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

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dc.contributor.authorTrifonov, Trifon
dc.contributor.authorBrahm, Rafael
dc.contributor.authorJordan, Andres
dc.contributor.authorHartogh, Christian
dc.contributor.authorHenning, Thomas
dc.contributor.authorHobson, Melissa J.
dc.contributor.authorSchlecker, Martin
dc.contributor.authorHoward, Saburo
dc.contributor.authorReichardt, Finja
dc.contributor.authorEspinoza, Nestor
dc.contributor.authorLee, Man Hoi
dc.contributor.authorNesvorny, David
dc.contributor.authorRojas, Felipe I.
dc.contributor.authorBarkaoui, Khalid
dc.contributor.authorKossakowski, Diana
dc.contributor.authorBoyle, Gavin
dc.contributor.authorDreizler, Stefan
dc.contributor.authorKuerster, Martin
dc.contributor.authorHeller, Rene
dc.contributor.authorGuillot, Tristan
dc.contributor.authorTriaud, Amaury H. M. J.
dc.contributor.authorAbe, Lyu
dc.contributor.authorAgabi, Abdelkrim
dc.contributor.authorBendjoya, Philippe
dc.contributor.authorCrouzet, Nicolas
dc.contributor.authorDransfield, Georgina
dc.contributor.authorGasparetto, Thomas
dc.contributor.authorGuenther, Maximilian N.
dc.contributor.authorMarie-Sainte, Wenceslas
dc.contributor.authorMekarnia, Djamel
dc.contributor.authorSuarez, Olga
dc.contributor.authorTeske, Johanna
dc.contributor.authorButler, R. Paul
dc.contributor.authorCrane, Jeffrey D.
dc.contributor.authorShectman, Stephen
dc.contributor.authorRicker, George R.
dc.contributor.authorShporer, Avi
dc.contributor.authorVanderspek, Roland
dc.contributor.authorJenkins, Jon M.
dc.contributor.authorWohler, Bill
dc.contributor.authorCollins, Karen A.
dc.contributor.authorCollins, Kevin I.
dc.contributor.authorCiardi, David R.
dc.contributor.authorBarclay, Thomas
dc.contributor.authorMireles, Ismael
dc.contributor.authorSeager, Sara
dc.contributor.authorWinn, Joshua N.
dc.date.accessioned2025-01-20T20:14:45Z
dc.date.available2025-01-20T20:14:45Z
dc.date.issued2023
dc.description.abstractThe K-type star TOI-2525 has an estimated mass of M = 0.849(-0.033)(+0.024) M-circle dot and radius of R = 0.785(-0.007)(+0.007) R-circle dot 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 similar to 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 rho(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.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-3881/acba9b
dc.identifier.eissn1538-3881
dc.identifier.issn0004-6256
dc.identifier.urihttps://doi.org/10.3847/1538-3881/acba9b
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/92217
dc.identifier.wosidWOS:000960020200001
dc.issue.numero4
dc.language.isoen
dc.revistaAstronomical journal
dc.rightsacceso restringido
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleTOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS
dc.typeartículo
dc.volumen165
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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