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41 results on '"Benjamin F Cooke"'

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

Author: Ares Osborn, David J Armstrong, Bryson Cale, Rafael Brahm, Robert A Wittenmyer, Fei Dai, Ian J M Crossfield, Edward M Bryant, Vardan Adibekyan, Ryan Cloutier, Karen A Collins, E Delgado Mena, Malcolm Fridlund, Coel Hellier, Steve B Howell, George W King, Jorge Lillo-Box, Jon Otegi, S Sousa, Keivan G Stassun, Elisabeth C Matthews, Carl Ziegler, George Ricker, Roland Vanderspek, David W Latham, S Seager, Joshua N Winn, Jon M Jenkins, Jack S Acton, Brett C Addison, David R Anderson, Sarah Ballard, David Barrado, Susana C C Barros, Natalie Batalha, Daniel Bayliss, Thomas Barclay, Björn Benneke, John Berberian, Francois Bouchy, Brendan P Bowler, César Briceño, Christopher J Burke, Matthew R Burleigh, Sarah L Casewell, David Ciardi, Kevin I Collins, Benjamin F Cooke, Olivier D S Demangeon, Rodrigo F Díaz, C Dorn, Diana Dragomir, Courtney Dressing, Xavier Dumusque, Néstor Espinoza, P Figueira, Benjamin Fulton, E Furlan, E Gaidos, C Geneser, Samuel Gill, Michael R Goad, Erica J Gonzales, Varoujan Gorjian, Maximilian N Günther, Ravit Helled, Beth A Henderson, Thomas Henning, Aleisha Hogan, Saeed Hojjatpanah, Jonathan Horner, Andrew W Howard, Sergio Hoyer, Dan Huber, Howard Isaacson, James S Jenkins, Eric L N Jensen, Andrés Jordán, Stephen R Kane, Richard C Kidwell, John Kielkopf, Nicholas Law, Monika Lendl, M Lund, Rachel A Matson, Andrew W Mann, James McCormac, Matthew W Mengel, Farisa Y Morales, Louise D Nielsen, Jack Okumura, Hugh P Osborn, Erik A Petigura, Peter Plavchan, Don Pollacco, Elisa V Quintana, Liam Raynard, Paul Robertson, Mark E Rose, Arpita Roy, Michael Reefe, Alexandre Santerne, Nuno C Santos, Paula Sarkis, J Schlieder, Richard P Schwarz, Nicholas J Scott, Avi Shporer, A M S Smith, C Stibbard, Chris Stockdale, Paul A Strøm, Joseph D Twicken, Thiam-Guan Tan, A Tanner, J Teske, Rosanna H Tilbrook, C G Tinney, Stephane Udry, Jesus Noel Villaseñor, Jose I Vines, Sharon X Wang, Lauren M Weiss, Richard G West, Peter J Wheatley, Duncan J Wright, Hui Zhang, and F Zohrabi
Published: 2021
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2. NGTS J214358.5−380102 – NGTS discovery of the most eccentric known eclipsing M-dwarf binary system

Author: Jack S Acton, Michael R Goad, Liam Raynard, Sarah L Casewell, James A G Jackman, Richard D Alexander, David R Anderson, Daniel Bayliss, Edward M Bryant, Matthew R Burleigh, Claudia Belardi, Benjamin F Cooke, Philipp Eigmüller, Samuel Gill, James S Jenkins, Monika Lendl, Tom Louden, James McCormac, Maximiliano Moyano, Louise D Nielsen, Rosanna H Tilbrook, Stéphane Udry, Christopher A Watson, Richard G West, Peter J Wheatley, and Jose I Vines
Published: 2020
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3. HD 213885b: a transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS

Author: Néstor Espinoza, Rafael Brahm, Thomas Henning, Andrés Jordán, Caroline Dorn, Felipe Rojas, Paula Sarkis, Diana Kossakowski, Martin Schlecker, Matías R Díaz, James S Jenkins, Claudia Aguilera-Gomez, Jon M Jenkins, Joseph D Twicken, Karen A Collins, Jack Lissauer, David J Armstrong, Vardan Adibekyan, David Barrado, Susana C C Barros, Matthew Battley, Daniel Bayliss, François Bouchy, Edward M Bryant, Benjamin F Cooke, Olivier D S Demangeon, Xavier Dumusque, Pedro Figueira, Helen Giles, Jorge Lillo-Box, Christophe Lovis, Louise D Nielsen, Francesco Pepe, Don Pollacco, Nuno C Santos, Sergio G Sousa, Stéphane Udry, Peter J Wheatley, Oliver Turner, Maxime Marmier, Damien Ségransan, George Ricker, David Latham, Sara Seager, Joshua N Winn, John F Kielkopf, Rhodes Hart, Geof Wingham, Eric L N Jensen, Krzysztof G Hełminiak, A Tokovinin, C Briceño, Carl Ziegler, Nicholas M Law, Andrew W Mann, Tansu Daylan, John P Doty, Natalia Guerrero, Patricia Boyd, Ian Crossfield, Robert L Morris, Christopher E Henze, and Aaron Dean Chacon
Published: 2019
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4. NGTS-6b: an ultrashort period hot-Jupiter orbiting an old K dwarf

Author: Jose I Vines, James S Jenkins, Jack S Acton, Joshua Briegal, Daniel Bayliss, François Bouchy, Claudia Belardi, Edward M Bryant, Matthew R Burleigh, Juan Cabrera, Sarah L Casewell, Alexander Chaushev, Benjamin F Cooke, Szilárd Csizmadia, Philipp Eigmüller, Anders Erikson, Emma Foxell, Samuel Gill, Edward Gillen, Michael R Goad, James A G Jackman, George W King, Tom Louden, James McCormac, Maximiliano Moyano, Louise D Nielsen, Don Pollacco, Didier Queloz, Heike Rauer, Liam Raynard, Alexis M S Smith, Maritza G Soto, Rosanna H Tilbrook, Ruth Titz-Weider, Oliver Turner, Stéphane Udry, Simon R Walker, Christopher A Watson, Richard G West, and Peter J Wheatley
Published: 2019
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5. A remnant planetary core in the hot-Neptune desert

Author: David J. Armstrong, Théo A. Lopez, Vardan Adibekyan, Richard A. Booth, Edward M. Bryant, Karen A. Collins, Magali Deleuil, Alexandre Emsenhuber, Chelsea X. Huang, George W. King, Jorge Lillo-Box, Jack J. Lissauer, Elisabeth Matthews, Olivier Mousis, Louise D. Nielsen, Hugh Osborn, Jon Otegi, Nuno C. Santos, Sérgio G. Sousa, Keivan G. Stassun, Dimitri Veras, Carl Ziegler, Jack S. Acton, Jose M. Almenara, David R. Anderson, David Barrado, Susana C. C. Barros, Daniel Bayliss, Claudia Belardi, Francois Bouchy, César Briceño, Matteo Brogi, David J. A. Brown, Matthew R. Burleigh, Sarah L. Casewell, Alexander Chaushev, Kevin I. Collins, Knicole D. Colón, Benjamin F. Cooke, Ian J. M. Crossfield, Rodrigo F. Díaz, Elisa Delgado Mena, Olivier D. S. Demangeon, Caroline Dorn, Xavier Dumusque, Philipp Eigmüller, Michael Fausnaugh, Pedro Figueira, Tianjun Gan, Siddharth Gandhi, Samuel Gill, Erica J. Gonzales, Michael R. Goad, Ravit Helled, Saeed Hojjatpanah, Steve B. Howell, James Jackman, James S. Jenkins, Jon M. Jenkins, Eric L. N. Jensen, Grant M. Kennedy, David W. Latham, Nicholas Law, Monika Lendl, Michael Lozovsky, Andrew W. Mann, Maximiliano Moyano, James McCormac, Farzana Meru, Christoph Mordasini, Ares Osborn, Don Pollacco, Didier Queloz, Liam Raynard, George R. Ricker, Pamela Rowden, Alexandre Santerne, Joshua E. Schlieder, Sara Seager, Lizhou Sha, Thiam-Guan Tan, Rosanna H. Tilbrook, Eric Ting, Stéphane Udry, Roland Vanderspek, Christopher A. Watson, Richard G. West, Paul A. Wilson, Joshua N. Winn, Peter Wheatley, Jesus Noel Villasenor, Jose I. Vines, and Zhuchang Zhan
Subjects: Exobiology, Lunar And Planetary Science And Exploration
Abstract: The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune ‘desert’ (a region in mass–radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b and NGTS-4b, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune’s but an anomalously large mass of 39.1(+2.7−2.6) Earth masses and a density of 5.2(+0.7−0.8) grams per cubic centimetre, similar to Earth’s. Interior-structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9(+0.8−0.9) per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet.
Published: 2020
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6. NGTS-2b: an inflated hot-Jupiter transiting a bright F-dwarf

Author: Liam Raynard, Michael R Goad, Edward Gillen, Louise D Nielsen, Christopher A Watson, Andrew P G Thompson, James McCormac, Daniel Bayliss, Maritza Soto, Szilard Csizmadia, Alexander Chaushev, Matthew R Burleigh, Richard Alexander, David J Armstrong, François Bouchy, Joshua T Briegal, Juan Cabrera, Sarah L Casewell, Bruno Chazelas, Benjamin F Cooke, Philipp Eigmüller, Anders Erikson, Boris T Gänsicke, Andrew Grange, Maximilian N Günther, Simon T Hodgkin, Matthew J Hooton, James S Jenkins, Gregory Lambert, Tom Louden, Lionel Metrailler, Maximiliano Moyano, Don Pollacco, Katja Poppenhaeger, Didier Queloz, Roberto Raddi, Heike Rauer, Andrew M Read, Barry Smalley, Alexis M S Smith, Oliver Turner, Stéphane Udry, Simon R Walker, Richard G West, and Peter J Wheatley
Published: 2018
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7. NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event

Author: Samuel Gill, Peter J. Wheatley, Benjamin F. Cooke, Andrés Jordán, Louise D. Nielsen, Daniel Bayliss, David R. Anderson, Jose I. Vines, Monika Lendl, Jack S. Acton, David J. Armstrong, François Bouchy, Rafael Brahm, Edward M. Bryant, Matthew R. Burleigh, Sarah L. Casewell, Philipp Eigmüller, Néstor Espinoza, Edward Gillen, Michael R. Goad, Nolan Grieves, Maximilian N. Günther, Thomas Henning, Melissa J. Hobson, Aleisha Hogan, James S. Jenkins, James McCormac, Maximiliano Moyano, Hugh P. Osborn, Don Pollacco, Didier Queloz, Heike Rauer, Liam Raynard, Felipe Rojas, Paula Sarkis, Alexis M. S. Smith, Marcelo Tala Pinto, Rosanna H. Tilbrook, Stéphane Udry, Christopher A. Watson, and Richard G. West
Published: 2020
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8. A transit timing variation observed for the long-period extremely low-density exoplanet HIP 41378 f

Author: J. I. Vines, Chris Stockdale, Samantha Thompson, Michaël Gillon, Sarah L. Casewell, Richard G. West, C. Murray, Akihiko Fukui, Julien de Wit, Stéphane Udry, Rosanna H. Tilbrook, David J. Armstrong, Douglas R. Alves, L. Delrez, Benjamin V. Rackham, Edward M. Bryant, Valerio Nascimbeni, David R. Anderson, Samuel Gill, Matthew R. Burleigh, Enric Palle, Elsa Ducrot, Maximiliano Moyano, P. P. Pedersen, Monika Lendl, Peter J. Wheatley, Molly R. Kosiarek, Michael R. Goad, James S. Jenkins, Thiam-Guan Tan, Brice-Olivier Demory, Jack S. Acton, Amaury H. M. J. Triaud, Daniel Bayliss, Prajwal Niraula, Beth A. Henderson, Tianjun Gan, Norio Narita, Caroline Odden, Bronwen J. Hardee, Alexandre Santerne, Philipp Eigmüller, Maximilian N. Günther, A. Burdanov, D. Sebastian, Benjamin F. Cooke, Supachai Awiphan, Francisco J. Pozuelos, Hannu Parviainen, Emmanuel Jehin, 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), University of Warwick [Coventry], Institut d'Optique Graduate School (IOGS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, National Astronomical Research Institute of Thailand (NARIT), Department of Physics and Astronomy [Leicester], University of Leicester, Cavendish Laboratory, University of Cambridge [UK] (CAM), Center for Space and Habitability (CSH), University of Bern, The University of Tokyo (UTokyo), Instituto de Astrofisica de Canarias (IAC), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Universidad de Chile = University of Chile [Santiago] (UCHILE), Department of Astronomy and Astrophysics [UCSC Santa Cruz], University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Austrian Academy of Sciences (OeAW), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatoire Astronomique de l'Université de Genève (ObsGE), and Université de Genève = University of Geneva (UNIGE)
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, techniques: photometric, Planet, Long period, 0103 physical sciences, Low density, Transit (astronomy), 10. No inequality, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, planets and satellites: individual: HIP 41378 f, Transit-timing variation, 010308 nuclear & particles physics, 520 Astronomy, Astronomy and Astrophysics, Orbital period, Exoplanet, Photometry (astronomy), 13. Climate action, Space and Planetary Science, stars: individual: HIP 41378, Astrophysics - Earth and Planetary Astrophysics
Abstract: HIP 41378 f is a temperate $9.2\pm0.1 R_{\oplus}$ planet with period of 542.08 days and an extremely low density of $0.09\pm0.02$ g cm$^{-3}$. It transits the bright star HIP 41378 (V=8.93), making it an exciting target for atmospheric characterization including transmission spectroscopy. HIP 41378 was monitored photometrically between the dates of 2019 November 19 and November 28. We detected a transit of HIP 41378 f with NGTS, just the third transit ever detected for this planet, which confirms the orbital period. This is also the first ground-based detection of a transit of HIP 41378 f. Additional ground-based photometry was also obtained and used to constrain the time of the transit. The transit was measured to occur 1.50 hours earlier than predicted. We use an analytic transit timing variation (TTV) model to show the observed TTV can be explained by interactions between HIP 41378 e and HIP 41378 f. Using our TTV model, we predict the epochs of future transits of HIP 41378 f, with derived transit centres of T$_{C,4} = 2459355.087^{+0.031}_{-0.022}$ (May 2021) and T$_{C,5} = 2459897.078^{+0.114}_{-0.060}$ (Nov 2022)., Comment: Accepted for publication in MNRAS Letters. 6 pages, 2 figures
Published: 2021
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9. NGTS 15b, 16b, 17b, and 18b: four hot Jupiters from the Next-Generation Transit Survey

Author: Jessymol K. Thomas, Stéphane Udry, Alexander Chaushev, Matthew R. Burleigh, Louise D. Nielsen, Alexis M. S. Smith, Michael R. Goad, Richard G. West, James McCormac, Liam Raynard, James S. Jenkins, Sarah L. Casewell, Benjamin F. Cooke, Rosanna H. Tilbrook, François Bouchy, Ramotholo Sefako, Peter J. Wheatley, Beth A. Henderson, Joshua T. Briegal, Christopher A. Watson, Jose I. Vines, Daniel Bayliss, J. Costes, Jack S. Acton, Hannah L. Worters, Simon Hodgkin, Didier Queloz, H. Breytenbach, Samuel Gill, Maximiliano Moyano, Monika Lendl, Edward Gillen, David R. Anderson, Maximilian N. Günther, Philipp Eigmüller, Aleisha Hogan, David J. Armstrong, Douglas R. Alves, Edward M. Bryant, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Inflation (cosmology), planets and satellites: detection, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Planetary system, Parameter space, 01 natural sciences, planets and satellites: gaseous planets, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Transit (astronomy), 10. No inequality, planetary systems, 010303 astronomy & astrophysics, Main sequence, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of four new hot Jupiters with the Next Generation Transit Survey (NGTS). NGTS-15b, NGTS-16b, NGTS-17b, and NGTS-18b are short-period ($P, Accepted for publication in MNRAS
Published: 2021
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10. Resolving period aliases for TESS monotransits recovered during the extended mission

Author: Benjamin F. Cooke, Samuel Gill, Monika Lendl, Stéphane Udry, Don Pollacco, Peter J. Wheatley, David R. Anderson, François Bouchy, Nolan Grieves, Daniel Bayliss, and Louise D. Nielsen
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Alias, 010308 nuclear & particles physics, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Planetary system, Q1, 01 natural sciences, Exoplanet, Photometry (astronomy), Upgrade, Space and Planetary Science, Planet, QB460, 0103 physical sciences, Transit (astronomy), education, 010303 astronomy & astrophysics, QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract: We set out to explore how best to mitigate the number of period aliases for a transiting TESS system with two identified transits separated by a large time period on the order of years. We simulate a realistic population of doubly transiting planets based on the observing strategy of the TESS primary and extended missions. We next simulate additional observations using photometry (NGTS) and spectroscopy (HARPS and CORALIE) and assess its impact on the period aliases of systems with two TESS transits. We find that TESS will detect around 400 exoplanets that exhibit one transit in each of the primary and extended missions. Based on the temporal coverage, each of these systems will have an average of 38 period aliases. We find that, assuming a combination of NGTS and CORALIE over observing campaigns spanning 50 days, we can find the true alias, and thus solve the period, for up to 207 of these systems with even more being solved if the observing campaigns are extended or we upgrade to HARPS over CORALIE., 11 pages, 8 figures. Accepted for publication in MNRAS
Published: 2020
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11. specphot: a comparison of spectroscopic and photometric exoplanet follow-up methods

Author: Don Pollacco and Benjamin F. Cooke
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Rank (linear algebra), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Planetary system, Parameter space, 01 natural sciences, Exoplanet, Photometry (optics), symbols.namesake, Space and Planetary Science, Planet, 0103 physical sciences, symbols, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Doppler effect, Astrophysics - Earth and Planetary Astrophysics
Abstract: We set out a simulation to explore the follow-up of exoplanet candidates. We look at comparing photometric (transit method) and spectroscopic (Doppler shift method) techniques using three instruments: NGTS, HARPS and CORALIE. We take into account precision of follow-up and required observing time in attempt to rank each method for a given set of planetary system parameters. The methods are assessed on two criteria, SNR of the detection and follow-up time before characterisation. We find that different follow-up techniques are preferred for different regions of parameter space. For SNR we find that the ratio of spectroscopic to photometric SNR for a given system goes like $R_p/P^{\frac{1}{3}}$. For follow-up time we find that photometry is favoured for the shortest period systems ($, 10 pages, 7 figures. Accepted for publication in MNRAS
Published: 2020
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12. 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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13. 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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14. NGTS-14Ab: a Neptune-sized transiting planet in the desert

Author: Ph. Eigmüller, Edward M. Bryant, Rafael Brahm, Jack S. Acton, Samuel Gill, Aleisha Hogan, Maximiliano Moyano, Andrés Jordán, Monika Lendl, David R. Anderson, Alexander Chaushev, Sz. Csizmadia, Claudia Belardi, Benjamin F. Cooke, Maximilian N. Günther, Oliver Turner, Daniel Bayliss, Richard G. West, James McCormac, David J. Armstrong, Liam Raynard, Matthew R. Burleigh, Alexis M. S. Smith, Christopher A. Watson, Peter J. Wheatley, Anders Erikson, Jose I. Vines, Louise D. Nielsen, Juan Cabrera, François Bouchy, Rosanna H. Tilbrook, Heike Rauer, Edward Gillen, Michael R. Goad, Stéphane Udry, Beth A. Henderson, Joshua T. Briegal, and J. Costes
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, planets and satellites: individual: NGTS-14Ab, 010504 meteorology & atmospheric sciences, Stellar mass, FOS: Physical sciences, Context (language use), 01 natural sciences, Neptune, Planet, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, planetary systems, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Leitungsbereich PF, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Photometry (astronomy), binaries: general, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: The sub-Jovian or Neptunian desert is a previously-identified region of parameter space where there is a relative dearth of intermediate-mass planets at short orbital periods. Aims: We present the discovery of a new transiting planetary system within the Neptunian desert, NGTS-14. Methods: Transits of NGTS-14Ab were discovered in photometry from the Next Generation Transit Survey (NGTS). Follow-up transit photometry was conducted from several ground-based facilities, as well as extracted from TESS full-frame images. We combine radial velocities from the HARPS spectrograph with the photometry in a global analysis to determine the system parameters. Results: NGTS-14Ab has a radius about 30 per cent larger than that of Neptune ($0.444\pm0.030~\mathrm{R_{Jup}}$), and is around 70 per cent more massive than Neptune ($0.092 \pm 0.012~\mathrm{M_{Jup}}$). It transits the main-sequence K1 star, NGTS-14A, with a period of 3.54 days, just far enough to have maintained at least some of its primordial atmosphere. We have also identified a possible long-period stellar mass companion to the system, NGTS-14B, and we investigate the binarity of exoplanet host stars inside and outside the Neptunian desert using Gaia., 11 pages, 7 figures. Accepted for publication in A&A
Published: 2021
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15. 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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16. NGTS-13b: a hot 4.8 Jupiter-mass planet transiting a subgiant star

Author: Maximiliano Moyano, Andrés Jordán, Monika Lendl, Maximilian N. Günther, Peter J. Wheatley, Jack S. Acton, Beth A. Henderson, Sarah L. Casewell, Michael R. Goad, David R. Anderson, Alexander Chaushev, Samuel Gill, Richard G. West, James McCormac, Liam Raynard, Nolan Grieves, Didier Queloz, Julia V. Seidel, Jose I. Vines, Stéphane Udry, Louise D. Nielsen, François Bouchy, Rosanna H. Tilbrook, Benjamin F. Cooke, Daniel Bayliss, Matthew R. Burleigh, Damien Ségransan, P. Eigmueller, James S. Jenkins, Douglas R. Alves, Edward M. Bryant, Alexis M. S. Smith, Edward Gillen, Aleisha Hogan, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, 010504 meteorology & atmospheric sciences, planets and satellites: individual: NGTS-13b, Subgiant, Metallicity, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Accretion (astrophysics), Exoplanet, techniques: photometric, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, techniques: radial velocities, 010303 astronomy & astrophysics, Jupiter mass, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of the massive hot Jupiter NGTS-13b by the Next Generation Transit Survey (NGTS). The V = 12.7 host star is likely in the subgiant evolutionary phase with log g$_{*}$ = 4.04 $\pm$ 0.05, T$_{eff}$ = 5819 $\pm$ 73 K, M$_{*}$ = 1.30$^{+0.11}_{-0.18}$ M$_{\odot}$, and R$_{*}$ = 1.79 $\pm$ 0.06 R$_{\odot}$. NGTS detected a transiting planet with a period of P = 4.12 days around the star, which was later validated with the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame image photometry combined with CORALIE radial velocities we determine NGTS-13b to have a radius of R$_{P}$ = 1.142 $\pm$ 0.046 R$_{Jup}$, mass of M$_{P}$ = 4.84 $\pm$ 0.44 M$_{Jup}$ and eccentricity e = 0.086 $\pm$ 0.034. Some previous studies suggest that $\sim$4 M$_{Jup}$ may be a border between two separate formation scenarios (e.g., core accretion and disk instability) and that massive giant planets share similar formation mechanisms as lower-mass brown dwarfs. NGTS-13b is just above 4 M$_{Jup}$ making it an important addition to the statistical sample needed to understand the differences between various classes of substellar companions. The high metallicity, [Fe/H] = 0.25 $\pm$ 0.17, of NGTS-13 does not support previous suggestions that massive giants are found preferentially around lower metallicity host stars, but NGTS-13b does support findings that more massive and evolved hosts may have a higher occurrence of close-in massive planets than lower-mass unevolved stars., 11 pages, 9 figures, 4 tables, accepted by Astronomy & Astrophysics
Published: 2021
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17. NGTS-12b: A sub-Saturn mass transiting exoplanet in a 7.53 day orbit

Author: Benjamin F. Cooke, Jack S. Acton, Christopher A. Watson, Jose I. Vines, Maximilian N. Günther, Daniel Bayliss, Michael R. Goad, Samuel Gill, Richard G. West, James McCormac, David R. Anderson, Maximiliano Moyano, Sarah L. Casewell, Anders Erikson, Liam Raynard, Philipp Eigmüller, Monika Lendl, Juan Cabrera, Peter J. Wheatley, David J. Armstrong, Louise D. Nielsen, Aleisha Hogan, Heike Rauer, Dimitri Veras, Didier Queloz, François Bouchy, Edward Gillen, Szilard Csizmadia, Alexis M. S. Smith, Edward M. Bryant, Rosanna H. Tilbrook, Nolan Grieves, Beth A. Henderson, Joshua T. Briegal, Stéphane Udry, Alexander Chaushev, Matthew R. Burleigh, James S. Jenkins, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, Library science, FOS: Physical sciences, Q1, 01 natural sciences, techniques: photometric, Observatory, 0103 physical sciences, QB460, media_common.cataloged_instance, stars: individual: NGTS-12, European union, QA, 010303 astronomy & astrophysics, planetary systems, QB600, QC, media_common, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, European research, Leitungsbereich PF, Astronomy and Astrophysics, Exoplanet, Space and Planetary Science, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of the transiting exoplanet NGTS-12b by the Next Generation Transit Survey (NGTS). The host star, NGTS-12, is a V=12.38 mag star with an effective temperature of T$_{\rm eff}$=$5690\pm130$ K. NGTS-12b orbits with a period of $P=7.53$d, making it the longest period planet discovered to date by the main NGTS survey. We verify the NGTS transit signal with data extracted from the TESS full-frame images, and combining the photometry with radial velocity measurements from HARPS and FEROS we determine NGTS-12b to have a mass of $0.208\pm0.022$ M$_{J}$ and a radius of $1.048\pm0.032$ R$_{J}$. NGTS-12b sits on the edge of the Neptunian desert when we take the stellar properties into account, highlighting the importance of considering both the planet and star when studying the desert. The long period of NGTS-12b combined with its low density of just $0.223\pm0.029$ g cm$^{-3}$ make it an attractive target for atmospheric characterization through transmission spectroscopy with a Transmission Spectroscopy Metric of 89.4., Comment: Accepted for publication in MNRAS, 11 pages
Published: 2020

18. 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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19. 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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20. Simultaneous TESS and NGTS Transit Observations of WASP-166b

Author: Peter J. Wheatley, Jose I. Vines, Monika Lendl, Claudia Belardi, Rosie H. Tilbrook, Benjamin F. Cooke, Samuel Gill, Michael R. Goad, Alexis M. S. Smith, David R. Anderson, David J. Armstrong, Sarah L. Casewell, J. S. Acton, Didier Queloz, Don Pollacco, Edward M. Bryant, Daniel Bayliss, Matthew R. Burleigh, François Bouchy, Richard G. West, James McCormac, Liam Raynard, James S. Jenkins, Stéphane Udry, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, Physics::Instrumentation and Detectors, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ephemeris, 01 natural sciences, law.invention, Photometry (optics), Telescope, techniques: photometric, Planet, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Scintillation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, Light curve, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We observed a transit of WASP-166 b using nine NGTS telescopes simultaneously with TESS observations of the same transit. We achieved a photometric precision of 152 ppm per 30 minutes with the nine NGTS telescopes combined, matching the precision reached by TESS for the transit event around this bright (T=8.87) star. The individual NGTS light curve noise is found to be dominated by scintillation noise and appears free from any time-correlated noise or any correlation between telescope systems. We fit the NGTS data for $T_C$ and $R_p/R_*$. We find $T_C$ to be consistent to within 0.25$\sigma$ of the result from the TESS data, and the difference between the TESS and NGTS measured $R_p/R_*$ values is 0.9$\sigma$. This experiment shows that multi-telescope NGTS photometry can match the precision of TESS for bright stars, and will be a valuable tool in refining the radii and ephemerides for bright TESS candidates and planets. The transit timing achieved will also enable NGTS to measure significant transit timing variations in multi-planet systems., Comment: 10 pages, 8 figures. Accepted for publication in MNRAS
Published: 2020

21. 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
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22. 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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23. An Ultra-Hot Neptune in the Neptune desert

Author: Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, 010504 meteorology & atmospheric sciences, Leitungsbereich PF, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Northern ireland, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Political science, 0103 physical sciences, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Research center, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract: About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)
Published: 2020
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24. CHEOPS observations of TESS primary mission monotransits

Author: Andrea Fortier, Monika Lendl, Don Pollacco, Benjamin F. Cooke, and T. Kuntzer
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, media_common.quotation_subject, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Methods observational, 010309 optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Sky, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, media_common
Abstract: We set out to look at the overlap between CHEOPS sky coverage and TESS primary mission monotransits to determine what fraction of TESS monotransits may be observed by CHEOPS. We carry out a simulation of TESS transits based on the stellar population in TICv8 in the primary TESS mission. We then select the monotransiting candidates and determine their CHEOPS observing potential. We find that TESS will discover approximately 433 monotransits during its primary mission. Using a baseline observing efficiency of 40% we then find that 387 of these ($\sim$89%) will be observable by CHEOPS with an average observing time of $\sim$60 days per year. Based on the individual observing times and orbital periods of each system we predict that CHEOPS could observe additional transits for approximately 302 of the 433 TESS primary mission monotransits ($\sim$70%). Given that CHEOPS will require some estimate of period before observing a target we estimate that up to 250 ($\sim$58%) TESS primary mission monotransits could have solved periods prior to CHEOPS observations using a combination of photometry and spectroscopy., 7 pages, 8 figures. Accepted for publication in MNRAS
Published: 2020
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25. NGTS J214358.5−380102 – NGTS discovery of the most eccentric known eclipsing M-dwarf binary system

Author: Philipp Eigmüller, Benjamin F. Cooke, Matthew R. Burleigh, James S. Jenkins, Stéphane Udry, Sarah L. Casewell, Michael R. Goad, David R. Anderson, Richard G. West, James McCormac, Samuel Gill, Maximiliano Moyano, Liam Raynard, Monika Lendl, Louise D. Nielsen, Daniel Bayliss, Richard Alexander, Claudia Belardi, Rossanna H. Tilbrook, Tom Louden, Peter J. Wheatley, Jack S. Acton, James A. G. Jackman, Edward M. Bryant, Christopher A. Watson, and Jose I. Vines
Subjects: Physics, Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, European research, Library science, binaries: eclipsing, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, eclipsing [binaries], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Administration (government), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of NGTS J214358.5-380102, an eccentric M-dwarf binary discovered by the Next Generation Transit Survey. The system period of 7.618 days is greater than many known eclipsing M-dwarf binary systems. Its orbital eccentricity of $0.323^{+0.0014}_{-0.0037}$, is large relative to the period and semi-major axis of the binary. Global modelling of photometry and radial velocities indicate stellar masses of $M_A$=$0.426 ^{+0.0056}_{-0.0049}$, $M_B$=$0.455 ^{+0.0058}_{-0.0052}$ and stellar radii $R_A$=$0.461 ^{+0.038}_{-0.025}$ $R_B$=$0.411 ^{+0.027}_{-0.039}$, respectively. Comparisons with stellar models for low mass stars show that one star is consistent with model predictions whereas the other is substantially oversized. Spectral analysis of the system suggests a primary of spectral type M3V, consistent with both modelled masses and radii, and with SED fitting of NGTS photometry. As the most eccentric eclipsing M-dwarf binary known, NGTS J214358.5-380102 provides an interesting insight into the strength of tidal effects in the circularisation of stellar orbits., Comment: Accepted for Publication in MNRAS
Published: 2020
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26. A remnant planetary core in the hot-Neptune desert

Author: David J. Armstrong, Théo A. Lopez, Vardan Adibekyan, Richard A. Booth, Edward M. Bryant, Karen A. Collins, Magali Deleuil, Alexandre Emsenhuber, Chelsea X. Huang, George W. King, Jorge Lillo-Box, Jack J. Lissauer, Elisabeth Matthews, Olivier Mousis, Louise D. Nielsen, Hugh Osborn, Jon Otegi, Nuno C. Santos, Sérgio G. Sousa, Keivan G. Stassun, Dimitri Veras, Carl Ziegler, Jack S. Acton, Jose M. Almenara, David R. Anderson, David Barrado, Susana C. C. Barros, Daniel Bayliss, Claudia Belardi, Francois Bouchy, César Briceño, Matteo Brogi, David J. A. Brown, Matthew R. Burleigh, Sarah L. Casewell, Alexander Chaushev, David R. Ciardi, Kevin I. Collins, Knicole D. Colón, Benjamin F. Cooke, Ian J. M. Crossfield, Rodrigo F. Díaz, Elisa Delgado Mena, Olivier D. S. Demangeon, Caroline Dorn, Xavier Dumusque, Philipp Eigmüller, Michael Fausnaugh, Pedro Figueira, Tianjun Gan, Siddharth Gandhi, Samuel Gill, Erica J. Gonzales, Michael R. Goad, Maximilian N. Günther, Ravit Helled, Saeed Hojjatpanah, Steve B. Howell, James Jackman, James S. Jenkins, Jon M. Jenkins, Eric L. N. Jensen, Grant M. Kennedy, David W. Latham, Nicholas Law, Monika Lendl, Michael Lozovsky, Andrew W. Mann, Maximiliano Moyano, James McCormac, Farzana Meru, Christoph Mordasini, Ares Osborn, Don Pollacco, Didier Queloz, Liam Raynard, George R. Ricker, Pamela Rowden, Alexandre Santerne, Joshua E. Schlieder, Sara Seager, Lizhou Sha, Thiam-Guan Tan, Rosanna H. Tilbrook, Eric Ting, Stéphane Udry, Roland Vanderspek, Christopher A. Watson, Richard G. West, Paul A. Wilson, Joshua N. Winn, Peter Wheatley, Jesus Noel Villasenor, Jose I. Vines, Zhuchang Zhan, 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 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, Armstrong, David J [0000-0002-5080-4117], Collins, Karen A [0000-0001-6588-9574], Emsenhuber, Alexandre [0000-0002-8811-1914], Lillo-Box, Jorge [0000-0003-3742-1987], Lissauer, Jack J [0000-0001-6513-1659], Santos, Nuno C [0000-0003-4422-2919], Stassun, Keivan G [0000-0002-3481-9052], Veras, Dimitri [0000-0001-8014-6162], Barrado, David [0000-0002-5971-9242], Collins, Kevin I [0000-0003-2781-3207], Demangeon, Olivier DS [0000-0001-7918-0355], Dumusque, Xavier [0000-0002-9332-2011], Eigmüller, Philipp [0000-0003-4096-0594], Jenkins, Jon M [0000-0002-4715-9460], Jensen, Eric LN [0000-0002-4625-7333], Kennedy, Grant M [0000-0001-6831-7547], Mordasini, Christoph [0000-0002-1013-2811], Santerne, Alexandre [0000-0002-3586-1316], Seager, Sara [0000-0002-6892-6948], Sha, Lizhou [0000-0001-5401-8079], Udry, Stéphane [0000-0001-7576-6236], West, Richard G [0000-0001-6604-5533], Wilson, Paul A [0000-0002-7823-1090], Winn, Joshua N [0000-0002-4265-047X], Wheatley, Peter [0000-0003-1452-2240], Apollo - University of Cambridge Repository, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Collins, K. A. [0000-0002-4317-142X], Lillo Box, J. [0000-0003-3742-1987], Matthews, E. [0000-0003-0593-1560], Sousa, S. [0000-0002-3631-6440], National Aeronautics and Space Administration (NASA), Fundação para a Ciência e a Tecnologia (FCT), Agencia Estatal de Investigación (AEI), Science and Technology Facilities Council (STFC), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Unidad de Excelencia María de Maeztu del Instituto Nacional de Técnica Aeroespacial y CSIC, and French Programme National de Planetologie
Subjects: Extrasolare Planeten und Atmosphären, astro-ph.SR, 010504 meteorology & atmospheric sciences, Gas giant, 530 Physics, FOS: Physical sciences, TOI-849b, 01 natural sciences, Astrobiology, Planet, 0103 physical sciences, Planetary Core, Astrophysics::Solar and Stellar Astrophysics, Hot Neptune, Desert, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Multidisciplinary, Planetary core, 520 Astronomy, Giant planet, 620 Engineering, Accretion (astrophysics), Exoplanet, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, [SDU]Sciences of the Universe [physics], astro-ph.EP, Neptune, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune 'desert' (a region in mass-radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b and NGTS-4b, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune's but an anomalously large mass of $39.1^{+2.7}_{-2.6}$ Earth masses and a density of $5.2^{+0.7}_{-0.8}$ grams per cubic centimetre, similar to Earth's. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than $3.9^{+0.8}_{-0.9}$ per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet., Published in Nature. This is a preprint of the article, before minor changes made during the refereeing and editing process. The published PDF is at https://www.nature.com/articles/s41586-020-2421-7 and can be accessed for free by following this link: https://rdcu.be/b5miB . Abstract updated to match published version
Published: 2020
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27. Weighing in on the masses of retired A stars with asteroseismology: K2 observations of the exoplanet-host star HD 212771

Author: Tiago L. Campante, Mikkel N. Lund, Andrea Miglio, Benjamin F. Cooke, Guy R. Davies, T. S. Rodrigues, Yvonne Elsworth, William J. Chaplin, Thierry Morel, Andrew Vanderburg, Daniel Huber, Dimitri Veras, John Asher Johnson, James S. Kuszlewicz, and Thomas S. H. North
Subjects: PLANET HOSTS, Stellar mass, individual: HD 212771 [stars], FOS: Physical sciences, STELLAR ASTROPHYSICS MESA, asteroseismology, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, star interactions, 01 natural sciences, Asteroseismology, photometric [techniques], ATMOSPHERIC PARAMETERS, Planet, 0103 physical sciences, EVOLVED STARS, Astrophysics::Solar and Stellar Astrophysics, MAIN-SEQUENCE, planetary systems, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, RED-CLUMP STARS, 010308 nuclear & particles physics, Subgiant, Astronomy, Astronomy and Astrophysics, Planetary system, GIANT STARS, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, FUNDAMENTAL PROPERTIES, planet, Space and Planetary Science, Stellar mass loss, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, BOLOMETRIC CORRECTIONS, SOLAR-LIKE OSCILLATIONS, Astrophysics - Earth and Planetary Astrophysics
Abstract: Doppler-based planet surveys point to an increasing occurrence rate of giant planets with stellar mass. Such surveys rely on evolved stars for a sample of intermediate-mass stars (so-called retired A stars), which are more amenable to Doppler observations than their main-sequence progenitors. However, it has been hypothesised that the masses of subgiant and low-luminosity red-giant stars targeted by these surveys --- typically derived from a combination of spectroscopy and isochrone fitting --- may be systematically overestimated. Here, we test this hypothesis for the particular case of the exoplanet-host star HD 212771 using K2 asteroseismology. The benchmark asteroseismic mass ($1.45^{+0.10}_{-0.09}\:\text{M}_{\odot}$) is significantly higher than the value reported in the discovery paper ($1.15\pm0.08\:\text{M}_{\odot}$), which has been used to inform the stellar mass-planet occurrence relation. This result, therefore, does not lend support to the above hypothesis. Implications for the fates of planetary systems are sensitively dependent on stellar mass. Based on the derived asteroseismic mass, we predict the post-main-sequence evolution of the Jovian planet orbiting HD 212771 under the effects of tidal forces and stellar mass loss., Accepted for publication in MNRAS; 10 pages, 3 figures, 2 tables
Published: 2017
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28. NGTS and WASP photometric recovery of a single-transit candidate from TESS

Author: Andrew Collier Cameron, Alexis M. S. Smith, Louise D. Nielsen, Maximiliano Moyano, Monika Lendl, Claudia Belardi, Oliver Turner, Rosanna H. Tilbrook, Richard G. West, James McCormac, Stéphane Udry, Liam Raynard, Michael R. Goad, Alexander Chaushev, Samuel Gill, Matthew R. Burleigh, James S. Jenkins, Maximilian N. Günther, Sarah L. Casewell, François Bouchy, David R. Anderson, Peter J. Wheatley, Jack S. Acton, Benjamin F. Cooke, Daniel Bayliss, Coel Hellier, James A. G. Jackman, Don Pollacco, Edward M. Bryant, 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: Extrasolare Planeten und Atmosphären, FOS: Physical sciences, Library science, Q1, 01 natural sciences, QB460, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, QC, QB600, Solar and Stellar Astrophysics (astro-ph.SR), QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, eclipsing [Binaries], binaries: eclipsing, Astronomy and Astrophysics, 3rd-DAS, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite (\tess) produces a large number of single-transit event candidates, since the mission monitors most stars for only $\sim$27\,days. Such candidates correspond to long-period planets or eclipsing binaries. Using the \tess\ Sector 1 full-frame images, we identified a 7750\,ppm single-transit event with a duration of 7\,hours around the moderately evolved F-dwarf star \tic\ (Tmag=10.23, \teff=6280$\pm{85}$\,K). Using archival WASP photometry we constrained the true orbital period to one of three possible values. We detected a subsequent transit-event with NGTS, which revealed the orbital period to be 38.20\,d. Radial velocity measurements from the CORALIE Spectrograph show the secondary object has a mass of $M_2$= $0.148\pm{0.003}$\,M$_{\odot}$, indicating this system is an F-M eclipsing binary. The radius of the M-dwarf companion is $R_2$ = $0.171\pm{0.003}$\,R$_{\odot}$, making this one of the most well characterised stars in this mass regime. We find that its radius is 2.3-$\sigma$ lower than expected from stellar evolution models., Comment: 6 pages, 5 Figures, 1 Table. Submitted to MNRAS letters
Published: 2019

29. An examination of the effect of the TESS extended mission on southern hemisphere monotransits

Author: Benjamin F. Cooke, Don Pollacco, and Daniel Bayliss
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Ecliptic, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Time gap, 01 natural sciences, Space and Planetary Science, Climatology, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, Southern Hemisphere, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: NASA recently announced an extended mission for TESS. As a result it is expected that the southern ecliptic hemisphere will be re-observed approximately two years after the initial survey. Aims: We aim to explore how TESS re-observing the southern ecliptic hemisphere will impact the number and distribution of mono-transits discovered during the first year of observations. This simulation will be able to be scaled to any future TESS re-observations. Methods: We carry out an updated simulation of TESS detections in the southern ecliptic hemisphere. This simulation includes realistic Sector window-functions based on the first 11 sectors of SPOC 2 min SAP lightcurves. We then extend this simulation to cover the expected Year 4 of the mission when TESS will re-observed the southern ecliptic fields. For recovered monotransits we also look at the possibility of predicting the period based on the coverage in the TESS data. Results: We find an updated prediction of 339 monotransits from the TESS Year 1 southern ecliptic hemisphere, and that approximately 80% of these systems (266/339) will transit again in the Year 4 observations. The Year 4 observations will also contribute new monotransits not seen in Year 1, resulting in a total of 149 monotransits from the combined Year 1 and Year 4 data sets. We find that 75% (189/266) of recovered Year 1 monotransits will only transit once in the Year 4 data set. For these systems we will be able to constrain possible periods, but period aliasing due to the large time gap between Year 1 and Year 4 observations means that the true period will remain unknown with further spectroscopic or photometric follow-up., 6 pages, 6 figures. Version to be published Astronomy and Astrophysics
Published: 2019

30. NGTS-10b: The shortest period hot Jupiter yet discovered

Author: Michael R. Goad, Oliver Turner, Richard G. West, James McCormac, Liam Raynard, Juan Cabrera, Matthew J. Hooton, Christopher A. Watson, Matthew R. Burleigh, François Bouchy, Jose I. Vines, Joshua T. Briegal, Maximiliano Moyano, James S. Jenkins, Boris T. Gänsicke, E. Foxell, Simon Hodgkin, Benjamin F. Cooke, Monika Lendl, David R. Anderson, Alexander Chaushev, Paul Chote, Philipp Eigmüller, Louise D. Nielsen, M. Soto, Tom Louden, Stéphane Udry, David J. Armstrong, Bruno Chazelas, Simon R. Walker, Alexis M. S. Smith, Peter J. Wheatley, James A. G. Jackman, Don Pollacco, Gregory Lambert, Daniel Bayliss, Anders Erikson, Edward Gillen, Sarah L. Casewell, Szilard Csizmadia, Emma Longstaff, Maximilian N. Günther, Heike Rauer, Barry Smalley, David Brown, Didier Queloz, J. Costes, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Hooton, Matthew John [0000-0003-0030-332X], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, techniques: photometric, QB460, stars: individual: NGTS-10, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planetary systems, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, European research, Leitungsbereich PF, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a new ultra-short period transiting hot Jupiter from the Next Generation Transit Survey (NGTS). NGTS-10b has a mass and radius of $2.162\,^{+0.092}_{-0.107}$ M$_{\rm J}$ and $1.205\,^{+0.117}_{-0.083}$ R$_{\rm J}$ and orbits its host star with a period of $0.7668944\pm0.0000003$ days, making it the shortest period hot Jupiter yet discovered. The host is a $10.4\pm2.5$ Gyr old K5V star ($T_\mathrm{eff}$=$4400\pm100$\,K) of Solar metallicity ([Fe/H] = $-0.02\pm0.12$\,dex) showing moderate signs of stellar activity. NGTS-10b joins a short list of ultra-short period Jupiters that are prime candidates for the study of star-planet tidal interactions. NGTS-10b orbits its host at just $1.46\pm0.18$ Roche radii, and we calculate a median remaining inspiral time of $38$\,Myr and a potentially measurable transit time shift of $7$\,seconds over the coming decade, assuming a stellar tidal quality factor $Q'_{\rm s}=2\times10^{7}$., 16 pages, 19 figures and 5 tables. Submitted 27 Sept 2019. Accepted 10 Jan 2020. Published 20 Feb 2020
Published: 2019
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31. NGTS-6b: An Ultra Short Period Hot-Jupiter Orbiting an Old K Dwarf

Author: Heike Rauer, Samuel Gill, Szilard Csizmadia, Maximiliano Moyano, Philipp Eigmüller, Christopher A. Watson, Sarah L. Casewell, Jose I. Vines, Ruth Titz-Weider, Claudia Belardi, Benjamin F. Cooke, Juan Cabrera, George W. King, Anders Erikson, François Bouchy, Alexis M. S. Smith, Daniel Bayliss, Michael R. Goad, E. Foxell, Edward Gillen, James A. G. Jackman, Don Pollacco, Edward M. Bryant, M. G. Soto, Oliver Turner, Jack S. Acton, Richard G. West, James McCormac, Liam Raynard, Simon R. Walker, Peter J. Wheatley, Louise D. Nielsen, Didier Queloz, Rosanna H. Tilbrook, Stéphane Udry, Alexander Chaushev, Matthew R. Burleigh, James S. Jenkins, Tom Louden, and Joshua T. Briegal
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, 010504 meteorology & atmospheric sciences, Gas giant, Population, FOS: Physical sciences, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, Transit (astronomy), education, planetary systems, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Leitungsbereich PF, Astronomy, Astronomy and Astrophysics, Planetary system, Photoevaporation, Orbit, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a new ultra-short period hot Jupiter from the Next Generation Transit Survey. NGTS-6b orbits its star with a period of 21.17~h, and has a mass and radius of $1.330^{+0.024}_{-0.028}$\mjup\, and $1.271^{+0.197}_{-0.188}$\rjup\, respectively, returning a planetary bulk density of 0.711$^{+0.214}_{-0.136}$~g~cm$^{-3}$. Conforming to the currently known small population of ultra-short period hot Jupiters, the planet appears to orbit a metal-rich star ([Fe/H]$=+0.11\pm0.09$~dex). Photoevaporation models suggest the planet should have lost 5\% of its gaseous atmosphere over the course of the 9.6~Gyrs of evolution of the system. NGTS-6b adds to the small, but growing list of ultra-short period gas giant planets, and will help us to understand the dominant formation and evolutionary mechanisms that govern this population., 10 pages, 11 figures. Paper accepted for publication in MNRAS
Published: 2019

32. HD 213885b: A transiting 1-day-period super-Earth with an Earth-like composition around a bright ($V=7.9$) star unveiled by TESS

Author: Rafael Brahm, Caroline Dorn, Andrés Jordán, Christopher E. Henze, Jack J. Lissauer, Néstor Espinoza, Thomas Henning, Rhodes Hart, Olivier Demangeon, John F. Kielkopf, Eric L. N. Jensen, Andrei Tokovinin, Stéphane Udry, Sara Seager, Natalia Guerrero, J. Lillo-Box, Krzysztof G. Hełminiak, Benjamin F. Cooke, Oliver Turner, H. Giles, Nuno C. Santos, David W. Latham, Joshua N. Winn, Geof Wingham, Maxime Marmier, David Barrado, Damien Ségransan, Tansu Daylan, Patricia T. Boyd, Felipe Rojas, George R. Ricker, François Bouchy, John P. Doty, Martin Schlecker, P. Figueira, S. G. Sousa, Joseph D. Twicken, Karen A. Collins, Diana Kossakowski, Francesco Pepe, Peter J. Wheatley, David J. Armstrong, Matthew P. Battley, James S. Jenkins, Louise D. Nielsen, Daniel Bayliss, Vardan Adibekyan, Robert L. Morris, Aaron Dean Chacon, Ian J. M. Crossfield, Carl Ziegler, Matías R. Díaz, Claudia Aguilera-Gómez, Nicholas M. Law, Paula Sarkis, Jon M. Jenkins, C. Briceño, Christophe Lovis, S. C. C. Barros, Don Pollacco, Xavier Dumusque, Edward M. Bryant, Andrew W. Mann, Barrado, D. [https://orcid.org/0000-0002-5971-9242], Lillo Box, J. [https://orcid.org/0000-0003-3742-1987], Díaz, M. [https://orcid.org/0000-0002-2100-3257], Wheatley, P. [https://orcid.org/0000-0003-1452-2240], Nielsen, L. D. [https://orcid.org/0000-0002-5254-2499], Figueira, P. [https://orcid.org/0000-0001-8504-283X], Jenssen, E. [https://orcid.org/0000-0002-4625-7333], Barros, S. [https://orcid.org/0000-0003-2434-3625], Espinoza Pérez, N. [https://orcid.org/0000-0001-9513-1449], Armstrong, D. J. [https://orcid.org/0000-0002-5080-4117], Bayliss, D. [https://orcid.org/0000-0001-6023-1335], Turner, O. [https://orcid.org/0000-0002-8216-2796], Sousa, S. G. [https://orcid.org/0000-0001-9047-2965], Kielpof, J. F. [https://orcid.org/0000-0003-0497-2651], Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Science and Technology Facilities Council (STFC), Swiss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), National Science Centre, Poland (NCN), and Millennium Institute of Astrophysics (MAS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, TOI-141, 010504 meteorology & atmospheric sciences, radial velocities [Techniques], photometric [Techniques], individual [Planets and satellites], FOS: Physical sciences, Astronomy and Astrophysics, TIC 403224672, HD213885, 01 natural sciences, detection [Planets and satellites], Space and Planetary Science, 0103 physical sciences, Christian ministry, dunfamental parameters [Planets and satellites], 85-XX, 010303 astronomy & astrophysics, Humanities, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Espinoza, N. et al., We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 ±0.6M for this 1.74±0.05R exoplanet, which provides enough information to constrain its bulk composition - similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whose minimum mass of 19.9 ± 1.4 M makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2019

33. NGTS-5b: A highly inflated planet offering insights into the sub-Jovian desert

Author: Philipp Eigmüller, Alexander Chaushev, Andrew Grange, Christopher A. Watson, Katja Poppenhaeger, Matthew R. Burleigh, Boris T. Gänsicke, Sarah L. Casewell, James S. Jenkins, Daniel Bayliss, Anders Erikson, James A. G. Jackman, Don Pollacco, Bruno Chazelas, Oliver Turner, Richard G. West, James McCormac, Maximilian N. Günther, Maximiliano Moyano, Liam Raynard, Szilard Csizmadia, Michael R. Goad, Stéphane Udry, Benjamin F. Cooke, Didier Queloz, Edward Gillen, Heike Rauer, Claudia Belardi, Louise D. Nielsen, Barry Smalley, Juan Cabrera, François Bouchy, Alexis M. S. Smith, Simon R. Walker, Peter J. Wheatley, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: planets and satellites: detection, gaseous planets [planets and satellites], detection [planets and satellites], Population, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Jovian, Planet, 0103 physical sciences, Transit (astronomy), 010306 general physics, education, 010303 astronomy & astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Astronomy, Astronomy and Astrophysics, Light curve, Orbital period, Exoplanet, planets and satellites: gaseous planets, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: Planetary population analysis gives us insight into formation and evolution processes. For short-period planets, the subJovian desert has been discussed in recent years with regard to the planet population in the mass/period and radius/period parameter space without taking stellar parameters into account. The Next Generation Transit Survey (NGTS) is optimised for detecting planets in this regime, which allows for further analysis of the sub-Jovian desert. Aims: With high-precision photometric surveys (e.g. with NGTS and TESS), which aim to detect short period planets especially around M/K-type host stars, stellar parameters need to be accounted for when empirical data are compared to model predictions. Presenting a newly discovered planet at the boundary of the sub-Jovian desert, we analyse its bulk properties and use it to show the properties of exoplanets that border the sub-Jovian desert. Methods: Using NGTS light curve and spectroscopic follow-up observations, we confirm the planetary nature of planet NGTS-5b and determine its mass. Using exoplanet archives, we set the planet in context with other discoveries. Results: NGTS-5b is a short-period planet with an orbital period of 3.3569866 +- 0.0000026 days. With a mass of 0.229 +- 0.037 MJup and a radius of 1.136 +- 0.023 RJup, it is highly inflated. Its mass places it at the upper boundary of the sub-Jovian desert. Because the host is a K2 dwarf, we need to account for the stellar parameters when NGTS-5b is analysed with regard to planet populations. Conclusions: With red-sensitive surveys (e.g. with NGTS and TESS), we expect many more planets around late-type stars to be detected. An empirical analysis of the sub-Jovian desert should therefore take stellar parameters into account., 10 pages, 12 figures, accepted for publication in A&A
Published: 2019
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34. HD219666b: A hot-Neptune from TESS Sector 1

Author: V. Van Eylen, J. N. Winn, Teriyuki Hirano, M. Esposito, D. L. Pollacco, Ignasi Ribas, J. de León, M. Tala-Pinto, David Nespral, H. J. Deeg, P. Figueira, S. Hojjatpanah, O. D. S. Demangeon, Grzegorz Nowak, M. Hjorth, John H. Livingston, Hugh P. Osborn, Farzana Meru, François Bouchy, William D. Cochran, Alexis M. S. Smith, S. C. C. Barros, Davide Gandolfi, Edward M. Bryant, Anders Erikson, N. C. Santos, Louise D. Nielsen, Michael Endl, Norio Narita, Vardan Adibekyan, Sascha Grziwa, K. W. F. Lam, D. Hidalgo, P. G. Beck, Duncan A. Brown, Peter J. Wheatley, Carina M. Persson, Mikkel N. Lund, Xavier Dumusque, Savita Mathur, A. P. Hatzes, Judith Korth, Anders Bo Justesen, Szilard Csizmadia, J. Prieto-Arranz, Fei Dai, J. Cabrera, Francesca Faedi, Rafael Luque, Emil Knudstrup, E. Delgado Mena, M. Pätzold, M. Fridlund, Oscar Barragán, Eike W. Guenther, J. Lillo-Box, Benjamin F. Cooke, Heike Rauer, Luca Fossati, Prajwal Niraula, S. Redfield, M. M. Musso, Patricio Cubillos, Roi Alonso, Rodrigo F. Díaz, Stéphane Udry, David Barrado, Enric Palle, A. S. Bonomo, P. Montanes Rodriguez, David J. Armstrong, Philipp Eigmüller, M. Deleuil, S. G. Sousa, D. Bayliss, A. Fukui, 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: Dwarf star, 010504 meteorology & atmospheric sciences, fundamental parameters [Planets and satellites], FOS: Physical sciences, Astrophysics, Planets and satellites: individual: HD 219666 b, 01 natural sciences, fundamental parameters [Stars], Planet, 0103 physical sciences, Planets and satellites: detection, Planets and satellites: fundamental parameters, Stars: fundamental parameters, Techniques: photometric, Techniques: radial velocities, Hot Neptune, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], photometric [Techniques], Astronomy and Astrophysics, Radius, Light curve, Orbital period, Exoplanet, detection [Planets and satellites], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], individual: HD 219666 b [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract: We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD219666 (Mstar = 0.92 +/- 0.03 MSun, Rstar = 1.03 +/- 0.03 RSun, tau_star = 10 +/- 2 Gyr). With a mass of Mb = 16.6 +/- 1.3 MEarth, a radius of Rb = 4.71 +/- 0.17 REarth, and an orbital period of P ~ 6 days, HD219666b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with HARPS@ESO3.6m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (Teff = 5527 +/- 65 K, log g = 4.40 +/- 0.11 (cgs), [Fe/H]= 0.04 +/- 0.04 dex, log R'HK = -5.07 +/- 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmospheric metal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects., Comment: Accepted for publication in A&A
Published: 2019
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35. Author Correction: An ultrahot Neptune in the Neptune desert

Author: Benjamin F. Cooke, Matias Diaz, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, Michael R. Goad, James A. G. Jackman, Don Pollacco, Edward M. Bryant, James S. Jenkins, Andrew W. Mann, Giovanni Isopi, Jack J. Lissauer, Jack S. Acton, Samuel Gill, Christopher A. Watson, Todd C. Klaus, Rosanna H. Tilbrook, Christopher E. Henze, Philipp Eigmüller, Daniel Bayliss, David R. Ciardi, Norio Narita, Maximiliano Moyano, Cristobal Petrovich, Matthew J. Hooton, Didier Queloz, Stéphane Udry, Jessie L. Christiansen, Jose I. Vines, Andrés Jordán, Eric D. Lopez, M. G. Soto, Charles Beichman, Alexis M. S. Smith, Roland Vanderspek, Ruth Titz-Weider, Simon R. Walker, Jerome de Leon, K. I. Collins, Peter J. Wheatley, David W. Latham, Motohide Tamura, Michael Vezie, George R. Ricker, David J. Armstrong, Samuel N. Quinn, Rafael Brahm, Louise D. Nielsen, Oliver Turner, Sarah L. Casewell, Mayuko Mori, Carl Ziegler, Richard G. West, James McCormac, Anders Erikson, Néstor Espinoza, E. Foxell, Claudia Belardi, Juan Cabrera, George W. King, Liam Raynard, J. Villasenor, Tom Louden, Joshua N. Winn, Pablo Rojas, Edward Gillen, François Bouchy, Andrea Ercolino, Boris T. Gänsicke, Christopher J. Burke, Allyson Bieryla, Karen A. Collins, Heike Rauer, F. Mallia, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Jon M. Jenkins, Pía Cortés-Zuleta, Taku Nishiumi, Nicholas M. Law, and Pascal Torres
Subjects: Desert (philosophy), Neptune, Astronomy and Astrophysics, Geology, Astrobiology
Published: 2020
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36. 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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37. NGTS-4b: A sub-Neptune Transiting in the Desert

Author: Michaël Gillon, Anders Erikson, Benjamin F. Cooke, Alexis M. S. Smith, Sandrine Sohy, Y. Almleaky, Paul Chote, George W. King, Michael R. Goad, Christopher A. Watson, Szilard Csizmadia, Daniel Bayliss, Edward Gillen, Philipp Eigmüller, Juan Cabrera, Matthew R. Burleigh, Artem Burdanov, Simon R. Walker, François Bouchy, Oliver Turner, Richard G. West, James McCormac, Emma Longstaff, Laetitia Delrez, James S. Jenkins, Boris T. Gänsicke, Claudia Belardi, Simon Hodgkin, Peter J. Wheatley, M. Soto, Maximilian N. Günther, Liam Raynard, M. Moyano, Alexander Chaushev, Stéphane Udry, Didier Queloz, David J. Armstrong, E. Foxell, Heike Rauer, Samantha Thompson, Sarah L. Casewell, Bruno Chazelas, Joshua T. Briegal, Louise D. Nielsen, C. Murray, Elsa Ducrot, Emmanuel Jehin, Tom Louden, James A. G. Jackman, Don Pollacco, Gregory Lambert, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, detection [planets and satellites], FOS: Physical sciences, 01 natural sciences, photometric [techniques], techniques: photometric, photometric, stars: individual: NGTS-4- planetary systems, satellites, planets, Neptune, Planet, stars: individual: NGTS-4 planetary systems, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, planetary systems, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Leitungsbereich PF, Desert (particle physics), Astronomy, Astronomy and Astrophysics, NGTS-4, Radius, Planetary system, Orbit, individual: NGTS-4- planetary systems [stars], 13. Climate action, Space and Planetary Science, Magnitude (astronomy), Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of NGTS-4b, a sub-Neptune-sized planet transiting a 13th magnitude K-dwarf in a 1.34d orbit. NGTS-4b has a mass M=$20.6\pm3.0$M_E and radius R=$3.18\pm0.26$R_E, which places it well within the so-called "Neptunian Desert". The mean density of the planet ($3.45\pm0.95$g/cm^3) is consistent with a composition of 100% H$_2$O or a rocky core with a volatile envelope. NGTS-4b is likely to suffer significant mass loss due to relatively strong EUV/X-ray irradiation. Its survival in the Neptunian desert may be due to an unusually high core mass, or it may have avoided the most intense X-ray irradiation by migrating after the initial activity of its host star had subsided. With a transit depth of $0.13\pm0.02$%, NGTS-4b represents the shallowest transiting system ever discovered from the ground, and is the smallest planet discovered in a wide-field ground-based photometric survey., Submitted to MNRAS
Published: 2018
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38. Unmasking the hidden NGTS-3Ab: a hot Jupiter in an unresolved binary system

Author: Maximilian N. Günther, Katja Poppenhaeger, Maximiliano Moyano, Philipp Eigmüller, Y. Almleaky, Laetitia Delrez, Matthew R. Burleigh, Michaël Gillon, Michael R. Goad, Anders Erikson, Didier Queloz, Samantha Thompson, James S. Jenkins, Sarah L. Casewell, David J. Armstrong, Richard G. West, James McCormac, Juan Cabrera, Don Pollacco, Boris T. Gänsicke, Liam Raynard, Neale P. Gibson, Christopher A. Watson, Heike Rauer, Daniel Bayliss, Artem Burdanov, Alexis M. S. Smith, Barry Smalley, Stéphane Udry, Emmanuel Jehin, Sandrine Sohy, Peter J. Wheatley, Tom Louden, François Bouchy, Szilard Csizmadia, Benjamin F. Cooke, Edward Gillen, C. Murray, Elsa Ducrot, Queloz, Didier [0000-0002-3012-0316], Gillen, Edward [0000-0003-2851-3070], and Apollo - University of Cambridge Repository
Subjects: •surveys, Eclipses, Binary number, FOS: Physical sciences, Astrophysics, Joint analysis, Surveys, 01 natural sciences, Photometry (optics), •eclipses, •planets and satellites: detection, 0103 physical sciences, Hot Jupiter, QB460, Binary system, 010303 astronomy & astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), •binaries: eclipsing, •occultations, 010308 nuclear & particles physics, eclipsing [Binaries], Centroid, •Astrophysics - Earth and Planetary Astrophysics, Astronomy and Astrophysics, Radial velocity, detection [Planets and satellites], Space and Planetary Science, astro-ph.EP, Occultations, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of NGTS-3Ab, a hot Jupiter found transiting the primary star of an unresolved binary system. We develop a joint analysis of multi-colour photometry, centroids, radial velocity (RV) cross-correlation function (CCF) profiles and their bisector inverse slopes (BIS) to disentangle this three-body system. Data from the Next Generation Transit Survey (NGTS), SPECULOOS and HARPS are analysed and modelled with our new blendfitter software. We find that the binary consists of NGTS-3A (G6V-dwarf) and NGTS-3B (K1V-dwarf) at 5 arcsec) and are prone to contamination by blended objects. With TESS on the horizon, it is pivotal for the candidate vetting to incorporate all available follow-up information from multi-colour photometry and RV CCF profiles., Accepted for publication in MNRAS 2 May 2018. 20 pages, 11 figures, 9 tables. This is the authors' version of the manuscript
Published: 2018
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39. NGTS-2b: An inflated hot-Jupiter transiting a bright F-dwarf

Author: Katja Poppenhaeger, Don Pollacco, Lionel Metrailler, Maximiliano Moyano, Matthew R. Burleigh, Richard Alexander, Bruno Chazelas, Benjamin F. Cooke, Alexander Chaushev, James S. Jenkins, Daniel Bayliss, Michael R. Goad, Didier Queloz, Philipp Eigmüller, Heike Rauer, Szilard Csizmadia, Simon Hodgkin, Anders Erikson, Grégory L'Ambert, Edward Gillen, Oliver Turner, Richard G. West, James McCormac, Liam Raynard, Barry Smalley, Joshua T. Briegal, Matthew J. Hooton, Simon R. Walker, Stéphane Udry, Andrew Grange, Maximilian N. Günther, Peter J. Wheatley, Alexis M. S. Smith, Boris T. Gänsicke, A. Thompson, Christopher A. Watson, Louise D. Nielsen, Roberto Raddi, Sarah L. Casewell, M. Soto, Tom Louden, A. M. Read, Juan Cabrera, François Bouchy, David J. Armstrong, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Hooton, Matthew John [0000-0003-0030-332X], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, detection [planets and satellites], Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Exoplanet, Photometry (optics), Transmission spectroscopy, fundamental parameters [planets and satellites], Space and Planetary Science, Planet, planets and satellites: detection – planets and satellites: fundamental parameters, 0103 physical sciences, Hot Jupiter, QB460, 010306 general physics, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, Rapid rotation, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of NGTS-2b, an inflated hot-Jupiter transiting a bright F5V star (2MASS J14202949-3112074; $T_{\rm eff}$=$6478^{+94}_{-89}$ K), discovered as part of the Next Generation Transit Survey (NGTS). The planet is in a P=4.51 day orbit with mass $0.74^{+0.13}_{-0.12}$ M$_{J}$, radius $1.595^{+0.047}_{-0.045}$ R$_{J}$ and density $0.226^{+0.040}_{-0.038}$ g cm$^{-3}$; therefore one of the lowest density exoplanets currently known. With a relatively deep 1.0% transit around a bright V=10.96 host star, NGTS-2b is a prime target for probing giant planet composition via atmospheric transmission spectroscopy. The rapid rotation ($vsin$i=$15.2\pm0.8$ km s$^{-1}$) also makes this system an excellent candidate for Rossiter-McLaughlin follow-up observations, to measure the sky-projected stellar obliquity. NGTS-2b was confirmed without the need for follow-up photometry, due to the high precision of the NGTS photometry., 12 pages, 8 figures, accepted for publication in MNRAS
Published: 2018
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40. The masses of retired A stars with asteroseismology:Kepler and K2 observations of exoplanet hosts

Author: Samuel K. Grunblatt, Daniel Huber, Andxsrea Miglio, Tiago L. Campante, Thomas S. H. North, Mikkel N. Lund, James S. Kuszlewicz, Benjamin F. Cooke, Guy R. Davies, and William J. Chaplin
Subjects: RED-GIANT STARS, fundamental parameters [stars], FOS: Physical sciences, PLANET, Astrophysics, asteroseismology, 01 natural sciences, Kepler, Asteroseismology, MAGNETIC-FIELDS, PARAMETERS, photometric [techniques], Error bar, 0103 physical sciences, Range (statistics), 010303 astronomy & astrophysics, Absolute scale, Solar and Stellar Astrophysics (astro-ph.SR), MISSION, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, COMPANIONS, Astronomy, CORES, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, STELLAR EVOLUTION, evolution [stars], BOLOMETRIC CORRECTIONS, SOLAR-LIKE OSCILLATIONS, Astrophysics - Earth and Planetary Astrophysics
Abstract: We investigate the masses of "retired A stars" using asteroseismic detections on seven low-luminosity red-giant and sub-giant stars observed by the NASA Kepler and K2 Missions. Our aim is to explore whether masses derived from spectroscopy and isochrone fitting may have been systematically overestimated. Our targets have all previously been subject to long term radial velocity observations to detect orbiting bodies, and satisfy the criteria used by Johnson et al. (2006) to select survey stars that may have had A-type (or early F-type) main-sequence progenitors. The sample actually spans a somewhat wider range in mass, from $\approx 1\,\rm M_{\odot}$ up to $\approx 1.7\,\rm M_{\odot}$. Whilst for five of the seven stars the reported discovery mass from spectroscopy exceeds the mass estimated using asteroseismology, there is no strong evidence for a significant, systematic bias across the sample. Moreover, comparisons with other masses from the literature show that the absolute scale of any differences is highly sensitive to the chosen reference literature mass, with the scatter between different literature masses significantly larger than reported error bars. We find that any mass difference can be explained through use of differing constraints during the recovery process. We also conclude that underestimated uncertainties on the input parameters can significantly bias the recovered stellar masses, which may have contributed to the controversy on the mass scale for retired A stars., Comment: Accepted MNRAS, 14 pages, 7 Figures, 3 Tables
Published: 2017
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41. Single site observations of TESS single transit detections

Author: Don Pollacco, Peter J. Wheatley, Benjamin F. Cooke, Richard G. West, and James McCormac
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Planetary system, 01 natural sciences, Upper and lower bounds, Exoplanet, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Satellite, Transit (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: Context. The Transiting Exoplanet Survey Satellite (TESS) has been successfully launched and has begin data acquisition. To expedite the science that may be performed with the resulting data it is necessary to gain a good understanding of planetary yields. Given the observing strategy employed by TESS the probability of detecting single transits in long period systems is increased. These systems require careful consideration. Aims. We aim to simulate the number of TESS transit detections during its two-year mission with a particular emphasis on single transits. We also aim to determine the feasibility of ground-based follow-up observations from a single site. Methods. A distribution of planets was simulated around the approximately four million stars in the TESS candidate target list. These planets were tested for detectable transits and characterised. Based on simulated parameters the single transit detections were further analysed to determine which are amenable to ground-based follow-up. Results. TESS will discover an approximate lower bound of 4700 planets with around 460 being single transits. A large fraction of these will be observable from a single ground-based site. This paper finds that, in a single year, approximately 1000 transit events of around 320 unique TESS single transit detections are theoretically observable. Conclusions. As we consider longer period exoplanets, the need for exploring single transit detections increases. For periods ≳45 days the number of single transit detections outnumber multitransits by a factor of three (82 ± 18 and 25 ± 7, respectively) a factor which only grows as longer period detections are considered. Therefore, based on this paper, it is worth expending the extra effort required to follow-up these more challenging, but potentially very rewarding, discoveries. Additionally, we conclude that a large fraction of these targets can be theoretically observed from a single ground-based site. However, further work is required to determine whether these follow-up efforts are feasible when accounting for target specific criteria.
Published: 2018
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