University of Birmingham The discovery of WASP-151b, WASP-153b, WASP- 156b Demangeon, Olivier D. S.; Faedi, F.; Hébrard, G.; Brown, D. J. A.; Barros, S. C. C.; Doyle, A. P.; Maxted, P. F. L.; Cameron, A. Collier; Hay, K. L.; Alikakos, J.; Anderson, D. R.; Armstrong, D. J.; Boumis, P.; Bonomo, A. S.; Bouchy, F.; Haswell, C. A.; Hellier, C.; Kiefer, F.; Lam, K. W. F.; Mancini, L. DOI: 10.1051/0004-6361/201731735 License: None: All rights reserved Document Version Publisher's PDF, also known as Version of record Citation for published version (Harvard): Demangeon, ODS, Faedi, F, Hébrard, G, Brown, DJA, Barros, SCC, Doyle, AP, Maxted, PFL, Cameron, AC, Hay, KL, Alikakos, J, Anderson, DR, Armstrong, DJ, Boumis, P, Bonomo, AS, Bouchy, F, Haswell, CA, Hellier, C, Kiefer, F, Lam, KWF, Mancini, L, McCormac, J, Norton, AJ, Osborn, HP, Palle, E, Pepe, F, Pollacco, DL, Prieto-Arranz, J, Queloz, D, Ségransan, D, Smalley, B, Triaud, AHMJ, Udry, S, West, R & Wheatley, PJ 2018, 'The discovery of WASP-151b, WASP-153b, WASP-156b: Insights on giant planet migration and the upper boundary of the Neptunian desert', Astronomy and Astrophysics, vol. 610, A63. https://doi.org/10.1051/0004- 6361/201731735 Link to publication on Research at Birmingham portal Publisher Rights Statement: Checked for eligibility: 12/07/2019 This document appears in its final form in [JournalTitle], copyright © ESO 2018. 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Where a licence is displayed above, please note the terms and conditions of the licence govern your use of this document. When citing, please reference the published version. Take down policy While the University of Birmingham exercises care and attention in making items available there are rare occasions when an item has been uploaded in error or has been deemed to be commercially or otherwise sensitive. If you believe that this is the case for this document, please contact [email protected] providing details and we will remove access to the work immediately and investigate. Download date: 02. Oct. 2021 A&A 610, A63 (2018) Astronomy DOI: 10.1051/0004-6361/201731735 & c ESO 2018 Astrophysics The discovery of WASP-151b, WASP-153b, WASP-156b: Insights on giant planet migration and the upper boundary of the Neptunian desert? O. D. S. Demangeon1, F. Faedi2; 9, G. Hébrard3; 4, D. J. A. Brown2, S. C. C. Barros1, A. P. Doyle2, P. F. L. Maxted12, A. Collier Cameron7, K. L. Hay7, J. Alikakos18, D. R. Anderson12, D. J. Armstrong2; 6, P. Boumis18, A. S. Bonomo8, F. Bouchy5, L. Delrez21; 10, M. Gillon21, C. A. Haswell17, C. Hellier12, E. Jehin21, F. Kiefer3, K. W. F. Lam2, M. Lendl20; 5, L. Mancini19; 16; 8, J. McCormac2, A. J. Norton17, H. P. Osborn2, E. Palle14; 15, F. Pepe5, D. L. Pollacco2, J. Prieto-Arranz14; 15, D. Queloz10; 5, D. Ségransan5, B. Smalley12, A. H. M. J. Triaud11; 13, S. Udry5, R. West2, and P. J. Wheatley2 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 University of Warwick, Department of Physics, Gibbet Hill Road, Coventry CV4 7AL, UK 3 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France 4 Observatoire de Haute-Provence, Université d’Aix-Marseille & CNRS, 04870 Saint Michel l’Observatoire, France 5 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland 6 Astrophysics Research Centre, Queen’s University Belfast, University Road, Belfast BT7 1NN, UK 7 Centre for Exoplanet Science, SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK 8 INAF–Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy 9 INAF–Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy 10 Cavendish Laboratory, JJ Thompson Avenue, CB3 0HE Cambridge, UK 11 Institute of Astronomy, Madingley Road, CB3 0HA Cambridge, UK 12 Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK 13 School of Physics & Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK 14 Instituto de Astrosfísica de Canarias (IAC), 38205 La Laguna, Tenerife, Spain 15 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La laguna, Tenerife, Spain 16 Max Planck Institue for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 17 School of Physical Sciences, The Open University, Milton Keynes MK7 6 AA, UK 18 Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, 15236 Penteli, Greece 19 Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy 20 Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria 21 Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 17, Bat. B5C, 4000 Liège, Belgium Received 7 August 2017 / Accepted 16 October 2017 ABSTRACT To investigate the origin of the features discovered in the exoplanet population, the knowledge of exoplanets’ mass and radius with a good precision (.10%) is essential. To achieve this purpose the discovery of transiting exoplanets around bright stars is of prime interest. In this paper, we report the discovery of three transiting exoplanets by the SuperWASP survey and the SOPHIE spectrograph with mass and radius determined with a precision better than 15%. WASP-151b and WASP-153b are two hot Saturns with masses, +0:04 +0:03 +0:03 +20 +0:02 +0:10 radii, densities and equilibrium temperatures of 0:31−0:03 MJ, 1:13−0:03 RJ, 0:22−0:02 ρJ and 1290−10 K, and 0:39−0:02 MJ, 1:55−0:08 RJ, +0:02 +40 0:11−0:02 ρJ and 1700−40 K, respectively. Their host stars are early G type stars (with mag V ∼ 13) and their orbital periods are 4.53 and +0:010 3.33 days, respectively. WASP-156b is a super-Neptune orbiting a K type star (mag V = 11:6). It has a mass of 0:128−0:009 MJ, a radius +0:02 +0:1 +30 of 0:51−0:02 RJ, a density of 1:0−0:1 ρJ, an equilibrium temperature of 970−20 K and an orbital period of 3.83 days. The radius of WASP- 151b appears to be only slightly inflated, while WASP-153b presents a significant radius anomaly compared to a recently published model. WASP-156b, being one of the few well characterized super-Neptunes, will help to constrain the still debated formation of Neptune size planets and the transition between gas and ice giants. The estimates of the age of these three stars confirms an already observed tendency for some stars to have gyrochronological ages significantly lower than their isochronal ages. We propose that high eccentricity migration could partially explain this behavior for stars hosting a short period planet. Finally, these three planets also lie close to (WASP-151b and WASP-153b) or below (WASP-156b) the upper boundary of the Neptunian desert. Their characteristics support that the ultra-violet irradiation plays an important role in this depletion of planets observed in the exoplanet population. Key words. planets and satellites: detection – techniques: radial velocities – techniques: photometric – stars: individual: WASP-151 – stars: individual: WASP-153 – stars: individual: WASP-156 ? The radial velocity (Tables A.1–A.3) and the high resolution photometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/610/A63 Article published by EDP Sciences A63, page 1 of 19 A&A 610, A63 (2018) 1. Introduction the migration of the hot giant planet population and the upper boundary of the Neptunian desert. The successful harvest of exoplanets (see for example exo- planet.eu, Schneider et al. 2011) during the last two decades completely metamorphosed the field of exoplanet science. The 2. Observations initial assumption that the solar system was a typical example of planetary systems is long gone (as stated by Mayor & Queloz 2.1. Discovery: WASP 2012). The Kepler mission (Borucki et al. 2010) delivered 4496 The Wide Angle Search for Planets (WASP) operates two robotic transiting planetary candidates, including 2248 confirmed plan- 1 telescope arrays, each consisting of eight Canon 200m, f/1.8 ets (according to the NASA Exoplanet Archive , August 2017). lenses with e2v 2048 × 2048, Peltier-cooled CCDs, giving a This sample revealed various features of the exoplanet popula- field of view of 7:8 × 7:8 degrees and a pixel scale of 13.700 tion demonstrating the necessity of a very large sample to en- (Pollacco et al. 2006). SuperWASP is located at the Roque de los compass the exoplanets’ diversity (see Borucki 2017, for a re- Muchachos Observatory on La Palma (ORM – ING, Canary Is- cent review).