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TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet

Korth, J. LU ; Gandolfi, D. ; Šubjak, J. ; Howard, S. ; Ataiee, S. ; Collins, K. A. ; Quinn, S. N. ; Mustill, A. J. LU orcid ; Guillot, T. and Lodieu, N. , et al. (2023) In Astronomy & Astrophysics 675.
Abstract
The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c on an 8.4-day orbit that is accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We performed a photodynamical modeling of the HARPS and PFS RVs, along with transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program (TFOP). We determined the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 ± 0.97M⊕ and Rb = 3.56 ± 0.13 R⊕, and Mc = 325.59 ± 5.59M⊕ and Rc = 13.32−1.41+1.55 R⊕,... (More)
The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c on an 8.4-day orbit that is accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We performed a photodynamical modeling of the HARPS and PFS RVs, along with transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program (TFOP). We determined the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 ± 0.97M⊕ and Rb = 3.56 ± 0.13 R⊕, and Mc = 325.59 ± 5.59M⊕ and Rc = 13.32−1.41+1.55 R⊕, respectively. We have spectroscopically confirmed the existence of TOI-1130 b, which had previously only been validated. We find that the two planets have orbits with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small, yet growing population of hot Jupiters with an inner low-mass planet that poses a challenge to the pathway scenario for hot Jupiter formation. We also detected a linear RV trend that is possibly due to the presence of an outer massive companion. (Less)
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organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
planetary systems, planets and satellites: individual: TOI-1130, techniques: photometric, techniques: radial velocities, Astrophysics - Earth and Planetary Astrophysics
in
Astronomy & Astrophysics
volume
675
article number
A115
publisher
EDP Sciences
external identifiers
  • scopus:85165527366
ISSN
1432-0746
DOI
10.1051/0004-6361/202244617
project
Consolidating CHEOPS and preparing for PLATO: Exoplanet studies in the 2020s
A unified picture of white dwarf planetary systems
language
English
LU publication?
yes
id
6c386e28-8aaa-4ea1-842d-1e2c2f47c014
date added to LUP
2023-08-18 12:06:25
date last changed
2023-11-15 11:17:20
@article{6c386e28-8aaa-4ea1-842d-1e2c2f47c014,
  abstract     = {{The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c on an 8.4-day orbit that is accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We performed a photodynamical modeling of the HARPS and PFS RVs, along with transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program (TFOP). We determined the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 ± 0.97M⊕ and Rb = 3.56 ± 0.13 R⊕, and Mc = 325.59 ± 5.59M⊕ and Rc = 13.32−1.41+1.55 R⊕, respectively. We have spectroscopically confirmed the existence of TOI-1130 b, which had previously only been validated. We find that the two planets have orbits with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small, yet growing population of hot Jupiters with an inner low-mass planet that poses a challenge to the pathway scenario for hot Jupiter formation. We also detected a linear RV trend that is possibly due to the presence of an outer massive companion.}},
  author       = {{Korth, J. and Gandolfi, D. and Šubjak, J. and Howard, S. and Ataiee, S. and Collins, K. A. and Quinn, S. N. and Mustill, A. J. and Guillot, T. and Lodieu, N. and Smith, A. M. S. and Esposito, M. and Rodler, F. and Muresan, A. and Abe, L. and Albrecht, S. H. and Alqasim, A. and Barkaoui, K. and Beck, P. G. and Burke, C. J. and Butler, R. P. and Conti, D. M. and Collins, K. I. and Crane, J. D. and Dai, F. and Deeg, H. J. and Evans, P. and Grziwa, S. and Hatzes, A. P. and Hirano, T. and Horne, K. and Huang, C. X. and Jenkins, J. M. and Kabáth, P. and Kielkopf, J. F. and Knudstrup, E. and Latham, D. W. and Livingston, J. and Luque, R. and Mathur, S. and Murgas, F. and Osborne, H. L. M. and Palle, E. and Persson, C. M. and Rodriguez, J. E. and Rose, M. and Rowden, P. and Schwarz, R. P. and Seager, S. and Serrano, L. M. and Sha, L. and Shectman, S. A. and Shporer, A. and Srdoc, G. and Stockdale, C. and Tan, T.-G. and Teske, J. K. and Van Eylen, V. and Vanderburg, A. and Vanderspek, R. and Wang, S. X. and Winn, J. N.}},
  issn         = {{1432-0746}},
  keywords     = {{planetary systems; planets and satellites: individual: TOI-1130; techniques: photometric; techniques: radial velocities; Astrophysics - Earth and Planetary Astrophysics}},
  language     = {{eng}},
  month        = {{07}},
  publisher    = {{EDP Sciences}},
  series       = {{Astronomy & Astrophysics}},
  title        = {{TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet}},
  url          = {{http://dx.doi.org/10.1051/0004-6361/202244617}},
  doi          = {{10.1051/0004-6361/202244617}},
  volume       = {{675}},
  year         = {{2023}},
}