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22 results on '"J. F. Otegi"'

1. 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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2. 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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3. 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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4. Mass Determinations of the Three Mini-Neptunes Transiting TOI-125

Author: L D Nielsen, D. Gandolfi, D J Armstrong, James 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
Subjects: Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, a steady progress was made in achieving the mission’s primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, the TESS’s observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V = 11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c, and TOI-125d. TOI-125b has an orbital period of 4.65 d, a radius of 2.726 ± 0.075 R(E), a mass of 9.50 ± 0.88 M(E), and is near the 2:1 mean motion resonance with TOI-125c at 9.15 d. TOI-125c has a similar radius of 2.759 ± 0.10 R(E) and a mass of 6.63 ± 0.99 M(E), being the puffiest of the three planets. TOI-125d has an orbital period of 19.98 d and a radius of 2.93 ± 0.17 R(E) and mass 13.6 ± 1.2 M(E). For TOI-125b and d, we find unusual high eccentricities of 0.19 ± 0.04 and 0.17(sup +0.08, sub −0.06), respectively. Our analysis also provides upper mass limits for the two low-SNR planet candidates in the system; for TOI-125.04 (R(P) = 1.36 R(E), P = 0.53 d), we find a 2σ upper mass limit of 1.6 M(E), whereas TOI-125.05 (R(P) = 4.2(sup +2.4, sub −1.4 R(E), P = 13.28 d) is unlikely a viable planet candidate with an upper mass limit of 2.7 M(E). We discuss the internal structure of the three confirmed planets, as well as dynamical stability and system architecture for this intriguing exoplanet system.
Published: 2020
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5. GJ 3090 b: one of the most favourable mini-Neptune for atmospheric characterisation

Author: J. M. Almenara, X. Bonfils, J. F. Otegi, O. Attia, M. Turbet, N. Astudillo-Defru, K. A. Collins, A. S. Polanski, V. Bourrier, C. Hellier, C. Ziegler, F. Bouchy, C. Briceno, D. Charbonneau, M. Cointepas, K. I. Collins, I. Crossfield, X. Delfosse, R. F. Diaz, C. Dorn, J. P. Doty, T. Forveille, G. Gaisné, T. Gan, R. Helled, K. Hesse, J. M. Jenkins, E. L. N. Jensen, D. W. Latham, N. Law, A. W. Mann, S. Mao, B. McLean, F. Murgas, G. Myers, S. Seager, A. Shporer, T. G. Tan, J. D. Twicken, and J. Winn
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of GJ 3090 b (TOI-177.01), a mini-Neptune on a 2.9-day orbit transiting a bright (K = 7.3 mag) M2 dwarf located at 22 pc. The planet was identified by the Transiting Exoplanet Survey Satellite and was confirmed with the High Accuracy Radial velocity Planet Searcher radial velocities. Seeing-limited photometry and speckle imaging rule out nearby eclipsing binaries. Additional transits were observed with the LCOGT, Spitzer, and ExTrA telescopes. We characterise the star to have a mass of 0.519 $\pm$ 0.013 M$_\odot$ and a radius of 0.516 $\pm$ 0.016 R$_\odot$. We modelled the transit light curves and radial velocity measurements and obtained a planetary mass of 3.34 $\pm$ 0.72 M$_\oplus$, a radius of 2.13 $\pm$ 0.11 R$_\oplus$, and a mean density of 1.89$^{+0.52}_{-0.45}$ g/cm$^3$. The low density of the planet implies the presence of volatiles, and its radius and insolation place it immediately above the radius valley at the lower end of the mini-Neptune cluster. A coupled atmospheric and dynamical evolution analysis of the planet is inconsistent with a pure H-He atmosphere and favours a heavy mean molecular weight atmosphere. The transmission spectroscopy metric of 221$^{+66}_{-46}$ means that GJ 3090 b is the second or third most favourable mini-Neptune after GJ 1214 b whose atmosphere may be characterised. At almost half the mass of GJ 1214 b, GJ 3090 b is an excellent probe of the edge of the transition between super-Earths and mini-Neptunes. We identify an additional signal in the radial velocity data that we attribute to a planet candidate with an orbital period of 13 days and a mass of 17.1$^{+8.9}_{-3.2}$ M$_\oplus$, whose transits are not detected., Comment: 25 pages, 26 figures, accepted for publication in A&A
Published: 2022
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6. 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

7. 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

8. TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author: Sara Seager, Eric B. Ting, Felipe Murgas, Nicholas M. Law, D. Maurel, S. Curaba, Tianjun Gan, S. Rochat, Richard G. West, George R. Ricker, Francesco Pepe, René Doyon, P. Kern, Coel Hellier, Jon M. Jenkins, Thibaut Moulin, I. C. Leão, G. Gaisne, Caroline Dorn, Xavier Bonfils, Laurent Jocou, Yves Magnard, J.-J. Correia, Eric Stadler, P. Rabou, C. Melo, Joshua N. Winn, C. Ziegler, J. D. Twicken, C. Lovis, Karen A. Collins, Nicola Astudillo-Defru, B. L. Canto Martins, Aurélien Wyttenbach, X. Delfosse, Alain Roux, Kevin I. Collins, Alain Delboulbé, J. F. Otegi, David R. Anderson, Jose-Manuel Almenara, William Waalkes, Ravit Helled, Marion Cointepas, François Bouchy, J. R. De Medeiros, Roland Vanderspek, Étienne Artigau, David Charbonneau, Pedro Figueira, T. Forveille, David W. Latham, L. Gluck, David R. Rodriguez, Andrew W. Mann, A. Wunsche, S. Lafrasse, Nuno C. Santos, Damien Ségransan, Rodrigo F. Díaz, Stéphane Udry, Philippe Feautrier, 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), 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]), and Université de Montréal (UdeM)
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, 01 natural sciences, Transmission spectroscopy, Photometry (optics), Neptune, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Radius, Orbital period, Exoplanet, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC 220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d = 57 pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P = 3.6977104 +- 0.0000037 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8 +- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions., Comment: 23 pages, 16 figures, Accepted for publication in A&A
Published: 2021

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

Author: Sara Seager, Ravit Helled, Rodrigo F. Díaz, Douglas A. Caldwell, Tansu Daylan, Stéphane Udry, Don Pollacco, J. F. Otegi, David R. Anderson, Keivan G. Stassun, Elisa Delgado-Mena, David J. Armstrong, D. W. Latham, H. P. Osborn, Jeffrey C. Smith, S. C. C. Barros, Edward M. Bryant, Nuno C. Santos, Diana Dragomir, David Barrado, Eric L. N. Jensen, Nicholas M. Law, N. Scott, Cesar Briceno, C. Ziegler, Benjamin V. Rackham, Daniel Bayliss, J. Villasenor, Jon M. Jenkins, Richard G. West, Andrew W. Mann, Peter J. Wheatley, George R. Ricker, Vardan Adibekyan, Magali Deleuil, Jorge Lillo-Box, Louise D. Nielsen, Christopher J. Burke, P. A. Strøm, Karen A. Collins, D. R. Rodriguez, Olivier Demangeon, D. J. A. Brown, Roland Vanderspek, A. Osborn, Coel Hellier, Sergio Hoyer, Joshua N. Winn, P. Figueira, Steve B. Howell, George W. King, Dana R. Louie, François Bouchy, Caroline Dorn, S. G. Sousa, Dennis M. Conti, 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), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Dorn, C. [0000-0001-6110-4610], Anderson, D. [0000-0001-7416-7522], Barros, S. [0000-0003-2434-3625], Adibekyan, V. [0000-0002-0601-6199], Armstrong, D. [0000-0002-5080-4117], Santos, N. [0000-0003-4422-2919], Fundacao para a Ciencia e a Tecnologia (FCT), Science and Technology Facilities Council (STFC), Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), and UK Space Agency
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Atmosphere, purl.org/becyt/ford/1 [https], Planet, QB460, 0103 physical sciences, DETECTION [PLANETS AND SATELLITES], INDIVIDUAL: HD110113 [STARS], 010303 astronomy & astrophysics, QB600, QC, QB, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stellar rotation, Astronomy and Astrophysics, Radius, purl.org/becyt/ford/1.3 [https], Exoplanet, Radial velocity, Photometry (astronomy), Space and Planetary Science, [SDU]Sciences of the Universe [physics], Mini-Neptune, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of HD 110113 b (TOI-755.01), a transiting mini-Neptune exoplanet on a 2.5-day orbit around the solar-analogue HD 110113 (Teff = 5730K). Using TESS photometry and HARPS radial velocities gathered by the NCORES program, we find HD 110113 b has a radius of $2.05\pm0.12$ $R_\oplus$ and a mass of $4.55\pm0.62$ $M_\oplus$. The resulting density of $2.90^{+0.75}_{-0.59}$ g cm^{-3} is significantly lower than would be expected from a pure-rock world; therefore, HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. The high incident flux places it within the so-called radius valley; however, HD 110113 b was able to hold onto a substantial (0.1-1\%) H-He atmosphere over its $\sim4$ Gyr lifetime. Through a novel simultaneous gaussian process fit to multiple activity indicators, we were also able to fit for the strong stellar rotation signal with period $20.8\pm1.2$ d from the RVs and confirm an additional non-transiting planet with a mass of $10.5\pm1.2$ $M_\oplus$ and a period of $6.744^{+0.008}_{-0.009}$ d., Comment: 17 pages, 11 figures. Accepted for publication at MNRAS. HARPS RVs available at https://dace.unige.ch/radialVelocities/?pattern=HD110113
Published: 2021

10. Impact of the measured parameters of exoplanets on the inferred internal structure

Author: Yann Alibert, J. F. Otegi, Ravit Helled, J. Haldemann, Caroline Dorn, and François Bouchy
Subjects: Physics, Planet, Entropy (statistical thermodynamics), Posterior probability, Exoplanetology, Context (language use), Astrophysics::Earth and Planetary Astrophysics, Statistical physics, Radius, Exoplanet, Nested sampling algorithm
Abstract: Exoplanet characterization is one of the main foci of current exoplanetary science. For super-Earths and sub-Neptunes, we mostly rely on mass and radius measurements, which allow us to derive the mean density of the body and give a rough estimate of the bulk composition of the planet. However, the determination of planetary interiors is a very challenging task. In addition to the uncertainty in the observed fundamental parameters, theoretical models are limited owing to the degeneracy in determining the planetary composition. We aim to study several aspects that affect the internal characterization of super-Earths and sub-Neptunes: observational uncertainties, location on the M-R diagram, impact of additional constraints such as bulk abundances or irradiation, and model assumptions. We used a full probabilistic Bayesian inference analysis that accounts for observational and model uncertainties. We employed a nested sampling scheme to efficiently produce the posterior probability distributions for all the planetary structural parameter of interest. We included a structural model based on self-consistent thermodynamics of core, mantle, high-pressure ice, liquid water, and H-He envelope. Regarding the effect of mass and radius uncertainties on the determination of the internal structure, we find three different regimes: below the Earth-like composition line and above the pure-water composition line smaller observational uncertainties lead to better determination of the core and atmosphere mass, respectively; and between these regimes internal structure characterization only weakly depends on the observational uncertainties. We also find that using the stellar Fe/Si and Mg/Si abundances as a proxy for the bulk planetary abundances does not always provide additional constraints on the internal structure. Finally we show that small variations in the temperature or entropy profiles lead to radius variations that are comparable to the observational uncertainty. This suggests that uncertainties linked to model assumptions can eventually become more relevant to determine the internal structure than observational uncertainties.
Published: 2021

11. A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)

Author: J. I. González Hernández, Thomas Barclay, Yann Alibert, George R. Ricker, Keivan G. Stassun, Paolo Molaro, Stefano Cristiani, J. Haldemann, Jorge Lillo-Box, M. Fasnaugh, Giuseppina Micela, Stéphane Udry, François Bouchy, Baptiste Lavie, Enric Palle, G. Lo Curto, S. G. Sousa, J. F. Otegi, Francesco Pepe, Mahmoudreza Oshagh, Rafael Rebolo, Valentina D'Odorico, Jon M. Jenkins, Pedro Figueira, Nuno C. Santos, Carlos Martins, Nelson J. Nunes, Daniel Conde Rodriguez, Aldo S. Bonomo, David Ehrenreich, Joshua N. Winn, Mario Damasso, Ennio Poretti, Romain Allart, A. Suárez Mascareño, C. Lovis, Alexandre Cabral, J. D. Twicken, V. Adibekyan, Sara Seager, David R. Ciardi, M. R. Zapatero Osorio, P. Di Marcantonio, S. C. C. Barros, D. Mégevand, Alessandro Sozzetti, David W. Latham, Andrea Mehner, Sozzetti, A. [0000-0002-7504-365X], Nunes, N. [0000-0002-3837-6914], Haldemann, J. [0000-0003-1231-2389], Istituto Nazionale di Astrofisica (INAF), Agenzia Spaziale Italiana (ASI), iss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), European Commission (EC), European Research Council (ERC), Ministerio de Economía y Competitividad (MINECO), and Agencia Estatal de Investigación (AEI) http://dx.doi.org/10.13039/501100011033
Subjects: 530 Physics, FOS: Physical sciences, Astrophysics, 01 natural sciences, individual: HD 5278 (TOI-130) [Stars], Espresso, Neptune, 0103 physical sciences, miscellaneous [Methods], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 010308 nuclear & particles physics, 520 Astronomy, photometric [Techniques], Astronomy and Astrophysics, Planetary system, 500 Science, 620 Engineering, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, composition [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. Transiting sub-Neptune-type planets, with radii approximately between 2 and 4 R⊕, are of particular interest as their study allows us to gain insight into the formation and evolution of a class of planets that are not found in our Solar System. Aims. We exploit the extreme radial velocity (RV) precision of the ultra-stable echelle spectrograph ESPRESSO on the VLT to unveil the physical properties of the transiting sub-Neptune TOI-130 b, uncovered by the TESS mission orbiting the nearby, bright, late F-type star HD 5278 (TOI-130) with a period of Pb = 14.3 days. Methods. We used 43 ESPRESSO high-resolution spectra and broad-band photometry information to derive accurate stellar atmospheric and physical parameters of HD 5278. We exploited the TESS light curve and spectroscopic diagnostics to gauge the impact of stellar activity on the ESPRESSO RVs. We performed separate as well as joint analyses of the TESS photometry and the ESPRESSO RVs using fully Bayesian frameworks to determine the system parameters. Results. Based on the ESPRESSO spectra, the updated stellar parameters of HD 5278 are Teff = 6203 ± 64 K, log g = 4.50 ± 0.11 dex, [Fe/H] = −0.12 ± 0.04 dex, M⋆ = 1.126−0.035+0.036 M⊙, and R⋆ = 1.194−0.016+0.017 R⊙. We determine HD 5278 b’s mass and radius to be Mb = 7.8−1.4+1.5 M⊕ and Rb = 2.45 ± 0.05R⊕. The derived mean density, ϱb = 2.9−0.5+0.6 g cm−3, is consistent with the bulk composition of a sub-Neptune with a substantial (~ 30%) water mass fraction and with a gas envelope comprising ~17% of the measured radius. Given the host brightness and irradiation levels, HD 5278 b is one of the best targetsorbiting G-F primaries for follow-up atmospheric characterization measurements with HST and JWST. We discover a second, non-transiting companion in the system, with a period of Pc = 40.87−0.17+0.18 days and a minimum mass of Mc sin ic = 18.4−1.9+1.8 M⊕. We study emerging trends in parameters space (e.g., mass, radius, stellar insolation, and mean density) of the growing population of transiting sub-Neptunes, and provide statistical evidence for a low occurrence of close-in, 10 − 15M⊕ companions around G-F primaries with Teff ≳ 5500 K. The authors acknowledge the ESPRESSO project team for its effort and dedication in building the ESPRESSO instrument. This work has received financial support from the ASI-INAF agreement no. 2018-16-HH.0. M.D. acknowledges financial support from the FP7-SPACE Project ETAEARTH (GA No. 313014). A.S. We gratefully acknowledges support from the Italian Space Agency (ASI) under contract 2018-24-HH.0. The INAF authors acknowledge financial support of the Italian Ministry of Education, University, and Research with PRIN 201278X4FL and the Progetti Premiali funding scheme.to acknowledge the Swiss National Science Foundation (SNSF) for supporting research with ESPRESSO through the SNSF grants no. 140649, 152721, and 166227. The ESPRESSO Instrument Project was partially funded through SNSF's FLARE Programme for large infrastructures. This work has been carried out in part within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This work was supported by FCT -Funda cao para a Ciencia e Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionaliza cao by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987; PTDC/FIS-OUT/29048/2017 & IF/00852/2015. S.C.C.B. acknowledges support from FCT through contract nr. IF/01312/2014/CP1215/CT0004. S.G.S acknowledges the support from FCT through Investigator FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Four Aces, grant agreement no. 724427). V.A. acknowledges the support from FCT through Investigator FCT contract nr. IF/00650/2015/CP1273/CT0001. Y.A. and J.H. acknowledge the Swiss National Science Foundation (SNSF) for supporting research through the SNSF grant 200 020_192038. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramon y Cajal programme RYC-2013-14 875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86 389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. R.A. is a Trottier Postdoctoral Fellow and acknowledges support from the Trottier Family Foundation. This work was supported in part through a grant from FRQNT. 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 publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch.This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).; We acknowledge the use of public TESS Alert 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. Peerreview
Published: 2021
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12. The impact of exoplanets' measured parameters on the inferred internal structure

Author: François Bouchy, Ravit Helled, Yann Alibert, J. Haldemann, Caroline Dorn, and J. F. Otegi
Subjects: Physics, Planet, Entropy (statistical thermodynamics), Posterior probability, Exoplanetology, Astrophysics::Earth and Planetary Astrophysics, Statistical physics, Radius, Bayesian inference, Exoplanet, Nested sampling algorithm
Abstract: Exoplanet characterization is one of the main foci of current exoplanetary science. For super-Earths and sub-Neptunes, we mostly rely on mass and radius measurements, which allow to derive the body’s mean density and give a rough estimate of the planet’s bulk composition. However, the determination of planetary interiors is a very challenging task. In addition to the uncertainty in the observed fundamental parameters, theoretical models are limited due to the degeneracy in determining the planetary composition. We aim to study several aspects that affect internal characterization of super-Earths and sub-Neptunes: observational uncertainties, location on the M-R diagram, impact of additional constraints as bulk abundances or irradiation, and model assumptions. We use a full probabilistic Bayesian inference analysis that accounts for observational and model uncertainties. We employ a Nested Sampling scheme to efficiently produce the posterior probability distributions for all the planetary structural parameter of interest. We include a structural model based on self-consistent thermodynamics of core, mantle, high-pressure ice, liquid water, and H-He envelope. Regarding the effect of mass and radius uncertainties on the determination of the internal structure, we find three different regimes: below the Earth-like composition line and above the pure-water composition line smaller observational uncertainties lead to better determination of the core and atmosphere mass respectively, and between them internal structure characterization only weakly depends on the observational uncertainties. We also find that using the stellar Fe/Si and Mg/Si abundances as a proxy for the bulk planetary abundances does not always provide additional constraints on the internal structure. Finally we show that small variations in the temperature or entropy profiles lead to radius variations that are comparable to the observational uncertainty. This suggests that uncertainties linked to model assumptions can eventually become more relevant to determine the internal structure than observational uncertainties.
Published: 2020

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

Author: Farzana Meru, Matías R. Díaz, John H. Livingston, Florian Rodler, Samuel N. Quinn, Pablo Rojas, Heike Rauer, Diana Kossakowski, Isabelle Boisse, George R. Ricker, P. T. Boyd, Ravit Helled, Judith Korth, S. C. C. Barros, L. A. dos Santos, A. P. Hatzes, S. Sabotta, Rafael Luque, M. Stalport, Andrew Vanderburg, Jason H. Steffen, Vincent Van Eylen, Edward M. Bryant, Jon M. Jenkins, David J. Armstrong, L. González-Cuesta, S. Hojjatpanah, Norio Narita, Felipe Murgas, Savita Mathur, J. F. Otegi, Paul Wilson, Iskra Georgieva, Nicolás T. Kurtovic, Sara Seager, Emeline Bolmont, Xavier Dumusque, Jose I. Vines, M. Esposito, Z. M. Berdinas, Sascha Grziwa, Olivier Demangeon, J. M. Almenara, O. Mousis, Julia V. Seidel, D. J. A. Brown, T. Lopez, A. Santerne, S. G. Sousa, Benjamin F. Cooke, Davide Gandolfi, R. A. Garcia, Eric B. Ting, Fei Dai, David W. Latham, Daniel Bayliss, Romain Allart, Peter J. Wheatley, François Bouchy, Christopher J. Burke, Vardan Adibekyan, Seth Redfield, Hugh P. Osborn, Natalia Guerrero, Joshua N. Winn, Malcolm Fridlund, Martin Turbet, Louise D. Nielsen, Chris Henze, Caroline Dorn, J. Dittman, K. W. F. Lam, Carina M. Persson, William D. Cochran, Jorge Lillo-Box, Rodrigo F. Díaz, Stéphane Udry, Nuno C. Santos, David Barrado, Enric Palle, James S. Jenkins, Roland Vanderspek, 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), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Vanderburg, A. [0000-0001-7246-5438], Dos Santos, L. [0000-0002-2248-3838], Barrado, D. [0000-0002-5971-9242], Cochran, W. [0000-0001-9662-3496], Lillo Box, J. [0000-0003-3742-1987], Barros, S. [0000-0003-2434-3625], Stalport, M. [0000-0003-0996-6402], Dorn, C. [0000-0001-6110-4610], Nielsen, L. D. [0000-0002-5254-2499], Seidel, J. V. [0000-0002-7990-9596], Diaz, M. R. [0000-0002-2100-3257], Bolmont, E. [0000-0001-5657-4503], Adibekyan, V. [0000-0002-0601-6199], Van Eylen, V. [0000-0001-5542-8870], Armstrong, D. [0000-0002-5080-4117], Korth, J. [0000-0002-0076-6239], Díaz, R. [0000-0001-9289-5160], Santos, N. [0000-0003-4422-2919], Luque, R. [0000-0002-4671-2957], Turbet, M. [0000-0003-2260-9856], Mathur, S. [0000-0002-0129-0316], Strom, P. A. [0000-0002-7823-1090], Sabotta, S. [0000-0001-9078-5574], Wheatley, P. [0000-0003-1452-2240], Hojjatpanah, S. [0000-0002-0417-1902], Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Swiss National Science Foundation (SNSF), Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), European Southern Observatory (ESO), Swiss National Centre of Competence inResearch (NCCR), National Aeronautics and Space Administration (NASA), Fundacao para a Ciencia e a Tecnologia (FCT), European Research Council (ERC), European Southern Observatory, STFC via an Ernest Rutherford Fellowship, FEDER -Fundo Europeu de Desenvolvimento Regional through COMPETE2020-Programa Operacional Competitividade e Internacionalizacao, Portuguese Foundation for Science and Technology, CONICYT-PFCHA/Doctorado Nacional, Comision Nacional de Investigacion Cientifica y Tecnologica CONICYT FONDECYT, German Research Foundation (DFG), Spanish State Research Agency (AEI), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, and Spanish Ministry under the Ramon y Cajal fellowship
Subjects: 010504 meteorology & atmospheric sciences, Planets and satellites: detection, Planets and satellites: individual: (TOI-125, TIC 52368076), FOS: Physical sciences, 01 natural sciences, Neptune, Planet, TIC 52368076), 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], individual: TOI-125, TIC 52368076 [Planets and satellites], Ecliptic, Astronomy, Astronomy and Astrophysics, Radius, Planets and satellites: detection, Orbital period, Exoplanet, Radial velocity, detection [Planets and satellites], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics, Planets and satellites: individual: (TOI-125
Abstract: The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, steady progress was made in achieving the mission's primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, TESS's observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V=11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c and TOI-125d. TOI-125b has an orbital period of 4.65 days, a radius of $2.726 \pm 0.075 ~\mathrm{R_{\rm E}}$, a mass of $ 9.50 \pm 0.88 ~\mathrm{M_{\rm E}}$ and is near the 2:1 mean motion resonance with TOI-125c at 9.15 days. TOI-125c has a similar radius of $2.759 \pm 0.10 ~\mathrm{R_{\rm E}}$ and a mass of $ 6.63 \pm 0.99 ~\mathrm{M_{\rm E}}$, being the puffiest of the three planets. TOI-125d, has an orbital period of 19.98 days and a radius of $2.93 \pm 0.17~\mathrm{R_{\rm E}}$ and mass $13.6 \pm 1.2 ~\mathrm{M_{\rm E}}$. For TOI-125b and TOI-125d we find unusual high eccentricities of $0.19\pm 0.04$ and $0.17^{+0.08}_{-0.06}$, respectively. Our analysis also provides upper mass limits for the two low-SNR planet candidates in the system; for TOI-125.04 ($R_P=1.36 ~\mathrm{R_{\rm E}}$, $P=$0.53 days) we find a $2\sigma$ upper mass limit of $1.6~\mathrm{M_{\rm E}}$, whereas TOI-125.05 ( $R_P=4.2^{+2.4}_{-1.4} ~\mathrm{R_{\rm E}}$, $P=$ 13.28 days) is unlikely a viable planet candidate with upper mass limit $2.7~\mathrm{M_{\rm E}}$. We discuss the internal structure of the three confirmed planets, as well as dynamical stability and system architecture for this intriguing exoplanet system., Comment: Accepted for publication in MNRAS
Published: 2020

14. TESS Reveals a Short-period Sub-Neptune Sibling (HD 86226c) to a Known Long-period Giant Planet

Author: J. Haldemann, Eric L. N. Jensen, Enric Palle, Damien Ségransan, Roland Vanderspek, James S. Jenkins, Rafael Luque, Coel Hellier, Caroline Dorn, Matías R. Díaz, Johanna Teske, Stephen A. Shectman, Maxime Marmier, Ian Wong, Erin Flowers, Sara Seager, David W. Latham, Sharon X. Wang, Louise D. Nielsen, Julia V. Seidel, Joshua N. Winn, Douglas A. Caldwell, Stephen R. Kane, Ravit Helled, François Bouchy, Nicholas M. Law, Mark E. Rose, Kevin I. Collins, Jack J. Lissauer, Andrew W. Mann, Avi Shporer, Angie Wolfgang, J. F. Otegi, David R. Anderson, George R. Ricker, Jeffrey D. Crane, Jason D. Eastman, Karen A. Collins, Jennifer Burt, Stéphane Udry, Teo Mocnik, Carl Ziegler, Guillermo Torres, Fabo Feng, R. Paul Butler, Thomas Barclay, and Jon M. Jenkins
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Neptune, Long period, 0103 physical sciences, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB600, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), European research, Astronomy and Astrophysics, Space and Planetary Science, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, Administration (government), Humanities, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite mission was designed to find transiting planets around bright, nearby stars. Here we present the detection and mass measurement of a small, short-period ($\approx\,4$\,days) transiting planet around the bright ($V=7.9$), solar-type star HD 86226 (TOI-652, TIC 22221375), previously known to host a long-period ($\sim$1600 days) giant planet. HD 86226c (TOI-652.01) has a radius of $2.16\pm0.08$ $R_{\oplus}$ and a mass of 7.25$^{+1.19}_{-1.12}$ $M_{\oplus}$ based on archival and new radial velocity data. We also update the parameters of the longer-period, not-known-to-transit planet, and find it to be less eccentric and less massive than previously reported. The density of the transiting planet is $3.97$ g cm$^{-3}$, which is low enough to suggest that the planet has at least a small volatile envelope, but the mass fractions of rock, iron, and water are not well-constrained. Given the host star brightness, planet period, and location of the planet near both the ``radius gap'' and the ``hot Neptune desert'', HD 86226c is an interesting candidate for transmission spectroscopy to further refine its composition., Accepted in AJ on 22 June 2020
Published: 2020
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15. Impact of the measured parameters of exoplanets on the inferred internal structure

Author: J. F. Otegi, J. Haldemann, François Bouchy, Yann Alibert, Caroline Dorn, Ravit Helled, University of Zurich, and Otegi, J F
Subjects: 010504 meteorology & atmospheric sciences, 530 Physics, Posterior probability, Exoplanetology, FOS: Physical sciences, Bayesian inference, 01 natural sciences, 1912 Space and Planetary Science, Planet, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, Nested sampling algorithm, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Entropy (statistical thermodynamics), 520 Astronomy, Astronomy and Astrophysics, Radius, 500 Science, 620 Engineering, Exoplanet, 13. Climate action, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Exoplanet characterization is one of the main foci of current exoplanetary science. For super-Earths and sub-Neptunes, we mostly rely on mass and radius measurements, which allow to derive the body's mean density and give a rough estimate of the planet's bulk composition. However, the determination of planetary interiors is a very challenging task. In addition to the uncertainty in the observed fundamental parameters, theoretical models are limited due to the degeneracy in determining the planetary composition. We aim to study several aspects that affect internal characterization of super-Earths and sub-Neptunes: observational uncertainties, location on the M-R diagram, impact of additional constraints as bulk abundances or irradiation, and model assumptions. We use a full probabilistic Bayesian inference analysis that accounts for observational and model uncertainties. We employ a Nested Sampling scheme to efficiently produce the posterior probability distributions for all the planetary structural parameter of interest. We include a structural model based on self-consistent thermodynamics of core, mantle, high-pressure ice, liquid water, and H-He envelope. Regarding the effect of mass and radius uncertainties on the determination of the internal structure, we find three different regimes: below the Earth-like composition line and above the pure-water composition line smaller observational uncertainties lead to better determination of the core and atmosphere mass respectively, and between them structure characterization only weakly depends on the observational uncertainties. We show that small variations in the temperature or entropy profiles lead to radius variations that are comparable to the observational uncertainty, suggesting that uncertainties linked to model assumptions can become more relevant to determine the internal structure than observational uncertainties., Comment: 12 pages, 12 figures
Published: 2020
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16. Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b

Author: Z. Csubry, C. Lovis, Matthew R. Burleigh, Damien Ségransan, George R. Ricker, L. A. dos Santos, Norio Narita, Jack S. Acton, Oliver Turner, Logan Pearce, Motohide Tamura, James McCormac, James S. Jenkins, K. I. Collins, Sara Seager, Paula Sarkis, Liam Raynard, K. A. Collins, Th. Henning, F. Pozuelos, David W. Latham, Diana Kossakowski, Avi Shporer, Roland Vanderspek, Tianjun Gan, Trifon Trifonov, Jon M. Jenkins, Mayuko Mori, Andrew Vanderburg, Khalid Barkaoui, Michaël Gillon, Néstor Espinoza, M. Stalport, Chelsea X. Huang, François Bouchy, Stéphane Udry, Baptiste Lavie, David R. Ciardi, Rhodes Hart, Maximiliano Moyano, Emmanuel Jehin, Andrés Jordán, Rosanna H. Tilbrook, G. Wingham, David J. Osip, Cesar Briceno, Monika Lendl, Michael Fausnaugh, Gáspár Á. Bakos, Benjamin F. Cooke, Saul Rappaport, Julia V. Seidel, Christopher Stockdale, Vincent Suc, Eric B. Ting, Natalia Guerrero, J. P. de Leon, John F. Kielkopf, Janis Hagelberg, Howard M. Relles, Zhuchang Zhan, Nicholas M. Law, Rafael Brahm, Joshua N. Winn, Thiam-Guan Tan, Waqas Bhatti, Peter J. Wheatley, Louise D. Nielsen, Ph. Eigmüller, Edward M. Bryant, C. Ziegler, Francesco Pepe, Andrew W. Mann, Maxime Marmier, Thomas Barclay, M. R. Goad, and J. F. Otegi
Subjects: Extrasolare Planeten und Atmosphären, Physics, planets and satellites: detection, planets and satellites: individual: TOI-129, media_common.quotation_subject, planets and satellites: individual: HIP 65A, planets and satellites: individual: TOI-157, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Neptune, Sky, Planet, 0103 physical sciences, Hot Jupiter, Roche lobe, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, media_common
Abstract: We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V = 11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 ± 0.078 MJ planet in a grazing transit configuration with an impact parameter of b = 1.17−0.08+0.10. As a result the radius is poorly constrained, 2.03−0.49+0.61RJ. The planet’s distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs′ = 107 − 109. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 ± 0.13 MJ and a radius of 1.29 ± 0.02 RJ. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V = 12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V = 12.4 G-type star. It has a mass of 0.79 ±0.06 MJ and a radius of 1.09−0.05+0.08RJ. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe / H] ranging from 0.18 to0.24.
Published: 2020
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17. Revisited mass-radius relations for exoplanets below 120 M⊕

Author: J. F. Otegi, Ravit Helled, and François Bouchy
Subjects: Physics, education.field_of_study, 010504 meteorology & atmospheric sciences, Diagram, Population, Astronomy and Astrophysics, Radius, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Space and Planetary Science, Planet, 0103 physical sciences, Range (statistics), education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract: The masses and radii of exoplanets are fundamental quantities needed for their characterisation. Studying the different populations of exoplanets is important for understanding the demographics of the different planetary types, which can then be linked to planetary formation and evolution. We present an updated exoplanet catalogue based on reliable, robust, and, as much as possible accurate mass and radius measurements of transiting planets up to 120 M⊕. The resulting mass-radius (M-R) diagram shows two distinct populations, corresponding to rocky and volatile-rich exoplanets which overlap in both mass and radius. The rocky exoplanet population shows a relatively small density variability and ends at mass of ~25 M⊕, possibly indicating the maximum core mass that can be formed. We use the composition line of pure water to separate the two populations, and infer two new empirical M-R relations based on this data: M = (0.9 ± 0.06) R(3.45±0.12) for the rocky population, and M = (1.74 ± 0.38) R(1.58±0.10) for the volatile-rich population. While our results for the two regimes are in agreement with previous studies, the new M-R relations better match the population in the transition region from rocky to volatile-rich exoplanets, which correspond to a mass range of 5–25 M⊕, and a radius range of 2–3 R⊕.
Published: 2020

18. A Jovian planet in an eccentric 11.5 day orbit around HD1397 discovered by TESS

Author: Peter Plavchan, C. G. Tinney, Douglas A. Caldwell, A. Suárez Mascareño, M. Stalport, Stephen R. Kane, H. Giles, J. F. Otegi, Stéphane Udry, C. A. Beichman, James E Francis, Chengxi Huang, Matthew W. Mengel, Erica J. Gonzales, George R. Ricker, Ian Crossfield, Francesco Pepe, C. Lovis, Damien Ségransan, Sara Seager, Rachel A. Matson, Joshua Pepper, Mark E. Rose, Scott Cartwright, François Bouchy, Jake T. Clark, Jonathan Horner, David R. Ciardi, Keivan G. Stassun, John F. Kielkopf, Robert A. Wittenmyer, J. Villasenor, Louise D. Nielsen, Steve B. Howell, Brett C. Addison, Jack Okumura, Hui Zhang, Maxime Marmier, Karen A. Collins, Duncan J. Wright, David W. Latham, Elisabeth Matthews, G. Ottoni, Roland Vanderspek, Joshua E. Schlieder, Natalia Guerrero, Joshua N. Winn, Oliver Turner, Jon M. Jenkins, Brendan P. Bowler, B. Wohler, and Timothy D. Morton
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Subgiant, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, 01 natural sciences, Exoplanet, Jovian, Radial velocity, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite TESS has begun a new age of exoplanet discoveries around bright host stars. We present the discovery of HD 1397b (TOI-120.01), a giant planet in an 11.54day eccentric orbit around a bright (V=7.9) G-type subgiant. We estimate both host star and planetary parameters consistently using EXOFASTv2 based on TESS time-series photometry of transits and CORALIE radial velocity measurements. We find that HD 1397b is a Jovian planet, with a mass of $0.419\pm-0.024$ M$_{\rm Jup}$ and a radius of $1.023^{+0.023}_{-0.026$}$ R$_{\rm Jup}$. Characterising giant planets in short-period eccentric orbits, such as HD 1397b, is important for understanding and testing theories for the formation and migration of giant planets as well as planet-star interactions., Accepted for publication in A&A
Published: 2018

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

Author: 'J. F. Otegi

20. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Author: Xavier Dumusque, Jon M. Jenkins, Jason D. Eastman, Ravit Helled, Samuel N. Quinn, M. Soto, Elisabeth Matthews, Roland Vanderspek, J. Haldemann, Jennifer Burt, Maximilian N. Günther, Sara Seager, Stephen A. Shectman, Karen A. Collins, Thiam-Guan Tan, George Zhou, Fabo Feng, Tansu Daylan, R. Paul Butler, George R. Ricker, Andrew Vanderburg, Sharon X. Wang, Keivan G. Stassun, Julia V. Seidel, Louise D. Nielsen, Joseph E. Rodriguez, Laura Kreidberg, Erin Flowers, Thomas Barclay, Jeffrey D. Crane, Jeffrey C. Smith, Gilbert A. Esquerdo, Benjamin T. Montet, Chelsea X. Huang, Eric E. Mamajek, Eric L. N. Jensen, Peter Tenenbaum, John F. Kielkopf, Tianjun Gan, Samuel Halverson, François Bouchy, Jack J. Lissauer, Damien Segransen, David W. Latham, Adina D. Feinstein, Caroline Dorn, Joshua Pepper, Johanna Teske, Eric D. Lopez, Joshua N. Winn, Dennis M. Conti, Kevin I. Collins, Joseph D. Twicken, J. F. Otegi, Scott Cartwright, Yuri Beletski, and William Fong
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Star (game theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Exoplanet, Radial velocity, Atmosphere, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planet, Neptune, 0103 physical sciences, Hot Neptune, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the \textit{Transiting Exoplanet Survey Satellite} (TESS). The newly discovered planet has a radius, $R_{\rm{p}}$ = 2.93 $\pm$ 0.20 R$_{\oplus}$, and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph (PFS) and the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph confirm the existence of the planet and we estimate its mass to be $M_{\rm{p}}$ = 18.47 $\pm$ 1.84 M$_{\oplus}$. The planet's mean density is $\rho_{\rm{p}}$ = 4.03$^{+0.98}_{-0.78}$ g cm$^{-3}$ making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud free atmosphere, and thus an excellent candidate for follow up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated, small planet at the edge of the hot Neptune desert that has retained its atmosphere to date., Comment: 22 pages, 10 figures. Accepted for publication in the Astronomical Journal
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21. 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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22. The HD 137496 system: A dense, hot super-Mercury and a cold Jupiter

Author: Pedro Figueira, T. A. Silva, Nuno C. Santos, David Barrado, Caroline Dorn, Xavier Dumusque, S. Hojjatpanah, Keivan G. Stassun, S. G. Sousa, A. Hadjigeorghiou, E. Delgado-Mena, Isabelle Boisse, V. Adibekyan, O. Mousis, Diego Bossini, D. J. A. Brown, J. F. Otegi, Jose-Manuel Almenara, P. A. Strøm, Jorge Lillo-Box, David J. Armstrong, Daniel Bayliss, Louise D. Nielsen, S. C. C. Barros, Olivier Demangeon, Rodrigo F. Díaz, Stéphane Udry, Peter J. Wheatley, Sergio Hoyer, A. Osborn, Alexandre Santerne, 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), European Southern Observatory (ESO), 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), University of Warwick [Coventry], Instituto de Astrofísica e Ciências do Espaço (IASTRO), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, University of St Andrews [Scotland], Faculdade de Ciências [Lisboa], Universidade de Lisboa = University of Lisbon (ULISBOA), 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), Institut für Virologie, Philipps University, Vanderbilt University [Nashville], 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, Department of Physics [Coventry], Centro de Astrobiologia [Madrid] (CAB), and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, planets and satellites: detection, stars: individual: HD 137496, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Gas giant, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Star (game theory), Giant planet, planets and satellites: composition, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, Jupiter, Photometry (astronomy), techniques: photometric, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Planet, Neptune, techniques: radial velocities, QC, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract: Most of the currently known planets are small worlds with radii between that of the Earth and that of Neptune. The characterization of planets in this regime shows a large diversity in compositions and system architectures, with distributions hinting at a multitude of formation and evolution scenarios. Using photometry from the K2 satellite and radial velocities measured with the HARPS and CORALIE spectrographs, we searched for planets around the bright and slightly evolved Sun-like star HD 137496. We precisely estimated the stellar parameters, $M_*$ = 1.035 +/- 0.022 $M_\odot$, $R_*$ = 1.587 +/- 0.028 $R_\odot$, $T_\text{eff}$ = 5799 +/- 61 K, together with the chemical composition of the slightly evolved star. We detect two planets orbiting HD 137496. The inner planet, HD 137496 b, is a super-Mercury (an Earth-sized planet with the density of Mercury) with a mass of $M_b$ = 4.04 +/- 0.55 $M_\oplus$, a radius of $R_b = 1.31_{-0.05}^{+0.06} R_\oplus,$ and a density of $\rho_b = 10.49_{-1.82}^{+2.08}$ $\mathrm{g cm^{-3}}$. With an interior modeling analysis, we find that the planet is composed mainly of iron, with the core representing over 70% of the planet's mass ($M_{core}/M_{total} = 0.73^{+0.11}_{-0.12}$). The outer planet, HD 137496 c, is an eccentric ($e$ = 0.477 +/- 0.004), long period ($P$ = $479.9_{-1.1}^{+1.0}$ days) giant planet ($M_c\sin i_c$ = 7.66 +/- 0.11 $M_{Jup}$) for which we do not detect a transit. HD 137496 b is one of the few super-Mercuries detected to date. The accurate characterization reported here enhances its role as a key target to better understand the formation and evolution of planetary systems. The detection of an eccentric long period giant companion also reinforces the link between the presence of small transiting inner planets and long period gas giants., Comment: 20 pages, 14 figures, 10 tables. To be published in A&A
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22 results on '"J. F. Otegi"'

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

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

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

4. Mass Determinations of the Three Mini-Neptunes Transiting TOI-125

5. GJ 3090 b: one of the most favourable mini-Neptune for atmospheric characterisation

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

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

8. TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

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

10. Impact of the measured parameters of exoplanets on the inferred internal structure

11. A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)

12. The impact of exoplanets' measured parameters on the inferred internal structure

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

14. TESS Reveals a Short-period Sub-Neptune Sibling (HD 86226c) to a Known Long-period Giant Planet

15. Impact of the measured parameters of exoplanets on the inferred internal structure

16. Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b

17. Revisited mass-radius relations for exoplanets below 120 M⊕

18. A Jovian planet in an eccentric 11.5 day orbit around HD1397 discovered by TESS

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

20. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

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

22. The HD 137496 system: A dense, hot super-Mercury and a cold Jupiter

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22 results on '"J. F. Otegi"'

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