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1. Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS

Author: G Lacedelli, T G Wilson, L Malavolta, M J Hooton, A Collier Cameron, Y Alibert, A Mortier, A Bonfanti, R D Haywood, S Hoyer, G Piotto, A Bekkelien, A M Vanderburg, W Benz, X Dumusque, A Deline, M López-Morales, L Borsato, K Rice, L Fossati, D W Latham, A Brandeker, E Poretti, S G Sousa, A Sozzetti, S Salmon, C J Burke, V Van Grootel, M M Fausnaugh, V Adibekyan, C X Huang, H P Osborn, A J Mustill, E Pallé, V Bourrier, V Nascimbeni, R Alonso, G Anglada, T Bárczy, D Barrado y Navascues, S C C Barros, W Baumjohann, M Beck, T Beck, N Billot, X Bonfils, C Broeg, L A Buchhave, J Cabrera, S Charnoz, R Cosentino, Sz Csizmadia, M B Davies, M Deleuil, L Delrez, O Demangeon, B -O Demory, D Ehrenreich, A Erikson, E Esparza-Borges, H G Florén, A Fortier, M Fridlund, D Futyan, D Gandolfi, A Ghedina, M Gillon, M Güdel, P Guterman, A Harutyunyan, K Heng, K G Isaak, J M Jenkins, L Kiss, J Laskar, A Lecavelier des Etangs, M Lendl, C Lovis, D Magrin, L Marafatto, A F Martinez Fiorenzano, P F L Maxted, M Mayor, G Micela, E Molinari, F Murgas, N Narita, G Olofsson, R Ottensamer, I Pagano, A Pasetti, M Pedani, F A Pepe, G Peter, D F Phillips, D Pollacco, D Queloz, R Ragazzoni, N Rando, F Ratti, H Rauer, I Ribas, N C Santos, D Sasselov, G Scandariato, S Seager, D Ségransan, L M Serrano, A E Simon, A M S Smith, M Steinberger, M Steller, Gy Szabó, N Thomas, J D Twicken, S Udry, N Walton, and J N Winn
Published: 2022
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2. A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113

Author: H P Osborn, D J Armstrong, V Adibekyan, K A Collins, E Delgado-Mena, S B Howell, C Hellier, G W King, J Lillo-Box, L D Nielsen, J F Otegi, N C Santos, C Ziegler, D R Anderson, C Briceño, C Burke, D Bayliss, D Barrado, E M Bryant, D J A Brown, S C C Barros, F Bouchy, D A Caldwell, D M Conti, R F Díaz, D Dragomir, M Deleuil, O D S Demangeon, C Dorn, T Daylan, P Figueira, R Helled, S Hoyer, J M Jenkins, E L N Jensen, D W Latham, N Law, D R Louie, A W Mann, A Osborn, D L Pollacco, D R Rodriguez, B V Rackham, G Ricker, N J Scott, S G Sousa, S Seager, K G Stassun, J C Smith, P Strøm, S Udry, J Villaseñor, R Vanderspek, R West, P J Wheatley, and J N Winn
Published: 2021
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3. Mass determinations of the three mini-Neptunes transiting TOI-125

Author: L D Nielsen, D Gandolfi, D J Armstrong, J S Jenkins, M Fridlund, N C Santos, F Dai, V Adibekyan, R Luque, J H Steffen, M Esposito, F Meru, S Sabotta, E Bolmont, D Kossakowski, J F Otegi, F Murgas, M Stalport, F Rodler, M R Díaz, N T Kurtovic, G Ricker, R Vanderspek, D W Latham, S Seager, J N Winn, J M Jenkins, R Allart, J M. Almenara, D Barrado, S C C Barros, D Bayliss, Z M Berdiñas, I Boisse, F Bouchy, P Boyd, D J A Brown, E M Bryant, C Burke, W D Cochran, B F Cooke, O D S Demangeon, R F Díaz, J Dittman, C Dorn, X Dumusque, R A García, L González-Cuesta, S Grziwa, I Georgieva, N Guerrero, A P Hatzes, R Helled, C E Henze, S Hojjatpanah, J Korth, K W F Lam, J Lillo-Box, T A Lopez, J Livingston, S Mathur, O Mousis, N Narita, H P Osborn, E Palle, P A Peña Rojas, C M Persson, S N Quinn, H Rauer, S Redfield, A Santerne, L A dos Santos, J V Seidel, S G Sousa, E B Ting, M Turbet, S Udry, A Vanderburg, V Van Eylen, J I Vines, P J Wheatley, and P A Wilson
Published: 2020
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4. TESS and HARPS reveal two sub-Neptunes around TOI 1062

Author: J. F. Otegi, F. Bouchy, R. Helled, D. J. Armstrong, M. Stalport, A. Psaridi, J.-B. Delisle, K.G. Stassun, E. Delgado-Mena, N. C. Santos, N. C. Hara, K. Collins, S. Gandhi, C. Dorn, M. Brogi, M. Fridlund, H. P. Osborn, S. Hoyer, S. Udry, S. Hojjatpanah, L. D. Nielsen, X. Dumusque, V. Adibekyan, D. Conti, R. Schwarz, G. Wang, P. Figueira, J. Lillo-Box, A. Hadjigeorghiou, D. Bayliss, P. A. Strøm, S. G. Sousa, D. Barrado, A. Osborn, S. C. C. Barros, D. J. A. Brown, J. D. Eastman, D. R. Ciardi, A. Vanderburg, R. F. Goeke, N. M. Guerrero, P. T. Boyd, D. A. Caldwell, C. E. Henze, B. McLean, G. Ricker, R. Vanderspek, D. W. Latham, S. Seager, J. Winn, and J. M. Jenkins
Subjects: Astronomy, Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite (TESS) mission was designed to perform an all-sky search of planets around bright and nearby stars. Here we report the discovery of two sub-Neptunes orbiting around TOI 1062 (TIC 299799658), a V = 10.25 G9V star observed in the TESS Sectors 1, 13, 27, and 28. We use precise radial velocity observations from HARPS to confirm and characterize these two planets. TOI 1062b has a radius of 2.265(-0.091,+0.096) Rꚛ, a mass of 10.15 ± 0.8 Mꚛ, and an orbital period of 4.1130 ± 0.0015 days. The second planet is not transiting, has a minimum mass of 9.78(−1.18,+1.26) Mꚛ and is near the 2:1 mean motion resonance with the innermost planet with an orbital period of 7.972(−0.024,+0.018) days. We performed a dynamical analysis to explore the proximity of the system to this resonance, and to attempt further constraining the orbital parameters. The transiting planet has a mean density of 4.85(−0.74,+0.84) g/cu. cm and an analysis of its internal structure reveals that it is expected to have a small volatile envelope accounting for 0.35% of the mass at most. The star’s brightness and the proximity of the inner planet to what is know as the radius gap make it an interesting candidate for transmission spectroscopy, which could further constrain the composition and internal structure of TOI 1062b.
Published: 2021
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5. HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS

Author: Eric L. N. Jensen, Sara Seager, Brett C. Addison, Jack Okumura, Stephen R. Kane, Martin Paegert, Gavin Wang, J. Dittman, Guillermo Torres, David W. Latham, Thomas Barclay, Karen A. Collins, Laura Kreidberg, Sharon X. Wang, Matthew W. Mengel, Jeffrey C. Smith, Jonathan Horner, C. G. Tinney, Sarah Ballard, Keivan G. Stassun, Edward H. Morgan, John F. Kielkopf, Ian Crossfield, H. P. Osborn, Avi Shporer, Tianjun Gan, Roland Vanderspek, Hui Zhang, Nicholas M. Law, Shude Mao, Lorenzo Spina, Robert A. Wittenmyer, Peter Plavchan, Richard P. Schwarz, Cesar Briceno, C. Ziegler, Jacob L. Bean, Bernie Shiao, Joshua N. Winn, Jon M. Jenkins, Steve B. Howell, Coel Hellier, Daniel Foreman-Mackey, Andrew W. Mann, Megan Bedell, Brendan P. Bowler, Michael Vezie, Duncan J. Wright, George R. Ricker, Jorge Melendez, and Joseph D. Twicken
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Star (game theory), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Spectral line, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Neptune, QB460, 0103 physical sciences, 010303 astronomy & astrophysics, QB600, Solar and Stellar Astrophysics (astro-ph.SR), QB, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright ($V=8.75$ mag, $K=7.15$ mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located $56.8\pm0.1$ pc away with a radius of $R_{\ast}=0.97\pm0.02\ R_{\odot}$ and a mass of $M_{\ast}=1.03\pm0.05\ M_{\odot}$. We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of $R_{p}=3.53\pm0.13\ R_{\oplus}$ on a $17.47$ day orbit with a mass of $M_{p}=11.2\pm5.4\ M_{\oplus}$ ($3\sigma$ mass upper limit of $27.4\ M_{\oplus}$). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin sample, without a statistically significant refractory element depletion., Comment: 20 pages, 15 figures, accepted for publication in MNRAS
Published: 2021
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6. Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS

Author: Sergio Hoyer, Vardan Adibekyan, J.-B. Delisle, Nuno C. Santos, David Barrado, Enric Palle, Damien Ségransan, Isabella Pagano, Malcolm Fridlund, Antonio García Muñoz, M. Steller, A. Deline, Guillem Anglada-Escudé, A. Bekkelien, Nicolas Billot, Ignasi Ribas, Don Pollacco, Roberto Ragazzoni, Yann Alibert, T. Bárczy, Gaetano Scandariato, H. P. Osborn, L. Borsato, Alain Lecavelier des Etangs, Heike Rauer, Thomas G. Wilson, M. Beck, Mahmoudreza Oshagh, L. Delrez, Nicholas A. Walton, Roi Alonso, S. G. Sousa, Stéphane Udry, M. J. Hooton, Kevin Heng, S. Sulis, Manuel Guedel, Göran Olofsson, Vincent Bourrier, Michaël Gillon, Anders Erikson, Monika Lendl, Didier Queloz, Davide Gandolfi, Olivier Demangeon, Luca Fossati, Nicolas Thomas, Wolfgang Baumjohann, Pierre F. L. Maxted, Brice-Olivier Demory, S. C. C. Barros, Alexis M. S. Smith, Willy Benz, Andrea Bonfanti, Sébastien Charnoz, Melvyn B. Davies, Juan Cabrera, Magali Deleuil, Alexis Brandeker, J. Haldemann, László L. Kiss, Giampaolo Piotto, Valerio Nascimbeni, Christopher Broeg, Andrea Fortier, Jacques Laskar, Christophe Lovis, D. Futyan, Valérie Van Grootel, Pascal Guterman, Gyula M. Szabó, A. E. Simon, Francisco J. Pozuelos, Andrew Collier Cameron, David Ehrenreich, S. Salmon, Xavier Bonfils, Nathan Hara, Fundação para a Ciência e a Tecnologia (Portugal), European Commission, Swiss National Science Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Belgian Science Policy Office, Université de Liège, Austrian Research Promotion Agency, Hungarian Scientific Research Fund, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Cavendish Laboratory, University of Cambridge [UK] (CAM), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), Université de Genève (UNIGE), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)
Subjects: 010504 meteorology & atmospheric sciences, 530 Physics, FOS: Physical sciences, Astrophysics - Earth and planetary astrophysics, Q1, 01 natural sciences, Planet, QB460, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, QB600, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, 520 Astronomy, Astronomy, Astronomy and Astrophysics, Radius, 620 Engineering, Exoplanet, Orbit, Stars, 13. Climate action, Satellite, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], QB799
Abstract: Delrez, L., et al., Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior and orbital properties of the planetary companions. ν Lupi (HD 136352) is a naked-eye (V = 5.78) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6 and 107.6 d via radial-velocity monitoring. The two inner planets (b and c) were recently found to transit, prompting a photometric follow-up by the brand new Characterising Exoplanets Satellite (CHEOPS). Here, we report that the outer planet d is also transiting, and measure its radius and mass to be 2.56 ± 0.09 R and 8.82 ± 0.94 M, respectively. With its bright Sun-like star, long period and mild irradiation (~5.7 times the irradiation of Earth), ν Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b probably has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen–helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the ν Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets., The MOC activities have been supported by ESA contract 4000124370. S.C. acknowledges financial support by LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001). This work was supported by FCT (Fundação para a Ciência e a Tecnologia) through national funds and by FEDER (Fundo Europeu de Desenvolvimento Regional) through COMPETE2020—Programa Operacional Competitividade e Internacionalização with these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B., S.G.S. and V.A. acknowledge support from FCT through contracts IF/01312/2014/CP1215/CT0004, CEECIND/00826/2018, POPH/FSE (EC) and IF/00650/2015/CP1273/CT0001. O.D.S.D. is supported in the form of a work contract (DL 57/2016/CP1364/CT0004) with national funds through FCT. M.J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. A.D. and D.E. acknowledge support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement 724427). S.H. acknowledges CNES funding through grant 837319. The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33 and MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The Belgian participation in CHEOPS has been supported by the Belgian Federal Science Policy Office in the framework of the PRODEX Programme of the ESA under contract PEA 4000131343, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia–Brussels Federation. L.D. is an FRS-FNRS Postdoctoral Researcher. M. Gillon is an FRS–FNRS Senior Research Associate. V.V.G. is an FRS–FNRS Research Associate. M.L. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 ‘GRAPPA’. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). S. Salmon has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement 833925, project STAREX). G.M.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS activities have been supported by the Italian Space Agency, under the programmes ASI-INAF 2013-016-R.0 and ASI-INAF 2019-29-HH.0. L.B., G.P., I.P., G.S. and V.N. acknowledge funding support from the Italian Space Agency (ASI) regulated by ‘Accordo ASI-INAF 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015’. A.C.C. and T.G.W. acknowledge support from STFC consolidated grant ST/M001296/1. D.G., X.B., S.C., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. We thank S. R. Kane for sharing some RV data before their publication and L. D. Nielsen for helping to plan the CHEOPS observations on the basis of her analysis of the TESS data. We also thank M. Cretignier for his independent analysis of the HARPS RV data.
Published: 2021
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7. Rapid classification of TESS planet candidates with convolutional neural networks

Author: H. P. Osborn, M. Ansdell, Y. Ioannou, M. Sasdelli, D. Angerhausen, D. Caldwell, J. M. Jenkins, C. Räissi, and J. C. Smith
Published: 2020
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8. The young HD 73583 (TOI-560) planetary system: Two 10-M⊕ mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf

Author: O Barragán, D J Armstrong, D Gandolfi, I Carleo, A A Vidotto, C Villarreal D’Angelo, A Oklopčić, H Isaacson, D Oddo, K Collins, M Fridlund, S G Sousa, C M Persson, C Hellier, S Howell, A Howard, S Redfield, N Eisner, I Y Georgieva, D Dragomir, D Bayliss, L D Nielsen, B Klein, S Aigrain, M Zhang, J Teske, J D Twicken, J Jenkins, M Esposito, V Van Eylen, F Rodler, V Adibekyan, J Alarcon, D R Anderson, J M Akana Murphy, D Barrado, S C C Barros, B Benneke, F Bouchy, E M Bryant, R P Butler, J Burt, J Cabrera, S Casewell, P Chaturvedi, R Cloutier, W D Cochran, J Crane, I Crossfield, N Crouzet, K I Collins, F Dai, H J Deeg, A Deline, O D S Demangeon, X Dumusque, P Figueira, E Furlan, C Gnilka, M R Goad, E Goffo, F Gutiérrez-Canales, A Hadjigeorghiou, Z Hartman, A P Hatzes, M Harris, B Henderson, T Hirano, S Hojjatpanah, S Hoyer, P Kabáth, J Korth, J Lillo-Box, R Luque, M Marmier, T Močnik, A Muresan, F Murgas, E Nagel, H L M Osborne, A Osborn, H P Osborn, E Palle, M Raimbault, G R Ricker, R A Rubenzahl, C Stockdale, N C Santos, N Scott, R P Schwarz, S Shectman, S Seager, D Ségransan, L M Serrano, M Skarka, A M S Smith, J Šubjak, T G Tan, S Udry, C Watson, P J Wheatley, R West, J N Winn, S X Wang, A Wolfgang, C Ziegler, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Swiss National Science Foundation, Fondazione Cassa di Risparmio di Torino, Centre National D'Etudes Spatiales (France), and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Stars: activity, Planets and satellites: individual: HD 73583 (TOI-560), radial velocities [Techniques], photometric [Techniques], FOS: Physical sciences, Astronomy and Astrophysics, Q1, individual: HD 73583 (TOI-560) [Planets and satellites], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Techniques: radial velocities, activity [Stars], Solar and Stellar Astrophysics (astro-ph.SR), Techniques: photometric, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.--Full list of authors: Barragan, O.; Armstrong, D. J.; Gandolfi, D.; Carleo, I; Vidotto, A. A.; D'Angelo, C. Villarreal; Oklopcic, A.; Isaacson, H.; Oddo, D.; Collins, K.; Fridlund, M.; Sousa, S. G.; Persson, C. M.; Hellier, C.; Howell, S.; Howard, A.; Redfield, S.; Eisner, N.; Georgieva, I. Y.; Dragomir, D.; Bayliss, D.; Nielsen, L. D.; Klein, B.; Aigrain, S.; Zhang, M.; Teske, J.; Twicken, J. D.; Jenkins, J.; Esposito, M.; Van Eylen, V.; Rodler, F.; Adibekyan, V; Alarcon, J.; Anderson, D. R.; Murphy, J. M. Akana; Barrado, D.; Barros, S. C. C.; Benneke, B.; Bouchy, F.; Bryant, E. M.; Butler, R. P.; Burt, J.; Cabrera, J.; Casewell, S.; Chaturvedi, P.; Cloutier, R.; Cochran, W. D.; Crane, J.; Crossfield, I; Crouzet, N.; Collins, K., I; Dai, F.; Deeg, H. J.; Deline, A.; Demangeon, O. D. S.; Dumusque, X.; Figueira, P.; Furlan, E.; Gnilka, C.; Goad, M. R.; Goffo, E.; Gutierrez-Canales, F.; Hadjigeorghiou, A.; Hartman, Z.; Hatzes, A. P.; Harris, M.; Henderson, B.; Hirano, T.; Hojjatpanah, S.; Hoyer, S.; Kabath, P.; Korth, J.; Lillo-Box, J.; Luque, R.; Marmier, M.; Mocnik, T.; Muresan, A.; Murgas, F.; Nagel, E.; Osborne, H. L. M.; Osborn, A.; Osborn, H. P.; Palle, E.; Raimbault, M.; Ricker, G. R.; Rubenzahl, R. A.; Stockdale, C.; Santos, N. C.; Scott, N.; Schwarz, R. P.; Shectman, S.; Seager, S.; Segransan, D.; Serrano, L. M.; Skarka, M.; Smith, A. M. S.; Subjak, J.; Tan, T. G.; Udry, S.; Watson, C.; Wheatley, P. J.; West, R.; Winn, J. N.; Wang, S. X.; Wolfgang, A.; Ziegler, C.; KESPRINT Team., We present the discovery and characterization of two transiting planets observed by TESS in the light curves of the young and bright (V = 9.67) star HD73583 (TOI-560). We perform an intensive spectroscopic and photometric space- and ground-based follow-up in order to confirm and characterize the system. We found that HD73583 is a young (∼500 Myr) active star with a rotational period of 12.08 ± 0.11 d, and a mass and radius of 0.73 ± 0.02 M⊙ and 0.65 ± 0.02 R⊙, respectively. HD 73583 b (Pb = 6.3980420+0.0000067−0.0000062 d) has a mass and radius of 10.2+3.4−3.1 M⊕ and 2.79 ± 0.10 R⊕, respectively, which gives a density of 2.58+0.95−0.81 gcm−3⁠. HD 73583 c (Pc = 18.87974+0.00086−0.00074 d) has a mass and radius of 9.7+1.8−1.7 M⊕ and 2.39+0.10−0.09 R⊕, respectively, which translates to a density of 3.88+0.91−0.80 gcm−3⁠. Both planets are consistent with worlds made of a solid core surrounded by a volatile envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies. We expect ongoing atmospheric mass-loss for both planets caused by stellar irradiation. We estimate that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments. © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society., This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions (http://www.kesprint.science). We thank the referee for their helpful comments and suggestions that improved the quality of this manuscript. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work uses observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper is in part based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) projects ST/M001962/1 and ST/S002642/1. This research has used 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. Some of the observations in the paper used the High-Resolution Imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). OB, BK, and SA acknowledge that this publication is part of a project that has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 865624). DG and LMS gratefully acknowledge financial support from the Cassa di Risparmio di Torino foundation under Grant No. 2018.2323 ‘Gaseous or rocky? Unveiling the nature of small worlds’. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). APH and ME acknowledges grant HA 3279/12-1 within the DFG Schwerpunkt SPP 1992, ‘Exploring the Diversity of Extrasolar Planets’. JS and PK would like to acknowledge support from MSMT grant LTT-20015. We acknowledges the support by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FISAST /28953/2017 & POCI-01-0145-FEDER-028953. AD acknowledges the financial support of the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). AD also acknowledges financial support of the the Swiss National Science Foundation (SNSF) through the National Centre for Competence in Research ‘PlanetS’. MF, IYG, JK, and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 177/19, 174/18, 2020-00104, 65/19). FGC thanks the Mexican national council for science and technology (CONACYT, CVU-1005374). MS acknowledge financial support of the Inter-transfer grant no LTT-20015. JL-B acknowledges financial support received from ‘la Caixa’ Foundation (ID 100010434) and from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 847648, with fellowship code LCF/BQ/PI20/11760023. AAV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 817540, ASTROFLOW). JMAM is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1842400. JMAM acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. RAR is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. RL acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence ‘Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). PC acknowledges the generous support from Deutsche Forschungsgemeinschaft (DFG) of the grant CH 2636/1-1. SH acknowledges CNES funding through the grant 837319. VA acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). AO is supported by an STFC studentship. XD would like to acknowledge the funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement SCORE No 851555). HJD acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under the grant ‘Contribution of the IAC to the PLATO Space Mission’ with reference PID2019-107061GB-C66, DOI: 10.13039/501100011033. DD acknowledges support from the TESS Guest Investigator Program grant 80NSSC19K1727 and NASA Exoplanet Research Program grant 18-2XRP18_2-0136. AO gratefully acknowledges support from the Dutch Research Council NWO Veni grant.
Published: 2022
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9. TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter

Author: J. Lillo-Box, D. Gandolfi, D. J. Armstrong, K. A. Collins, L. D. Nielsen, R. Luque, J. Korth, S. G. Sousa, S. N. Quinn, L. Acuña, S. B. Howell, G. Morello, C. Hellier, S. Giacalone, S. Hoyer, K. Stassun, E. Palle, A. Aguichine, O. Mousis, V. Adibekyan, T. Azevedo Silva, D. Barrado, M. Deleuil, J. D. Eastman, A. Fukui, F. Hawthorn, J. M. Irwin, J. M. Jenkins, D. W. Latham, A. Muresan, N. Narita, C. M. Persson, A. Santerne, N. C. Santos, A. B. Savel, H. P. Osborn, J. Teske, P. J. Wheatley, J. N. Winn, S. C. C. Barros, R. P. Butler, D. A. Caldwell, D. Charbonneau, R. Cloutier, J. D. Crane, O. D. S. Demangeon, R. F. Díaz, X. Dumusque, M. Esposito, B. Falk, H. Gill, S. Hojjatpanah, L. Kreidberg, I. Mireles, A. Osborn, G. R. Ricker, J. E. Rodriguez, R. P. Schwarz, S. Seager, J. Serrano Bell, S. A. Shectman, A. Shporer, M. Vezie, S. X. Wang, G. Zhou, Ministerio de Ciencia e Innovación (España), Fundación 'la Caixa', European Commission, and European Research Council
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, Techniques: radial velocities, Stars: individual: TOI-969, FOS: Physical sciences, Astronomy and Astrophysics, Planets and satellites: detection, Planets and satellites: fundamental parameters, Techniques: photometric, Planets and satellites: composition, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Lillo-Box, J.; Gandolfi, D.; Armstrong, D. J.; Collins, K. A.; Nielsen, L. D.; Luque, R.; Korth, J.; Sousa, S. G.; Quinn, S. N.; Acuña, L.; Howell, S. B.; Morello, G.; Hellier, C.; Giacalone, S.; Hoyer, S.; Stassun, K.; Palle, E.; Aguichine, A.; Mousis, O.; Adibekyan, V.; Azevedo Silva, T.; Barrado, D.; Deleuil, M.; Eastman, J. D.; Fukui, A.; Hawthorn, F.; Irwin, J. M.; Jenkins, J. M.; Latham, D. W.; Muresan, A.; Narita, N.; Persson, C. M.; Santerne, A.; Santos, N. C.; Savel, A. B.; Osborn, H. P.; Teske, J.; Wheatley, P. J.; Winn, J. N.; Barros, S. C. C.; Butler, R. P.; Caldwell, D. A.; Charbonneau, D.; Cloutier, R.; Crane, J. D.; Demangeon, O. D. S.; Díaz, R. F.; Dumusque, X.; Esposito, M.; Falk, B.; Gill, H.; Hojjatpanah, S.; Kreidberg, L.; Mireles, I.; Osborn, A.; Ricker, G. R.; Rodriguez, J. E.; Schwarz, R. P.; Seager, S.; Serrano Bell, J.; Shectman, S. A.; Shporer, A.; Vezie, M.; Wang, S. X.; Zhou, G.--This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. Aims. In this paper, we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star. Methods. We use a set of precise radial velocity observations from HARPS, PFS, and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system. Results. We find that TOI-969 b is a transiting close-in (Pb ~ 1.82 days) mini-Neptune planet (mb = 9.1−1.0+1.1 M⊕, Rb = 2.765−0.097+0.088 R⊕), placing it on the lower boundary of the hot-Neptune desert (Teq,b = 941 ± 31 K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of Pc = 1700−280+290 days, a minimum mass of mc sin ic = 11.3−0.9+1.1 MJup, and a highly eccentric orbit of ec = 0.628−0.036+0.043. Conclusions. The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93 and orbits a moderately bright (G = 11.3 mag) star, making it an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems. © The Authors 2023., J.L-B. acknowledges financial support received from “la Caixa” Foundation (ID 100010434) and from the European Unions Horizon 2020 research and innovation programme under the Marie Slodowska-Curie grant agreement No 847648, with fellowship code LCF/BQ/PI20/11760023. This research has also been partly funded by the Spanish State Research Agency (AEI) Projects No.PID2019-107061GB-C6l and No. MDM-2017-0737 Unidad de Excelencia “Maria de Maeztu” – Centro de Astrobiología (INTA-CSIC). R.L. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). DJ.A. acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). S.G.S acknowledges the support from FCT through Estimulo FCT contract nr.CEECIND/00826/2018 and POPH/FSE (EC). G.M. has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 895525. S.H. acknowledges CNES funding through the grant 837319. The French group acknowledges financial support from the French Programme National de Planétologie (PNP, INSU). This work is partly financed by the Spanish Mnistry of Economics and Competitiveness through grants PGC2018-098153-B-C31. We acknowledge the support by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FISAST/28953/2017 & POCI-01-0145-FEDER-028953. P.J.W is supported by an STFC consolidated grant (ST/T000406/1). F.H. is funded by an STFC studentship. T.A.S acknowledges support from the Fundação para a Ciência e a Tecnologia (FCT) through the Fellowship PD/BD/150416/2019 and POCH/FSE (EC). C.M.P. acknowledges support from the SNSA (dnr 65/19P). This work has been carried out within the framework of the National Centre of Competence in Research (NCCR) PlanetS supported by the Swiss National Science Foundation. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement SCORE No 851555). O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e a Tecnologia (FCT). M.E. acknowledges the support of the DFG priority programSPP 1992 “Exploring the Diversity of Extrasolar Planets” (HA 3279/12-1). A.O. is funded by an STFC studentship. J.K. gratefully acknowledge the support of the Swedish National Space Agency (SNSA; DNR 2020-00104). This work makes use of observations from the LCOGT network. This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by ISPS KAKENHI (IP18H05439) and 1ST PRESTO (IPMIPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. Some of the observations in the paper made use of the High-Resolution Imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nie Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. The MEarth Team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST-1616624, and upon work supported by the National Aeronautics and Space Administration under Grant No. 80NSSC18K0476 issued through the XRP Program. This work is made possible by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This research made use of Astropy, (a community-developed core Python package for Astronomy, Astropy Collaboration 2013, 2018), SciPy (Virtanen et al. 2020), matplotlib (a Python library for publication quality graphics Hunter 2007), and numpy (Harris et al. 2020). This research has made use of NASA’s Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
Published: 2022
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10. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author: Andrés Jordán, Sara Seager, Brett C. Addison, Maximilian N. Günther, Monika Lendl, Jack Okumura, Jorge Lillo-Box, Jon M. Jenkins, Roland Vanderspek, C. G. Tinney, Benjamin J. Fulton, Peter J. Wheatley, Erik A. Petigura, Beth A. Henderson, C. Stibbard, P. Figueira, Rafael Brahm, Eric L. N. Jensen, Michael Reefe, Cesar Briceno, Chris Stockdale, S. Hojjatpanah, Farisa Y. Morales, Alexis M. S. Smith, Caroline Dorn, Thomas Henning, Vardan Adibekyan, George W. King, Lauren M. Weiss, David R. Ciardi, Howard Isaacson, Richard P. Schwarz, Thomas Barclay, Stephen R. Kane, Keivan G. Stassun, David W. Latham, Malcolm Fridlund, Jack S. Acton, Ravit Helled, Sharon X. Wang, John Berberian, Joseph D. Twicken, J. F. Otegi, David R. Anderson, Sarah L. Casewell, Elise Furlan, Elisabeth Matthews, Johanna Teske, Rodrigo F. Díaz, Samuel Gill, Daniel Bayliss, Ian Crossfield, Peter Plavchan, Matthew W. Mengel, Joshua E. Schlieder, John F. Kielkopf, Stéphane Udry, E. Delgado Mena, H. P. Osborn, Avi Shporer, R. Cloutier, J. Villasenor, Duncan J. Wright, E. Gaidos, A. Osborn, K. I. Collins, Angelle Tanner, Nicholas M. Law, Björn Benneke, Joshua N. Winn, Fei Dai, Nicholas J. Scott, Erica J. Gonzales, Courtney D. Dressing, Sarah Ballard, Don Pollacco, Coel Hellier, Michael R. Goad, David J. Armstrong, Varoujan Gorjian, Paula Sarkis, Richard C. Kidwell, F. Zohrabi, Nuno C. Santos, David Barrado, Matthew R. Burleigh, Sergio Hoyer, Claire Geneser, Christopher J. Burke, Richard G. West, James McCormac, P. A. Strøm, Daniel Huber, Aleisha Hogan, Paul Robertson, Natalie M. Batalha, Edward M. Bryant, Liam Raynard, Karen A. Collins, Robert A. Wittenmyer, Mark E. Rose, Rachel A. Matson, Steve B. Howell, James S. Jenkins, Jose I. Vines, S. C. C. Barros, Néstor Espinoza, B. Cale, Andrew W. Howard, Diana Dragomir, Alexandre Santerne, M. Lund, Olivier Demangeon, Brendan P. Bowler, Benjamin F. Cooke, Xavier Dumusque, Andrew W. Mann, Hui Zhang, Carl Ziegler, Arpita Roy, Rosanna H. Tilbrook, Sérgio F. Sousa, George R. Ricker, Jonathan Horner, Elisa V. Quintana, Thiam-Guan Tan, Louise D. Nielsen, François Bouchy, University of New South Wales [Sydney] (UNSW), McDonald Observatory, University of Texas at Austin [Austin], Leiden Observatory [Leiden], Universiteit Leiden, Chalmers University of Technology [Gothenburg, Sweden], NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département de Physique [Montréal], Université de Montréal (UdeM), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Optimisation - Système - Energie (GEPEA-OSE), Laboratoire de génie des procédés - environnement - agroalimentaire (GEPEA), Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN)-Université de Nantes (UN)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut Universitaire de Technologie Saint-Nazaire (IUT Saint-Nazaire), Université de Nantes (UN)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-École nationale vétérinaire, agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Universitaire de Technologie - La Roche-sur-Yon (IUT La Roche-sur-Yon), Université de Nantes (UN)-Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN), Institut für Virologie, Philipps University, MIT Kavli Institute for Astrophysics and Space Research, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Geology and Geophysics [Mānoa], University of Hawai‘i [Mānoa] (UHM), Universität Zürich [Zürich] = University of Zurich (UZH), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Universidad de Chile = University of Chile [Santiago] (UCHILE), Pontificia Universidad Católica de Chile (UC), University of Louisville, Austrian Academy of Sciences (OeAW), Lund University [Lund], University of Warwick [Coventry], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), German Aerospace Center (DLR), Swiss Bee Research Centre, Centre for Medical Image Computing (CMIC), and University College of London [London] (UCL)
Subjects: (TOI-431, planets and satellites: detection, Fundamental Parameters, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], (TOI-431, TIC 31374837), FOS: Physical sciences, Individual, Astrophysics, Q1, 01 natural sciences, Neptune, Planet, QB460, 0103 physical sciences, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, QB600, QC, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, Astronomy and Astrophysics, Planets and Satellites, Radius, Light curve, Exoplanet, Radial velocity, Photometry (astronomy), Detection, 13. Climate action, Space and Planetary Science, planets and satellites: individual: (TOI-431, TIC 31374837), Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the bright (V$_{mag} = 9.12$), multi-planet system TOI-431, characterised with photometry and radial velocities. We estimate the stellar rotation period to be $30.5 \pm 0.7$ days using archival photometry and radial velocities. TOI-431b is a super-Earth with a period of 0.49 days, a radius of 1.28 $\pm$ 0.04 R$_{\oplus}$, a mass of $3.07 \pm 0.35$ M$_{\oplus}$, and a density of $8.0 \pm 1.0$ g cm$^{-3}$; TOI-431d is a sub-Neptune with a period of 12.46 days, a radius of $3.29 \pm 0.09$ R$_{\oplus}$, a mass of $9.90^{+1.53}_{-1.49}$ M$_{\oplus}$, and a density of $1.36 \pm 0.25$ g cm$^{-3}$. We find a third planet, TOI-431c, in the HARPS radial velocity data, but it is not seen to transit in the TESS light curves. It has an $M \sin i$ of $2.83^{+0.41}_{-0.34}$ M$_{\oplus}$, and a period of 4.85 days. TOI-431d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterisation, while the super-Earth TOI-431b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431b is a prime TESS discovery for the study of rocky planet phase curves., Comment: 21 pages, 11 figures, 3 appendices, accepted for publication in MNRAS
Published: 2021
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11. TOI-220 b: a warm sub-Neptune discovered by TESS

Author: Petr Kabath, K. I. Collins, Florian Rodler, Christopher Stockdale, Sara Seager, T. Lopez, S. Hojjatpanah, Steve B. Howell, S. Sabotta, Nuno C. Santos, David Barrado, Enric Palle, Jan Subjak, M. Esposito, John P. Doty, Rafael Luque, Artyom Aguichine, Karen A. Collins, Olivier Demangeon, Vincent Van Eylen, J. R. De Medeiros, M. Fridlund, N. Scott, Susan E. Mullally, E. Goffo, J. F. Otegi, D. W. Latham, Oscar Barragán, Jon M. Jenkins, Rodrigo F. Díaz, L. M. Serrano, Stéphane Udry, P. Figueira, A. P. Hatzes, Vardan Adibekyan, Davide Gandolfi, P. Cortés-Zuleta, W. Fong, J. Cabrera, Peter J. Wheatley, Seth Redfield, Sascha Grziwa, A. Santerne, Benjamin F. Cooke, Sergio Hoyer, L. Acuña, Daniel Bayliss, J. D. Twicken, S. G. Sousa, A. Osborn, Joshua N. Winn, P. A. Strøm, Hans J. Deeg, E. Delgado Mena, H. P. Osborn, William D. Cochran, Rachel A. Matson, Elise Furlan, Jorge Lillo-Box, P. T. Boyd, John H. Livingston, I. C. Leão, James A. G. Jackman, Edward M. Bryant, François Bouchy, Magali Deleuil, O. Mousis, Jose-Manuel Almenara, Carina M. Persson, Judith Korth, Roland Vanderspek, Louise D. Nielsen, B. L. Canto Martins, David J. Armstrong, Eric L. N. Jensen, Emil Knudstrup, D. A. Yahalomi, Jeffrey C. Smith, S. C. C. Barros, Xavier Dumusque, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Department of Brain and Behavioural Sciences, University of Pavia, European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Department of Geosciences and Natural Resource Management [Copenhagen] (IGN), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), University of Warwick [Coventry], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics [Coventry], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Marine and Antarctic Studies [Horbat] (IMAS), University of Tasmania [Hobart, Australia] (UTAS), PSE-ENV/SEDRE/LETIS, Institut de Radioprotection et de Sûreté Nucléaire (IRSN), European Southern Observatory [Santiago] (ESO), Thüringer Landessternwarte Tautenburg (TLS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Universidad de Córdoba [Cordoba], Instituto de Astrofisica de Canarias (IAC), Wesleyan University, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Pavia = University of Pavia (UNIPV), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Universidade do Porto = University of Porto, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université de Genève = University of Geneva (UNIGE), Institute for Marine and Antarctic Studies [Hobart] (IMAS), Laboratoire d'étude et de recherche sur les transferts et les interactions dans les sous-sols (IRSN/PSE-ENV/SEDRE/LETIS), Service des déchets radioactifs et des transferts dans la géosphère (IRSN/PSE-ENV/SEDRE), Institut de Radioprotection et de Sûreté Nucléaire (IRSN)-Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Universidad de Córdoba = University of Córdoba [Córdoba], and Universidade do Porto = University of Porto-Universidade do Porto = University of Porto
Subjects: Dwarf star, Fundamental Parameters, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Individual, Astrophysics, Photometric, planets and satellites: individual: TYC 8897-01263-1, 01 natural sciences, techniques: photometric, Planet, Neptune, 0103 physical sciences, techniques: radial velocities, Radial Velocities, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, TYC 8897-01263-1, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Planets and Satellites, Radius, Planetary system, Stars, Exoplanet, Techniques, Radial velocity, 13. Climate action, Space and Planetary Science, echniques: photometric, stars: fundamental parameters, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.03 $\pm$ 0.15 R$_{Earth}$, implying a bulk density of 2.73 $\pm$ 0.47 $\textrm{g cm}^{-3}$. TOI-220 $b$ orbits a relative bright (V=10.4) and old (10.1$\pm$1.4 Gyr) K dwarf star with a period of $\sim$10.69 d. Thus, TOI-220 $b$ is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 $b$ internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core., Comment: Accepted for publication in MNRAS
Published: 2021
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12. Discovery and characterization of the exoplanets WASP-148b and c

Author: Jose-Manuel Almenara, K. Lam, Coel Hellier, Jorge Prieto-Arranz, Barry Smalley, Olivier Demangeon, Pierre F. L. Maxted, M. Martin-Lagarde, Flavien Kiefer, S. C. C. Barros, G. Boué, Carole A. Haswell, T. Lopez, Richard G. West, P. A. Wilson, D. Verilhac, Don Pollacco, D. J. A. Brown, Alexandre Santerne, P. Boumis, Jacques Laskar, Oliver Turner, Enric Palle, H. P. Osborn, James McCormac, Alexandre C. M. Correia, Aldo S. Bonomo, Peter J. Wheatley, Guillaume Hébrard, Didier Queloz, M. Deleuil, Ulrich Kolb, Louise D. Nielsen, Isabelle Boisse, Rodrigo F. Díaz, Stéphane Udry, A. Collier Cameron, A. Lecavelier des Etangs, François Bouchy, David R. Anderson, Amanda P. Doyle, S. Dalal, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Fisica [Aveiro], Universidade de Aveiro, University of St Andrews [Scotland], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Inflammatory Bowel Disease Center,, Cedars-Sinai Medical Center, Université Paris-Sud - Paris 11 (UP11), Laboratoire de Génie de la Conception (LGeco), Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Institute of Physical Chemistry, Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), University of Toronto, Institut National de la Santé et de la Recherche Médicale (INSERM), University of Warwick [Coventry], Department of Geosciences and Natural Resource Management [Copenhagen] (IGN), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, The University of Sydney, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Johannes Gutenberg - Universität Mainz (JGU), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université de Genève (UNIGE), Universidade do Porto, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Orbital plane, FOS: Physical sciences, Astrophysics, 01 natural sciences, spectroscopic [Techniques], techniques: photometric, Planet, QB460, 0103 physical sciences, Hot Jupiter, techniques: radial velocities, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, QA, 010303 astronomy & astrophysics, planetary systems, QB600, QC, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], 010308 nuclear & particles physics, photometric [Techniques], Astronomy and Astrophysics, DAS, Planetary system, Light curve, Orbital period, Exoplanet, Radial velocity, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery and characterization of WASP-148, a new extrasolar system that includes at least two giant planets. The host star is a slowly rotating inactive late-G dwarf with a V=12 magnitude. The planet WASP-148b is a hot Jupiter of 0.72 R_Jup and 0.29 M_Jup that transits its host with an orbital period of 8.80 days. We found the planetary candidate with the SuperWASP photometric survey, then characterized it with the SOPHIE spectrograph. Our radial velocity measurements subsequently revealed a second planet in the system, WASP-148c, with an orbital period of 34.5 days and a minimum mass of 0.40 M_Jup. No transits of this outer planet were detected. The orbits of both planets are eccentric and fall near the 4:1 mean-motion resonances. This configuration is stable on long timescales, but induces dynamical interactions so that the orbits differ slightly from purely Keplerian orbits. In particular, WASP-148b shows transit-timing variations of typically 15 minutes, making it the first interacting system with transit-timing variations that is detected on ground-based light curves. We establish that the mutual inclination of the orbital plane of the two planets cannot be higher than 35 degrees, and the true mass of WASP-148c is below 0.60 M_Jup. We present photometric and spectroscopic observations of this system that cover a time span of ten years. We also provide their Keplerian and Newtonian analyses; these analyses should be significantly improved through future TESS~observations., 16 pages, 10 figures, 7 tables, A&A in press
Published: 2021
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13. Six transiting planets and a chain of Laplace resonances in TOI-178

Author: A. Leleu, Nathan Hara, Rosanna H. Tilbrook, Matthew J. Hooton, Jack S. Acton, Giuseppina Micela, Heike Rauer, Francisco J. Pozuelos, Xavier Dumusque, Michael R. Goad, T. Bárczy, Andrew Collier Cameron, Francesco Pepe, G. Lo Curto, Rafael Rebolo, Juan Cabrera, Pedro Figueira, M. Buder, Willy Benz, Romain Allart, Oliver Turner, Enric Palle, Alexis M. S. Smith, Ignasi Ribas, F. Ratti, M. Steller, Richard G. West, James McCormac, A. Lecavelier des Etangs, Alexandre C. M. Correia, Daniel Sebastian, S. G. Sousa, Emmanuel Jehin, Mathias Beck, J. Schneider, François Bouchy, Baptiste Lavie, J.-B. Delisle, Liam Raynard, Roberto Ragazzoni, K. Lam, H. Venus, Kate Gudrun Isaak, Roi Alonso, C. Murray, Laetitia Delrez, Martti H. Kristiansen, Mario Damasso, A. Bonfanti, David Ehrenreich, Stéphane Udry, Samuel Gill, Sergio Hoyer, Lionel Garcia, V. Adibekyan, Carina M. Persson, Maximiliano Moyano, Beth A. Henderson, Giampaolo Piotto, Andrés Jordán, Samantha Thompson, Alexis Brandeker, Elsa Ducrot, Daniel Angerhausen, Nuno C. Santos, David Barrado, Xavier Bonfils, Vincent Bourrier, F. Verrecchia, Monika Lendl, Andrea Mehner, C. Broeg, M. R. Zapatero Osorio, Matthew R. Burleigh, D. Futyan, Damien Ségransan, Amaury H. M. J. Triaud, Mahmoudreza Oshagh, C. Allende Prieto, J. Asquier, B. O. Demory, Philippe Robutel, C. Corral Van Damme, Nicola Rando, Malcolm Fridlund, Gisbert Peter, Roland Ottensamer, Alessandro Sozzetti, Paolo Molaro, James S. Jenkins, Melvyn B. Davies, Jorge Lillo-Box, S. Chamberlain, Thomas Beck, P. Di Marcantonio, Carlos Martins, Maximilian N. Günther, Daniel Bayliss, Jacques Laskar, Peter J. Wheatley, P. P. Pedersen, Nicolas Thomas, Nicholas A. Walton, Göran Olofsson, Marko Sestovic, David R. Anderson, Artem Burdanov, Kevin Heng, Manuel Guedel, Jose I. Vines, A. García Muñoz, Edward Gillen, Valérie Van Grootel, T. G. Wilson, Michaël Gillon, Olivier Demangeon, D. Wolter, Demetrio Magrin, G. Polenta, G. Anglada Escudé, Stefano Cristiani, J. Haldemann, László L. Kiss, H. P. Osborn, Valerio Nascimbeni, Aleisha Hogan, Ennio Poretti, Pierre F. L. Maxted, S. C. C. Barros, G. Boué, Sébastien Charnoz, Benjamin F. Cooke, Nicolas Billot, C. Reimers, Don Pollacco, Gaetano Scandariato, Luca Fossati, Douglas R. Alves, J. I. González Hernández, Edward M. Bryant, Anders Erikson, Nelson J. Nunes, Wolfgang Baumjohann, Yann Alibert, A. Suárez Mascareño, Antoine Simon, Gy. M. Szabó, C. Lovis, Magali Deleuil, Andrea Fortier, Isabella Pagano, A. Bekkelien, G. Di Persio, Didier Queloz, Davide Gandolfi, Centre Hospitalier Régional Universitaire [Lille] (CHRU Lille), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ITA, USA, GBR, FRA, DEU, AUT, BEL, CHL, DNK, NLD, PRT, SWE, CHE, HUN, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Genève (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Swiss National Science Foundation, Agence Nationale de la Recherche (France), Science and Technology Facilities Council (UK), Belgian Science Policy Office, Université de Liège, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Alvarez, M. [0000-0002-6786-2620], Carrasco Martínez, J. M. [0000-0002-3029-5853], Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: Brightness, planets and satellites: detection, Laplace resonance, 010504 meteorology & atmospheric sciences, spectroscopic techniques, planets and satellites: dynamical evolution and stability, Astrophysics, 01 natural sciences, Transits, spectroscopic [Techniques], techniques: photometric, Planet, QB460, QB Astronomy, 010303 astronomy & astrophysics, planets and satellites dynamical evolution and stability, QC, Institut für Optische Sensorsysteme, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Laplace transform, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, photmetric [Techniques], 3rd-DAS, dynamical evolution and stability [Planets and satellites], planets and satellites detection, Astrophysics::Earth and Planetary Astrophysics, Extrasolare Planeten und Atmosphären, Techniques: photmetric, FOS: Physical sciences, Context (language use), SPECULOOS, Earth radius, Mean-motion resonance, 0103 physical sciences, Celestial mechanics, CHEOPS, QB600, 0105 earth and related environmental sciences, photometric techniques, TESS, Scattering, Leitungsbereich PF, photometric [Techniques], Astronomy and Astrophysics, celestial mechanics, 620 Engineering, detection [Planets and satellites], QC Physics, 13. Climate action, Space and Planetary Science, NGTS, Planetare Sensorsysteme, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics), techniques: spectroscopic, QB799, Planets and satellites: Detection, Planets and satellites: Dynamical evolution and stability, Techniques: Photometric, Techniques: Spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: Leleu, A., et al., Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152to 2.87Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02to 0.177times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes., The authors acknowledge support from the Swiss NCCR PlanetS and the Swiss National Science Foundation. Y.A. and M.J.H. acknowledge the support of the Swiss National Fund under grant 200020_172746. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/M001296/1. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. SH acknowledges CNES funding through the grant 837319. Based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) project ST/M001962/1. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. V.A. acknowledges the support from FCT through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. ABr was supported by the SNSA. A.C. acknowledges support by CFisUC projects (UIDB/04564/2020 and UIDP/04564/2020), GRAVITY (PTDC/FIS-AST/7002/2020), ENGAGE SKA (POCI-01-0145-FEDER-022217), and PHOBOS (POCI-01-0145-FEDER-029932), funded by COMPETE 2020 and FCT, Portugal. This work was supported by FCT - Fundaçãopara a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa OperacionalCompetitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER- 032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). M.F. and C.M.P. gratefully acknowledgethe support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a WintonExoplanet Fellowship. M.G. is an F.R.S.-FNRS Senior Research Associate. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal programme RYC-2013-14875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. MNG ackowledges support from the MIT Kavli Institute as a Juan Carlos Torres Fellow. J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme.She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection forthe programme. J.S.J. acknowledges support by FONDECYT grant 1201371, and partial support from CONICYT project Basal AFB-170002. A.J. acknowledges support from ANID - Millennium Science Initiative - ICN12_009 and from FONDECYT project 1171208. P.M. acknowledges support from STFC research grant number ST/M001040/1. N.J.N is supported by the contract and exploratory project IF/00852/2015, and projects UID/FIS/04434/2019, PTDC/FIS-OUT/29048/2017, COMPETE2020: POCI-01-0145-FEDER-028987 & FCT: PTDC/FIS-AST/28987/2017. N.J.N is supported by the contract and exploratory project IF/00852/2015, and project PTDC/FIS-OUT/29048/2017. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). Acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). 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 project has been supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grants GINOP-2.3.2-15-2016-00003, K-119517, K-125015, and the City of Szombathely under Agreement No. 67.177-21/2016. This research received funding from the MERAC foundation, from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no 803193/ BEBOP, and from the Science and Technology Facilites Council (STFC, grant no ST/S00193X/1). V.V.G. is an F.R.S-FNRS Research Associate. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. M. R. Z. O. acknowledges financial support from projects AYA2016-79425-C3-2-P and PID2019-109522GB-C51 from the Spanish Ministry of Science, Innovation and Universities.
Published: 2021
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14. TOI-1296b and TOI-1298b observed with TESS and SOPHIE: Two hot Saturn-mass exoplanets with different densities around metal-rich stars

Author: T. Lopez, Isabelle Boisse, S. Deheuvels, Zahra Essack, David Baker, F. Debras, P. C. König, T. Forveille, J. Villasenor, Sergio Hoyer, X. Delfosse, Keivan G. Stassun, Patricia T. Boyd, Nuno C. Santos, George R. Ricker, Guillaume Hébrard, Olivier Demangeon, C. Moutou, H. P. Osborn, C. Ziegler, P. Guerra, D. Laloum, S. C. C. Barros, Michael Vezie, R. Vanderspek, X. Bonfils, Flavien Kiefer, Joshua N. Winn, Katharine Hesse, D. W. Latham, S. Dalal, Magali Deleuil, Sara Seager, Jose-Manuel Almenara, P. Cortés-Zuleta, E. Girardin, Eder Martioli, Jon M. Jenkins, Paul Benni, Allyson Bieryla, Karen A. Collins, N. Heidari, Bill Wohler, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Toulouse Biotechnology Institute (TBI), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institute for Marine and Antarctic Studies [Horbat] (IMAS), University of Tasmania [Hobart, Australia] (UTAS), Inflammatory Bowel Disease Center, The University of Chicago Medicine [Chicago], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), Stephen F. Austin State University, Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Universidade do Porto = University of Porto, Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institute for Marine and Antarctic Studies [Hobart] (IMAS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, and ANR-18-CE31-0019,SPlaSH,Recherche de planètes habitables avec SPIRou(2018)
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, techniques: photometric, Planet, Saturn, 0103 physical sciences, techniques: radial velocities, 010303 astronomy & astrophysics, Spectrograph, planetary systems, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Subgiant, Astronomy and Astrophysics, Radius, Exoplanet, planets and satellites: gaseous planets, Radial velocity, Stars, Space and Planetary Science, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of two new transiting extrasolar planet candidates identified as TOI-1296.01 and TOI-1298.01 by the Transiting Exoplanet Survey Satellite (TESS). The planetary nature of these candidates has been secured with the SOPHIE high-precision spectrograph through the measurement of the companion’s mass with the radial velocity method. Both planets are similar to Saturn in mass and have similar orbital periods of a few days. They, however, show discrepant radii and therefore different densities. The radius discrepancy might be explained by the different levels of irradiation by the host stars. The subgiant star TOI-1296 hosts a low-density planet with 1.2 RJup while the less luminous, lower-size star TOI-1298 hosts a much denser planet with a 0.84 RJup radius, resulting in bulk densities of 0.198 and 0.743 g cm−3, respectively.In addition, both stars are strongly enriched in heavy elements, having metallicities of +0.44 and +0.49 dex, respectively. The planet masses and orbital periods are 0.298 ± 0.039 MJup and 3.9443715 ± 5.8 ± 10−6 days for TOI-1296b, and 0.356 ± 0.032 MJup and 4.537164 ± 1.2 ± 10−5 days for TOI-1298b. The mass measurements have a relative precision of better than 13%.
Published: 2021
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15. The TESS Objects of Interest Catalog from the TESS Prime Mission

Author: David W. Latham, Nicholas Mehrle, Gáspár Á. Bakos, Scott W. Fleming, Clara Sousa-Silva, Ana Glidden, Alton Spencer, Aylin Garcia Soto, Ashley Chontos, Stephen R. Kane, Joshua E. Schlieder, David Berardo, David Charbonneau, Zhuchang Zhan, Rahul Jayaraman, Chelsea X. Huang, H. P. Osborn, David Watanabe, Natalia Guerrero, Jack J. Lissauer, Joshua N. Winn, Eric B. Ting, Zahra Essack, Douglas N. C. Lin, Thomas Mikal-Evans, M. Swain, Pamela Rowden, Allyson Bieryla, Norio Narita, Knicole D. Colón, Karen A. Collins, Steven Villanueva, Laura Kreidberg, Peter Tenenbaum, Ismael Mireles, Jeffrey L. Coughlin, Thomas Barclay, Akshata Krishnamurthy, Jacob L. Bean, Guillermo Torres, William Fong, Luke G. Bouma, Zachory K. Berta-Thompson, Martin Paegert, Patricia T. Boyd, Alessandro Sozzetti, Goran Zivanovic, Ian Wong, Susan E. Mullally, Robert L. Morris, Maximilian N. Günther, Benjamin V. Rackham, Ian J. M. Crossfield, Dana R. Louie, Lars A. Buchhave, Sara Seager, Christopher J. Burke, András Pál, Sarah Ballard, Michael B. Lund, Joseph E. Rodriguez, Michael Fausnaugh, Bill Wohler, Jon M. Jenkins, Samuel N. Quinn, Avi Shporer, Diana Dragomir, David R. Ciardi, Gilbert A. Esquerdo, Chris Henze, Hans Kjeldsen, Roland Vanderspek, Prajwal Niraula, Stéphane Udry, Jason A. Dittmann, Mark Clampin, Jennifer Burt, Enric Palle, Lizhou Sha, S. Rinehart, Jeffrey C. Smith, Matthew J. Holman, David R. Rodriguez, Elisa V. Quintana, Natalie M. Batalha, Mark E. Rose, Stephen J. L. Rowden, Tansu Daylan, Keivan G. Stassun, Dimitar Sasselov, Nathaniel R. Butler, Jessie L. Christiansen, Katharine Hesse, Liang Yu, Douglas A. Caldwell, Joseph D. Twicken, George R. Ricker, Jian Ge, Joshua Pepper, Andrew W. Howard, Lisa Kaltenegger, Andrew Vanderburg, John P. Doty, Daniel A. Yahalomi, and Charlotte Minsky
Subjects: Data products, Physics::Instrumentation and Detectors, Exoplanet astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Prime (order theory), 010309 optics, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Exoplanet catalogs, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Light curve, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Satellite, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present 2,241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its two-year prime mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously-known planets recovered by TESS observations. We describe the process used to identify TOIs and investigate the characteristics of the new planet candidates, and discuss some notable TESS planet discoveries. The TOI Catalog includes an unprecedented number of small planet candidates around nearby bright stars, which are well-suited for detailed follow-up observations. The TESS data products for the Prime Mission (Sectors 1-26), including the TOI Catalog, light curves, full-frame images, and target pixel files, are publicly available on the Mikulski Archive for Space Telescopes., Comment: 39 pages, 16 figures. The Prime Mission TOI Catalog is included in the ancillary data as a CSV. For the most up-to-date catalog, refer to https://tess.mit.edu/toi-releases/
Published: 2021
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16. A long period (P = 61.8-d) M5V dwarf eclipsing a Sun-like star from TESS and NGTS

Author: Michael R. Goad, Jack S. Acton, Maximilian N. Günther, Samuel Gill, Maximiliano Moyano, Monika Lendl, Fracois Bouchy, Stéphane Udry, Claudia Belardi, Daniel Bayliss, Peter J. Wheatley, Alexander Chaushev, Sarah L. Casewell, Matthew R. Burleigh, David R. Anderson, Rossana H. Tilbrook, Oliver Turner, Christopher A. Watson, Richard G. West, James McCormac, Alexis M. S. Smith, James A. G. Jackman, Don Pollacco, James S. Jenkins, Edward M. Bryant, Louise D. Nielsen, Liam Raynard, Jose I. Vines, H. P. Osborn, and Benjamin F. Cooke
Subjects: Physics, Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, binaries: eclipsing, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, eclipsing [binaries], Space and Planetary Science, Long period, 0103 physical sciences, 010303 astronomy & astrophysics, Humanities, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite (TESS) has produced a large number of single transit event candidates which are being monitored by the Next Generation Transit Survey (NGTS). We observed a second epoch for the TIC-231005575 system (Tmag = 12.06, Teff = 5500 +- 85 K) with NGTS and a third epoch with Las Cumbres Observatory's (LCO) telescope in South Africa to constrain the orbital period (P = 61.777 d). Subsequent radial velocity measurements with CORALIE revealed the transiting object has a mass of M2 = 0.128 +- 0.003 M$_\odot$, indicating the system is a G-M binary. The radius of the secondary is R2 = 0.154 +- 0.008 R$_\odot$ and is consistent with models of stellar evolution to better than 1-$\sigma$., Comment: 8 pages, 5 figures, 3 tables. Accepted for publication in MNRAS
Published: 2020
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17. Two Transiting Hot Jupiters from the WASP Survey: WASP-150b and WASP-176b

Author: Andrew Collier Cameron, Louise D. Nielsen, Jorge Prieto-Arranz, Didier Queloz, Francisco J. Pozuelos, Sergio Velasco, Pierre F. L. Maxted, Alexios Liakos, J. Alikakos, Luigi Mancini, Enric Palle, Thomas Henning, T. Lopez, Guillaume Hébrard, Khalid Barkaoui, Artem Burdanov, James A. Blake, Y. Almleaky, Giuseppe D'Ago, Michaël Gillon, Paul Chote, George W. King, Mario Damasso, P. J. Wheatley, Oliver Turner, Richard G. West, François Bouchy, Samantha Thompson, Flavien Kiefer, James McCormac, Laetitia Delrez, Ivan Bruni, Rosemary A. Mardling, A. Daassou, Coel Hellier, Don Pollacco, P. Boumis, Barry Smalley, Amanda P. Doyle, John Southworth, Duncan A. Brown, Francesco Pepe, C. Murray, Elsa Ducrot, Emmanuel Jehin, H. P. Osborn, Benjamin F. Cooke, S. Dalal, Zouhair Benkhaldoun, Stéphane Udry, Damien Ségransan, N. Schanche, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: Radial velocity, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Photometry, Planet, 0103 physical sciences, Hot Jupiter, QB Astronomy, Exoplanet detection methods, 010303 astronomy & astrophysics, Exoplanet systems, QC, QB600, QB, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Settore FIS/05, Astronomy and Astrophysics, 3rd-DAS, Exoplanet, QC Physics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric ($e$ = 0.38) hot Jupiter on a 5.6 day orbit around a $V$ = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4 $\rm M_{\odot}$ and 1.7 $\rm R_{\odot}$ respectively. WASP-150b has a mass and radius of 8.5 $\rm M_J$ and 1.1 $\rm R_J$, leading to a large planetary bulk density of 6.4 $\rm \rho_J$. WASP-150b is found to be $\sim3$ Gyr old, well below its circularisation timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a $V$ = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 $\rm M_{\odot}$ and 1.9 $\rm R_{\odot}$. WASP-176b has a mass and radius of 0.86 $\rm M_J$ and 1.5 $\rm R_J$ respectively, leading to a planetary bulk density of 0.23 $\rm \rho_J$., Comment: 15 pages, 14 figures. Accepted for publication in The Astronomical Journal
Published: 2020
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18. The TESS-Keck Survey. I. A Warm Sub-Saturn-mass Planet and a Caution about Stray Light in TESS Cameras

Author: M. F. Andersen, Jeffrey C. Smith, Lauren M. Weiss, Enric Palle, Andrew W. Mayo, Teo Mocnik, Robert F. Goeke, David W. Latham, Ashley Chontos, Aida Behmard, Sara Seager, Howard Isaacson, Courtney D. Dressing, Daryll LaCourse, Judah Van Zandt, Joshua E. Schlieder, Monika Lendl, Chelsea X. Huang, Steven Giacalone, Paul A. Dalba, Joshua N. Winn, Erik A. Petigura, Joseph E. Rodriguez, Douglas A. Caldwell, Corey Beard, Roland Vanderspek, Stephen R. Kane, Lea A. Hirsch, Steven Villanueva, Martti H. Kristiansen, Nicholas Scarsdale, Emil Knudstrup, William Fong, Lee J. Rosenthal, Andrew Vanderburg, Paul Robertson, Ryan A. Rubenzahl, Samuel N. Quinn, Michelle L. Hill, George R. Ricker, Diana Dragomir, Molly R. Kosiarek, Arpita Roy, Tansu Daylan, Ian J. M. Crossfield, David R. Ciardi, Pamela Rowden, Natalie M. Batalha, Mark E. Rose, Allyson Bieryla, Gilbert A. Esquerdo, Keivan G. Stassun, Daniel J. Stevens, Jack Lubin, Joshua Pepper, Andrew W. Howard, Jon M. Jenkins, Benjamin J. Fulton, Arvind F. Gupta, H. P. Osborn, Tom Jacobs, Joseph M. Akana Murphy, Xinyu Yao, Daniel Huber, Frank Grundahl, and Ryan Cloutier
Subjects: Dwarf star, Radial velocity, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, FOS: Physical sciences, 01 natural sciences, METHANE, Planet, 0103 physical sciences, Exoplanet detection methods, Direct imaging, Transit (astronomy), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Spectroscopy, 0105 earth and related environmental sciences, Physics, JUPITER, Earth and Planetary Astrophysics (astro-ph.EP), ERROR-CORRECTION, Exoplanets, Astronomy, Astronomy and Astrophysics, Surface gravity, Light curve, Orbital period, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, F dwarf stars, STATISTICAL PROPERTIES, Transit photometry, Astrophysics - Instrumentation and Methods for Astrophysics, STARS, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of a Saturn-size exoplanet orbiting HD 332231 (TOI 1456) in light curves from the Transiting Exoplanet Survey Satellite (TESS). HD 332231, an F8 dwarf star with a V-band magnitude of 8.56, was observed by TESS in Sectors 14 and 15. We detect a single-transit event in the Sector 15 presearch data conditioning (PDC) light curve. We obtain spectroscopic follow-up observations of HD 332231 with the Automated Planet Finder, Keck I, and SONG telescopes. The orbital period we infer from the radial velocity (RV) observations leads to the discovery of another transit in Sector 14 that was masked by PDC due to scattered light contamination. A joint analysis of the transit and RV data confirms the planetary nature of HD 332231 b, a Saturn-size ($0.867^{+0.027}_{-0.025} \; R_{\rm J}$), sub-Saturn-mass ($0.244\pm0.021 \; M_{\rm J}$) exoplanet on a 18.71 day circular orbit. The low surface gravity of HD 332231 b and the relatively low stellar flux it receives make it a compelling target for transmission spectroscopy. Also, the stellar obliquity is likely measurable via the Rossiter-McLaughlin effect, an exciting prospect given the 0.14 au orbital separation of HD 332231 b. The spectroscopic observations do not provide substantial evidence for any additional planets in the HD 332231 system, but continued RV monitoring is needed to further characterize this system. We also predict that the frequency and duration of masked data in the PDC light curves for TESS Sectors 14-16 could hide transits of some exoplanets with orbital periods between 10.5 and 17.5 days., Comment: 17 pages, 9 figures, 4 tables. Published in the Astronomical Journal
Published: 2020
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19. KELT-9 b's Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin-Orbit Misalignment

Author: Jason W. Barnes, Daniel J. Stevens, John P. Ahlers, H. P. Osborn, Martin Paegert, Robert F. Goeke, David W. Latham, Peter Tenenbaum, Jon M. Jenkins, Sara Seager, Joshua N. Winn, Marshall C. Johnson, Roland Vanderspek, Knicole D. Colón, Keivan G. Stassun, George R. Ricker, Karen A. Collins, Pamela Rowden, B. Scott Gaudi, Douglas A. Caldwell, Joseph E. Rodriguez, and Thomas G. Beatty
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Stellar rotation, Polar orbit, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Effective temperature, Light curve, 01 natural sciences, Exoplanet, Von Zeipel theorem, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Gravity darkening, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: KELT-9 b is an ultra hot Jupiter transiting a rapidly rotating, oblate early-A-type star in a polar orbit. We model the effect of rapid stellar rotation on KELT-9 b's transit light curve using photometry from the Transiting Exoplanet Survey Satellite (\tess) to constrain the planet's true spin-orbit angle and to explore how KELT-9 b may be influenced by stellar gravity darkening. We constrain the host star's equatorial radius to be $1.089\pm0.017$ times as large as its polar radius and its local surface brightness to vary by $\sim38$\% between its hot poles and cooler equator. We model the stellar oblateness and surface brightness gradient and find that it causes the transit light curve to lack the usual symmetry around the time of minimum light. We take advantage of the light curve asymmetry to constrain KELT-9 b's true spin orbit angle (${87^\circ}^{+10^\circ}_{-11^\circ}$), agreeing with \citet{gaudi2017giant} that KELT-9 b is in a nearly polar orbit. We also apply a gravity darkening correction to the spectral energy distribution model from \citet{gaudi2017giant} and find that accounting for rapid rotation gives a better fit to available spectroscopy and yields a more reliable estimate for the star's polar effective temperature., Accepted for Publication in ApJ. arXiv admin note: text overlap with arXiv:1911.05025
Published: 2020

20. TOI 122b and TOI 237b, two small warm planets orbiting inactive M dwarfs, found by \textit{TESS}

Author: David R. Ciardi, Emmanuel Jehin, Giovanni Isopi, Robert F. Goeke, K. I. Collins, Jessica E. Libby-Roberts, Bárbara Rojas-Ayala, Jacob L. Bean, Khalid Barkaoui, Francisco J. Pozuelos, M. L. Silverstein, George R. Ricker, David W. Latham, F. Mallia, Joshua N. Winn, Alan M. Levine, William Waalkes, Jessie L. Christiansen, Carl Ziegler, Zachory K. Berta-Thompson, Sara Seager, Elisabeth R. Newton, Joseph D. Twicken, Roland Vanderspek, Tianjun Gan, S. A. Rinehart, Dennis M. Conti, Benjamin M. Tofflemire, Benjamin T. Montet, Karen A. Collins, Michaël Gillon, Mark E. Rose, Adina D. Feinstein, Eric L. N. Jensen, Andrew W. Mann, H. P. Osborn, Nicholas M. Law, Jon M. Jenkins, Cesar Briceno, Eric B. Ting, John F. Kielkopf, and Howard M. Relles
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Exoplanet, 010309 optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery and validation of TOI 122b and TOI 237b, two warm planets transiting inactive M dwarfs observed by \textit{TESS}. Our analysis shows TOI 122b has a radius of 2.72$\pm$0.18 R$_\rm{e}$ and receives 8.8$\pm$1.0$\times$ Earth's bolometric insolation, and TOI 237b has a radius of 1.44$\pm$0.12 R$_\rm{e}$ and receives 3.7$\pm$0.5$\times$ Earth insolation, straddling the 6.7$\times$ Earth insolation that Mercury receives from the sun. This makes these two of the cooler planets yet discovered by \textit{TESS}, even on their 5.08-day and 5.43-day orbits. Together, they span the small-planet radius valley, providing useful laboratories for exploring volatile evolution around M dwarfs. Their relatively nearby distances (62.23$\pm$0.21 pc and 38.11$\pm$0.23 pc, respectively) make them potentially feasible targets for future radial velocity follow-up and atmospheric characterization, although such observations may require substantial investments of time on large telescopes., Comment: 21 pages, 9 figures, 4 tables, accepted to AJ
Published: 2020
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21. Transits of Known Planets Orbiting a Naked-eye Star

Author: Stephen R. Kane, Tiago L. Campante, Ekrem Murat Esmer, Rodrigo F. Díaz, Özgür Baştürk, Magali Deleuil, Stéphane Udry, Natalie R. Hinkel, Howard Isaacson, Simon J. O'Toole, Brad D. Carter, Maxime Marmier, Damien Ségransan, Margaret C. Turnbull, R. Paul Butler, H. P. Osborn, Jason T. Wright, Francesco Pepe, Christophe Lovis, Andrew W. Howard, Xavier Dumusque, Jon M. Jenkins, François Bouchy, Sara Seager, Jeremy Bailey, Robert A. Wittenmyer, Andrew Vanderburg, Geoffrey W. Marcy, Joshua N. Winn, Duncan J. Wright, Roland Vanderspek, Martti H. Kristiansen, Louise D. Nielsen, Darin Ragozzine, Hugh R. A. Jones, Jacob L. Bean, David Ehrenreich, Tansu Daylan, Selçuk Yalçınkaya, George R. Ricker, C. G. Tinney, Romain Allart, David W. Latham, Jonathan Horner, Colby Ostberg, Tara Fetherolf, Paul A. Dalba, Teo Mocnik, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Radial velocity, 010504 meteorology & atmospheric sciences, Star (game theory), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Astronomy and Astrophysics, Planetary system, Exoplanet, Exoplanet structure, Orbit, Stars, Photometry (astronomy), 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Transit photometry, Exoplanet atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract: Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite ({\it TESS}) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD~136352 (Nu$^2$~Lupi) is a naked-eye ($V = 5.78$) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the HARPS spectrograph. We present the detection and characterization of transits for the two inner planets of the HD~136352 system, revealing radii of $1.482^{+0.058}_{-0.056}$~$R_\oplus$ and $2.608^{+0.078}_{-0.077}$~$R_\oplus$ for planets b and c, respectively. We combine new HARPS observations with RV data from Keck/HIRES and the AAT, along with {\it TESS} photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of $\rho_b = 7.8^{+1.2}_{-1.1}$~gcm$^{-3}$ and $\rho_c = 3.50^{+0.41}_{-0.36}$~gcm$^{-3}$ for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multi-transiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds., Comment: 13 pages, 4 figures, 3 tables, accepted for publication in the Astronomical Journal
Published: 2020
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22. Masses for the seven planets in K2-32 and K2-233

Author: J. Lillo-Box, T. A. Lopez, A. Santerne, L. D. Nielsen, S. C. C. Barros, M. Deleuil, L. Acuña, O. Mousis, S. G. Sousa, V. Adibekyan, D. J. Armstrong, D. Barrado, D. Bayliss, D. J. A. Brown, O. D. S. Demangeon, X. Dumusque, P. Figueira, S. Hojjatpanah, H. P. Osborn, N. C. Santos, S. Udry
Published: 2020
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23. HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs*

Author: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, W. C. Waalkes, European Commission, Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), Comisión Nacional de Investigación Científica y Tecnológica (Chile), and Ministry of Education, Culture, Sports, Science and Technology (Japan)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Settore FIS/05, Space and Planetary Science, Exoplanets, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.-- Full list of authors: Jordán, Andrés; Hartman, J. D.; Bayliss, D.; Bakos, G. Á.; Brahm, R.; Bryant, E. M.; Csubry, Z.; Henning, Th.; Hobson, M.; Mancini, L.; Penev, K.; Rabus, M.; Suc, V.; de Val-Borro, M.; Wallace, J.; Barkaoui, K.; Ciardi, David R.; Collins, K. A.; Esparza-Borges, E.; Furlan, E.; Gan, T.; Benkhaldoun, Z.; Ghachoui, M.; Gillon, M.; Howell, S.; Jehin, E.; Fukui, A.; Kawauchi, K.; Livingston, J. H.; Luque, R.; Matson, R.; Matthews, E. C.; Osborn, H. P.; Murgas, F.; Narita, Norio; Palle, E.; Parvianen, H.; Waalkes, W. C., The relative rarity of giant planets around low-mass stars compared with solar-type stars is a key prediction from the core-accretion planet formation theory. In this paper we report on the discovery of four gas giant planets that transit low-mass late K and early M dwarfs. The planets HATS-74Ab (TOI 737b), HATS-75b (TOI 552b), HATS-76b (TOI 555b), and HATS-77b (TOI 730b) were all discovered from the HATSouth photometric survey and follow-up using TESS and other photometric facilities. We use the new ESPRESSO facility at the VLT to confirm systems and measure their masses. We find that these planets have masses of 1.46 ± 0.14 MJ, 0.491 ± 0.039 MJ, 2.629 ± 0.089 MJ, and ${1.374}_{-0.074}^{+0.100}\,$ MJ, respectively, and radii of 1.032 ± 0.021 RJ, 0.884 ± 0.013 RJ, 1.079 ± 0.031 RJ, and 1.165 ± 0.021 RJ, respectively. The planets all orbit close to their host stars with orbital periods ranging from 1.7319 days to 3.0876 days. With further work, we aim to test core-accretion theory by using these and further discoveries to quantify the occurrence rate of giant planets around low-mass host stars. © 2022. The Author(s). Published by the American Astronomical Society., Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G, NNX12AH91H, and NNX17AB61G, and follow-up observations have received partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1210718, and ANID—Millennium Science Initiative—ICN12_009. J.H. acknowledges partial support from the TESS GI Program, programs G011103 and G022117, through NASA grants 80NSSC19K0386 and 80NSSC19K1728. L.M. acknowledges support from the Italian Minister of Instruction, University and Research (MIUR) through FFABR 2017 fund. L.M. acknowledges support from the University of Rome Tor Vergata through "Mission: Sustainability 2016" fund. K.P. acknowledges support from NASA ATP grant 80NSSC18K1009. M.R. acknowledges support from the Universidad Católica de lo Santísima Concepción grant DI-FIAI 03/2021. R.L. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52/AEI/10.13039/501100011033, and the Centre of Excellence "Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). Based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 0103.C-0449(A). Part of this work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation. ECM acknowledges the financial support of the SNSF. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper is partly based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This work is partly supported by JSPS KAKENHI grant No. JP20K14518. Some of the Observations in the paper made use of the High-Resolution Imaging instrument(s) `Alopeke (and/or Zorro). `Alopeke (and/or Zorro) was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Data were reduced using a software pipeline originally written by Elliott Horch and Mark Everett. `Alopeke (and/or Zorro) was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovaçóes e Comunicaçóes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. TRAPPIST-South is a project funded by the Belgian F.R.S.-FNRS under grant PDR T.0120.21, with the participation of the Swiss FNS. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. EJ and MG are F.R.S.-FNRS Senior Research Associates. This work is partly supported by JSPS KAKENHI grant No. JP18H05439, JST CREST grant No. JPMJCR1761, the Astrobiology Center of National Institutes of Natural Sciences (NINS; grant No. AB031010). 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 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. This research has made use NASA's Astrophysics Data System Bibliographic Services.
Published: 2022
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24. XO-7 b: A transiting hot Jupiter with a massive companion on a wide orbit

Author: Nicolas Crouzet, Guillaume Hébrard, Brian F. Healy, Jos de Bruijne, Peter R. McCullough, Pilar Montañés-Rodríguez, Matthieu Conjat, H. P. Osborn, Ignasi Ribas, Phillip Vo, Nuno C. Santos, Jerry Foote, Louise D. Nielsen, Joe Garlitz, Doug Long, Enrique Herrero, S. Dalal, Francesc Vilardell, Enrique Garcia-Melendo, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. TUAREG - Turbulence and Aerodynamics in Mechanical and Aerospace Engineering Research Group, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Radial velocity, Extrasolar gas giants, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Fotometria, Outer planets, Surveys, Spectroscopic, Transits, 01 natural sciences, Photometry, Observatory, High resolution spectroscopy, Astrophysics::Solar and Stellar Astrophysics, Exoplanet systems, Observational, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Exoplanets, SIMBAD, Individual (XO-7 b), Exoplanet, Astrophysics - Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, Transit photometry, Astrophysics - Instrumentation and Methods for Astrophysics, Hot Jupiters, FOS: Physical sciences, Photometric, 0103 physical sciences, Hot Jupiter, Instrumentation and Methods for Astrophysics (astro-ph.IM), Planetes exteriors, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astronomy and Astrophysics, Visible astronomy, Spectrum analysis, Anàlisi espectral, Planetary systems, Transit instruments, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Humanities, Astrophysics - Earth and Planetary Astrophysics
Abstract: Transiting planets orbiting bright stars are the most favorable targets for follow-up and characterization. We report the discovery of the transiting hot Jupiter XO-7 b and of a second, massive companion on a wide orbit around a circumpolar, bright, and metal rich G0 dwarf (V = 10.52, $T_{\rm eff} = 6250 \pm 100 \; \rm K$, $\rm[Fe/H] = 0.432 \pm 0.057 \; \rm dex$). We conducted photometric and radial velocity follow-up with a team of amateur and professional astronomers. XO-7 b has a period of $ 2.8641424 \pm 0.0000043$ days, a mass of $0.709 \pm 0.034 \; \rm M_{\rm J}$, a radius of $1.373 \pm 0.026 \; \rm R_{\rm J}$, a density of $0.340 \pm 0.027 \; \rm g \, {cm}^{-3}$, and an equilibrium temperature of $1743 \pm 23 \; \rm K$. Its large atmospheric scale height and the brightness of the host star make it well suited to atmospheric characterization. The wide orbit companion is detected as a linear trend in radial velocities with an amplitude of $\sim100 \; \rm m \, {s}^{-1}$ over two years, yielding a minimum mass of $4 \; \rm M_{\rm J}$; it could be a planet, a brown dwarf, or a low mass star. The hot Jupiter orbital parameters and the presence of the wide orbit companion point towards a high eccentricity migration for the hot Jupiter. Overall, this system will be valuable to understand the atmospheric properties and migration mechanisms of hot Jupiters and will help constrain the formation and evolution models of gas giant exoplanets., 16 pages, 6 figures, Accepted for publication in AJ
Published: 2019
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25. The changing face of AU Mic b: stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS

Author: Wolfgang Baumjohann, Pierre F. L. Maxted, A. Luntzer, S. C. C. Barros, K. G. Isaak, Xavier Bonfils, H. P. Osborn, Gy. M. Szabó, Nicolas Billot, A. García Muñoz, Sébastien Charnoz, Sergio Hoyer, Yann Alibert, Roberto Ragazzoni, Alexis Brandeker, P. Guterman, C. Corral Van Damme, Nicola Rando, Malcolm Fridlund, Thomas Beck, Valérie Van Grootel, Isabella Pagano, A. Collier Cameron, Melvyn B. Davies, L. Borsato, A. Bekkelien, G. Olofsson, Giampaolo Piotto, T. Bárczy, M.-D. Busch, D. Sicilia, L. M. Serrano, S. G. Sousa, M. Steller, Ignasi Ribas, Monika Lendl, A. Lecavelier des Etangs, Kevin Heng, Manuel Guedel, Roi Alonso, G. Anglada Escudé, David Ehrenreich, Alexis M. S. Smith, Stéphane Udry, Roland Ottensamer, J. Cabrera, Laetitia Delrez, Willy Benz, Nuno C. Santos, David Barrado, C. Lovis, Enric Palle, Damien Ségransan, N. A. Walton, Sz. Csizmadia, L. Kiss, B. O. Demory, Valerio Nascimbeni, M. Beck, Daniele Piazza, G. Lacedelli, Gisbert Peter, C. Broeg, A. E. Simon, Didier Queloz, T. G. Wilson, Davide Gandolfi, Michaël Gillon, Anders Erikson, Olivier Demangeon, Z. Garai, N. Thomas, Demetrio Magrin, Luca Fossati, Heike Rauer, Jacques Laskar, D. Futyan, Don Pollacco, Gaetano Scandariato, Magali Deleuil, Andrea Fortier, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Department of Brain and Behavioural Sciences, University of Pavia, Stockholm University, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: Rotation period, FOS: Physical sciences, Astrophysics, Q1, 01 natural sciences, Planet, QB460, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), QA, 010303 astronomy & astrophysics, QB600, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Commensurability (astronomy), Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, 520 Astronomy, Astronomy and Astrophysics, 3rd-DAS, Planetary system, 620 Engineering, Orbital period, Exoplanet, Planetary systems, Photometry (astronomy), QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Szabó, Gy. M., et al., AU Mic is a young planetary system with a resolved debris disc showing signs of planet formation and two transiting warm Neptunes near mean-motion resonances. Here we analyse three transits of AU Mic b observed with the CHaracterising ExOPlanet Satellite (CHEOPS), supplemented with sector 1 and 27 Transiting Exoplanet Survey Satellite (TESS) photometry, and the All-Sky Automated Survey from the ground. The refined orbital period of AU Mic b is 8.462995 ± 0.000003 d, whereas the stellar rotational period is Prot = 4.8367 ± 0.0006 d. The two periods indicate a 7:4 spin-orbit commensurability at a precision of 0.1%. Therefore, all transits are observed in front of one of the four possible stellar central longitudes. This is strongly supported by the observation that the same complex star-spot pattern is seen in the second and third CHEOPS visits that were separated by four orbits (and seven stellar rotations). Using a bootstrap analysis we find that flares and star spots reduce the accuracy of transit parameters by up to 10% in the planet-to-star radius ratio and the accuracy on transit time by 3-4 min. Nevertheless, occulted stellar spot features independently confirm the presence of transit timing variations (TTVs) with an amplitude of at least 4 min. We find that the outer companion, AU Mic c, may cause the observed TTVs.
Published: 2021
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26. Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

Author: Arthur Vigan, H. Giles, E. Foxell, Emma Carli, Louise D. Nielsen, B. Brugger, Duncan A. Brown, Alexandre Santerne, Don Pollacco, Isabelle Boisse, Pedro Figueira, J.-M. Almenara, H. J. da Nobrega, Aldo S. Bonomo, François Bouchy, David J. Armstrong, James Kirk, V. Adibekyan, Peter J. Wheatley, C. Lovis, Xavier Dumusque, Magali Deleuil, O. Mousis, Daniel Bayliss, Jorge Lillo-Box, S. Hojjatpanah, Francesco Pepe, S. G. Sousa, H. P. Osborn, João P. Faria, S. C. C. Barros, Olivier Demangeon, J. J. Neal, Stéphane Udry, T. Lopez, Guillaume Hébrard, Rodrigo F. Díaz, Nuno C. Santos, David Barrado, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Instituto de Astrofisica de Canarias (IAC), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), School of Physics and Astronomy [Cardiff], Cardiff University, European Southern Observatory (ESO), European Organization for Nuclear Research (CERN), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Université de Genève = University of Geneva (UNIGE), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: detection [planets and satellites], FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, fundamental parameters [planets and satellites], photometric [techniques], Planet, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, individual: K2-138 [stars], ComputingMilieux_MISCELLANEOUS, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Transit-timing variation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, radial velocities [techniques], Astronomy and Astrophysics, Exoplanet, Photometry (astronomy), Orbit, 13. Climate action, Space and Planetary Science, Satellite, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The detection of low-mass transiting exoplanets in multiple systems brings new constraints to planetary formation and evolution processes and challenges the current planet formation theories. Nevertheless, only a mere fraction of the small planets detected by Kepler and K2 have precise mass measurements, which are mandatory to constrain their composition. We aim to characterise the planets that orbit the relatively bright star K2-138. This system is dynamically particular as it presents the longest chain known to date of planets close to the 3:2 resonance. We obtained 215 HARPS spectra from which we derived the radial-velocity variations of K2-138. Via a joint Bayesian analysis of both the K2 photometry and HARPS radial-velocities (RVs), we constrained the parameters of the six planets in orbit. The masses of the four inner planets, from b to e, are 3.1, 6.3, 7.9, and 13.0 M⊕ with a precision of 34, 20, 18, and 15%, respectively. The bulk densities are 4.9, 2.8, 3.2, and 1.8 g cm-3, ranging from Earth to Neptune-like values. For planets f and g, we report upper limits. Finally, we predict transit timing variations of the order two to six minutes from the masses derived. Given its peculiar dynamics, K2-138 is an ideal target for transit timing variation (TTV) measurements from space with the upcoming CHaracterizing ExOPlanet Satellite (CHEOPS) to study this highly-packed system and compare TTV and RV masses. Full Table A.3 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A90
Published: 2019
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27. K2-265 b: a transiting rocky super-Earth

Author: T. Lopez, E. Foxell, Nuno C. Santos, David Barrado, Xavier Dumusque, Jorge Lillo-Box, Louise D. Nielsen, Tom Louden, François Bouchy, S. G. Sousa, James A. G. Jackman, Arthur Vigan, Don Pollacco, H. P. Osborn, James Kirk, George W. King, David R. Ciardi, Olivier Demangeon, Peter J. Wheatley, C. Lovis, S. C. C. Barros, R. Ligi, K. W. F. Lam, David J. Armstrong, Magali Deleuil, O. Mousis, V. Adibekyan, B. Brugger, Duncan A. Brown, E. Delgado Mena, Francesca Faedi, Jose-Manuel Almenara, Daniel Bayliss, James McCormac, Stéphane Udry, Alexandre Santerne, Aldo S. Bonomo, University of Warwick [Coventry], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Centro de Astrofísica da Universidade do Porto (CAUP), Instituto de Astrofisica de Canarias (IAC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Université Paris-Sud - Paris 11 (UP11), INAF - Osservatorio Astrofisico di Catania (OACT), School of Physics and Astronomy [Cardiff], Cardiff University, European Southern Observatory (ESO), Universidade do Porto, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Université de Genève (UNIGE)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Super-Earth, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Planetary core, FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Orbital period, 01 natural sciences, Photoevaporation, Radial velocity, Photometry (astronomy), 13. Climate action, Space and Planetary Science, Planet, [SDU]Sciences of the Universe [physics], 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of the super-Earth K2-265 b detected with K2 photometry. The planet orbits a bright (V_mag = 11.1) star of spectral type G8V with a period of 2.37 days. We obtained high-precision follow-up radial velocity measurements from HARPS, and the joint Bayesian analysis showed that K2-265 b has a radius of 1.71 +/- 0.11 R_earth and a mass of 6.54 +/- 0.84 M_earth, corresponding to a bulk density of 7.1 +/- 1.8 g/cm^3 . Composition analysis of the planet reveals an Earth-like, rocky interior, with a rock mass fraction of 80%. The short orbital period and small radius of the planet puts it below the lower limit of the photoevaporation gap, where the envelope of the planet could have eroded due to strong stellar irradiation, leaving behind an exposed core. Knowledge of the planet core composition allows us to infer the possible formation and evolution mechanism responsible for its current physical parameters., 14 pages, 9 figures, Accepted for publication in A&A
Published: 2018
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28. Spitzer Reveals Evidence of Molecular Absorption in the Atmosphere of the Hot Neptune LTT 9779b

Author: Varoujan Gorjian, Sara Seager, Ian Wong, Natalia Guerrero, Jessie L. Christiansen, Mark E. Rose, Joshua N. Winn, Katharine Hesse, Willie Fong, Stephen R. Kane, Tansu Daylan, Matias Diaz, Paul Mollière, Björn Benneke, Michael W. Werner, Laura Kreidberg, David Berardo, George R. Ricker, H. P. Osborn, Diana Dragomir, Jon M. Jenkins, Courtney D. Dressing, Farisa Y. Morales, Ian Crossfield, Jeffrey C. Smith, James S. Jenkins, Eric B. Ting, Drake Deming, Knicole D. Colón, Thomas Mikal-Evans, and Roland Vanderspek
Subjects: Physics, 010504 meteorology & atmospheric sciences, Library science, Astronomy and Astrophysics, 01 natural sciences, Carbon oxide, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Hot Neptune, 010303 astronomy & astrophysics, Molecular absorption, 0105 earth and related environmental sciences
Abstract: Non-rocky sub-Jovian exoplanets in high-irradiation environments are rare. LTT 9779b, also known as Transiting Exoplanet Survey Satellite (TESS) object of interest (TOI) 193.01, is one of the few such planets discovered to date, and the first example of an ultrahot Neptune. The planet’s bulk density indicates that it has a substantial atmosphere, so to investigate its atmospheric composition and shed further light on its origin, we obtained Spitzer InfraRed Array Camera secondary eclipse observations of LTT 9779b at 3.6 and 4.5 μm. We combined the Spitzer observations with a measurement of the secondary eclipse in the TESS bandpass. The resulting secondary eclipse spectrum strongly prefers a model that includes CO absorption over a blackbody spectrum, incidentally making LTT 9779b the first TESS exoplanet (and the first ultrahot Neptune) with evidence of a spectral feature in its atmosphere. We did not find evidence of a thermal inversion, at odds with expectations based on the atmospheres of similarly irradiated hot Jupiters. We also report a nominal dayside brightness temperature of 2305 ± 141 K (based on the 3.6 μm secondary eclipse measurement), and we constrained the planet’s orbital eccentricity to e
Published: 2020
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29. NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event

Author: Christopher A. Watson, Jose I. Vines, Philipp Eigmüller, Thomas Henning, Rafael Brahm, Richard G. West, James McCormac, Samuel Gill, Jack S. Acton, Benjamin F. Cooke, Liam Raynard, Daniel Bayliss, Heike Rauer, Maximiliano Moyano, Andrés Jordán, David R. Anderson, Monika Lendl, Don Pollacco, Michael R. Goad, Louise D. Nielsen, Matthew R. Burleigh, Néstor Espinoza, Alexis M. S. Smith, Edward M. Bryant, Maximilian N. Günther, Melissa J. Hobson, Edward Gillen, H. P. Osborn, Sarah L. Casewell, Rosanna H. Tilbrook, François Bouchy, Paula Sarkis, Aleisha Hogan, Felipe Alejandro Lagos Rojas, James S. Jenkins, Peter J. Wheatley, Nolan Grieves, Didier Queloz, Marcelo Tala Pinto, David J. Armstrong, Stéphane Udry, Gill, S [0000-0002-4259-0155], Wheatley, PJ [0000-0003-1452-2240], Cooke, BF [0000-0002-8824-9956], Jordán, A [0000-0002-5389-3944], Nielsen, LD [0000-0002-5254-2499], Bayliss, D [0000-0001-6023-1335], Anderson, DR [0000-0001-7416-7522], Vines, JI [0000-0002-1896-2377], Lendl, M [0000-0001-9699-1459], Armstrong, DJ [0000-0002-5080-4117], Brahm, R [0000-0002-9158-7315], Burleigh, MR [0000-0003-0684-7803], Casewell, SL [0000-0003-2478-0120], Espinoza, N [0000-0001-9513-1449], Gillen, E [0000-0003-2851-3070], Grieves, N [0000-0001-8105-0373], Günther, MN [0000-0002-3164-9086], Henning, T [0000-0002-1493-300X], Hobson, MJ [0000-0002-5945-7975], Jenkins, JS [0000-0003-2733-8725], Osborn, HP [0000-0002-4047-4724], Pollacco, D [0000-0001-9850-9697], Queloz, D [0000-0002-3012-0316], Sarkis, P [0000-0001-8128-3126], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, astro-ph.SR, Extrasolar gas giants, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Gas giant, FOS: Physical sciences, 01 natural sciences, Photometry, Photometry (optics), Planet, High resolution spectroscopy, 0103 physical sciences, Exoplanet detection methods, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Exoplanets, Astronomy, Astronomy and Astrophysics, Radius, Orbital period, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of NGTS-11 b (=TOI-1847 b), a transiting Saturn in a 35.46-day orbit around a mid K-type star (Teff=5050 K). We initially identified the system from a single-transit event in a TESS full-frame image light-curve. Following seventy-nine nights of photometric monitoring with an NGTS telescope, we observed a second full transit of NGTS-11 b approximately one year after the TESS single-transit event. The NGTS transit confirmed the parameters of the transit signal and restricted the orbital period to a set of 13 discrete periods. We combined our transit detections with precise radial velocity measurements to determine the true orbital period and measure the mass of the planet. We find NGTS-11 b has a radius of 0.817+0.028-0.032 $R_J$, a mass of 0.344+0.092-0.073 $M_J$, and an equilibrium temperature of just 435+34-32 K, making it one of the coolest known transiting gas giants. NGTS-11 b is the first exoplanet to be discovered after being initially identified as a TESS single-transit event, and its discovery highlights the power of intense photometric monitoring in recovering longer-period transiting exoplanets from single-transit events., Comment: 8 pages, 3 Figures, 1 table. Accepted to ApJ letters
Published: 2020
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30. Transiting planet candidate from K2 with the longest period

Author: H. Giles, Stéphane Udry, Oliver Turner, A. Collier Cameron, Christophe Lovis, Sergi Blanco-Cuaresma, F. Bouchy, Patrick Eggenberger, Martti H. Kristiansen, Daniel Bayliss, H. P. Osborn, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Spectral line, spectroscopic [Techniques], Planet, 0103 physical sciences, QB Astronomy, Transit (astronomy), 010306 general physics, 010303 astronomy & astrophysics, individual: EPIC248847494 [Stars], QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], photometric [Techniques], Astronomy and Astrophysics, Radius, 3rd-DAS, Planetary system, Radial velocity, detection [Planets and satellites], Planetary systems, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Event (particle physics), Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: We present the transit and follow-up of a single transit event from Campaign 14 of K2, EPIC248847494b, which has a duration of 54 hours and a 0.18% depth. Aims: Using photometric tools and conducting radial velocity follow-up, we vet and characterise this very strong candidate. Methods: Owing to the long, unknown period, standard follow-up methods needed to be adapted. The transit was fitted using Namaste, and the radial velocity slope was measured and compared to a grid of planet-like orbits with varying masses and periods. These used stellar parameters measured from spectra and the distance as measured by Gaia. Results: Orbiting around a sub-giant star with a radius of 2.70$\pm$0.12R$_{\rm Sol}$, the planet has a radius of 1.11$_{-0.07}^{+0.07}$R$_{\rm Jup}$ and a period of 3650$_{-1130}^{+1280}$ days. The radial velocity measurements constrain the mass to be lower than 13M$_{\rm Jup}$, which implies a planet-like object. Conclusions: We have found a planet at 4.5 AU from a single-transit event. After a full radial velocity follow-up campaign, if confirmed, it will be the longest-period transiting planet discovered., Comment: 5 pages, 3 figures. Published in A&A. Updated with correct title and full edits
Published: 2018
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31. Precise masses for the transiting planetary system HD 106315 with HARPS

Author: Isabelle Boisse, James A. G. Jackman, William D. Cochran, Don Pollacco, S. G. Sousa, Francesca Faedi, R. Ligi, Pedro Figueira, David J. Armstrong, Néstor Espinoza, C. Melo, J. Bento, Olivier Demangeon, Arthur Vigan, Xavier Dumusque, Monika Lendl, V. Adibekyan, H. P. Osborn, E. Foxell, Aurélien Wyttenbach, C. Lovis, S. C. C. Barros, Daniel Bayliss, Magali Deleuil, O. Mousis, Avi Shporer, Aldo S. Bonomo, H. Gosselin, James D. Armstrong, E. Delgado Mena, Amanda P. Doyle, Amaury H. M. J. Triaud, João P. Faria, A. Collier Cameron, Alexandre Santerne, David Ehrenreich, S. Hojjatpanah, Ramotholo Sefako, Guillaume Hébrard, B. Brugger, Duncan A. Brown, Rodrigo F. Díaz, Stéphane Udry, Nuno C. Santos, David Barrado, François Bouchy, J. J. Neal, Jorge Lillo-Box, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: 010504 meteorology & atmospheric sciences, Ciencias Físicas, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Spectral line, COMPOSITION [PLANETS AND SATELLITES], purl.org/becyt/ford/1 [https], Planet, 0103 physical sciences, DETECTION [PLANETS AND SATELLITES], fundamental parameters [Planetary systems], QB Astronomy, Transit (astronomy), 010303 astronomy & astrophysics, QC, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], detection [Planetary systems], photometric [Techniques], Astronomy and Astrophysics, Radius, purl.org/becyt/ford/1.3 [https], 3rd-DAS, Planetary system, individual HD 106315, EPIC 201437844 [Stars], Radial velocity, Astronomía, Photometry (astronomy), QC Physics, 13. Climate action, Space and Planetary Science, composition [Planetary systems], FUNDAMENTAL PARAMETERS [PLANETS AND SATELLITES], CIENCIAS NATURALES Y EXACTAS, INDIVIDUAL: HD 106315 [STARS], Astrophysics - Earth and Planetary Astrophysics
Abstract: The multi-planetary system HD 106315 was recently found in K2 data . The planets have periods of $P_b \sim9.55$ and $P_c \sim 21.06\,$days, and radii of $ r_b = 2.44 \pm 0.17\, $ and $r_c = 4.35 \pm 0.23\, $ $R_{\oplus}$. The brightness of the host star (V=9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. We obtained high precision radial velocities for HD~106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. We estimate the mass of HD 106315b to be 12.6 $\pm$ 3.2 $M_{\oplus}$ and the density to be $4.7 \pm 1.7\, g\,cm^{-3}$, while for HD 106315c we estimate a mass of 15.2 $\pm$ 3.7 $M_{\oplus}$ and a density of $1.01 \pm 0.29\, $g\,cm$^{-3}$. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29\%, and the water mass fraction to be 10-50\%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions., 16 pages, 9 figures, A\&A accepted
Published: 2017
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32. WASP-104b and WASP-106b : two transiting hot Jupiters in 1.75-day and 9.3-day orbits

Author: Barry Smalley, François Bouchy, Guillaume Montagnier, J. W. Rostron, Monika Lendl, Francesca Faedi, Y. Gómez Maqueo Chew, Oliver Turner, Didier Queloz, H. P. Osborn, Emmanuel Jehin, Richard G. West, Duncan A. Brown, Michaël Gillon, Don Pollacco, Aldo S. Bonomo, David R. Anderson, Pierre F. L. Maxted, S. C. C. Barros, M. Neveu-VanMalle, Amaury H. M. J. Triaud, Susan Walker, Alexis M. S. Smith, Stéphane Udry, A. Collier Cameron, Francesco Pepe, Damien Ségransan, Tom Louden, Laetitia Delrez, David J. Armstrong, Guillaume Hébrard, Peter J. Wheatley, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Department of Medicine - Halifax (DRA), Dalhousie University [Halifax], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews [Scotland], Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, European Southern Observatory (ESO), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Star (game theory), fundamental parameters [Planets and satellites], FOS: Physical sciences, Orbital eccentricity, Astrophysics, individual: WASP-104b [Stars], Jupiter, Planet, Hot Jupiter, QB Astronomy, 10. No inequality, QC, individual: WASP-106b [Stars], QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Orbital period, detection [Planets and satellites], Planetary systems, QC Physics, Space and Planetary Science, Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery from the WASP survey of two exoplanetary systems, each consisting of a Jupiter-sized planet transiting an 11th magnitude (V) main-sequence star. WASP-104b orbits its star in 1.75 d, whereas WASP-106b has the fourth-longest orbital period of any planet discovered by means of transits observed from the ground, orbiting every 9.29 d. Each planet is more massive than Jupiter (WASP-104b has a mass of $1.27 \pm 0.05 \mathrm{M_{Jup}}$, while WASP-106b has a mass of $1.93 \pm 0.08 \mathrm{M_{Jup}}$). Both planets are just slightly larger than Jupiter, with radii of $1.14 \pm 0.04$ and $1.09 \pm 0.04 \mathrm{R_{Jup}}$ for WASP-104 and WASP-106 respectively. No significant orbital eccentricity is detected in either system, and while this is not surprising in the case of the short-period WASP-104b, it is interesting in the case of WASP-106b, because many otherwise similar planets are known to have eccentric orbits., Comment: 8 pages, 6 figures, 5 tables. Accepted for publication in A&A
Published: 2014
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33. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author: A. Santerne, G. Hébrard, J. Lillo-Box, D. J. Armstrong, S. C. C. Barros, O. Demangeon, D. Barrado, A. Debackere, M. Deleuil, E. Delgado Mena, M. Montalto, D. Pollacco, H. P. Osborn, S. G. Sousa, L. Abe, V. Adibekyan, J.-M. Almenara, P. André, G. Arlic, G. Barthe, P. Bendjoya, R. Behrend, I. Boisse, F. Bouchy, H. Boussier, M. Bretton, D. J. A. Brown, B. Carry, A. Cailleau, E. Conseil, G. Coulon, B. Courcol, B. Dauchet, J.-C. Dalouzy, M. Deldem, O. Desormières, P. Dubreuil, J.-M. Fehrenbach, S. Ferratfiat, R. Girelli, J. Gregorio, S. Jaecques, F. Kugel, J. Kirk, O. Labrevoir, J.-C. Lachurié, K. W. F. Lam, P. Le Guen, P. Martinez, L. P. A. Maurin, J. McCormac, J-B. Pioppa, U. Quadri, A. Rajpurohit, J. Rey, J.-P. Rivet, R. Roy, N. C. Santos, F. Signoret, L. Strabla, O. Suarez, D. Toublanc, M. Tsantaki, J.-M. Vienney, P. A. Wilson, M. Bachschmidt, F. Colas, O. Gerteis, P. Louis, J.-C. Mario, C. Marlot, J. Montier, V. Perroud, V. Pic, D. Romeuf, S. Ubaud, D. Verilhac, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Geneva Observatory, University of Geneva [Switzerland], CdR & CdL group, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, School of Physics and Astronomy [Cardiff], Cardiff University, Hôpital Européen Georges Pompidou [APHP] (HEGP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département RadioChimie et Procédés (DRCP), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval [Québec] (ULaval), Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), Universidade do Porto [Porto], Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval, Departamento de Física e Astronomia [Porto], Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Paris-Sud - Paris 11 ( UP11 ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), LAEX, Depto. Astrofísica, Centro de Astrobiología, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofisica de Canarias ( IAC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Université Côte d'Azur ( UCA ), Observatoire de Haute-Provence ( OHP ), Institut Pythéas ( OSU PYTHEAS ), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), School of Physis & Astronomy, Hôpital Européen Georges Pompidou [APHP] ( HEGP ), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux ( EPOC ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -École pratique des hautes études ( EPHE ) -Centre National de la Recherche Scientifique ( CNRS ), Département RadioChimie et Procédés ( DRCP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables ( CdR & CdL group ), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Genève = University of Geneva (UNIGE), Environnements et Paléoenvironnements OCéaniques (EPOC), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École Pratique des Hautes Études (EPHE), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto-Universidade do Porto, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: Physics, 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Stellar rotation, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, 01 natural sciences, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Visual binary
Abstract: International audience; In the present paper we report the discovery of a new hot Jupiter, K2-29 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25 days, a mass of 0.73 +/- 0.04M(sic), and a radius of 1.19 +/- 0.02 R(sic). The host star is a relatively bright (V = 12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of lithium, we find that the system might be as young as similar to 450 Myr. The observation of the Rossiter-McLaughlin effect shows that the planet is aligned with respect to the stellar spin. Given the deep transit (20 mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where both stars are relatively bright.
Published: 2016
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34. TESS and HARPS reveal two sub-Neptunes around TOI 1062

Author: J. N. Winn, Roland Vanderspek, A. Hadjigeorghiou, Sergio Hoyer, J. F. Otegi, Caroline Dorn, Brian McLean, Vardan Adibekyan, J.-B. Delisle, Matteo Brogi, Angelica Psaridi, George R. Ricker, David R. Ciardi, Nathan Hara, Karen A. Collins, D. A. Caldwell, Stéphane Udry, R. Schwarz, Keivan G. Stassun, Chris Henze, Daniel Bayliss, Elisa Delgado-Mena, Andrew Vanderburg, Louise D. Nielsen, David J. Armstrong, Sara Seager, S. C. C. Barros, Nuno C. Santos, David Barrado, M. Fridlund, Siddharth Gandhi, Ravit Helled, M. Stalport, P. Figueira, Xavier Dumusque, G. Wang, H. P. Osborn, Robert F. Goeke, Jason D. Eastman, Jon M. Jenkins, François Bouchy, S. G. Sousa, P. A. Strøm, Natalia Guerrero, Dennis M. Conti, D. W. Latham, D. J. A. Brown, A. Osborn, J. Lillo-Box, P. T. Boyd, S. Hojjatpanah, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Orbital elements, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Planets and satellites: detection, Astrophysics - Earth and planetary astrophysics, Orbital period, 01 natural sciences, Exoplanet, Planets and satellites: composition, Radial velocity, Stars, Mean motion, Planets and satellites: general, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, QB, 0105 earth and related environmental sciences
Abstract: The Transiting Exoplanet Survey Satellite (\textit{TESS}) mission was designed to perform an all-sky search of planets around bright and nearby stars. Here we report the discovery of two sub-Neptunes orbiting around the TOI 1062 (TIC 299799658), a V=10.25 G9V star observed in the TESS Sectors 1, 13, 27 & 28. We use precise radial velocity observations from HARPS to confirm and characterize these two planets. TOI 1062b has a radius of 2.265^{+0.095}_{-0.091} Re, a mass of 11.8 +\- 1.4 Me, and an orbital period of 4.115050 +/- 0.000007 days. The second planet is not transiting, has a minimum mass of 7.4 +/- 1.6 Me and is near the 2:1 mean motion resonance with the innermost planet with an orbital period of 8.13^{+0.02}_{-0.01} days. We performed a dynamical analysis to explore the proximity of the system to this resonance, and to attempt at further constraining the orbital parameters. The transiting planet has a mean density of 5.58^{+1.00}_{-0.89} g cm^-3 and an analysis of its internal structure reveals that it is expected to have a small volatile envelope accounting for 0.35% of the mass at maximum. The star's brightness and the proximity of the inner planet to the "radius gap" make it an interesting candidate for transmission spectroscopy, which could further constrain the composition and internal structure of TOI 1062b., 14 pages, 11 figures
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34 results on '"H. P. Osborn"'

1. Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS

2. A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113

3. Mass determinations of the three mini-Neptunes transiting TOI-125

4. TESS and HARPS reveal two sub-Neptunes around TOI 1062

5. HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS

6. Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS

7. Rapid classification of TESS planet candidates with convolutional neural networks

8. The young HD 73583 (TOI-560) planetary system: Two 10-M⊕ mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf

9. TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter

10. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

11. TOI-220 b: a warm sub-Neptune discovered by TESS

12. Discovery and characterization of the exoplanets WASP-148b and c

13. Six transiting planets and a chain of Laplace resonances in TOI-178

14. TOI-1296b and TOI-1298b observed with TESS and SOPHIE: Two hot Saturn-mass exoplanets with different densities around metal-rich stars

15. The TESS Objects of Interest Catalog from the TESS Prime Mission

16. A long period (P = 61.8-d) M5V dwarf eclipsing a Sun-like star from TESS and NGTS

17. Two Transiting Hot Jupiters from the WASP Survey: WASP-150b and WASP-176b

18. The TESS-Keck Survey. I. A Warm Sub-Saturn-mass Planet and a Caution about Stray Light in TESS Cameras

19. KELT-9 b's Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin-Orbit Misalignment

20. TOI 122b and TOI 237b, two small warm planets orbiting inactive M dwarfs, found by \textit{TESS}

21. Transits of Known Planets Orbiting a Naked-eye Star

22. Masses for the seven planets in K2-32 and K2-233

23. HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs*

24. XO-7 b: A transiting hot Jupiter with a massive companion on a wide orbit

25. The changing face of AU Mic b: stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS

26. Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

27. K2-265 b: a transiting rocky super-Earth

28. Spitzer Reveals Evidence of Molecular Absorption in the Atmosphere of the Hot Neptune LTT 9779b

29. NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event

30. Transiting planet candidate from K2 with the longest period

31. Precise masses for the transiting planetary system HD 106315 with HARPS

32. WASP-104b and WASP-106b : two transiting hot Jupiters in 1.75-day and 9.3-day orbits

33. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

34. TESS and HARPS reveal two sub-Neptunes around TOI 1062

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34 results on '"H. P. Osborn"'

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