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HIP 41378 observed by CHEOPS: Where is planet d?

Sulis, S. ; Davies, M.B. LU ; Korth, J. LU and Zingales, T. (2024) In Astronomy and Astrophysics 686.
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... (More)
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. © 2024 The Authors. (Less)
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Contribution to journal
publication status
published
subject
keywords
HIP 41378, individual, Planets and satellites, Orbits, Satellites, Individual, Most likely, Non-detection, Observation window, Orbital periods, Orbitals, Timing variations, Transit timing, Planets
in
Astronomy and Astrophysics
volume
686
article number
L18
publisher
EDP Sciences
external identifiers
  • scopus:85201083317
ISSN
0004-6361
DOI
10.1051/0004-6361/202449689
language
English
LU publication?
yes
id
e033c414-bc5a-40ac-89cb-ac3faad2e4d9
date added to LUP
2024-10-02 13:09:39
date last changed
2024-10-02 13:09:39
@article{e033c414-bc5a-40ac-89cb-ac3faad2e4d9,
  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.  © 2024 The Authors.}},
  author       = {{Sulis, S. and Davies, M.B. and Korth, J. and Zingales, T.}},
  issn         = {{0004-6361}},
  keywords     = {{HIP 41378; individual; Planets and satellites; Orbits; Satellites; Individual; Most likely; Non-detection; Observation window; Orbital periods; Orbitals; Timing variations; Transit timing; Planets}},
  language     = {{eng}},
  publisher    = {{EDP Sciences}},
  series       = {{Astronomy and Astrophysics}},
  title        = {{HIP 41378 observed by CHEOPS: Where is planet d?}},
  url          = {{http://dx.doi.org/10.1051/0004-6361/202449689}},
  doi          = {{10.1051/0004-6361/202449689}},
  volume       = {{686}},
  year         = {{2024}},
}