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HIP 41378 observed by CHEOPS: Where is planet d?⋆⋆⋆
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-21 , DOI: 10.1051/0004-6361/202449689 S. Sulis , L. Borsato , S. Grouffal , H.P. Osborn , A. Santerne , A. Brandeker , M.N. Günther , A. Heitzmann , M. Lendl , M. Fridlund , D. Gandolfi , Y. Alibert , R. Alonso , T. Bárczy , D. Barrado Navascues , S.C. Barros , W. Baumjohann , T. Beck , W. Benz , M. Bergomi , N. Billot , A. Bonfanti , C. Broeg , A. Collier Cameron , C. Corral van Damme , A.C.M. Correia , Sz. Csizmadia , P.E. Cubillos , M.B. Davies , M. Deleuil , A. Deline , L. Delrez , O.D.S. Demangeon , B.-O. Demory , A. Derekas , B. Edwards , D. Ehrenreich , A. Erikson , A. Fortier , L. Fossati , K. Gazeas , M. Gillon , M. Güdel , Ch. Helling , S. Hoyer , K.G. Isaak , L. Kiss , J. Korth , K.W.F. Lam , J. Laskar , A. Lecavelier des Etangs , D. Magrin , P.F.L. Maxted , C. Mordasini , V. Nascimbeni , G. Olofsson , R. Ottensamer , I. Pagano , E. Pallé , G. Peter , D. Piazza , G. Piotto , D. Pollacco , D. Queloz , R. Ragazzoni , N. Rando , H. Rauer , I. Ribas , N.C. Santos , G. Scandariato , D. Ségransan , A.E. Simon , A.M.S. Smith , S.G. Sousa , M. Stalport , M. Steinberger , M. Gy. Szabó , A. Tuson , S. Udry , S. Ulmer-Moll , V. Van Grootel , J. Venturini , E. Villaver , N.A. Walton , T.G. Wilson , D. Wolter , T. Zingales
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-21 , DOI: 10.1051/0004-6361/202449689 S. Sulis , L. Borsato , S. Grouffal , H.P. Osborn , A. Santerne , A. Brandeker , M.N. Günther , A. Heitzmann , M. Lendl , M. Fridlund , D. Gandolfi , Y. Alibert , R. Alonso , T. Bárczy , D. Barrado Navascues , S.C. Barros , W. Baumjohann , T. Beck , W. Benz , M. Bergomi , N. Billot , A. Bonfanti , C. Broeg , A. Collier Cameron , C. Corral van Damme , A.C.M. Correia , Sz. Csizmadia , P.E. Cubillos , M.B. Davies , M. Deleuil , A. Deline , L. Delrez , O.D.S. Demangeon , B.-O. Demory , A. Derekas , B. Edwards , D. Ehrenreich , A. Erikson , A. Fortier , L. Fossati , K. Gazeas , M. Gillon , M. Güdel , Ch. Helling , S. Hoyer , K.G. Isaak , L. Kiss , J. Korth , K.W.F. Lam , J. Laskar , A. Lecavelier des Etangs , D. Magrin , P.F.L. Maxted , C. Mordasini , V. Nascimbeni , G. Olofsson , R. Ottensamer , I. Pagano , E. Pallé , G. Peter , D. Piazza , G. Piotto , D. Pollacco , D. Queloz , R. Ragazzoni , N. Rando , H. Rauer , I. Ribas , N.C. Santos , G. Scandariato , D. Ségransan , A.E. Simon , A.M.S. Smith , S.G. Sousa , M. Stalport , M. Steinberger , M. Gy. Szabó , A. Tuson , S. Udry , S. Ulmer-Moll , V. Van Grootel , J. Venturini , E. Villaver , N.A. Walton , T.G. Wilson , D. Wolter , T. Zingales
HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter–McLaughlin effect, Pd = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on Pd = 278.36 d, but the observations show no transit. We find that large (> 22.4 h) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd ≠ 278.36 d, the periods that minimize the eccentricity would be 101.22 d and 371.14 d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs.
更新日期：2024-06-21
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