The Spin–Orbit Alignment of Eight Warm Gas Giant Systems

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dc.article.number70
dc.catalogadorpva
dc.contributor.authorEspinoza Retamal, Juan Ignacio
dc.contributor.authorJordán Colzani, Andrés Cristóbal
dc.contributor.authorBrahm Scott, Rafael
dc.contributor.authorPetrovich Balbontín, Cristóbal
dc.contributor.authorSedaghati, Elyar
dc.contributor.authorStefánsson, Guðmundur
dc.contributor.authorHobson, Melissa J.
dc.contributor.authorTala Pinto, Marcelo Said
dc.contributor.authorMuñoz, Diego J.
dc.contributor.authorBoyle, Gavin
dc.contributor.authorLeiva, Rodrigo
dc.contributor.authorSuc, Vincent
dc.date.accessioned2025-07-18T18:07:14Z
dc.date.available2025-07-18T18:07:14Z
dc.date.issued2025
dc.description.abstractEssential information about the formation and evolution of planetary systems can be found in their architectures—in particular, in stellar obliquity (ψ)—as they serve as a signature of their dynamical evolution. Here we present ESPRESSO observations of the Rossiter–McLaughlin (RM) effect of eight warm gas giants, revealing that, independently of the eccentricities, all of them have relatively aligned orbits. Our five warm Jupiters (WASP-106 b, WASP-130 b, TOI-558 b, TOI-4515 b, and TOI-5027 b) have sky-projected obliquities |λ| ≃ 0–10°, while the two less massive warm Saturns (K2-139 b and K2-329 A b) are slightly misaligned, having |λ| ≃ 15–25°. Furthermore, for K2-139 b, K2-329 A b, and TOI-4515 b, we also measure true 3D obliquities ψ ≃ 15–30°. We also report a nondetection of the RM effect produced by TOI-2179 b. Through hierarchical Bayesian modeling of the true 3D obliquities of hot and warm Jupiters, we find that around single stars warm Jupiters are statistically more aligned than hot Jupiters. Independent of eccentricities, 95% of the warm Jupiters have ψ ≲ 25° with no misaligned planets, while hot Jupiters show an almost isotropic distribution of misaligned systems. This implies that around single stars warm Jupiters form in primordially aligned protoplanetary disks and subsequently evolve in a more quiescent way than hot Jupiters. Finally, we find that Saturns may have slightly more misaligned orbits than warm Jupiters, but more obliquity measurements are necessary to be conclusive.
dc.fechaingreso.objetodigital2025-07-18
dc.format.extent29 páginas
dc.fuente.origenORCID
dc.identifier.doi10.3847/1538-3881/ade22e
dc.identifier.urihttps://doi.org/10.3847/1538-3881/ade22e
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/104966
dc.information.autorucInstituto de Astrofísica; Espinoza Retamal, Juan Ignacio; S/I; 1025598
dc.information.autorucInstituto de Astrofísica; Jordán Colzani, Andrés Cristóbal; S/I; 176960
dc.information.autorucInstituto de Física; Brahm Scott, Rafael; 0000-0002-9158-7315; 162088
dc.information.autorucInstituto de Astrofísica; Petrovich Balbontín, Cristóbal; S/I; 131196
dc.information.autorucInstituto de Física; Tala Pinto, Marcelo Said; S/I; 171043
dc.issue.numero2
dc.language.isoen
dc.nota.accesocontenido completo
dc.publisherAmerican Astronomical Society
dc.revistaThe Astronomical Journal
dc.rightsacceso abierto
dc.rights.licenseAttribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectExoplanets
dc.subjectExoplanet systems
dc.subjectPlanetary alignment
dc.subjectExoplanet migration
dc.subjectExoplanet dynamics
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleThe Spin–Orbit Alignment of Eight Warm Gas Giant Systems
dc.typeartículo
dc.volumen170
sipa.codpersvinculados1025598
sipa.codpersvinculados176960
sipa.codpersvinculados162088
sipa.codpersvinculados131196
sipa.codpersvinculados171043
sipa.trazabilidadORCID;2025-07-14
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