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Article: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS*

TitleTOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS*
Authors
Trifonov, TBrahm, RJordan, AHartogh, CHenning, THobson, MJSchlecker, MHoward, SReichardt, FEspinoza, NLee, MHNesvorny, DRojas, FIBarkaoui, KKossakowski, DBoyle, GDreizler, SKurster, MHeller, RGuillot, TTriaud, AHMJAbe, LAgabi, ABendjoya, PCrouzet, NDransfield, GGasparetto, TGunther, MNMarie-Sainte, WMekarnia, DSuarez, OTeske, JButler, RPCrane, JDShectman, SRicker, GRShporer, AVanderspek, RJenkins, JMWohler, BCollins, KACollins, KICiardi, DRBarclay, TMireles, ISeager, SWinn, JN
Issue Date28-Mar-2023
PublisherIOP Publishing
Citation
Astronomical Journal, 2023, v. 165, n. 4, p. 1-23 How to Cite?
DOI: http://dx.doi.org/10.3847/1538-3881/acba9b
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 mb = ${0.088}_{-0.004}^{+0.005}$ and mc = ${0.709}_{-0.033}^{+0.034}$ MJup, radii of rb = ${0.88}_{-0.02}^{+0.02}$ and rc = ${0.98}_{-0.02}^{+0.02}$ RJup, and orbital periods of Pb = ${23.288}_{-0.002}^{+0.001}$ and Pc = ${49.260}_{-0.001}^{+0.001}$ 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 ρb = ${0.174}_{-0.015}^{+0.016}$ 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.


Persistent Identifierhttp://hdl.handle.net/10722/332234
ISSN
0004-6256
2021 Impact Factor: 5.491
2020 SCImago Journal Rankings: 2.610

 

DC FieldValueLanguage
dc.contributor.authorTrifonov, T-
dc.contributor.authorBrahm, R-
dc.contributor.authorJordan, A-
dc.contributor.authorHartogh, C-
dc.contributor.authorHenning, T-
dc.contributor.authorHobson, MJ-
dc.contributor.authorSchlecker, M-
dc.contributor.authorHoward, S-
dc.contributor.authorReichardt, F-
dc.contributor.authorEspinoza, N-
dc.contributor.authorLee, MH-
dc.contributor.authorNesvorny, D-
dc.contributor.authorRojas, FI-
dc.contributor.authorBarkaoui, K-
dc.contributor.authorKossakowski, D-
dc.contributor.authorBoyle, G-
dc.contributor.authorDreizler, S-
dc.contributor.authorKurster, M-
dc.contributor.authorHeller, R-
dc.contributor.authorGuillot, T-
dc.contributor.authorTriaud, AHMJ-
dc.contributor.authorAbe, L-
dc.contributor.authorAgabi, A-
dc.contributor.authorBendjoya, P-
dc.contributor.authorCrouzet, N-
dc.contributor.authorDransfield, G-
dc.contributor.authorGasparetto, T-
dc.contributor.authorGunther, MN-
dc.contributor.authorMarie-Sainte, W-
dc.contributor.authorMekarnia, D-
dc.contributor.authorSuarez, O-
dc.contributor.authorTeske, J-
dc.contributor.authorButler, RP-
dc.contributor.authorCrane, JD-
dc.contributor.authorShectman, S-
dc.contributor.authorRicker, GR-
dc.contributor.authorShporer, A-
dc.contributor.authorVanderspek, R-
dc.contributor.authorJenkins, JM-
dc.contributor.authorWohler, B-
dc.contributor.authorCollins, KA-
dc.contributor.authorCollins, KI-
dc.contributor.authorCiardi, DR-
dc.contributor.authorBarclay, T-
dc.contributor.authorMireles, I-
dc.contributor.authorSeager, S-
dc.contributor.authorWinn, JN-
dc.date.accessioned2023-10-04T07:21:07Z-
dc.date.available2023-10-04T07:21:07Z-
dc.date.issued2023-03-28-
dc.identifier.citationAstronomical Journal, 2023, v. 165, n. 4, p. 1-23-
dc.identifier.issn0004-6256-
dc.identifier.urihttp://hdl.handle.net/10722/332234-
dc.description.abstract<p>The K-type star TOI-2525 has an estimated mass of <em>M</em> = <img alt="${0.849}_{-0.033}^{+0.024}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn1.gif?Expires=1696498982&Signature=Bxvv3BFPJGOhaVXbNz~DVYaUBg4p9fzBQURE4N2iriSHxohA0tZoyuGWlX5eNYPCx93u5xE30KS8m0xerDiYNe-PoyKknJXPbvSeQW972qlBKocfe7y7GNxaZuwdHpPA~-iTIIBv4j-hRrCpTtzVWxXmqwm71qdYiZ6gF79DZEhl~k~D0KSX-mgiFLEczlkDnE0PHMUDl~DIjFcNfh~2GWSjwWLmePp0c3bvTwVYI7uS3xXpY3u~17fReXiWdbxRuB6YXjomM~pC28Jx2xpVFN1wJLwwqohOrBtlmudndCMhFxP7SARrftFaMvlIUkJsticbkbhJL6zHzkCCg3~u2w__&Key-Pair-Id=KL1D8TIY3N7T8"> <em>M</em><sub>⊙</sub> and radius of <em>R</em> = <img alt="${0.785}_{-0.007}^{+0.007}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn2.gif?Expires=1696498982&Signature=hl~k9ciPfdsYdA5NFyUvsZ03FiBxHcD5d7TEwT-z65pLKxkakUTIcd6cTn-1bO4W3xDWm5pZkKG5G1i3vBwur3mMhlgv9Cy00UXunGufzVmZCEsDKGtN1DVat-JZog5lEOCNzVCFSPM7seXNYNdTrxLRgNRKEJojjJfMfAWipjHjRDLM5uSg3ppimf92K2d9oUufoC5~f6sRUO4T1w~WqI4bkkNqbHkd5vmVqdfs7UvTn3xaRyx6zbrWIecPD4PXIbwC1harkReCx5l31TQTV5vHCoj9SiL9QjkFMB07Ebjfkz05CQFnmdwfhtrTyzKQGRf4Y2EaNPP91aAko6ONig__&Key-Pair-Id=KL1D8TIY3N7T8"> <em>R</em><sub>⊙</sub> 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 <em>m</em><sub>b</sub> = <img alt="${0.088}_{-0.004}^{+0.005}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn3.gif?Expires=1696498982&Signature=hxaoPiWTtVPRqU3uwPk8ipScO73os45f6HvOnW~OKZh35pDzSYz0~4lGl8tvBwqmcKD4P3-Xw9GKdYZTMwLlVdgiZsncWB6PtUjmeG4BsbqHMXo8S~cOPG0LaT9m2Lx5rfb1-biy7F~Lfwg7EEiEbb5Q85avs899J3TcI0sJkKXRD2F-NWRObLtxmwdBWaQb7aaa8Npc11okZWX1FB2iDB7H50oyaDz3apajhcBHPwIeDcsAlqiowRwEMVl5P55tOnFUpXh-m9gXuiu8sy~dQK1v6Jreuo6g4o5S7u0gI7XhnkhiIWAw5sZPtz3Pema-dpU7JDoWHNUlz0p-PM2-nw__&Key-Pair-Id=KL1D8TIY3N7T8"> and <em>m</em><sub>c</sub> = <img alt="${0.709}_{-0.033}^{+0.034}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn4.gif?Expires=1696498982&Signature=hmxp10e77zCzI9XseGRc6W14sBmYk0VeAI0L5Sp9hOY6L7413O6lIJRAIOIAY9tYtrkCe51ZMTNuV2sjkQiqBNo8Ss~QPahCKQvcXg34EGESV7-Gq3IunuMC24rVnh8zqcbVo0~hpsf1q70ddXGQKQW1n4kd0Tu7pMMRvWdEZ3T8bKA0HZoofYyunsolBdMDLvfFhsm~s8e42WKu5I44FE-R9OTMxF8Ozb--cY2yM7L~1A9e-QZpRsJLEZ3riqdbn1HGC8QtDLQdlbnP1m2Ulg~3jCZtLR3JYLE5aCwkcjTS9ryhJlvdyFCaeDJn~ao-Ry~Y1x4tuFEqVw0Aalfpcg__&Key-Pair-Id=KL1D8TIY3N7T8"> <em>M</em><sub>Jup</sub>, radii of <em>r</em><sub><em>b</em> </sub>= <img alt="${0.88}_{-0.02}^{+0.02}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn5.gif?Expires=1696498982&Signature=RqkTlKZ5UFmD-EO4Hil8bS9R3KNt~PDuDWlQkb4gsfLhjs~Zzzcvbx0E6JntxewYqvdBM6vinVc8BUnnn9ejyQVev9z9VjO~fjVwaK50jyR2FnSiENiw05Cek3nv6kkfL4JOD0ewSstcnPifv6hnuuu3wJRn9oYJeVaoHc6lY0dfPDGcJ1j-xt~mnBjJeFO-n5b4~uk3VXDBIYr8AOKYDfHriKNLqlHGvfMz-IofzyO8kItOOU0A0CAR-NPTjjZy9NpByTTIrHMSFV-P6RovKwUqP0owMeJ5IjFeMsO7U5XnxhTkZLr6TxjoXaL97VB6KJjsHV5CdZTbDcxbgAm5dA__&Key-Pair-Id=KL1D8TIY3N7T8"> and <em>r</em><sub><em>c</em> </sub>= <img alt="${0.98}_{-0.02}^{+0.02}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn6.gif?Expires=1696498982&Signature=uBSmbUIOHkWfFCUpJu0iq5hPvUjlqSxC5573Q6goNe-FjeVuQV6lQtNwn8cwRxTFLl4OPfxowtKaVsd0DnFIy9VK5hm8j0McOQ-EzWCD-OItaGCXdGATAGF0efDAtSfUCbxuFLFFR7dHgnqU8H9e8loIPWFJnUtpQx~ZTmhmoXqQ78GY-a9KMFexaGXWFcsAVSlqtwIooPrzrB5kCOlLG1Pqm6mw~Ef9Z46lK7~3k8ZkN5vjey6REx0rbFqec8wipr0gThpPfMawRWkHG-Wv3l9sU-pwUqPMDimNRMqFyc-1LRACGwzmkze6d4oWNMZarSaYJAbWMULjTY4VCR5RpQ__&Key-Pair-Id=KL1D8TIY3N7T8"> <em>R</em><sub>Jup</sub>, and orbital periods of <em>P</em><sub>b</sub> = <img alt="${23.288}_{-0.002}^{+0.001}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn7.gif?Expires=1696498982&Signature=kz8n7fBW3t9bIL~EUHHTxk1OFHgtL~N4BI8NOt-jZ12T3cjKfpLgYzantW6~51SOOlpIvXHouv-N7GTWIBDLojrs7OUjIxTwlv4C2VH652VkjNwbJ3wr76h7nqtWxkghOnIe3p7xNvmzWte6VX001wAsl4cZdd7T-zl1OZqYFdMjxfGxq0HL3rAbXK96X4EB1fyzwE-hpyhLenDi9m-R3bTKNxYH4jBHrRh5p5sjmfdyvkqWXqSlEagKTJzgqZ0sTDlYqsN3kVGvrU-b9dYD2WcSpo-DeUlZ1WqQqPlcbaBmqb-R1YrvbhHDfGDwktZ68Znl50eAmglwdN0qLNMDdQ__&Key-Pair-Id=KL1D8TIY3N7T8"> and <em>P</em><sub>c</sub> = <img alt="${49.260}_{-0.001}^{+0.001}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn8.gif?Expires=1696498982&Signature=mYnWSgq2a91gGIPgaL6ySwJx2O3yg-l83zq7V19yDpeRWsFKsRTdusu7zhe8vN8tgXR-06Ac2N-NlgbF4pXlmD~HgxOxpB3UjApzBLE-w2O-LDMcM-A3lp9ZbIl89qKE0jq5bi3poZljreTPdYgv7BqrLP24Slj38SBsXjQbVbgwo~T2udzZASAHsZdlTdEUH9g7V52QJJ-mmt1ICdcrOxlD25N74PTfHr1~J6casQ-1fEquHxoZR5o9vl6yLEaVGWy5US41KMd76TeRo6Lw-3otbc8JF~8YDFt4SvRdlUjD2aW2VxT3k-91C6Q3IrRvLTTiOHaVi2UYRdYND8Vyig__&Key-Pair-Id=KL1D8TIY3N7T8"> 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 <em>ρ</em><sub>b</sub> = <img alt="${0.174}_{-0.015}^{+0.016}$" src="https://content.cld.iop.org/journals/1538-3881/165/4/179/revision1/ajacba9bieqn9.gif?Expires=1696498982&Signature=vVJNgmbKwcss1yoWx6g~BFJCsBsv1jagiGuKWGb4fkZYK5H~0uWYUIvRKh~jehk7doUvdC9U5izlN~oP3AcUpO6tMQ1~rL-ULXJja4LmoU2EkaNIsSTEbsygor6-JTGbZYOkP0yhp3JZxImRyP4KxRGCldvO9dvbld-v9UTztgoJ67Y9HCm7CyRi~hijIxjFwWBiBeTZnAfGgc~nYv56P8RodMwMv9cXKMnd~Vvt~GK1sYqB8rmjkrJX4bZagTBy1gJ~FseO4tZDrNVam8LHLigQsNvAFu0oUXH29Rd3WK2d~3cV9V3CPYxPCKcbSEPibIzTY51rd66LslQrzCycAg__&Key-Pair-Id=KL1D8TIY3N7T8"> g cm<sup>−3</sup>. 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.</p>-
dc.languageeng-
dc.publisherIOP Publishing-
dc.relation.ispartofAstronomical Journal-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.titleTOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS*-
dc.typeArticle-
dc.identifier.doi10.3847/1538-3881/acba9b-
dc.identifier.scopuseid_2-s2.0-85151499769-
dc.identifier.volume165-
dc.identifier.issue4-
dc.identifier.spage1-
dc.identifier.epage23-
dc.identifier.eissn1538-3881-
dc.identifier.issnl0004-6256-

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