HIP 41378 observed by CHEOPS: Where is planet d?
Journal
Date Issued
2024
Author(s)
Sulis, S.
•
•
Grouffal, S.
•
Osborn, H. P.
•
Santerne, A.
•
Brandeker, A.
•
Günther, M. N.
•
Heitzmann, A.
•
Lendl, M.
•
Fridlund, M.
•
Gandolfi, D.
•
Alibert, Y.
•
Alonso, R.
•
Bárczy, T.
•
Barrado Navascues, D.
•
Barros, S. C.C.
•
Baumjohann, W.
•
Beck, T.
•
Benz, W.
•
•
Billot, N.
•
Bonfanti, A.
•
Broeg, C.
•
Collier Cameron, A.
•
Corral Van Damme, C.
•
Correia, A. C.M.
•
Csizmadia, Sz
•
Cubillos, P. E.
•
Davies, M. B.
•
Deleuil, M.
•
Deline, A.
•
Delrez, L.
•
Demangeon, O. D.S.
•
Demory, B. O.
•
Derekas, A.
•
Edwards, B.
•
Ehrenreich, D.
•
Erikson, A.
•
Fortier, A.
•
Fossati, L.
•
Gazeas, K.
•
Gillon, M.
•
Güdel, M.
•
Helling, Ch
•
Hoyer, S.
•
Isaak, K. G.
•
Kiss, L. L.
•
Korth, J.
•
Lam, K. W.F.
•
Laskar, J.
•
Lecavelier Des Etangs, A.
•
•
Maxted, P. F.L.
•
Mordasini, C.
•
•
Olofsson, G.
•
Ottensamer, R.
•
•
Pallé, E.
•
Peter, G.
•
Piazza, D.
•
Piotto, G.
•
Pollacco, D.
•
Queloz, D.
•
•
Rando, N.
•
Rauer, H.
•
Ribas, I.
•
Santos, N. C.
•
•
Ségransan, D.
•
Simon, A. E.
•
Smith, A. M.S.
•
Sousa, S. G.
•
Stalport, M.
•
Steinberger, M.
•
Szabó, Gy M.
•
Tuson, A.
•
Udry, S.
•
Ulmer-Moll, S.
•
Van Grootel, V.
•
Venturini, J.
•
Villaver, E.
•
Walton, N. A.
•
Wilson, T. G.
•
Wolter, D.
•
Zingales, T.
Abstract
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.
Volume
686
Start page
L18
Issn Identifier
0004-6361
Rights
open.access
File(s)![Thumbnail Image]()
Loading...
Name
aa49689-24.pdf
Description
Pdf editoriale
Size
889.23 KB
Format
Adobe PDF
Checksum (MD5)
f56f422f85298715d5f3967d402eb6a1