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

Department of Astrophysics

Publications: Contribution to journal › Article › Peer Reviewed

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 and Astrophysics
Volume	686
DOIs	https://doi.org/10.1051/0004-6361/202449689
Publication status	Published - 1 Jun 2024

Austrian Fields of Science 2012

103003 Astronomy
103004 Astrophysics
103038 Space exploration

Keywords

HIP 41378
individual
Planets and satellites

Access to Document

10.1051/0004-6361/202449689Licence: CC BY 4.0

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 and Astrophysics, 686, Article L18. https://doi.org/10.1051/0004-6361/202449689

@article{b6b50d02c4b5424ea7b01a6606de537a,

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

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 = "Publisher Copyright: {\textcopyright} 2024 The Authors.",

year = "2024",

month = jun,

day = "1",

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

language = "English",

volume = "686",

journal = "Astronomy and 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, BO, 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 and 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.

PY - 2024/6/1

Y1 - 2024/6/1

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 - HIP 41378

KW - individual

KW - Planets and satellites

UR - http://www.scopus.com/inward/record.url?scp=85201083317&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202449689

DO - 10.1051/0004-6361/202449689

M3 - Article

AN - SCOPUS:85201083317

SN - 0004-6361

VL - 686

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - L18

ER -

HIP 41378 observed by CHEOPS: Where is planet d?

Abstract

Austrian Fields of Science 2012

Keywords

Access to Document

Other files and links

Fingerprint

Cite this