A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)
| dc.contributor.author | Barclay, Thomas | |
| dc.contributor.author | et al. | |
| dc.date.accessioned | 2021-03-12T19:04:29Z | |
| dc.date.available | 2021-03-12T19:04:29Z | |
| dc.date.issued | 2021-01-28 | |
| dc.description | A. Sozzetti, M. Damasso, A. S. Bonomo, Y. Alibert, S. G. Sousa, V. Adibekyan, M. R. Zapatero Osorio, J. I. González Hernández, S. C. C. Barros, J. Lillo-Box, K. G. Stassun, J. Winn, S. Cristiani, F. Pepe, R. Rebolo, N. C. Santos, R. Allart, T. Barclay, F. Bouchy, A. Cabral, D. Ciardi, P. Di Marcantonio, V. D'Odorico, D. Ehrenreich, M. Fasnaugh, P. Figueira, J. Haldemann, J. M. Jenkins, D.W. Latham, B. Lavie, G. Lo Curto, C. Lovis, C. J . A. P. Martins, D. Mégevand, A. Mehner, G. Micela, P. Molaro, N. J. Nunes, M. Oshagh, J. Otegi, E. Pallé, E. Poretti, G. Ricker, D. Rodriguez, S. Seager, A. Suárez Mascareño, J. D. Twicken, S. Udry | en_US |
| dc.description.abstract | [Abridged] We exploit the extreme radial velocity (RV) precision of the ultra-stable echelle spectrograph ESPRESSO on the VLT to unveil the physical properties of the transiting sub-Neptune TOI-130 b, uncovered by TESS orbiting the nearby, bright, late F-type star HD 5278 (TOI-130) with a period Pb=14.3. We use 43 ESPRESSO high-resolution spectra and broad-band photometry information to derive accurate stellar atmospheric and physical parameters of HD 5278. We exploit the TESS light curve (LC) and spectroscopic diagnostics to gauge the impact of stellar activity on the ESPRESSO RVs. We perform a joint ESPRESSO RVs + TESS LC analysis using fully Bayesian frameworks to determine the system parameters. The updated stellar parameters of HD 5278 are Teff=6203±64 K, logg=4.50±0.11 dex, [Fe/H]=−0.12±0.04 dex, M⋆=1.126+0.036−0.035 M⊙ and R⋆=1.194+0.017−0.016 R⊙. We determine HD 5278 b's mass and radius to be Mb=7.8+1.5−1.4 M⊕ and Rb=2.45±0.05 R⊕. The derived mean density, ϱb=2.9+0.6−0.5 g cm⁻³, is consistent with a bulk composition with a substantial (∼30%) water mass fraction and a gas envelope comprising ∼17% of the measured radius. Given the host brightness and irradiation levels, HD 5278 b is one of the best targets orbiting G-F primaries for follow-up atmospheric characterization measurements with HST and JWST. We discover a second, non-transiting companion in the system, with a period Pc=40.87+0.18−0.17 days and a minimum mass Mcsinic=18.4+1.8−1.9 M⊕. We study emerging trends in the growing population of transiting sub-Neptunes, and provide statistical evidence for a low occurrence of close-in, 10−15 M⊕ companions around G-F primaries with Teff≳5500 K. | en_US |
| dc.description.sponsorship | The authors acknowledge the ESPRESSO project team for its effort and dedication in building the ESPRESSO instrument. This work has received financial support from the ASI-INAF agreement n.2018-16-HH.0. M.D. acknowledges financial support from the FP7-SPACE Project ETAEARTH (GA No. 313014). The INAF authors acknowledge financial support of the Italian Ministry of Education, University, and Research with PRIN 201278X4FL and the "Progetti Premiali" funding scheme.The ESPRESSO Instrument Project was partially funded through SNSF’s FLARE Programme for large infrastructures. This work has been carried out in part within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This work was supported by FCT - Funda cão para a Ciência e Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionaliza cão by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 POCI-01-0145-FEDER032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987; PTDC/FISOUT/29048/2017 & IF/00852/2015. S.C.C.B. acknowledges support from FCT through contract nr. IF/01312/2014/CP1215/CT0004. S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces, grant agreement No 724427). V.A. acknowledges the support from FCT through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. Y.A. and J.H. acknowledge the Swiss National Science Foundation (SNSF) for supporting research through the SNSF grant 200020_192038. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal programme RYC-2013-14875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. R. A. is a Trottier Postdoctoral Fellow and acknowledges support from the Trottier Family Foundation.This work was supported in part through a grant from FRQNT.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. 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 expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). We acknowledge the use of public TESS Alert 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. | en_US |
| dc.description.uri | https://arxiv.org/abs/2101.12300 | en_US |
| dc.format.extent | 26 pages | en_US |
| dc.genre | journal articles preprints | en_US |
| dc.identifier | doi:10.13016/m2ejrg-mpvb | |
| dc.identifier.citation | Barclay, T.; et al.; A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130); Earth and Planetary Astrophysics (2021); https://arxiv.org/abs/2101.12300 | en_US |
| dc.identifier.uri | http://hdl.handle.net/11603/21177 | |
| dc.language.iso | en_US | en_US |
| dc.relation.isAvailableAt | The University of Maryland, Baltimore County (UMBC) | |
| dc.relation.ispartof | UMBC Center for Space Sciences and Technology | |
| dc.relation.ispartof | UMBC Faculty Collection | |
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| dc.rights | Public Domain Mark 1.0 | * |
| dc.rights | This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law. | |
| dc.rights.uri | http://creativecommons.org/publicdomain/mark/1.0/ | * |
| dc.title | A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130) | en_US |
| dc.type | Text | en_US |