[{"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"03","doi":"10.1093/mnras/stz030","language":[{"iso":"eng"}],"oa":1,"external_id":{"arxiv":["1805.05956"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"quality_controlled":"1","extern":"1","author":[{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"}],"volume":484,"date_created":"2022-07-08T07:48:31Z","date_updated":"2022-08-19T06:42:43Z","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","year":"2019","publisher":"Oxford University Press","publication_status":"published","article_processing_charge":"No","day":"01","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"date_published":"2019-03-01T00:00:00Z","citation":{"ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","apa":"Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932. doi:10.1093/mnras/stz030","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932."},"publication":"Monthly Notices of the Royal Astronomical Society","page":"915-932","article_type":"original","issue":"1","abstract":[{"text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr.","lang":"eng"}],"type":"journal_article","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11540","intvolume":" 484","status":"public","title":"The origin of scatter in the star formation rate–stellar mass relation"},{"type":"journal_article","issue":"6","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"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11616","intvolume":" 157","title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","status":"public","oa_version":"Preprint","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","day":"30","citation":{"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.” The Astronomical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-3881/ab1488.","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).","mla":"Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” The Astronomical Journal, vol. 157, no. 6, 245, IOP Publishing, 2019, doi:10.3847/1538-3881/ab1488.","ieee":"D. Huber et al., “A hot Saturn orbiting an oscillating late subgiant discovered by TESS,” The Astronomical Journal, vol. 157, no. 6. IOP Publishing, 2019.","apa":"Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard, J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. IOP Publishing. https://doi.org/10.3847/1538-3881/ab1488","ista":"Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 157(6), 245.","ama":"Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 2019;157(6). doi:10.3847/1538-3881/ab1488"},"publication":"The Astronomical Journal","article_type":"original","date_published":"2019-05-30T00:00:00Z","article_number":"245","extern":"1","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).","year":"2019","publisher":"IOP Publishing","publication_status":"published","author":[{"full_name":"Huber, Daniel","first_name":"Daniel","last_name":"Huber"},{"last_name":"Chaplin","first_name":"William J.","full_name":"Chaplin, William J."},{"full_name":"Chontos, Ashley","last_name":"Chontos","first_name":"Ashley"},{"full_name":"Kjeldsen, Hans","last_name":"Kjeldsen","first_name":"Hans"},{"full_name":"Christensen-Dalsgaard, Jørgen","last_name":"Christensen-Dalsgaard","first_name":"Jørgen"},{"last_name":"Bedding","first_name":"Timothy R.","full_name":"Bedding, Timothy R."},{"last_name":"Ball","first_name":"Warrick","full_name":"Ball, Warrick"},{"first_name":"Rafael","last_name":"Brahm","full_name":"Brahm, Rafael"},{"first_name":"Nestor","last_name":"Espinoza","full_name":"Espinoza, Nestor"},{"last_name":"Henning","first_name":"Thomas","full_name":"Henning, Thomas"},{"first_name":"Andrés","last_name":"Jordán","full_name":"Jordán, Andrés"},{"last_name":"Sarkis","first_name":"Paula","full_name":"Sarkis, Paula"},{"full_name":"Knudstrup, Emil","first_name":"Emil","last_name":"Knudstrup"},{"full_name":"Albrecht, Simon","last_name":"Albrecht","first_name":"Simon"},{"last_name":"Grundahl","first_name":"Frank","full_name":"Grundahl, Frank"},{"last_name":"Andersen","first_name":"Mads Fredslund","full_name":"Andersen, Mads Fredslund"},{"full_name":"Pallé, Pere L.","last_name":"Pallé","first_name":"Pere L."},{"first_name":"Ian","last_name":"Crossfield","full_name":"Crossfield, Ian"},{"last_name":"Fulton","first_name":"Benjamin","full_name":"Fulton, Benjamin"},{"last_name":"Howard","first_name":"Andrew W.","full_name":"Howard, Andrew W."},{"last_name":"Isaacson","first_name":"Howard T.","full_name":"Isaacson, Howard T."},{"last_name":"Weiss","first_name":"Lauren M.","full_name":"Weiss, Lauren M."},{"full_name":"Handberg, Rasmus","last_name":"Handberg","first_name":"Rasmus"},{"full_name":"Lund, Mikkel N.","last_name":"Lund","first_name":"Mikkel N."},{"full_name":"Serenelli, Aldo M.","last_name":"Serenelli","first_name":"Aldo M."},{"full_name":"Rørsted Mosumgaard, Jakob","last_name":"Rørsted Mosumgaard","first_name":"Jakob"},{"last_name":"Stokholm","first_name":"Amalie","full_name":"Stokholm, Amalie"},{"full_name":"Bieryla, Allyson","last_name":"Bieryla","first_name":"Allyson"},{"first_name":"Lars A.","last_name":"Buchhave","full_name":"Buchhave, Lars A."},{"full_name":"Latham, David W.","last_name":"Latham","first_name":"David W."},{"last_name":"Quinn","first_name":"Samuel N.","full_name":"Quinn, Samuel N."},{"full_name":"Gaidos, Eric","last_name":"Gaidos","first_name":"Eric"},{"first_name":"Teruyuki","last_name":"Hirano","full_name":"Hirano, 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","first_name":"Sara","full_name":"Seager, Sara"},{"last_name":"Jenkins","first_name":"Jon M.","full_name":"Jenkins, Jon M."},{"last_name":"Winn","first_name":"Joshua N.","full_name":"Winn, Joshua N."},{"first_name":"H. M.","last_name":"Antia","full_name":"Antia, H. M."},{"last_name":"Appourchaux","first_name":"Thierry","full_name":"Appourchaux, Thierry"},{"full_name":"Basu, Sarbani","last_name":"Basu","first_name":"Sarbani"},{"first_name":"Keaton J.","last_name":"Bell","full_name":"Bell, Keaton J."},{"full_name":"Benomar, Othman","first_name":"Othman","last_name":"Benomar"},{"full_name":"Bonanno, Alfio","first_name":"Alfio","last_name":"Bonanno"},{"first_name":"Derek L.","last_name":"Buzasi","full_name":"Buzasi, Derek L."},{"first_name":"Tiago L.","last_name":"Campante","full_name":"Campante, Tiago L."},{"full_name":"Çelik Orhan, Z.","last_name":"Çelik Orhan","first_name":"Z."},{"last_name":"Corsaro","first_name":"Enrico","full_name":"Corsaro, Enrico"},{"full_name":"Cunha, Margarida S.","last_name":"Cunha","first_name":"Margarida S."},{"full_name":"Davies, Guy R.","first_name":"Guy R.","last_name":"Davies"},{"last_name":"Deheuvels","first_name":"Sebastien","full_name":"Deheuvels, Sebastien"},{"last_name":"Grunblatt","first_name":"Samuel K.","full_name":"Grunblatt, Samuel K."},{"full_name":"Hasanzadeh, Amir","last_name":"Hasanzadeh","first_name":"Amir"},{"full_name":"Di Mauro, Maria Pia","first_name":"Maria Pia","last_name":"Di Mauro"},{"full_name":"A. García, Rafael","last_name":"A. García","first_name":"Rafael"},{"first_name":"Patrick","last_name":"Gaulme","full_name":"Gaulme, Patrick"},{"full_name":"Girardi, Léo","last_name":"Girardi","first_name":"Léo"},{"full_name":"Guzik, Joyce A.","first_name":"Joyce A.","last_name":"Guzik"},{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"last_name":"Jiang","first_name":"Chen","full_name":"Jiang, Chen"},{"full_name":"Kallinger, Thomas","first_name":"Thomas","last_name":"Kallinger"},{"full_name":"Kawaler, Steven D.","first_name":"Steven D.","last_name":"Kawaler"},{"full_name":"Kuszlewicz, James S.","last_name":"Kuszlewicz","first_name":"James S."},{"full_name":"Lebreton, Yveline","last_name":"Lebreton","first_name":"Yveline"},{"first_name":"Tanda","last_name":"Li","full_name":"Li, Tanda"},{"full_name":"Lucas, Miles","first_name":"Miles","last_name":"Lucas"},{"full_name":"Lundkvist, Mia S.","last_name":"Lundkvist","first_name":"Mia S."},{"full_name":"Mann, Andrew W.","first_name":"Andrew W.","last_name":"Mann"},{"first_name":"Stéphane","last_name":"Mathis","full_name":"Mathis, Stéphane"},{"full_name":"Mathur, Savita","last_name":"Mathur","first_name":"Savita"},{"full_name":"Mazumdar, Anwesh","last_name":"Mazumdar","first_name":"Anwesh"},{"full_name":"Metcalfe, Travis S.","last_name":"Metcalfe","first_name":"Travis S."},{"full_name":"Miglio, Andrea","first_name":"Andrea","last_name":"Miglio"},{"first_name":"Mário J. P.","last_name":"F. G. Monteiro","full_name":"F. G. Monteiro, Mário J. P."},{"first_name":"Benoit","last_name":"Mosser","full_name":"Mosser, Benoit"},{"full_name":"Noll, Anthony","last_name":"Noll","first_name":"Anthony"},{"last_name":"Nsamba","first_name":"Benard","full_name":"Nsamba, Benard"},{"last_name":"Joel Ong","first_name":"Jia Mian","full_name":"Joel Ong, Jia Mian"},{"full_name":"Örtel, S.","first_name":"S.","last_name":"Örtel"},{"full_name":"Pereira, Filipe","last_name":"Pereira","first_name":"Filipe"},{"last_name":"Ranadive","first_name":"Pritesh","full_name":"Ranadive, Pritesh"},{"first_name":"Clara","last_name":"Régulo","full_name":"Régulo, Clara"},{"first_name":"Thaíse S.","last_name":"Rodrigues","full_name":"Rodrigues, Thaíse S."},{"full_name":"Roxburgh, Ian W.","last_name":"Roxburgh","first_name":"Ian W."},{"full_name":"Aguirre, Victor Silva","first_name":"Victor Silva","last_name":"Aguirre"},{"full_name":"Smalley, Barry","last_name":"Smalley","first_name":"Barry"},{"full_name":"Schofield, Mathew","last_name":"Schofield","first_name":"Mathew"},{"first_name":"Sérgio G.","last_name":"Sousa","full_name":"Sousa, Sérgio G."},{"first_name":"Keivan G.","last_name":"Stassun","full_name":"Stassun, Keivan G."},{"full_name":"Stello, Dennis","last_name":"Stello","first_name":"Dennis"},{"first_name":"Jamie","last_name":"Tayar","full_name":"Tayar, Jamie"},{"last_name":"White","first_name":"Timothy R.","full_name":"White, Timothy R."},{"full_name":"Verma, Kuldeep","first_name":"Kuldeep","last_name":"Verma"},{"first_name":"Mathieu","last_name":"Vrard","full_name":"Vrard, Mathieu"},{"last_name":"Yıldız","first_name":"M.","full_name":"Yıldız, M."},{"full_name":"Baker, David","last_name":"Baker","first_name":"David"},{"last_name":"Bazot","first_name":"Michaël","full_name":"Bazot, Michaël"},{"last_name":"Beichmann","first_name":"Charles","full_name":"Beichmann, Charles"},{"first_name":"Christoph","last_name":"Bergmann","full_name":"Bergmann, Christoph"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Cale, Bryson","last_name":"Cale","first_name":"Bryson"},{"first_name":"Roberto","last_name":"Carlino","full_name":"Carlino, Roberto"},{"full_name":"Cartwright, Scott M.","last_name":"Cartwright","first_name":"Scott M."},{"full_name":"Christiansen, Jessie L.","last_name":"Christiansen","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"},{"first_name":"Jason A.","last_name":"Dittmann","full_name":"Dittmann, Jason A."},{"last_name":"Nascimento","first_name":"Jose-Dias Do","full_name":"Nascimento, Jose-Dias Do"},{"last_name":"Eylen","first_name":"Vincent Van","full_name":"Eylen, Vincent Van"},{"full_name":"Fürész, Gabor","first_name":"Gabor","last_name":"Fürész"},{"full_name":"Gagné, Jonathan","first_name":"Jonathan","last_name":"Gagné"},{"full_name":"Gao, Peter","last_name":"Gao","first_name":"Peter"},{"full_name":"Gazeas, Kosmas","last_name":"Gazeas","first_name":"Kosmas"},{"first_name":"Frank","last_name":"Giddens","full_name":"Giddens, Frank"},{"first_name":"Oliver J.","last_name":"Hall","full_name":"Hall, Oliver J."},{"last_name":"Hekker","first_name":"Saskia","full_name":"Hekker, Saskia"},{"last_name":"Ireland","first_name":"Michael J.","full_name":"Ireland, Michael J."},{"full_name":"Latouf, Natasha","last_name":"Latouf","first_name":"Natasha"},{"full_name":"LeBrun, Danny","last_name":"LeBrun","first_name":"Danny"},{"full_name":"Levine, Alan M.","first_name":"Alan M.","last_name":"Levine"},{"full_name":"Matzko, William","first_name":"William","last_name":"Matzko"},{"last_name":"Natinsky","first_name":"Eva","full_name":"Natinsky, Eva"},{"first_name":"Emma","last_name":"Page","full_name":"Page, Emma"},{"last_name":"Plavchan","first_name":"Peter","full_name":"Plavchan, Peter"},{"full_name":"Mansouri-Samani, Masoud","first_name":"Masoud","last_name":"Mansouri-Samani"},{"full_name":"McCauliff, Sean","first_name":"Sean","last_name":"McCauliff"},{"full_name":"Mullally, Susan E.","first_name":"Susan E.","last_name":"Mullally"},{"first_name":"Brendan","last_name":"Orenstein","full_name":"Orenstein, Brendan"},{"full_name":"Soto, Aylin Garcia","first_name":"Aylin Garcia","last_name":"Soto"},{"first_name":"Martin","last_name":"Paegert","full_name":"Paegert, Martin"},{"full_name":"van Saders, Jennifer L.","last_name":"van Saders","first_name":"Jennifer L."},{"full_name":"Schnaible, Chloe","first_name":"Chloe","last_name":"Schnaible"},{"full_name":"Soderblom, David R.","first_name":"David R.","last_name":"Soderblom"},{"last_name":"Szabó","first_name":"Róbert","full_name":"Szabó, Róbert"},{"full_name":"Tanner, Angelle","first_name":"Angelle","last_name":"Tanner"},{"last_name":"Tinney","first_name":"C. G.","full_name":"Tinney, C. G."},{"first_name":"Johanna","last_name":"Teske","full_name":"Teske, Johanna"},{"first_name":"Alexandra","last_name":"Thomas","full_name":"Thomas, Alexandra"},{"first_name":"Regner","last_name":"Trampedach","full_name":"Trampedach, Regner"},{"first_name":"Duncan","last_name":"Wright","full_name":"Wright, Duncan"},{"full_name":"Yuan, Thomas T.","first_name":"Thomas T.","last_name":"Yuan"},{"last_name":"Zohrabi","first_name":"Farzaneh","full_name":"Zohrabi, Farzaneh"}],"volume":157,"date_created":"2022-07-18T14:29:07Z","date_updated":"2022-08-22T07:38:34Z","publication_identifier":{"issn":["0004-6256"]},"month":"05","external_id":{"arxiv":["1901.01643"]},"main_file_link":[{"url":"https://arxiv.org/abs/1901.01643","open_access":"1"}],"oa":1,"quality_controlled":"1","doi":"10.3847/1538-3881/ab1488","language":[{"iso":"eng"}]},{"publication_status":"published","publisher":"Frontiers Media","year":"2019","acknowledgement":"This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Partly Based on observations obtained with the HERMES spectrograph on the Mercator Telescope, which was supported by the Research Foundation—Flanders (FWO), Belgium, the Research Council of KU Leuven, Belgium, the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the Thüringer Landessternwarte Tautenburg, Germany. SM acknowledges support by the National Aeronautics and Space Administration under Grant NNX15AF13G, by the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. RG acknowledges the support from PLATO and GOLF CNES grants. ÂS acknowledges the support from National Aeronautics and Space Administration under Grant NNX17AF27G. PB acknowledges the support of the MINECO under the fellowship program Juan de la Cierva Incorporacion (IJCI-2015-26034).","date_updated":"2022-08-22T07:29:55Z","date_created":"2022-07-18T14:00:36Z","volume":6,"author":[{"full_name":"Mathur, Savita","last_name":"Mathur","first_name":"Savita"},{"full_name":"García, Rafael A.","first_name":"Rafael A.","last_name":"García"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"Ângela R.G.","last_name":"Santos","full_name":"Santos, Ângela R.G."},{"full_name":"Santiago, Netsha","last_name":"Santiago","first_name":"Netsha"},{"full_name":"Beck, Paul G.","last_name":"Beck","first_name":"Paul G."}],"article_number":"46","extern":"1","quality_controlled":"1","external_id":{"arxiv":["1907.01415"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1907.01415","open_access":"1"}],"language":[{"iso":"eng"}],"doi":"10.3389/fspas.2019.00046","month":"07","publication_identifier":{"eissn":["2296-987X"]},"status":"public","title":"Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler","intvolume":" 6","_id":"11613","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","type":"journal_article","abstract":[{"lang":"eng","text":"Over 2,000 stars were observed for 1 month with a high enough cadence in order to look for acoustic modes during the survey phase of the Kepler mission. Solar-like oscillations have been detected in about 540 stars. The question of why no oscillations were detected in the remaining stars is still open. Previous works explained the non-detection of modes with the high level of magnetic activity of the stars. However, the sample of stars studied contained some classical pulsators and red giants that could have biased the results. In this work, we revisit this analysis on a cleaner sample of main-sequence solar-like stars that consists of 1,014 stars. First we compute the predicted amplitude of the modes of that sample and for the stars with detected oscillation and compare it to the noise at high frequency in the power spectrum. We find that the stars with detected modes have an amplitude to noise ratio larger than 0.94. We measure reliable rotation periods and the associated photometric magnetic index for 684 stars out of the full sample and in particular for 323 stars where the amplitude of the modes is predicted to be high enough to be detected. We find that among these 323 stars 32% of them have a level of magnetic activity larger than the Sun during its maximum activity, explaining the non-detection of acoustic modes. Interestingly, magnetic activity cannot be the primary reason responsible for the absence of detectable modes in the remaining 68% of the stars without acoustic modes detected and with reliable rotation periods. Thus, we investigate metallicity, inclination angle of the rotation axis, and binarity as possible causes of low mode amplitudes. Using spectroscopic observations for a subsample, we find that a low metallicity could be the reason for suppressed modes. No clear correlation with binarity nor inclination is found. We also derive the lower limit for our photometric activity index (of 20–30 ppm) below which rotation and magnetic activity are not detected. Finally, with our analysis we conclude that stars with a photometric activity index larger than 2,000 ppm have 98.3% probability of not having oscillations detected."}],"article_type":"original","publication":"Frontiers in Astronomy and Space Sciences","citation":{"apa":"Mathur, S., García, R. A., Bugnet, L. A., Santos, Â. R. G., Santiago, N., & Beck, P. G. (2019). Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. Frontiers Media. https://doi.org/10.3389/fspas.2019.00046","ieee":"S. Mathur, R. A. García, L. A. Bugnet, Â. R. G. Santos, N. Santiago, and P. G. Beck, “Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler,” Frontiers in Astronomy and Space Sciences, vol. 6. Frontiers Media, 2019.","ista":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. 2019. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. 6, 46.","ama":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. 2019;6. doi:10.3389/fspas.2019.00046","chicago":"Mathur, Savita, Rafael A. García, Lisa Annabelle Bugnet, Ângela R.G. Santos, Netsha Santiago, and Paul G. Beck. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” Frontiers in Astronomy and Space Sciences. Frontiers Media, 2019. https://doi.org/10.3389/fspas.2019.00046.","short":"S. Mathur, R.A. García, L.A. Bugnet, Â.R.G. Santos, N. Santiago, P.G. Beck, Frontiers in Astronomy and Space Sciences 6 (2019).","mla":"Mathur, Savita, et al. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” Frontiers in Astronomy and Space Sciences, vol. 6, 46, Frontiers Media, 2019, doi:10.3389/fspas.2019.00046."},"date_published":"2019-07-10T00:00:00Z","keyword":["Astronomy and Astrophysics"],"scopus_import":"1","day":"10","article_processing_charge":"No"},{"quality_controlled":"1","oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1903.00115","open_access":"1"}],"external_id":{"arxiv":["1903.00115"]},"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stz622","month":"06","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","publisher":"Oxford University Press","acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","year":"2019","date_created":"2022-07-18T14:26:03Z","date_updated":"2022-08-22T07:35:19Z","volume":485,"author":[{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"first_name":"Dennis","last_name":"Stello","full_name":"Stello, Dennis"},{"full_name":"García, Rafael A","first_name":"Rafael A","last_name":"García"},{"full_name":"Mathur, Savita","last_name":"Mathur","first_name":"Savita"},{"first_name":"Sanjib","last_name":"Sharma","full_name":"Sharma, Sanjib"},{"first_name":"Isabel L","last_name":"Colman","full_name":"Colman, Isabel L"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"}],"extern":"1","article_type":"original","page":"5616-5630","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz622.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:10.1093/mnras/stz622.","ieee":"M. Hon et al., “A search for red giant solar-like oscillations in all Kepler data,” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., & Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz622","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 2019;485(4):5616-5630. doi:10.1093/mnras/stz622"},"date_published":"2019-06-01T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"scopus_import":"1","day":"01","article_processing_charge":"No","status":"public","title":"A search for red giant solar-like oscillations in all Kepler data","intvolume":" 485","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11615","oa_version":"Preprint","type":"journal_article","abstract":[{"text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars.","lang":"eng"}],"issue":"4"},{"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.09854"}],"external_id":{"arxiv":["1902.09854"]},"oa":1,"language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201834780","month":"04","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","publisher":"EDP Science","acknowledgement":"We thank the enitre T’DA team for useful comments and discussions, in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106).","year":"2019","date_created":"2022-07-18T14:13:34Z","date_updated":"2022-08-22T07:32:51Z","volume":624,"author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"last_name":"Davies","first_name":"G. R.","full_name":"Davies, G. R."},{"full_name":"Hall, O. J.","last_name":"Hall","first_name":"O. J."},{"first_name":"M. N.","last_name":"Lund","full_name":"Lund, M. N."},{"full_name":"Rendle, B. M.","last_name":"Rendle","first_name":"B. M."}],"article_number":"A79","extern":"1","article_type":"original","publication":"Astronomy & Astrophysics","citation":{"chicago":"Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall, M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” Astronomy & Astrophysics. EDP Science, 2019. https://doi.org/10.1051/0004-6361/201834780.","mla":"Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” Astronomy & Astrophysics, vol. 624, A79, EDP Science, 2019, doi:10.1051/0004-6361/201834780.","short":"L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M. Rendle, Astronomy & Astrophysics 624 (2019).","ista":"Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. 624, A79.","apa":"Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund, M. N., & Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. EDP Science. https://doi.org/10.1051/0004-6361/201834780","ieee":"L. A. Bugnet et al., “FliPerClass: In search of solar-like pulsators among TESS targets,” Astronomy & Astrophysics, vol. 624. EDP Science, 2019.","ama":"Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. 2019;624. doi:10.1051/0004-6361/201834780"},"date_published":"2019-04-19T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","day":"19","article_processing_charge":"No","title":"FliPerClass: In search of solar-like pulsators among TESS targets","status":"public","intvolume":" 624","_id":"11614","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","type":"journal_article","abstract":[{"text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide full-frame images of almost the entire sky. The amount of stellar data to be analysed represents hundreds of millions stars, which is several orders of magnitude more than the number of stars observed by the Convection, Rotation and planetary Transits satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying the newly observed stars with near real-time algorithms to better guide the subsequent detailed studies. In this paper, we present a classification algorithm built to recognise solar-like pulsators among classical pulsators. This algorithm relies on the global amount of power contained in the power spectral density (PSD), also known as the flicker in spectral power density (FliPer). Because each type of pulsating star has a characteristic background or pulsation pattern, the shape of the PSD at different frequencies can be used to characterise the type of pulsating star. The FliPer classifier (FliPerClass) uses different FliPer parameters along with the effective temperature as input parameters to feed a ML algorithm in order to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators with a 98% accuracy. Among them, solar-like pulsating stars are recognised with a 99% accuracy, which is of great interest for a further seismic analysis of these stars, which are like our Sun. Similar results are obtained when we trained our classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is part of the large TASC classification pipeline developed by the TESS Data for Asteroseismology (T’DA) classification working group.","lang":"eng"}]}]