planets and satellites: detection; stars: individual: TIC 198390247; stars: individual: TOI-1453; techniques: radial velocities; Low-mass; Neptune; Planets and satellites: detections; Star: individual: TIC 198390247; Star: individual: TOI-1453; Stars: individual: proxima Centauri; Stellars; Techniques: radial velocities; Viewing zone; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.EP
Abstract :
[en] Context. The TESS mission is searching for transiting planets over the entire sky, including two continuous viewing zones. Data from the continuous viewing zones span a long time baseline and offer ideal conditions for precise planet radius estimations, enabling the community to prepare for the PLATO mission. Aims. We report on the validation and characterisation of two transiting planets around TOI-1453, a K-dwarf star in the TESS northern continuous viewing zone. Methods. In addition to the TESS data, we used ground-based photometric, spectroscopic, and high-resolution imaging follow-up observations to validate the two planets. We obtained 100 HARPS-N high-resolution spectra over two seasons and used them together with the TESS light curve to constrain the mass, radius, and orbit of each planet. Results. TOI-1453 b is a super-Earth with an orbital period of Pb=4.314 days, a radius of Rb=1.17±0.06 R, and a mass lower than 2.32 M (99%). TOI-1453 c is a sub-Neptune with a period of Pc=6.589 days, radius of Rc=2.22±0.09 R, and mass of Mc=2.95−+00.8384 M. The two planets orbit TOI-1453 with a period ratio close to 3/2, although they are not in a mean motion resonance (MMR) state. We did not detect any transit timing variations in our attempt to further constrain the planet masses. TOI-1453 c has a very low bulk density and is one of the least massive sub-Neptunes discovered to date. It is compatible with having either a water-rich composition or a rocky core surrounded by a thick H/He atmosphere. However, we set constraints on the water mass fraction in the envelope according to either a water-rich or water-poor formation scenario. The star TOI-1453 belongs to the Galactic thin disc based on Gaia kinematics and has a sub-solar metallicity. This system is orbited by a fainter stellar companion at a projected distance of ∼150 AU, classifying TOI-1453 b and c of S-type planets. These various planetary and stellar characteristics make TOI-1453 a valuable system for understanding the origin of super-Earths and sub-Neptunes.
Research Center/Unit :
STAR - Space sciences, Technologies and Astrophysics Research - ULiège Astrobiology - ULiège
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Stalport, Manu ; Université de Liège - ULiège > Unités de recherche interfacultaires > Space sciences, Technologies and Astrophysics Research (STAR)
Mortier, A. ; School of Physics & Astronomy, University of Birmingham, Birmingham, United Kingdom
Cretignier, M. ; Department of Physics, University of Oxford, Oxford, United Kingdom
Egger, J.A. ; Weltraumforschung und Planetologie, Physikalisches Institut, University of Bern, Bern, Switzerland
Malavolta, L. ; Dipartimento di Fisica e Astronomia ‘Galileo Galilei’, Universitá di Padova, Padova, Italy ; INAF - Osservatorio Astronomico di Padova, Padova, Italy
Latham, D.W.; Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States
Collins, K.A.; Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States
Watkins, C.N.; Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States
Murgas, F. ; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Departamento de Astrofísica, Univ. de La Laguna, La Laguna, Spain
Buchhave, L.A. ; DTU Space, Technical University of Denmark, Kgs. Lyngby, Denmark
López-Morales, M.; Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States
Udry, S. ; Département d’Astronomie, Université de Genève, Versoix, Switzerland
Quinn, S.N.; Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, United States
Silva, A.M. ; Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal ; Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Porto, Portugal
Andreuzzi, G. ; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain ; INAF, Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy
Baker, D. ; Physics Department, Austin College, Sherman, United States
Boschin, W. ; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Departamento de Astrofísica, Univ. de La Laguna, La Laguna, Spain ; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain
Ciardi, D.R.; NASA Exoplanet Science Institute, IPAC, California Institute of Technology, Pasadena, United States
Damasso, M.; INAF, Osservatorio Astrofisico di Torino, Pino Torinese, Italy
Di Fabrizio, L.; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain
Dumusque, X. ; Département d’Astronomie, Université de Genève, Versoix, Switzerland
Fukui, A.; Komaba Institute for Science, The University of Tokyo, Tokyo, Japan
Haywood, R. ; Astrophysics Group, University of Exeter, Exeter, United Kingdom
Howell, S.B.; NASA Ames Research Center, Moffett Field, United States
Jenkins, J.M. ; NASA Ames Research Center, Moffett Field, United States
Leleu, A. ; Département d’Astronomie, Université de Genève, Versoix, Switzerland
Lewin, P.; The Maury Lewin Astronomical Observatory, Glendora, United States
Lillo-Box, J.; Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain
Fiorenzano, A.F. Martínez; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain
Narita, N. ; Komaba Institute for Science, The University of Tokyo, Tokyo, Japan
Pedani, M. ; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain
Pinamonti, M. ; INAF, Osservatorio Astrofisico di Torino, Pino Torinese, Italy
Poretti, E. ; Fundación Galileo Galilei - INAF (Telescopio Nazionale Galileo), Breña Baja, Spain
Schwarz, R.P. ; Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States
Seager, S. ; Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, United States ; Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, United States ; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, United States
Sozzetti, A. ; INAF, Osservatorio Astrofisico di Torino, Pino Torinese, Italy
Ting, E.B.; NASA Ames Research Center, Moffett Field, United States
Vanderburg, A.; Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, United States
Winn, J.N.; Department of Astrophysical Sciences, Princeton University, Princeton, United States
Ziegler, C.; Department of Physics, Engineering and Astronomy, Stephen F. Austin State University, Nacogdoches, United States
The authors thank the referee for a constructive report. This work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundaci\u00F3n Galileo Galilei (FGG) of the Istituto Nazionale di Astrofisica (INAF) at the Observatorio del Roque de los Muchachos (La Palma, Canary Islands, Spain). The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen\u2019s University Belfast, and University of Edinburgh. This paper made use of data collected by the TESS mission and are publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA\u2019s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. 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 publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch . M.S. thanks the Belgian Federal Science Policy Office (BELSPO) for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number C4000140754. A.M. acknowledges funding from a UKRI Future Leader Fellowship, grant number MR/X033244/1 and a UK Science and Technology Facilities Council (STFC) small grant ST/Y002334/1. MC acknowledges the SNSF support under grant P500PT_211024. KAC and CNW acknowledge support from the TESS mission via subaward s3449 from MIT. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. X.D acknowledges the support from the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation programme (grant agreement SCORE No 851555) and from the Swiss National Science Foundation under the grant SPECTRE (No. 200021_215200). This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. A.L. acknowledges support of the Swiss National Science Foundation under grant number TMSGI2_211697. 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 article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos S\u00E1nchez operated on the island of Tenerife by the IAC in the Spanish Observato- rio del Teide. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants PGC2018-098153-B-C31. As well, this work is supported by JSPS KAKENHI Grant Number JP24H00017, JP24K00689 and JSPS Bilateral Program Number JPJSBP120249910. This work is partly supported by JSPS KAKENHI Grant Numbers JP17H04574, JP18H01265, and JP18H05439, Grant-in-Aid for JSPS Fellows Grant Number JP20J21872, JST PRESTO Grant Number JPMJPR1775, and a University Research Support Grant from the National Astronomical Observatory of Japan (NAOJ). This paper is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos S\u00E1nchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. SNQ acknowledges support from the TESS mission via subaward s3449 from MIT. This work has been partially supported by the National Aeronautics and Space Administration under grant No. NNX17AB59G, issued through the Exoplanets Research Program. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. M.P. acknowledge support from the European Union - NextGen- erationEU (PRIN MUR 2022 20229R43BH) and the \u201CProgramma di Ricerca Fondamentale INAF 2023\u201D.
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