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K2-111 : an old system with two planets in near-resonance
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dc.contributor.author | Mortier, A | |
dc.contributor.author | Zapatero Osorio, M R | |
dc.contributor.author | Malavolta, L | |
dc.contributor.author | Alibert, Y | |
dc.contributor.author | Rice, K | |
dc.contributor.author | Lillo-Box, J | |
dc.contributor.author | Vanderburg, A | |
dc.contributor.author | Oshagh, M | |
dc.contributor.author | Buchhave, L | |
dc.contributor.author | Adibekyan, V | |
dc.contributor.author | Delgado Mena, E | |
dc.contributor.author | Lopez-Morales, M | |
dc.contributor.author | Charbonneau, D | |
dc.contributor.author | Sousa, S G | |
dc.contributor.author | Lovis, C | |
dc.contributor.author | Affer, L | |
dc.contributor.author | Allende Prieto, C | |
dc.contributor.author | Barros, S C C | |
dc.contributor.author | Benatti, S | |
dc.contributor.author | Bonomo, A S | |
dc.contributor.author | Boschin, W | |
dc.contributor.author | Bouchy, F | |
dc.contributor.author | Cabral, A | |
dc.contributor.author | Collier Cameron, A | |
dc.contributor.author | Cosentino, R | |
dc.contributor.author | Cristiani, S | |
dc.contributor.author | Demangeon, O D S | |
dc.contributor.author | Di Marcantonio, P | |
dc.contributor.author | D’Odorico, V | |
dc.contributor.author | Dumusque, X | |
dc.contributor.author | Ehrenreich, D | |
dc.contributor.author | Figueira, P | |
dc.contributor.author | Fiorenzano, A | |
dc.contributor.author | Ghedina, A | |
dc.contributor.author | González Hernández, J I | |
dc.contributor.author | Haldemann, J | |
dc.contributor.author | Harutyunyan, A | |
dc.contributor.author | Haywood, R D | |
dc.contributor.author | Latham, D W | |
dc.contributor.author | Lavie, B | |
dc.contributor.author | Lo Curto, G | |
dc.contributor.author | Maldonado, J | |
dc.contributor.author | Manescau, A | |
dc.contributor.author | Martins, C J A P | |
dc.contributor.author | Mayor, M | |
dc.contributor.author | Mégevand, D | |
dc.contributor.author | Mehner, A | |
dc.contributor.author | Micela, G | |
dc.contributor.author | Molaro, P | |
dc.contributor.author | Molinari, E | |
dc.contributor.author | Nunes, N J | |
dc.contributor.author | Pepe, F A | |
dc.contributor.author | Palle, E | |
dc.contributor.author | Phillips, D | |
dc.contributor.author | Piotto, G | |
dc.contributor.author | Pinamonti, M | |
dc.contributor.author | Poretti, E | |
dc.contributor.author | Riva, M | |
dc.contributor.author | Rebolo, R | |
dc.contributor.author | Santos, N C | |
dc.contributor.author | Sasselov, D | |
dc.contributor.author | Sozzetti, A | |
dc.contributor.author | Suárez Mascareño, A | |
dc.contributor.author | Udry, S | |
dc.contributor.author | West, R G | |
dc.contributor.author | Watson, C A | |
dc.contributor.author | Wilson, T G | |
dc.date.accessioned | 2020-12-16T17:30:06Z | |
dc.date.available | 2020-12-16T17:30:06Z | |
dc.date.issued | 2020-12 | |
dc.identifier | 271681993 | |
dc.identifier | 3b30e5d1-d709-4c3f-8f2b-6e59c77f34f3 | |
dc.identifier | 85096899656 | |
dc.identifier | 000599131700029 | |
dc.identifier.citation | Mortier , A , Zapatero Osorio , M R , Malavolta , L , Alibert , Y , Rice , K , Lillo-Box , J , Vanderburg , A , Oshagh , M , Buchhave , L , Adibekyan , V , Delgado Mena , E , Lopez-Morales , M , Charbonneau , D , Sousa , S G , Lovis , C , Affer , L , Allende Prieto , C , Barros , S C C , Benatti , S , Bonomo , A S , Boschin , W , Bouchy , F , Cabral , A , Collier Cameron , A , Cosentino , R , Cristiani , S , Demangeon , O D S , Di Marcantonio , P , D’Odorico , V , Dumusque , X , Ehrenreich , D , Figueira , P , Fiorenzano , A , Ghedina , A , González Hernández , J I , Haldemann , J , Harutyunyan , A , Haywood , R D , Latham , D W , Lavie , B , Lo Curto , G , Maldonado , J , Manescau , A , Martins , C J A P , Mayor , M , Mégevand , D , Mehner , A , Micela , G , Molaro , P , Molinari , E , Nunes , N J , Pepe , F A , Palle , E , Phillips , D , Piotto , G , Pinamonti , M , Poretti , E , Riva , M , Rebolo , R , Santos , N C , Sasselov , D , Sozzetti , A , Suárez Mascareño , A , Udry , S , West , R G , Watson , C A & Wilson , T G 2020 , ' K2-111 : an old system with two planets in near-resonance ' , Monthly Notices of the Royal Astronomical Society , vol. 499 , no. 4 , pp. 5004-5021 . https://doi.org/10.1093/mnras/staa3144 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | crossref: 10.1093/mnras/staa3144 | |
dc.identifier.other | Bibtex: 10.1093/mnras/staa3144 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/85562465 | |
dc.identifier.other | ORCID: /0000-0001-8749-1962/work/86987360 | |
dc.identifier.uri | https://hdl.handle.net/10023/21167 | |
dc.description | ACC acknowledges support from the Science and Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. CAW would like to acknowledge support from UK STFC grant ST/P000312/1. 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). | en |
dc.description.abstract | This paper reports on the detailed characterization of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry, as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved (log g = 4.17), iron-poor ([Fe/H] = −0.46), but alpha-enhanced ([α/Fe]=0.27), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT, shows that the transiting planet, K2-111 b, orbits with a period Pb = 5.3518 ± 0.0004 d and has a planet radius of 1.82+0.11−0.091.82−0.09+0.11 R⊕ and a mass of 5.29+0.76−0.775.29−0.77+0.76 M⊕, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111 b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111 c, with an orbital period of 15.6785 ± 0.0064 d, orbiting in near-3:1 mean motion resonance with the transiting planet, and a minimum planet mass of 11.3 ± 1.1 M⊕. Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters. | |
dc.format.extent | 18 | |
dc.format.extent | 3867038 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Techniques: photometric | en |
dc.subject | Techniques: radial velocities | en |
dc.subject | Techniques: spectroscopic | en |
dc.subject | Planets and satellites: detection | en |
dc.subject | Stars: individual (K2-111) | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | K2-111 : an old system with two planets in near-resonance | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/staa3144 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/R00824/1 | en |
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