. Cummings, P. Bergeron, P. Dufour, The Astrophysical Journal 880 (2019).","ama":"Richer HB, Kerr R, Heyl J, et al. A massive magnetic helium atmosphere white dwarf binary in a young star cluster. <i>The Astrophysical Journal</i>. 2019;880(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2874\">10.3847/1538-4357/ab2874</a>","apa":"Richer, H. B., Kerr, R., Heyl, J., Caiazzo, I., Cummings, J., Bergeron, P., &#38; Dufour, P. (2019). A massive magnetic helium atmosphere white dwarf binary in a young star cluster. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ab2874\">https://doi.org/10.3847/1538-4357/ab2874</a>"},"abstract":[{"text":"We have searched the Gaia DR2 catalog for previously unknown hot white dwarfs in the direction of young open star clusters. The aim of this experiment was to try and extend the initial–final mass relation (IFMR) to somewhat higher masses, potentially challenging the Chandrasekhar limit currently thought to be around 1.38 M⊙. We discovered a particularly interesting white dwarf in the direction of the young ∼150 Myr old cluster Messier 47 (NGC 2422). All Gaia indicators (proper motion, parallax, location in the Gaia color–magnitude diagram) suggest that it is a cluster member. Its spectrum, obtained from Gemini-South, yields a number of anomalies: it is a DB (helium-rich atmosphere) white dwarf, it has a large magnetic field (2.5 MG), is of high mass (∼1.06 M⊙), and its colors are very peculiar—particularly the redder ones (r, i, z and y), which suggests that it may have a late-type companion. This may be the only magnetized, detached binary white dwarf with a non-degenerate companion of any spectral type known in or out of a star cluster. If the white dwarf is a cluster member, as all indicators suggest, its progenitor had a mass just over 6 M⊙. It may, however, be telling an even more interesting story than the one related to the IFMR, one about the origin of stellar magnetic fields, SNe I, and gravitational waves from low-mass stellar systems.","lang":"eng"}],"arxiv":1,"title":"A massive magnetic helium atmosphere white dwarf binary in a young star cluster","date_published":"2019-07-26T00:00:00Z","article_processing_charge":"No","oa_version":"Preprint","date_updated":"2024-04-04T14:06:08Z","day":"26","publication_status":"published","status":"public","publication":"The Astrophysical Journal","date_created":"2024-03-26T10:37:01Z","author":[{"full_name":"Richer, Harvey B.","last_name":"Richer","first_name":"Harvey B."},{"full_name":"Kerr, Ronan","last_name":"Kerr","first_name":"Ronan"},{"full_name":"Heyl, Jeremy","last_name":"Heyl","first_name":"Jeremy"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"last_name":"Cummings","full_name":"Cummings, Jeffrey","first_name":"Jeffrey"},{"first_name":"Pierre","last_name":"Bergeron","full_name":"Bergeron, Pierre"},{"full_name":"Dufour, Patrick","last_name":"Dufour","first_name":"Patrick"}],"doi":"10.3847/1538-4357/ab2874","_id":"15230","scopus_import":"1","issue":"2","language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1906.04727"}],"year":"2019","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","article_number":"75","keyword":["Space and Planetary Science","Astronomy and Astrophysics"]},{"language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1807.03307"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"related_material":{"link":[{"relation":"erratum","url":"https://iopscience.iop.org/article/10.3847/1538-4357/ab84ea"}]},"year":"2019","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"1","date_created":"2024-03-26T10:37:20Z","author":[{"first_name":"Christopher R.","last_name":"Mann","full_name":"Mann, Christopher R."},{"full_name":"Richer, Harvey","last_name":"Richer","first_name":"Harvey"},{"last_name":"Heyl","full_name":"Heyl, Jeremy","first_name":"Jeremy"},{"full_name":"Anderson, Jay","last_name":"Anderson","first_name":"Jay"},{"first_name":"Jason","last_name":"Kalirai","full_name":"Kalirai, Jason"},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","first_name":"Ilaria"},{"first_name":"Swantje D.","full_name":"Möhle, Swantje D.","last_name":"Möhle"},{"last_name":"Knee","full_name":"Knee, Alan","first_name":"Alan"},{"full_name":"Baumgardt, Holger","last_name":"Baumgardt","first_name":"Holger"}],"scopus_import":"1","issue":"1","doi":"10.3847/1538-4357/ab0e6d","_id":"15231","title":"A multimass velocity dispersion model of 47 Tucanae indicates no evidence for an intermediate-mass black hole","abstract":[{"lang":"eng","text":"In this paper, we analyze stellar proper motions in the core of the globular cluster 47 Tucanae to explore the possibility of an intermediate-mass black hole (IMBH) influence on the stellar dynamics. Our use of short-wavelength photometry affords us an exceedingly clear view of stellar motions into the very center of the crowded core, yielding proper motions for >50,000 stars in the central 2′. We model the velocity dispersion profile of the cluster using an isotropic Jeans model. The density distribution is taken as a central IMBH point mass added to a combination of King templates. We individually model the general low-mass cluster objects (main sequence/giant stars), as well as the concentrated populations of heavy binary systems and dark stellar remnants. Using unbinned likelihood model fitting, we find that the inclusion of the concentrated populations in our model plays a crucial role in fitting for an IMBH mass. The concentrated binaries and stellar-mass black holes (BHs) produce a sufficient velocity dispersion signal in the core so as to make an IMBH unnecessary to fit the observations. We additionally determine that a stellar-mass BH retention fraction of 8.5% becomes incompatible with our observed velocities in the core."}],"arxiv":1,"publication_status":"published","publication":"The Astrophysical Journal","status":"public","article_processing_charge":"No","date_published":"2019-04-08T00:00:00Z","oa_version":"Preprint","date_updated":"2024-04-08T07:07:38Z","day":"08","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"intvolume":"       875","volume":875,"oa":1,"publisher":"American Astronomical Society","type":"journal_article","external_id":{"arxiv":["1807.03307"]},"month":"04","quality_controlled":"1","extern":"1","citation":{"ama":"Mann CR, Richer H, Heyl J, et al. A multimass velocity dispersion model of 47 Tucanae indicates no evidence for an intermediate-mass black hole. <i>The Astrophysical Journal</i>. 2019;875(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab0e6d\">10.3847/1538-4357/ab0e6d</a>","apa":"Mann, C. R., Richer, H., Heyl, J., Anderson, J., Kalirai, J., Caiazzo, I., … Baumgardt, H. (2019). A multimass velocity dispersion model of 47 Tucanae indicates no evidence for an intermediate-mass black hole. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ab0e6d\">https://doi.org/10.3847/1538-4357/ab0e6d</a>","ieee":"C. R. Mann <i>et al.</i>, “A multimass velocity dispersion model of 47 Tucanae indicates no evidence for an intermediate-mass black hole,” <i>The Astrophysical Journal</i>, vol. 875, no. 1. American Astronomical Society, 2019.","ista":"Mann CR, Richer H, Heyl J, Anderson J, Kalirai J, Caiazzo I, Möhle SD, Knee A, Baumgardt H. 2019. A multimass velocity dispersion model of 47 Tucanae indicates no evidence for an intermediate-mass black hole. The Astrophysical Journal. 875(1), 1.","chicago":"Mann, Christopher R., Harvey Richer, Jeremy Heyl, Jay Anderson, Jason Kalirai, Ilaria Caiazzo, Swantje D. Möhle, Alan Knee, and Holger Baumgardt. “A Multimass Velocity Dispersion Model of 47 Tucanae Indicates No Evidence for an Intermediate-Mass Black Hole.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab0e6d\">https://doi.org/10.3847/1538-4357/ab0e6d</a>.","mla":"Mann, Christopher R., et al. “A Multimass Velocity Dispersion Model of 47 Tucanae Indicates No Evidence for an Intermediate-Mass Black Hole.” <i>The Astrophysical Journal</i>, vol. 875, no. 1, 1, American Astronomical Society, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab0e6d\">10.3847/1538-4357/ab0e6d</a>.","short":"C.R. Mann, H. Richer, J. Heyl, J. Anderson, J. Kalirai, I. Caiazzo, S.D. Möhle, A. Knee, H. Baumgardt, The Astrophysical Journal 875 (2019)."},"article_type":"original"},{"_id":"11508","doi":"10.1051/0004-6361/201833528","acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","scopus_import":"1","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"first_name":"Mauro","full_name":"Stefanon, Mauro","last_name":"Stefanon"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"}],"date_created":"2022-07-06T11:14:23Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A136","year":"2018","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"main_file_link":[{"url":"https://arxiv.org/abs/1805.11621","open_access":"1"}],"language":[{"iso":"eng"}],"article_type":"original","citation":{"ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy &#38; Astrophysics. 619, A136.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>.","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, A136, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy &#38; Astrophysics 619 (2018).","ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>","apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., &#38; Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>"},"quality_controlled":"1","extern":"1","external_id":{"arxiv":["1805.11621"]},"type":"journal_article","month":"11","oa":1,"publisher":"EDP Sciences","volume":619,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"intvolume":"       619","oa_version":"Published Version","day":"19","date_updated":"2024-10-14T11:31:36Z","date_published":"2018-11-19T00:00:00Z","article_processing_charge":"No","publication_status":"published","publication":"Astronomy & Astrophysics","status":"public","abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z >  6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z >  5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR."}],"arxiv":1,"title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe"},{"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/sty925","_id":"11549","scopus_import":"1","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","issue":"3","date_created":"2022-07-08T11:48:48Z","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"first_name":"D","full_name":"Sobral, D","last_name":"Sobral"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"first_name":"P N","last_name":"Best","full_name":"Best, P N"},{"first_name":"I","last_name":"Smail","full_name":"Smail, I"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Darvish, B","last_name":"Darvish","first_name":"B"},{"last_name":"Nayyeri","full_name":"Nayyeri, H","first_name":"H"},{"first_name":"S","full_name":"Hemmati, S","last_name":"Hemmati"},{"full_name":"Stott, J P","last_name":"Stott","first_name":"J P"}],"date_published":"2018-08-01T00:00:00Z","article_processing_charge":"No","day":"01","date_updated":"2022-08-19T06:53:39Z","oa_version":"Published Version","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","status":"public","arxiv":1,"abstract":[{"text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.","lang":"eng"}],"title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","article_type":"original","citation":{"apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015. doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>.","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018.","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>."},"month":"08","type":"journal_article","external_id":{"arxiv":["1705.01101"]},"page":"2999-3015","extern":"1","quality_controlled":"1","intvolume":"       478","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"volume":478,"publisher":"Oxford University Press"},{"publication":"Monthly Notices of the Royal Astronomical Society","status":"public","publication_status":"published","oa_version":"Preprint","day":"01","date_updated":"2022-08-19T06:58:06Z","article_processing_charge":"No","date_published":"2018-07-01T00:00:00Z","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","abstract":[{"text":"We investigate the morphology of the [C II] emission in a sample of ‘normal’ star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [C II]. For several of the latter the [C II] emission breaks into multiple components. Only a fraction of these [C II] components, if any, is associated with the primary UV systems, while the bulk of the [C II] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L[CII]–SFR (star formation rate) relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L[CII]–SFR relation has a weak anticorrelation with the EW(Ly α). The morphological analysis also reveals that [C II] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterized by a [C II] surface brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation. These properties are likely a consequence of a combination of different effects, namely gas metallicity, [C II] emission from obscured star-forming regions, strong variations of the ionization parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies.","lang":"eng"}],"arxiv":1,"citation":{"apa":"Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara, A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(1):1170-1184. doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>","mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184.","ieee":"S. Carniani <i>et al.</i>, “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184."},"article_type":"original","oa":1,"publisher":"Oxford University Press","volume":478,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"intvolume":"       478","quality_controlled":"1","extern":"1","page":"1170-1184","external_id":{"arxiv":["1712.03985"]},"month":"07","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2018","main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"language":[{"iso":"eng"}],"issue":"1","acknowledgement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S, ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S, ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S, AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/ alma-data/archive. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.","scopus_import":"1","_id":"11555","doi":"10.1093/mnras/sty1088","author":[{"last_name":"Carniani","full_name":"Carniani, S","first_name":"S"},{"first_name":"R","full_name":"Maiolino, R","last_name":"Maiolino"},{"last_name":"Amorin","full_name":"Amorin, R","first_name":"R"},{"first_name":"L","full_name":"Pentericci, L","last_name":"Pentericci"},{"first_name":"A","full_name":"Pallottini, A","last_name":"Pallottini"},{"first_name":"A","last_name":"Ferrara","full_name":"Ferrara, A"},{"last_name":"Willott","full_name":"Willott, C J","first_name":"C J"},{"first_name":"R","full_name":"Smit, R","last_name":"Smit"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"last_name":"Santini","full_name":"Santini, P","first_name":"P"},{"last_name":"Castellano","full_name":"Castellano, M","first_name":"M"},{"first_name":"S","full_name":"De Barros, S","last_name":"De Barros"},{"first_name":"A","full_name":"Fontana, A","last_name":"Fontana"},{"first_name":"A","full_name":"Grazian, A","last_name":"Grazian"},{"first_name":"L","last_name":"Guaita","full_name":"Guaita, L"}],"date_created":"2022-07-11T08:05:42Z"},{"language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-12T07:18:02Z","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"first_name":"Philip N","full_name":"Best, Philip N","last_name":"Best"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"}],"scopus_import":"1","acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","issue":"2","doi":"10.1093/mnras/sty782","_id":"11557","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","arxiv":1,"abstract":[{"lang":"eng","text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠) and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent) have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated."}],"status":"public","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","article_processing_charge":"No","date_published":"2018-06-01T00:00:00Z","day":"01","date_updated":"2022-08-19T07:01:08Z","oa_version":"Preprint","intvolume":"       477","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":477,"oa":1,"publisher":"Oxford University Press","type":"journal_article","external_id":{"arxiv":["1802.10102"]},"month":"06","page":"2817-2840","extern":"1","quality_controlled":"1","citation":{"apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>","ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;477(2):2817-2840. doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>","short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>.","ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>.","ieee":"D. Sobral <i>et al.</i>, “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018."},"article_type":"original"},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.04451"}],"language":[{"iso":"eng"}],"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"date_created":"2022-07-12T10:41:08Z","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Sérgio","full_name":"Santos, Sérgio","last_name":"Santos"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"full_name":"Ribeiro, Bruno","last_name":"Ribeiro","first_name":"Bruno"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"first_name":"Ali A","last_name":"Khostovan","full_name":"Khostovan, Ali A"}],"doi":"10.1093/mnras/sty378","_id":"11558","scopus_import":"1","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","issue":"4","arxiv":1,"abstract":[{"text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape.","lang":"eng"}],"title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","date_published":"2018-06-01T00:00:00Z","article_processing_charge":"No","day":"01","date_updated":"2022-08-19T07:04:45Z","oa_version":"Preprint","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","type":"journal_article","external_id":{"arxiv":["1712.04451"]},"month":"06","page":"4725-4752","extern":"1","quality_controlled":"1","intvolume":"       476","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":476,"oa":1,"publisher":"Oxford University Press","article_type":"original","citation":{"ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>","ieee":"D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>.","short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752."}},{"month":"09","type":"journal_article","external_id":{"arxiv":["1802.06786"]},"page":"L34 - L39","extern":"1","quality_controlled":"1","intvolume":"       479","publication_identifier":{"issn":["1745-3925"],"eissn":["1745-3933"]},"volume":479,"publisher":"Oxford University Press","oa":1,"article_type":"original","citation":{"short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>.","ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018.","apa":"Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>"},"arxiv":1,"abstract":[{"text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements.","lang":"eng"}],"title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","article_processing_charge":"No","date_published":"2018-09-01T00:00:00Z","date_updated":"2024-10-14T11:37:53Z","day":"01","oa_version":"Preprint","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","status":"public","date_created":"2022-07-14T12:49:47Z","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"}],"doi":"10.1093/mnrasl/sly093","_id":"11584","scopus_import":"1","acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages.","issue":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.06786"}],"language":[{"iso":"eng"}],"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"]},{"citation":{"apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., &#38; Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. 2018;620. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 620, A38, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy &#38; Astrophysics 620 (2018).","ieee":"L. A. Bugnet <i>et al.</i>, “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 620. EDP Sciences, 2018.","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>.","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy &#38; Astrophysics. 620, A38."},"article_type":"original","publisher":"EDP Sciences","oa":1,"volume":620,"intvolume":"       620","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"extern":"1","quality_controlled":"1","external_id":{"arxiv":["1809.05105"]},"month":"12","type":"journal_article","publication_status":"published","status":"public","publication":"Astronomy & Astrophysics","day":"01","date_updated":"2024-10-14T11:40:17Z","oa_version":"Preprint","date_published":"2018-12-01T00:00:00Z","article_processing_charge":"No","title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","arxiv":1,"abstract":[{"text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties.","lang":"eng"}],"acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.","scopus_import":"1","_id":"11618","doi":"10.1051/0004-6361/201833106","author":[{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"first_name":"G. R.","full_name":"Davies, G. R.","last_name":"Davies"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"full_name":"Corsaro, E.","last_name":"Corsaro","first_name":"E."},{"first_name":"O. J.","full_name":"Hall, O. J.","last_name":"Hall"},{"first_name":"B. M.","full_name":"Rendle, B. M.","last_name":"Rendle"}],"date_created":"2022-07-18T14:37:39Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"article_number":"A38","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2018","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.05105"}],"language":[{"iso":"eng"}]},{"author":[{"full_name":"Gandolfi, D.","last_name":"Gandolfi","first_name":"D."},{"first_name":"O.","last_name":"Barragán","full_name":"Barragán, O."},{"first_name":"J. H.","last_name":"Livingston","full_name":"Livingston, J. H."},{"last_name":"Fridlund","full_name":"Fridlund, M.","first_name":"M."},{"first_name":"A. B.","last_name":"Justesen","full_name":"Justesen, A. B."},{"first_name":"S.","last_name":"Redfield","full_name":"Redfield, S."},{"first_name":"L.","last_name":"Fossati","full_name":"Fossati, L."},{"last_name":"Mathur","full_name":"Mathur, S.","first_name":"S."},{"first_name":"S.","last_name":"Grziwa","full_name":"Grziwa, S."},{"first_name":"J.","full_name":"Cabrera, J.","last_name":"Cabrera"},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Persson","full_name":"Persson, C. M.","first_name":"C. M."},{"last_name":"Van Eylen","full_name":"Van Eylen, V.","first_name":"V."},{"first_name":"A. P.","last_name":"Hatzes","full_name":"Hatzes, A. P."},{"full_name":"Hidalgo, D.","last_name":"Hidalgo","first_name":"D."},{"last_name":"Albrecht","full_name":"Albrecht, S.","first_name":"S."},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"},{"full_name":"Cochran, W. D.","last_name":"Cochran","first_name":"W. D."},{"first_name":"Sz.","full_name":"Csizmadia, Sz.","last_name":"Csizmadia"},{"last_name":"Deeg","full_name":"Deeg, H.","first_name":"H."},{"full_name":"Eigmüller, Ph.","last_name":"Eigmüller","first_name":"Ph."},{"last_name":"Endl","full_name":"Endl, M.","first_name":"M."},{"first_name":"A.","last_name":"Erikson","full_name":"Erikson, A."},{"last_name":"Esposito","full_name":"Esposito, M.","first_name":"M."},{"last_name":"Guenther","full_name":"Guenther, E.","first_name":"E."},{"first_name":"J.","last_name":"Korth","full_name":"Korth, J."},{"full_name":"Luque, R.","last_name":"Luque","first_name":"R."},{"first_name":"P.","last_name":"Montañes Rodríguez","full_name":"Montañes Rodríguez, P."},{"first_name":"D.","full_name":"Nespral, D.","last_name":"Nespral"},{"last_name":"Nowak","full_name":"Nowak, G.","first_name":"G."},{"last_name":"Pätzold","full_name":"Pätzold, M.","first_name":"M."},{"first_name":"J.","last_name":"Prieto-Arranz","full_name":"Prieto-Arranz, J."}],"date_created":"2022-07-18T14:41:16Z","_id":"11619","doi":"10.1051/0004-6361/201834289","scopus_import":"1","language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.07573"}],"article_number":"L10","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2018","keyword":["Space and Planetary Science","Astronomy and Astrophysics","planetary systems / planets and satellites","detection / planets and satellites","fundamental parameters / planets and satellites","terrestrial planets / stars","fundamental parameters"],"extern":"1","quality_controlled":"1","type":"journal_article","external_id":{"arxiv":["1809.07573"]},"month":"11","oa":1,"volume":619,"publisher":"EDP Sciences","intvolume":"       619","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"letter_note","citation":{"mla":"Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, L10, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834289\">10.1051/0004-6361/201834289</a>.","short":"D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S. Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson, V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran, S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther, J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J. Prieto-Arranz, Astronomy &#38; Astrophysics 619 (2018).","ieee":"D. Gandolfi <i>et al.</i>, “TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","ista":"Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy &#38; Astrophysics. 619, L10.","chicago":"Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen, S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201834289\">https://doi.org/10.1051/0004-6361/201834289</a>.","apa":"Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A. B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834289\">https://doi.org/10.1051/0004-6361/201834289</a>","ama":"Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834289\">10.1051/0004-6361/201834289</a>"},"arxiv":1,"abstract":[{"lang":"eng","text":"We report on the confirmation and mass determination of π Men c, the first transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES at AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we found that π Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based on the planet’s orbital period and size, π Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars."}],"title":"TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae","day":"22","date_updated":"2022-08-22T07:43:29Z","oa_version":"Preprint","date_published":"2018-11-22T00:00:00Z","article_processing_charge":"No","publication":"Astronomy & Astrophysics","publication_status":"published","status":"public"},{"date_published":"2018-08-01T00:00:00Z","article_processing_charge":"No","oa_version":"Preprint","day":"01","date_updated":"2022-08-22T07:45:38Z","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","abstract":[{"text":"We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙⁠, respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4+0.4−1.3Gyr⁠, and the non-detection of mixed modes. The star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity.","lang":"eng"}],"arxiv":1,"title":"HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2","article_type":"original","citation":{"short":"V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A. García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández, J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral, G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G. Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S. Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N. Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of the Royal Astronomical Society 478 (2018) 4866–4880.","mla":"Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>.","chicago":"Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>.","ista":"Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 478(4), 4866–4880.","ieee":"V. Van Eylen <i>et al.</i>, “HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4. Oxford University Press, pp. 4866–4880, 2018.","apa":"Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>","ama":"Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(4):4866-4880. doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>"},"page":"4866-4880","month":"08","external_id":{"arxiv":["1805.01860"]},"type":"journal_article","quality_controlled":"1","extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"intvolume":"       478","oa":1,"publisher":"Oxford University Press","volume":478,"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","planets and satellites: composition","planets and satellites: formation","planets and satellites: fundamental parameters"],"main_file_link":[{"url":"https://arxiv.org/abs/1805.01860","open_access":"1"}],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/sty1390","_id":"11620","scopus_import":"1","issue":"4","acknowledgement":"We gratefully acknowledge many helpful suggestions by the anonymous referee. Based on observations made with a) the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. DG gratefully acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). SaM would like to acknowledge support from the Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support by the Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA 3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. RAG and StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE 2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106) This 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 the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.","date_created":"2022-07-18T14:43:17Z","author":[{"first_name":"V","last_name":"Van Eylen","full_name":"Van Eylen, V"},{"full_name":"Dai, F","last_name":"Dai","first_name":"F"},{"last_name":"Mathur","full_name":"Mathur, S","first_name":"S"},{"last_name":"Gandolfi","full_name":"Gandolfi, D","first_name":"D"},{"last_name":"Albrecht","full_name":"Albrecht, S","first_name":"S"},{"first_name":"M","full_name":"Fridlund, M","last_name":"Fridlund"},{"full_name":"García, R A","last_name":"García","first_name":"R A"},{"last_name":"Guenther","full_name":"Guenther, E","first_name":"E"},{"last_name":"Hjorth","full_name":"Hjorth, M","first_name":"M"},{"last_name":"Justesen","full_name":"Justesen, A B","first_name":"A B"},{"first_name":"J","last_name":"Livingston","full_name":"Livingston, J"},{"first_name":"M N","full_name":"Lund, M N","last_name":"Lund"},{"first_name":"F","full_name":"Pérez Hernández, F","last_name":"Pérez Hernández"},{"full_name":"Prieto-Arranz, J","last_name":"Prieto-Arranz","first_name":"J"},{"last_name":"Regulo","full_name":"Regulo, C","first_name":"C"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"first_name":"M E","full_name":"Everett, M E","last_name":"Everett"},{"full_name":"Hirano, T","last_name":"Hirano","first_name":"T"},{"full_name":"Nespral, D","last_name":"Nespral","first_name":"D"},{"first_name":"G","full_name":"Nowak, G","last_name":"Nowak"},{"first_name":"E","last_name":"Palle","full_name":"Palle, E"},{"last_name":"Silva Aguirre","full_name":"Silva Aguirre, V","first_name":"V"},{"first_name":"T","full_name":"Trifonov, T","last_name":"Trifonov"},{"first_name":"J N","last_name":"Winn","full_name":"Winn, J N"},{"first_name":"O","last_name":"Barragán","full_name":"Barragán, O"},{"full_name":"Beck, P G","last_name":"Beck","first_name":"P G"},{"first_name":"W J","last_name":"Chaplin","full_name":"Chaplin, W J"},{"full_name":"Cochran, W D","last_name":"Cochran","first_name":"W D"},{"first_name":"S","last_name":"Csizmadia","full_name":"Csizmadia, S"},{"full_name":"Deeg, H","last_name":"Deeg","first_name":"H"},{"first_name":"M","full_name":"Endl, M","last_name":"Endl"},{"first_name":"P","last_name":"Heeren","full_name":"Heeren, P"},{"first_name":"S","full_name":"Grziwa, S","last_name":"Grziwa"},{"last_name":"Hatzes","full_name":"Hatzes, A P","first_name":"A P"},{"first_name":"D","full_name":"Hidalgo, D","last_name":"Hidalgo"},{"full_name":"Korth, J","last_name":"Korth","first_name":"J"},{"full_name":"Mathis, S","last_name":"Mathis","first_name":"S"},{"last_name":"Montañes Rodriguez","full_name":"Montañes Rodriguez, P","first_name":"P"},{"last_name":"Narita","full_name":"Narita, N","first_name":"N"},{"last_name":"Patzold","full_name":"Patzold, M","first_name":"M"},{"first_name":"C M","last_name":"Persson","full_name":"Persson, C M"},{"first_name":"F","full_name":"Rodler, F","last_name":"Rodler"},{"full_name":"Smith, A M S","last_name":"Smith","first_name":"A M S"}]},{"citation":{"short":"A. Schootemeijer, Y.L.L. Götberg, S.E. de Mink, D. Gies, E. Zapartas, Astronomy &#38; Astrophysics 615 (2018).","mla":"Schootemeijer, A., et al. “Clues about the Scarcity of Stripped-Envelope Stars from the Evolutionary State of the SdO+Be Binary System φ Persei.” <i>Astronomy &#38; Astrophysics</i>, vol. 615, A30, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201731194\">10.1051/0004-6361/201731194</a>.","ista":"Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. 2018. Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. Astronomy &#38; Astrophysics. 615, A30.","chicago":"Schootemeijer, A., Ylva Louise Linsdotter Götberg, S. E. de Mink, D. Gies, and E. Zapartas. “Clues about the Scarcity of Stripped-Envelope Stars from the Evolutionary State of the SdO+Be Binary System φ Persei.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201731194\">https://doi.org/10.1051/0004-6361/201731194</a>.","ieee":"A. Schootemeijer, Y. L. L. Götberg, S. E. de Mink, D. Gies, and E. Zapartas, “Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei,” <i>Astronomy &#38; Astrophysics</i>, vol. 615. EDP Sciences, 2018.","apa":"Schootemeijer, A., Götberg, Y. L. L., de Mink, S. E., Gies, D., &#38; Zapartas, E. (2018). Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201731194\">https://doi.org/10.1051/0004-6361/201731194</a>","ama":"Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. <i>Astronomy &#38; Astrophysics</i>. 2018;615. doi:<a href=\"https://doi.org/10.1051/0004-6361/201731194\">10.1051/0004-6361/201731194</a>"},"article_type":"original","publisher":"EDP Sciences","volume":615,"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"intvolume":"       615","quality_controlled":"1","extern":"1","external_id":{"arxiv":["1803.02379"]},"month":"07","type":"journal_article","status":"public","publication_status":"published","publication":"Astronomy & Astrophysics","oa_version":"Published Version","day":"06","date_updated":"2023-08-09T12:22:52Z","date_published":"2018-07-06T00:00:00Z","article_processing_charge":"No","title":"Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei","abstract":[{"lang":"eng","text":"Stripped-envelope stars form in binary systems after losing mass through Roche-lobe overflow. They bear astrophysical significance as sources of UV and ionizing radiation in older stellar populations and, if sufficiently massive, as stripped supernova progenitors. Binary evolutionary models predict that they are common, but only a handful of subdwarfs with B-type companions are known. The question is whether a large population of such systems has evaded detection as a result of biases, or whether the model predictions are wrong. We reanalyze the well-studied post-interaction binary φ Persei. Recently, new data have improved the orbital solution of the system, which contains an ~1.2M⊙ stripped-envelope star and a rapidly rotating ~9.6M⊙ Be star. We compare with an extensive grid of evolutionary models using a Bayesian approach and constrain the initial masses of the progenitor to 7.2 ± 0.4M⊙ for the stripped star and 3.8 ± 0.4M⊙ for the Be star. The system must have evolved through near-conservative mass transfer. These findings are consistent with earlier studies. The age we obtain, 57 ± 9 Myr, is in excellent agreement with the age of the α Persei cluster. We note that neither star was initially massive enough to produce a core-collapse supernova, but mass exchange pushed the Be star above the mass threshold. We find that the subdwarf is overluminous for its mass by almost an order of magnitude, compared to the expectations for a helium core burning star. We can only reconcile this if the subdwarf resides in a late phase of helium shell burning, which lasts only 2–3% of the total lifetime as a subdwarf. Assuming continuous star formation implies that up to ~50 less evolved, dimmer subdwarfs exist for each system similar to φ Persei, but have evaded detection so far. Our findings can be interpreted as a strong indication that a substantial population of stripped-envelope stars indeed exists, but has so far evaded detection because of observational biases and lack of large-scale systematic searches."}],"arxiv":1,"scopus_import":"1","_id":"13473","doi":"10.1051/0004-6361/201731194","author":[{"first_name":"A.","full_name":"Schootemeijer, A.","last_name":"Schootemeijer"},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"first_name":"S. E.","last_name":"de Mink","full_name":"de Mink, S. E."},{"last_name":"Gies","full_name":"Gies, D.","first_name":"D."},{"full_name":"Zapartas, E.","last_name":"Zapartas","first_name":"E."}],"date_created":"2023-08-03T10:14:37Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A30","year":"2018","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201731194","open_access":"1"}],"language":[{"iso":"eng"}]},{"doi":"10.1093/mnras/stx3181","_id":"13474","scopus_import":"1","issue":"1","date_created":"2023-08-03T10:14:47Z","author":[{"full_name":"Smith, Nathan","last_name":"Smith","first_name":"Nathan"},{"first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter"},{"last_name":"de Mink","full_name":"de Mink, Selma E","first_name":"Selma E"}],"year":"2018","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stx3181"}],"article_type":"original","citation":{"chicago":"Smith, Nathan, Ylva Louise Linsdotter Götberg, and Selma E de Mink. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/stx3181\">https://doi.org/10.1093/mnras/stx3181</a>.","ista":"Smith N, Götberg YLL, de Mink SE. 2018. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. Monthly Notices of the Royal Astronomical Society. 475(1), 772–782.","ieee":"N. Smith, Y. L. L. Götberg, and S. E. de Mink, “Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 1. Oxford University Press, pp. 772–782, 2018.","short":"N. Smith, Y.L.L. Götberg, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 475 (2018) 772–782.","mla":"Smith, Nathan, et al. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 1, Oxford University Press, 2018, pp. 772–82, doi:<a href=\"https://doi.org/10.1093/mnras/stx3181\">10.1093/mnras/stx3181</a>.","ama":"Smith N, Götberg YLL, de Mink SE. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;475(1):772-782. doi:<a href=\"https://doi.org/10.1093/mnras/stx3181\">10.1093/mnras/stx3181</a>","apa":"Smith, N., Götberg, Y. L. L., &#38; de Mink, S. E. (2018). Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx3181\">https://doi.org/10.1093/mnras/stx3181</a>"},"type":"journal_article","month":"03","external_id":{"arxiv":["1704.03516"]},"page":"772-782","extern":"1","quality_controlled":"1","intvolume":"       475","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":475,"oa":1,"publisher":"Oxford University Press","article_processing_charge":"No","date_published":"2018-03-01T00:00:00Z","date_updated":"2023-08-09T12:17:34Z","day":"01","oa_version":"Published Version","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","status":"public","arxiv":1,"abstract":[{"lang":"eng","text":"Recent surveys of the Magellanic Clouds have revealed a subtype of Wolf–Rayet (WR) star with peculiar properties. WN3/O3 spectra exhibit both WR-like emission and O3 V-like absorption – but at lower luminosity than O3 V or WN stars. We examine the projected spatial distribution of WN3/O3 stars in the Large Magellanic Cloud as compared to O-type stars. Surprisingly, WN3/O3 stars are among the most isolated of all classes of massive stars; they have a distribution similar to red supergiants dominated by initial masses of 10–15 M⊙, and are far more dispersed than classical WR stars or luminous blue variables. Their lack of association with clusters of O-type stars suggests strongly that WN3/O3 stars are not the descendants of single massive stars (30 M⊙ or above). Instead, they are likely products of interacting binaries at lower initial mass (10–18 M⊙). Comparison with binary models suggests a probable origin with primaries in this mass range that were stripped of their H envelopes through non-conservative mass transfer by a low-mass secondary. We show that model spectra and positions on the Hertzsprung–Russell diagram for binary-stripped stars are consistent with WN3/O3 stars. Monitoring radial velocities with high-resolution spectra can test for low-mass companions or runaway velocities. With lower initial mass and environments that avoid very massive stars, the WN3/O3 stars fit expectations for progenitors of Type Ib and possibly Type Ibn supernovae."}],"title":"Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries"}]