TOI-969 light and RV curves [Dataset]
The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. In this paper we focus on the confirmation and characterization of the components of the TOI-969...
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| Tipo de recurso: | conjunto de datos |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/365496 |
| Acceso en línea: | http://hdl.handle.net/10261/365496 https://ui.adsabs.harvard.edu/abs/2023A&A...669A.109L https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/669/A109 |
| Access Level: | acceso abierto |
| Palabra clave: | https://cdsarc.cds.unistra.fr/vizier/catstd/ADCkwds.htx Stars, double and multiple Exoplanets Radial velocities Photometry Optical |
| Sumario: | The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. In this paper we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star. We use a set of precise radial velocity observations from HARPS, PFS and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system. We find that TOI-969 b is a transiting close-in (Pb~1.82days) mini-Neptune planet (m_b_=9.1^+1.1^_1.0_M_{Earth}_, R_b_=2.765^+0.088^_0.097_R_{Earth}_), thus placing it on the {lower boundary} of the hot-Neptune desert (T_eq,b_=941+/-31K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of P_c_=1700^+290^_280_days and a minimum mass of m_c_sini_c_=11.3^+1.1^_0.9_M_Jup_, and with a highly-eccentric orbit of e_c_=0.628^+0.043^_0.036_. The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93, and it orbits a moderately bright (G=11.3mag) star, thus becoming an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems. |
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