{"paper":{"title":"CHEOPS observations of the HD 108236 planetary system: A fifth planet, improved ephemerides, and planetary radii","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"A. Bekkelien, A. Bonfanti, A. Brandeker, A. Collier Cameron, A. Erikson, A.E. Simon, A. Fortier, A. Garcia Mu\\~noz, A.J. Mustill, A. Lecavelier des Etangs, A.M.S. Smith, A. Tuson, B. Chazelas, B.-O. Demory, C. Broeg, C. Corral Van Damme, C. Lovis, C. Persson, D. Barrado, D. Ehrenreich, D. Futyan, D. Gandolfi, D. Magrin, D. Piazza, D. Pollacco, D. Queloz, D. S\\'egransan, D. Wolter, E. Hernandez, E. Pall\\'e, F. Ratti, F. Safa, F. Wildi, G. Lacedelli, G. Olofsson, G. Peter, G. Piotto, G. Scandariato, Gy.M. Szab\\'o, H. Michaelis, H. Ottacher, H.P. Osborn, H. Rauer, I. Pagano, I. Ribas, I. Walter, J. Asquier, J. Cabrera, J. Farinato, J. Hasiba, J. Laskar, K.G. Isaak, K. Heng, L. Borsato, L. Delrez, L. Fossati, L. Kiss, L. Malvasio, L. Marafatto, M.B. Davies, M. Beck, M. Bergomi, M-D. Busch, M. Deleuil, M. Fridlund, M. Gillon, M. Guedel, M.J. Hooton, M. Lendl, M. Munari, M. Rieder, M. Salatti, M. Sordet, M. Steller, M. Tschentscher, N.A. Walton, N. Billot, N.C. Santos, N. Rando, N. Thomas, O. Barrag\\'an, O.D.S. Demangeon, P.F.L. Maxted, P. Guterman, R. Alonso, R. Ottensamer, R. Ragazzoni, R. Rohlfs, S.C.C. Barros, S. Charnoz, S.G. Sousa, S. Hoyer, S. Salmon, S. Udry, T. Bandy, T. B\\'arczy, T. Beck, T.G. Wilson, T. Kuntzer, V. Adibekyan, V. Cessa, V. Nascimbeni, V. Van Eylen, V. Van Grootel, V. Viotto, W. Baumjohann, W. Benz, X. Bonfils, Y. Alibert","submitted_at":"2021-01-03T16:40:42Z","abstract_excerpt":"The detection of a super-Earth and three mini-Neptunes transiting the bright ($V$ = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2101.00663","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2101.00663/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}