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Ehrenreich, D.; Delrez, L.; Akinsanmi, B.; Wilson, T. G.; Bonfanti, A.; Beck, M.; Benz, W.; Hoyer, S.; Queloz, D.; Alibert, Y.; Charnoz, S.; Collier Cameron, A.; Deline, A.; Hooton, M.; Lendl, M.; Olofsson, G.; Sousa, S. G.; Adibekyan, V.; Alonso, R.; Anglada, G.; Barrado, D.; Barros, S. C. C.; Baumjohann, W.; Beck, T.; Bekkelien, A.; Bergomi, M.; Billot, N.; Bonfils, X.; Brandeker, A.; Broeg, C.; Bárczy, T.; Berta-Thompson, Z. K.; Cabrera, J.; Corral van Damme, C.; Csizmadia, S.; Davies, M. B.; Deleuil, M.; Demangeon, O.; Demory, B. -O.; Doty, J. P.; Erikson, A.; Fausnaugh, M. M.; Florén, H. -G.; Fortier, A.; Fossati, L.; Fridlund, M.; Futyan, D.; Gandolfi, D.; Gillon, M.; Guterman, P.; Güdel, M.; Heng, K.; Isaak, K. G.; Jäckel, A.; Jenkins, J. M.; Kiss, L. L.; Laskar, J.; Latham, D. W.; Lecavelier des Etangs, A.; Levine, A. M.; Lovis, C.; Magrin, D.; Maxted, P. F. L.; Morgan, E. H.; Nascimbeni, V.; Osborn, H. P.; Ottensamer, R.; Pagano, I.; Pallé, E.; Peter, G.; Piotto, G.; Pollacco, D.; Ragazzoni, R.; Rando, N.; Rauer, H.; Ribas, I.; Ricker, G. R.; Salmon, S.; Santos, N. C.; Scandariato, G.; Simon, A. E.; Smith, A. M. S.; Steinberger, M.; Steller, M.; Szabó, G. M.; Ségransan, D.; Shporer, A.; Thomas, N.; Tschentscher, M.; Udry, S.; Vanderspek, R.; van Grootel, V.; Walton, N. A.
Astronomy and astrophysics (Berlin), 2023, Letnik: 671Journal Article
The planetary system around the naked-eye star v2 Lupi (HD 136352; TOI-2011) is composed of three exoplanets with masses of 4.7, 11.2, and 8.6 Earth masses (M⊕). The TESS and CHEOPS missions revealed that all three planets are transiting and have radii straddling the radius gap separating volatile-rich and volatile-poor super-earths. Only a partial transit of planet d had been covered so we re-observed an inferior conjunction of the long-period 8.6 M⊕ exoplanet v2 Lup d with the CHEOPS space telescope. We confirmed its transiting nature by covering its whole 9.1 h transit for the first time. We refined the planet transit ephemeris to P = 107.1361−0.0022+0.0019 days and Tc = 2459009.7759−0.0096+0.0101 BJDTDB, improving by ~40 times on the previously reported transit timing uncertainty. This refined ephemeris will enable further follow-up of this outstanding long-period transiting planet to search for atmospheric signatures or explore the planet's Hill sphere in search for an exomoon. In fact, the CHEOPS observations also cover the transit of a large fraction of the planet's Hill sphere, which is as large as the Earth's, opening the tantalising possibility of catching transiting exomoons. We conducted a search for exomoon signals in this single-epoch light curve but found no conclusive photometric signature of additional transiting bodies larger than Mars. Yet, only a sustained follow-up of v2 Lup d transits will warrant a comprehensive search for a moon around this outstanding exoplanet. Undetrended and detrended light curves are only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A154
