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Borsato, L, Piotto, G, Gandolfi, D, Nascimbeni, V, Lacedelli, G, Marzari, F, Billot, N, Maxted, PFL, Sousa, S, Cameron, AC, Bonfanti, A, Wilson, TG, Serrano, LM, Garai, Z, Alibert, Y, Alonso, R, Asquier, J, Bárczy, T, Bandy, T, Barrado, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Benz, W, Bonfils, X, Brandeker, A, Broeg, C, Cabrera, J, Charnoz, S, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, O, Demory, B-O, des Etangs, AL, Ehrenreich, D, Erikson, A, Escudé, GA, Fortier, A, Fossati, L, Fridlund, M, Gillon, M, Guedel, M, Hasiba, J, Heng, K, Hoyer, S, Isaak, KG, Kiss, L, Kopp, E, Laskar, J, Lendl, M, Lovis, C, Magrin, D, Munari, M, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Ségransan, D, Santos, NC, Scandariato, G, Simon, A, Smith, AMS, Steller, M, Szabó, G, Thomas, N, Udry, S, Van Grootel, V and Walton, N (2021) Exploiting timing capabilities of the CHEOPS mission with warm-Jupiter planets. Monthly Notices of the Royal Astronomical Society, 506 (3). 3810 - 3830. ISSN 0035-8711

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Abstract

We present 17 transit light curves of seven known warm-Jupiters observed with the CHaracterising ExOPlanet Satellite (CHEOPS). The light curves have been collected as part of the CHEOPS Guaranteed Time Observation (GTO) program that searches for transit-timing variation (TTV) of warm-Jupiters induced by a possible external perturber to shed light on the evolution path of such planetary systems. We describe the CHEOPS observation process, from the planning to the data analysis. In this work, we focused on the timing performance of CHEOPS, the impact of the sampling of the transit phases, and the improvement we can obtain by combining multiple transits together. We reached the highest precision on the transit time of about 13-16 s for the brightest target (WASP-38, G = 9.2) in our sample. From the combined analysis of multiple transits of fainter targets with G >= 11, we obtained a timing precision of similar to 2 min. Additional observations with CHEOPS, covering a longer temporal baseline, will further improve the precision on the transit times and will allow us to detect possible TTV signals induced by an external perturber.

Item Type: Article
Additional Information: The final version of this article and all relevant information related to it, including copyright, can be found online at; https://academic.oup.com/mnras/article-abstract/506/3/3810/6308831?redirectedFrom=fulltext
Uncontrolled Keywords: techniques: photometric; planets and satellites: individual: HAT-P-17 b, KELT-6 b, WASP-8 b, WASP-38 b, WASP-106 b, WASP-130 b, K2-287 b
Subjects: Q Science > Q Science (General)
Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QB Astronomy > QB799 Stars
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 16 Sep 2021 12:38
Last Modified: 19 Nov 2021 15:52
URI: https://eprints.keele.ac.uk/id/eprint/10028

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