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dc.contributor.authorLangellier, N
dc.contributor.authorMilbourne, TW
dc.contributor.authorPhillips, DF
dc.contributor.authorHaywood, RD
dc.contributor.authorSaar, SH
dc.contributor.authorMortier, A
dc.contributor.authorMalavolta, L
dc.contributor.authorThompson, S
dc.contributor.authorCameron, AC
dc.contributor.authorDumusque, X
dc.contributor.authorCegla, HM
dc.contributor.authorLatham, DW
dc.contributor.authorMaldonado, J
dc.contributor.authorWatson, CA
dc.contributor.authorBuchschacher, N
dc.contributor.authorCecconi, M
dc.contributor.authorCharbonneau, D
dc.contributor.authorCosentino, R
dc.contributor.authorGhedina, A
dc.contributor.authorGonzalez, M
dc.contributor.authorLi, CH
dc.contributor.authorLodi, M
dc.contributor.authorLopez-Morales, M
dc.contributor.authorMicela, G
dc.contributor.authorMolinari, E
dc.contributor.authorPepe, F
dc.contributor.authorPoretti, E
dc.contributor.authorRice, K
dc.contributor.authorSasselov, D
dc.contributor.authorSozzetti, A
dc.contributor.authorUdry, S
dc.contributor.authorWalsworth, RL
dc.identifier.citationLangellier , N , Milbourne , TW , Phillips , DF , Haywood , RD , Saar , SH , Mortier , A , Malavolta , L , Thompson , S , Cameron , AC , Dumusque , X , Cegla , HM , Latham , DW , Maldonado , J , Watson , CA , Buchschacher , N , Cecconi , M , Charbonneau , D , Cosentino , R , Ghedina , A , Gonzalez , M , Li , CH , Lodi , M , Lopez-Morales , M , Micela , G , Molinari , E , Pepe , F , Poretti , E , Rice , K , Sasselov , D , Sozzetti , A , Udry , S & Walsworth , RL 2021 , ' Detection limits of low-mass, long-period exoplanets using Gaussian processes applied to HARPS-N solar radial velocities ' , Astronomical Journal , vol. 161 , no. 6 , 287 .
dc.identifier.otherPURE: 274675303
dc.identifier.otherPURE UUID: 75d8b3db-26b7-45c3-944b-5c344d97729f
dc.identifier.otherRIS: urn:51081A4B5A68EDF6BC31A5392FE646AB
dc.identifier.otherWOS: 000655754400001
dc.identifier.otherORCID: /0000-0002-8863-7828/work/95772332
dc.identifier.otherScopus: 85107921775
dc.descriptionFunding: A.C.C. acknowledges support from the Science and Technology Facilities Council (STFC) consolidated grant No. ST/R000824/1.en
dc.description.abstractRadial velocity (RV) searches for Earth-mass exoplanets in the habitable zone around Sun-like stars are limited by the effects of stellar variability on the host star. In particular, suppression of convective blueshift and brightness inhomogeneities due to photospheric faculae/plage and starspots are the dominant contribution to the variability of such stellar RVs. Gaussian process (GP) regression is a powerful tool for statistically modeling these quasi-periodic variations. We investigate the limits of this technique using 800 days of RVs from the solar telescope on the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N) spectrograph. These data provide a well-sampled time series of stellar RV variations. Into this data set, we inject Keplerian signals with periods between 100 and 500 days and amplitudes between 0.6 and 2.4 m s−1. We use GP regression to fit the resulting RVs and determine the statistical significance of recovered periods and amplitudes. We then generate synthetic RVs with the same covariance properties as the solar data to determine a lower bound on the observational baseline necessary to detect low-mass planets in Venus-like orbits around a Sun-like star. Our simulations show that discovering planets with a larger mass (~0.5 m s−1) using current-generation spectrographs and GP regression will require more than 12 yr of densely sampled RV observations. Furthermore, even with a perfect model of stellar variability, discovering a true exo-Venus (~0.1 m s−1) with current instruments would take over 15 yr. Therefore, next-generation spectrographs and better models of stellar variability are required for detection of such planets.
dc.relation.ispartofAstronomical Journalen
dc.rightsCopyright © 2021 American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at
dc.subjectGaussian regressionen
dc.subjectRadial velocityen
dc.subjectSolar activityen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleDetection limits of low-mass, long-period exoplanets using Gaussian processes applied to HARPS-N solar radial velocitiesen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.description.statusPeer revieweden

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