HIP 41378 observed by CHEOPS: where is planet d?

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. 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. 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; Gy M. 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

doi:10.1051/0004-6361/202449689

HIP 41378 observed by CHEOPS: where is planet d?

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. C. Barros, W. Baumjohann, T. Beck, W. Benz, M. BergomiN. 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. 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, Gy M. 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

^*Corresponding author for this work

Research output: Contribution to journal › Letter › peer-review

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, P_d = 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 P_d = 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 P_d ≠ 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.

Original language	English
Article number	L18
Number of pages	6
Journal	Astronomy & Astrophysics
Volume	686
Early online date	21 Jun 2024
DOIs	https://doi.org/10.1051/0004-6361/202449689
Publication status	Published - 21 Jun 2024

Keywords

Planets and satellites: individual: HIP 41378

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity
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1/08/24 → 31/07/30
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Cameron, A. C. (PI)
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Jardine, M. M. (PI), Bonnell, I. A. (CoI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Dominik, M. (CoI), Helling, C. (CoI), Horne, K. D. (CoI), Scholz, A. (CoI), Tojeiro, R. (CoI), Weijmans, A.-M. (CoI), Wild, V. (CoI), Woitke, P. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
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HIP 41378 velocity curve
Sulis, S. (Creator), Borsato, L. (Creator), Grouffal, S. (Creator), Osborn, H. P. (Creator), Santerne, A. (Creator), Brandeker, A. (Creator), Guenther, M. N. (Creator), Heitzmann, A. (Creator), Lendl, M. (Creator), Fridlund, M. (Creator), Gandolfi, D. (Creator), Alibert, Y. (Creator), Alonso, R. (Creator), Barczy, T. (Creator), Barrado Navascues, D. (Creator), Barros, S. C. C. (Creator), Baumjohann, W. (Creator), Beck, T. (Creator), Benz, W. (Creator), Bergomi, M. (Creator), Billot, N. (Creator), Bonfanti, A. (Creator), Broeg, C. (Creator), Collier Cameron, A. (Creator), Corral Van Damme, C. (Creator), Correia, A. C. M. (Creator), Sz, C. (Creator), Cubillos, P. E. (Creator), Davies, M. B. (Creator), Deleuil, M. (Creator), Deline, A. (Creator), Delrez, L. (Creator), Demangeon, O. D. S. (Creator), Demory, B.-O. (Creator), Derekas, A. (Creator), Edwards, B. (Creator), Ehrenreich, D. (Creator), Erikson, A. (Creator), Fortier, A. (Creator), Fossati, L. (Creator), Gazeas, K. (Creator), Gillon, M. (Creator), Guedel, M. (Creator), Helling, C. (Creator), Hoyer, S. (Creator), Isaak, K. G. (Creator), Kiss, L. L. (Creator), Korth, J. (Creator), K.W.F., L. (Creator), Laskar, J. (Creator), Lecavelier Des Etangs, A. (Creator), Magrin, D. (Creator), Maxted, P. F. L. (Creator), Mordasini, C. (Creator), Nascimbeni, V. (Creator), Olofsson, G. (Creator), Ottensamer, R. (Creator), Pagano, I. (Creator), Palle, E. (Creator), Peter, G. (Creator), Piazza, D. (Creator), Piotto, G. (Creator), Pollacco, D. (Creator), Queloz, D. (Creator), Ragazzoni, R. (Creator), Rando, N. (Creator), Rauer, H. (Creator), Ribas, I. (Creator), Santos, N. C. (Creator), Scandariato, G. (Creator), Segransan, D. (Creator), Simon, A. E. (Creator), Smith, A. M. S. (Creator), Sousa, S. G. (Creator), Stalport, M. (Creator), Steinberger, M. (Creator), GyM., S. (Creator), Tuson, A. (Creator), Udry, S. (Creator), Ulmer-Moll, S. (Creator), Van Grootel, V. (Creator), Venturini, J. (Creator), Villaver, E. (Creator), Walton, N. A. (Creator), Wilson, T. G. (Creator), Wolter, D. (Creator) & Zingales, T. (Creator), Centre de Donnees Strasbourg (CDS), 2024
DOI: 10.26093/cds/vizier.36869018
Dataset

Cite this

Sulis, S., Borsato, L., 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., ... Zingales, T. (2024). HIP 41378 observed by CHEOPS: where is planet d? Astronomy & Astrophysics, 686, Article L18. https://doi.org/10.1051/0004-6361/202449689

@article{61eff5598b554537a79ca1396a6e952c,

title = "HIP 41378 observed by CHEOPS: where is planet d?",

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.",

keywords = "Planets and satellites: individual: HIP 41378",

author = "S. Sulis and L. Borsato and S. Grouffal and Osborn, {H. P.} and A. Santerne and A. Brandeker and G{\"u}nther, {M. N.} and A. Heitzmann and M. Lendl and M. Fridlund and D. Gandolfi and Y. Alibert and R. Alonso and T. B{\'a}rczy and {Barrado Navascues}, D. and Barros, {S. C. C.} and W. Baumjohann and T. Beck and W. Benz and M. Bergomi and N. Billot and A. Bonfanti and C. Broeg and {Collier Cameron}, A. and {Corral Van Damme}, C. and Correia, {A. C. M.} and Sz Csizmadia and Cubillos, {P. E.} and Davies, {M. B.} and M. Deleuil and A. Deline and L. Delrez and Demangeon, {O. D. S.} and Demory, {B. -O.} and A. Derekas and B. Edwards and D. Ehrenreich and A. Erikson and A. Fortier and L. Fossati and K. Gazeas and M. Gillon and M. G{\"u}del and Ch Helling and S. Hoyer and Isaak, {K. G.} and Kiss, {L. L.} and J. Korth and Lam, {K. W. F.} and J. Laskar and {Lecavelier Des Etangs}, A. and D. Magrin and Maxted, {P. F. L.} and C. Mordasini and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and D. Piazza and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} and G. Scandariato and D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M. S.} and Sousa, {S. G.} and M. Stalport and M. Steinberger and Szab{\'o}, {Gy M.} and A. Tuson and S. Udry and S. Ulmer-Moll and {Van Grootel}, V. and J. Venturini and E. Villaver and Walton, {N. A.} and Wilson, {T. G.} and D. Wolter and T. Zingales",

note = "Funding: CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. CHEOPS data analysed in this article will be made available in the CHEOPS mission archive (https://cheops.unige.ch/archive_browser/). S.S. and M.D. acknowledge support from CNES, as well as the Programme National de Plan{\'e}tologie (PNP) of CNRS-INSU. L.B., G.B., V.N., I.P., G.P., R.R., G.S., V.S., and T.Z. acknowledge support from CHEOPS ASI-INAF agreement n. 2019-29-HH.0. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. A.B. was supported by the SNSA. M.N.G. is the ESA CHEOPS Project Scientist and Mission Representative, and as such also responsible for the Guest Observers (GO) Programme. M.N.G. does not relay proprietary information between the GO and Guaranteed Time Observation (GTO) Programmes, and does not decide on the definition and target selection of the GTO Programme. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. Y.A. acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. We acknowledge financial support from the Agencia Estatal de Investigaci{\'o}n of the Ministerio de Ciencia e Innovaci{\'o}n MCIN/AEI/10.13039/501100011033 and the ERDF “A way of making Europe” through projects PID2019-107061GB-C61, PID2019- 107061GB-C66, PID2021-125627OB-C31, and PID2021-125627OB-C32, from the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrof{\'i}sica de Canarias (CEX2019-000920-S), from the Centre of Excellence “Mar{\'i}a de Maeztu” award to the Institut de Ci{\`e}ncies de l{\textquoteright}Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. We acknowledge financial support from the Agencia Estatal de Investigaci{\'o}n of the Ministerio de Ciencia e Innovaci{\o}n MCIN ´ /AEI/10.13039/501100011033 and the ERDF “A way of making Europe” through projects PID2019-107061GB-C61, PID2019- 107061GB-C66, PID2021-125627OB-C31, and PID2021-125627OB-C32, from the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrof{\'i}sica de Canarias (CEX2019-000920-S), from the Centre of Excellence “Mar{\'i}a de Maeztu” award to the Institut de Ci{\`e}ncies de l{\textquoteright}Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. C.B. acknowledges support from the Swiss Space Office through the ESA PRODEX program. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. A.C.M.C. ackowledges support from the FCT, Portugal, through the CFisUC projects UIDB/04564/2020 and UIDP/04564/2020, with DOI identifiers 10.54499/UIDB/04564/2020 and 10.54499/UIDP/04564/2020, respectively. P.E.C. is funded by the Austrian Science Fund (FWF) Erwin Schroedinger Fellowship, program J4595-N. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Li{\`e}ge through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.D. thanks the Belgian Federal Science Policy Office (BELSPO) for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142531. This work was supported by FCT – Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia through national funds and by FEDER through COMPETE2020 through the research grants UIDB/04434/2020, UIDP/04434/2020, 2022.06962.PTDC. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. This project has received funding from the Swiss National Science Foundation for project 200021_200726. It has also been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grant 51NF40_205606. The authors acknowledge the financial support of the SNSF. M.G. is an F.R.S.-FNRS Senior Research Associate. Ch.H. acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). S.H. gratefully acknowledges CNES funding through the grant 837319. J.K. gratefully acknowledges the support of the Swedish Research Council (VR: Etableringsbidrag 2017-04945). A.C., A.D., B.E., K.G., and J.K. acknowledge their role as ESA-appointed CHEOPS Science Team Members. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d{\textquoteright}Avenir supervised by the Agence Nationale pour la Recherche. P.M. acknowledges support from STFC research grant number ST/R000638/1. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). N.C.S. acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. A.S. acknowledges support from the Swiss Space Office through the ESA PRODEX program. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). The Portuguese team thanks the Portuguese Space Agency for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142255. Gy.M.S. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lendulet LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S.-FNRS Research Associate. J.V. acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945. N.A.W. acknowledges UKSA grant ST/R004838/1. T.W. acknowledges support from the UKSA and the University of Warwick.",

year = "2024",

month = jun,

day = "21",

doi = "10.1051/0004-6361/202449689",

language = "English",

volume = "686",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Sulis, S, Borsato, L, Grouffal, S, Osborn, HP, Santerne, A, Brandeker, A, Günther, MN, Heitzmann, A, Lendl, M, Fridlund, M, Gandolfi, D, Alibert, Y, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, T, Benz, W, Bergomi, M, Billot, N, Bonfanti, A, Broeg, C, Collier Cameron, A, Corral Van Damme, C, Correia, ACM, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Gazeas, K, Gillon, M, Güdel, M, Helling, C, Hoyer, S, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier Des Etangs, A, Magrin, D, Maxted, PFL, Mordasini, C, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Sousa, SG, Stalport, M, Steinberger, M, Szabó, GM, Tuson, A, Udry, S, Ulmer-Moll, S, Van Grootel, V, Venturini, J, Villaver, E, Walton, NA, Wilson, TG, Wolter, D & Zingales, T 2024, 'HIP 41378 observed by CHEOPS: where is planet d?', Astronomy & Astrophysics, vol. 686, L18. https://doi.org/10.1051/0004-6361/202449689

TY - JOUR

T1 - HIP 41378 observed by CHEOPS

T2 - where is planet d?

AU - Sulis, S.

AU - Borsato, L.

AU - Grouffal, S.

AU - Osborn, H. P.

AU - Santerne, A.

AU - Brandeker, A.

AU - Günther, M. N.

AU - Heitzmann, A.

AU - Lendl, M.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Alibert, Y.

AU - Alonso, R.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, T.

AU - Benz, W.

AU - Bergomi, M.

AU - Billot, N.

AU - Bonfanti, A.

AU - Broeg, C.

AU - Collier Cameron, A.

AU - Corral Van Damme, C.

AU - Correia, A. C. M.

AU - Csizmadia, Sz

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Delrez, L.

AU - Demangeon, O. D. S.

AU - Demory, B. -O.

AU - Derekas, A.

AU - Edwards, B.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Helling, Ch

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Korth, J.

AU - Lam, K. W. F.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piazza, D.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Sousa, S. G.

AU - Stalport, M.

AU - Steinberger, M.

AU - Szabó, Gy M.

AU - Tuson, A.

AU - Udry, S.

AU - Ulmer-Moll, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

AU - Wilson, T. G.

AU - Wolter, D.

AU - Zingales, T.

N1 - Funding: CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. CHEOPS data analysed in this article will be made available in the CHEOPS mission archive (https://cheops.unige.ch/archive_browser/). S.S. and M.D. acknowledge support from CNES, as well as the Programme National de Planétologie (PNP) of CNRS-INSU. L.B., G.B., V.N., I.P., G.P., R.R., G.S., V.S., and T.Z. acknowledge support from CHEOPS ASI-INAF agreement n. 2019-29-HH.0. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. A.B. was supported by the SNSA. M.N.G. is the ESA CHEOPS Project Scientist and Mission Representative, and as such also responsible for the Guest Observers (GO) Programme. M.N.G. does not relay proprietary information between the GO and Guaranteed Time Observation (GTO) Programmes, and does not decide on the definition and target selection of the GTO Programme. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. Y.A. acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. We acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF “A way of making Europe” through projects PID2019-107061GB-C61, PID2019- 107061GB-C66, PID2021-125627OB-C31, and PID2021-125627OB-C32, from the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), from the Centre of Excellence “María de Maeztu” award to the Institut de Ciències de l’Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. We acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovaciøn MCIN ´ /AEI/10.13039/501100011033 and the ERDF “A way of making Europe” through projects PID2019-107061GB-C61, PID2019- 107061GB-C66, PID2021-125627OB-C31, and PID2021-125627OB-C32, from the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), from the Centre of Excellence “María de Maeztu” award to the Institut de Ciències de l’Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. C.B. acknowledges support from the Swiss Space Office through the ESA PRODEX program. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. A.C.M.C. ackowledges support from the FCT, Portugal, through the CFisUC projects UIDB/04564/2020 and UIDP/04564/2020, with DOI identifiers 10.54499/UIDB/04564/2020 and 10.54499/UIDP/04564/2020, respectively. P.E.C. is funded by the Austrian Science Fund (FWF) Erwin Schroedinger Fellowship, program J4595-N. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.D. thanks the Belgian Federal Science Policy Office (BELSPO) for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142531. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 through the research grants UIDB/04434/2020, UIDP/04434/2020, 2022.06962.PTDC. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. This project has received funding from the Swiss National Science Foundation for project 200021_200726. It has also been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grant 51NF40_205606. The authors acknowledge the financial support of the SNSF. M.G. is an F.R.S.-FNRS Senior Research Associate. Ch.H. acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). S.H. gratefully acknowledges CNES funding through the grant 837319. J.K. gratefully acknowledges the support of the Swedish Research Council (VR: Etableringsbidrag 2017-04945). A.C., A.D., B.E., K.G., and J.K. acknowledge their role as ESA-appointed CHEOPS Science Team Members. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. P.M. acknowledges support from STFC research grant number ST/R000638/1. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). N.C.S. acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. A.S. acknowledges support from the Swiss Space Office through the ESA PRODEX program. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). The Portuguese team thanks the Portuguese Space Agency for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142255. Gy.M.S. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lendulet LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S.-FNRS Research Associate. J.V. acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945. N.A.W. acknowledges UKSA grant ST/R004838/1. T.W. acknowledges support from the UKSA and the University of Warwick.

PY - 2024/6/21

Y1 - 2024/6/21

N2 - 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.

AB - 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.

KW - Planets and satellites: individual: HIP 41378

U2 - 10.1051/0004-6361/202449689

DO - 10.1051/0004-6361/202449689

M3 - Letter

AN - SCOPUS:85201083317

SN - 0004-6361

VL - 686

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - L18

ER -

HIP 41378 observed by CHEOPS: where is planet d?

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Projects

REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Datasets

HIP 41378 velocity curve

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