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http://hdl.handle.net/20.500.12386/34867
Titolo: | A pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 characterized with CHEOPS | Autori: | Wilson, Thomas G. Goffo, Elisa Alibert, Yann Gandolfi, Davide Bonfanti, Andrea Persson, Carina M. Collier Cameron, Andrew Fridlund, Malcolm Fossati, Luca Korth, Judith Benz, Willy Deline, Adrien Florén, Hans-Gustav Guterman, Pascal Adibekyan, Vardan Hooton, Matthew J. Hoyer, Sergio Leleu, Adrien Mustill, Alexander James Salmon, Sébastien Sousa, Sérgio G. Suarez, Olga Abe, Lyu Agabi, Abdelkrim Alonso, Roi Anglada, Guillem Asquier, Joel Bárczy, Tamas Barrado Navascues, David Barros, Susana C. C. Baumjohann, Wolfgang Beck, Mathias Beck, Thomas Billot, Nicolas Bonfils, Xavier Brandeker, Alexis Broeg, Christopher Bryant, Edward M. Burleigh, Matthew R. BUTTU, Marco Cabrera, Juan Charnoz, Sébastien Ciardi, David R. Cloutier, Ryan Cochran, William D. Collins, Karen A. Colón, Knicole D. Crouzet, Nicolas Csizmadia, Szilard Davies, Melvyn B. Deleuil, Magali Delrez, Laetitia Demangeon, Olivier Demory, Brice-Olivier Dragomir, Diana Dransfield, Georgina Ehrenreich, David Erikson, Anders Fortier, Andrea Gan, Tianjun Gill, Samuel Gillon, Michaël Gnilka, Crystal L. Grieves, Nolan Grziwa, Sascha Güdel, Manuel Guillot, Tristan Haldemann, Jonas Heng, Kevin Horne, Keith Howell, Steve B. Isaak, Kate G. Jenkins, Jon M. Jensen, Eric L. N. Kiss, Laszlo LACEDELLI, GAIA Lam, Kristine Laskar, Jacques Latham, David W. Lecavelier des Etangs, Alain Lendl, Monika Lester, Kathryn V. Levine, Alan M. Livingston, John Lovis, Christophe Luque, Rafael MAGRIN, DEMETRIO Marie-Sainte, Wenceslas Maxted, Pierre F. L. Mayo, Andrew W. McLean, Brian Mecina, Marko Mékarnia, Djamel NASCIMBENI, VALERIO Nielsen, Louise D. Olofsson, Göran Osborn, Hugh P. Osborne, Hannah L. M. Ottensamer, Roland PAGANO, Isabella Pallé, Enric Peter, Gisbert PIOTTO , GIAMPAOLO Pollacco, Don Queloz, Didier RAGAZZONI, Roberto Rando, Nicola Rauer, Heike Redfield, Seth Ribas, Ignasi Ricker, George R. Rieder, Martin Santos, Nuno C. SCANDARIATO, GAETANO Schmider, François-Xavier Schwarz, Richard P. Scott, Nicholas J. Seager, Sara Ségransan, Damien Serrano, Luisa Maria Simon, Attila E. Smith, Alexis M. S. Steller, Manfred Stockdale, Chris Szabó, Gyula Thomas, Nicolas Ting, Eric B. Triaud, Amaury H. M. J. Udry, Stéphane Van Eylen, Vincent Van Grootel, Valérie Vanderspek, Roland K. VIOTTO, VALENTINA Walton, Nicholas Winn, Joshua N. |
Data pubblicazione: | 2022 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 511 | Fascicolo: | 1 | Da pagina:: | 1043 | Abstract: | We report the discovery and characterization of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in the Transiting Exoplanet Survey Satellite (TESS) photometry. To characterize the system, we performed and retrieved the CHaracterising ExOPlanets Satellite (CHEOPS), TESS, and ground-based photometry, the High Accuracy Radial velocity Planet Searcher (HARPS) high-resolution spectroscopy, and Gemini speckle imaging. We characterize the host star and determine $T_{\rm eff, \star }=4734\pm 67\,\mathrm{ K}$, $R_{\star }=0.726\pm 0.007\, \mathrm{ R}_{\odot }$, and $M_{\star }=0.748\pm 0.032\, \mathrm{ M}_{\odot }$. We present a novel detrending method based on point spread function shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of P<SUB>b</SUB> = 6.44387 ± 0.00003 d, a radius of R<SUB>b</SUB> = 2.59 ± 0.04 R<SUB>⊕</SUB>, and a mass of $M_{\rm b} = 13.5_{-1.8}^{+1.7}$ M<SUB>⊕</SUB>, whilst TOI-1064 c has an orbital period of $P_{\rm c} = 12.22657^{+0.00005}_{-0.00004}$ d, a radius of R<SUB>c</SUB> = 2.65 ± 0.04 R<SUB>⊕</SUB>, and a 3σ upper mass limit of 8.5 M<SUB>⊕</SUB>. From the high-precision photometry we obtain radius uncertainties of ~1.6 per cent, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterized sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further radial velocities are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allow us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets. | URI: | http://hdl.handle.net/20.500.12386/34867 | URL: | https://academic.oup.com/mnras/article/511/1/1043/6506474?login=true http://arxiv.org/abs/2201.03570v1 |
ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stab3799 | Bibcode ADS: | 2022MNRAS.511.1043W | Fulltext: | open |
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