Abstract
The K-type star TOI-2525 has an estimated mass of M = 0.849 − 0.033 + 0.024 M ⊙ and radius of R = 0.785 − 0.007 + 0.007 R ⊙ observed by the TESS mission in 22 sectors (within sectors 1 and 39). The TESS light curves yield significant transit events of two companions, which show strong transit timing variations (TTVs) with a semiamplitude of ∼6 hr. We performed TTV dynamical and photodynamical light-curve analysis of the TESS data combined with radial velocity measurements from FEROS and PFS, and we confirmed the planetary nature of these companions. The TOI-2525 system consists of a transiting pair of planets comparable to Neptune and Jupiter with estimated dynamical masses of m b = 0.088 − 0.004 + 0.005 and m c = 0.709 − 0.033 + 0.034 M Jup, radii of r b = 0.88 − 0.02 + 0.02 and r c = 0.98 − 0.02 + 0.02 R Jup, and orbital periods of P b = 23.288 − 0.002 + 0.001 and P c = 49.260 − 0.001 + 0.001 days for the inner and outer planet, respectively. The period ratio is close to the 2:1 period commensurability, but the dynamical simulations of the system suggest that it is outside the mean-motion resonance (MMR) dynamical configuration. Object TOI-2525 b is among the lowest-density Neptune-mass planets known to date, with an estimated median density of ρ b = 0.174 − 0.015 + 0.016 g cm−3. The TOI-2525 system is very similar to the other K dwarf systems discovered by TESS, TOI-2202 and TOI-216, which are composed of almost identical K dwarf primaries and two warm giant planets near the 2:1 MMR.
| Original language | English |
|---|---|
| Article number | 179 |
| Journal | Astronomical Journal |
| Volume | 165 |
| Issue number | 4 |
| DOIs | |
| State | Published - 1 Apr 2023 |
| Externally published | Yes |
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In: Astronomical Journal, Vol. 165, No. 4, 179, 01.04.2023.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - TOI-2525 b and c
T2 - A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS
AU - Trifonov, Trifon
AU - Brahm, Rafael
AU - Jordán, Andrés
AU - Hartogh, Christian
AU - Henning, Thomas
AU - Hobson, Melissa J.
AU - Schlecker, Martin
AU - Howard, Saburo
AU - Reichardt, Finja
AU - Espinoza, Nestor
AU - Lee, Man Hoi
AU - Nesvorny, David
AU - Rojas, Felipe I.
AU - Barkaoui, Khalid
AU - Kossakowski, Diana
AU - Boyle, Gavin
AU - Dreizler, Stefan
AU - Kürster, Martin
AU - Heller, René
AU - Guillot, Tristan
AU - Triaud, Amaury H.M.J.
AU - Abe, Lyu
AU - Agabi, Abdelkrim
AU - Bendjoya, Philippe
AU - Crouzet, Nicolas
AU - Dransfield, Georgina
AU - Gasparetto, Thomas
AU - Günther, Maximilian N.
AU - Marie-Sainte, Wenceslas
AU - Mékarnia, Djamel
AU - Suarez, Olga
AU - Teske, Johanna
AU - Butler, R. Paul
AU - Crane, Jeffrey D.
AU - Shectman, Stephen
AU - Ricker, George R.
AU - Shporer, Avi
AU - Vanderspek, Roland
AU - Jenkins, Jon M.
AU - Wohler, Bill
AU - Collins, Karen A.
AU - Collins, Kevin I.
AU - Ciardi, David R.
AU - Barclay, Thomas
AU - Mireles, Ismael
AU - Seager, Sara
AU - Winn, Joshua N.
N1 - Funding Information: This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA’s Science Mission directorate. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Some of the data presented in this paper were obtained from MAST. The specific observations analyzed can be accessed via doi:10.17909/fwdt-2x66. This research made use of exoplanet (Foreman-Mackey et al. 2021, 2021) and its dependencies (Astropy Collaboration et al. 2013; Kipping 2013; Salvatier et al. 2016; Theano Development Team 2016; Foreman-Mackey et al. 2017a; Astropy Collaboration et al. 2018; Foreman-Mackey 2018; Kumar et al. 2019). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from INSU, ESA and the University of Birmingham. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars” project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program “VIHREN-2021” project No. K ∏-06-Д/5. M.H.L. was supported in part by Hong Kong RGC grant HKU 17305618. A.J., R.B., M.H., and F.R. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT project 11200751. M.N.G. acknowledges support from the European Space Agency (ESA) as an ESA Research Fellow. The results reported herein benefited from collaborations and/or information exchange within the program “Alien Earths” (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. This research is funded in part by the European Union’s Horizon 2020 research and innovation program (grant agreement No. 803193/BEBOP) and the Science and Technology Facilities Council (STFC; grant No. ST/S00193X/1). Funding Information: This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA’s Science Mission directorate. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Some of the data presented in this paper were obtained from MAST. The specific observations analyzed can be accessed via doi: 10.17909/fwdt-2x66 . This research made use of exoplanet (Foreman-Mackey et al. , ) and its dependencies (Astropy Collaboration et al. ; Kipping ; Salvatier et al. ; Theano Development Team ; Foreman-Mackey et al. ; Astropy Collaboration et al. ; Foreman-Mackey ; Kumar et al. ). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from INSU, ESA and the University of Birmingham. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars” project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program “VIHREN-2021” project No. K ∏-06-Д/5. M.H.L. was supported in part by Hong Kong RGC grant HKU 17305618. A.J., R.B., M.H., and F.R. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT project 11200751. M.N.G. acknowledges support from the European Space Agency (ESA) as an ESA Research Fellow. The results reported herein benefited from collaborations and/or information exchange within the program “Alien Earths” (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. This research is funded in part by the European Union’s Horizon 2020 research and innovation program (grant agreement No. 803193/BEBOP) and the Science and Technology Facilities Council (STFC; grant No. ST/S00193X/1). Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/4/1
Y1 - 2023/4/1
N2 - The K-type star TOI-2525 has an estimated mass of M = 0.849 − 0.033 + 0.024 M ⊙ and radius of R = 0.785 − 0.007 + 0.007 R ⊙ observed by the TESS mission in 22 sectors (within sectors 1 and 39). The TESS light curves yield significant transit events of two companions, which show strong transit timing variations (TTVs) with a semiamplitude of ∼6 hr. We performed TTV dynamical and photodynamical light-curve analysis of the TESS data combined with radial velocity measurements from FEROS and PFS, and we confirmed the planetary nature of these companions. The TOI-2525 system consists of a transiting pair of planets comparable to Neptune and Jupiter with estimated dynamical masses of m b = 0.088 − 0.004 + 0.005 and m c = 0.709 − 0.033 + 0.034 M Jup, radii of r b = 0.88 − 0.02 + 0.02 and r c = 0.98 − 0.02 + 0.02 R Jup, and orbital periods of P b = 23.288 − 0.002 + 0.001 and P c = 49.260 − 0.001 + 0.001 days for the inner and outer planet, respectively. The period ratio is close to the 2:1 period commensurability, but the dynamical simulations of the system suggest that it is outside the mean-motion resonance (MMR) dynamical configuration. Object TOI-2525 b is among the lowest-density Neptune-mass planets known to date, with an estimated median density of ρ b = 0.174 − 0.015 + 0.016 g cm−3. The TOI-2525 system is very similar to the other K dwarf systems discovered by TESS, TOI-2202 and TOI-216, which are composed of almost identical K dwarf primaries and two warm giant planets near the 2:1 MMR.
AB - The K-type star TOI-2525 has an estimated mass of M = 0.849 − 0.033 + 0.024 M ⊙ and radius of R = 0.785 − 0.007 + 0.007 R ⊙ observed by the TESS mission in 22 sectors (within sectors 1 and 39). The TESS light curves yield significant transit events of two companions, which show strong transit timing variations (TTVs) with a semiamplitude of ∼6 hr. We performed TTV dynamical and photodynamical light-curve analysis of the TESS data combined with radial velocity measurements from FEROS and PFS, and we confirmed the planetary nature of these companions. The TOI-2525 system consists of a transiting pair of planets comparable to Neptune and Jupiter with estimated dynamical masses of m b = 0.088 − 0.004 + 0.005 and m c = 0.709 − 0.033 + 0.034 M Jup, radii of r b = 0.88 − 0.02 + 0.02 and r c = 0.98 − 0.02 + 0.02 R Jup, and orbital periods of P b = 23.288 − 0.002 + 0.001 and P c = 49.260 − 0.001 + 0.001 days for the inner and outer planet, respectively. The period ratio is close to the 2:1 period commensurability, but the dynamical simulations of the system suggest that it is outside the mean-motion resonance (MMR) dynamical configuration. Object TOI-2525 b is among the lowest-density Neptune-mass planets known to date, with an estimated median density of ρ b = 0.174 − 0.015 + 0.016 g cm−3. The TOI-2525 system is very similar to the other K dwarf systems discovered by TESS, TOI-2202 and TOI-216, which are composed of almost identical K dwarf primaries and two warm giant planets near the 2:1 MMR.
UR - http://www.scopus.com/inward/record.url?scp=85151499769&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/acba9b
DO - 10.3847/1538-3881/acba9b
M3 - Article
AN - SCOPUS:85151499769
SN - 0004-6256
VL - 165
JO - Astronomical Journal
JF - Astronomical Journal
IS - 4
M1 - 179
ER -