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dc.contributor.authorCameron, A. Collier
dc.contributor.authorMortier, A.
dc.contributor.authorPhillips, D.
dc.contributor.authorDumusque, X.
dc.contributor.authorHaywood, R. D.
dc.contributor.authorLangellier, N.
dc.contributor.authorWatson, C. A.
dc.contributor.authorCegla, H. M.
dc.contributor.authorCostes, J.
dc.contributor.authorCharbonneau, D.
dc.contributor.authorCoffinet, A.
dc.contributor.authorLatham, D. W.
dc.contributor.authorLopez-Morales, M.
dc.contributor.authorMalavolta, L.
dc.contributor.authorMaldonado, J.
dc.contributor.authorMicela, G.
dc.contributor.authorMilbourne, T.
dc.contributor.authorMolinari, E.
dc.contributor.authorSaar, S. H.
dc.contributor.authorThompson, S.
dc.contributor.authorBuchschacher, N.
dc.contributor.authorCecconi, M.
dc.contributor.authorCosentino, R.
dc.contributor.authorGhedina, A.
dc.contributor.authorGlenday, A.
dc.contributor.authorGonzalez, M.
dc.contributor.authorLi, C. -H.
dc.contributor.authorLodi, M.
dc.contributor.authorLovis, C.
dc.contributor.authorPepe, F.
dc.contributor.authorPoretti, E.
dc.contributor.authorRice, K.
dc.contributor.authorSasselov, D.
dc.contributor.authorSozzetti, A.
dc.contributor.authorSzentgyorgyi, A.
dc.contributor.authorUdry, S.
dc.contributor.authorWalsworth, R.
dc.date.accessioned2019-07-03T15:30:03Z
dc.date.available2019-07-03T15:30:03Z
dc.date.issued2019-07
dc.identifier.citationCameron , A C , Mortier , A , Phillips , D , Dumusque , X , Haywood , R D , Langellier , N , Watson , C A , Cegla , H M , Costes , J , Charbonneau , D , Coffinet , A , Latham , D W , Lopez-Morales , M , Malavolta , L , Maldonado , J , Micela , G , Milbourne , T , Molinari , E , Saar , S H , Thompson , S , Buchschacher , N , Cecconi , M , Cosentino , R , Ghedina , A , Glenday , A , Gonzalez , M , Li , C -H , Lodi , M , Lovis , C , Pepe , F , Poretti , E , Rice , K , Sasselov , D , Sozzetti , A , Szentgyorgyi , A , Udry , S & Walsworth , R 2019 , ' Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum ' , Monthly Notices of the Royal Astronomical Society , vol. 487 , no. 1 , pp. 1082–1100 . https://doi.org/10.1093/mnras/stz1215en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 258803305
dc.identifier.otherPURE UUID: 112957bd-2942-4a7b-b995-f4bb85086e3e
dc.identifier.otherArXiv: http://arxiv.org/abs/1904.12186v1
dc.identifier.otherORCID: /0000-0002-8863-7828/work/59222243
dc.identifier.otherWOS: 000474907100084
dc.identifier.otherScopus: 85087388588
dc.identifier.urihttp://hdl.handle.net/10023/18038
dc.description.abstractThe time-variable velocity fields of solar-type stars limit the precision of radial-velocity determinations of their planets’ masses, obstructing detection of Earth twins. Since 2015 July, we have been monitoring disc-integrated sunlight in daytime using a purpose-built solar telescope and fibre feed to the HARPS-N stellar radial-velocity spectrometer. We present and analyse the solar radial-velocity measurements and cross-correlation function (CCF) parameters obtained in the first 3 yr of observation, interpreting them in the context of spatially resolved solar observations. We describe a Bayesian mixture-model approach to automated data-quality monitoring. We provide dynamical and daily differential-extinction corrections to place the radial velocities in the heliocentric reference frame, and the CCF shape parameters in the sidereal frame. We achieve a photon-noise-limited radial-velocity precision better than 0.43 m s−1 per 5-min observation. The day-to-day precision is limited by zero-point calibration uncertainty with an RMS scatter of about 0.4 m s−1. We find significant signals from granulation and solar activity. Within a day, granulation noise dominates, with an amplitude of about 0.4 m s−1 and an autocorrelation half-life of 15 min. On longer time-scales, activity dominates. Sunspot groups broaden the CCF as they cross the solar disc. Facular regions temporarily reduce the intrinsic asymmetry of the CCF. The radial-velocity increase that accompanies an active-region passage has a typical amplitude of 5 m s−1 and is correlated with the line asymmetry, but leads it by 3 d. Spectral line-shape variability thus shows promise as a proxy for recovering the true radial velocity.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2019, the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with the publisher's policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz1215en
dc.subjectTechniques: radial velocitiesen
dc.subjectSun: activityen
dc.subjectSun: faculae, plagesen
dc.subjectSun: granulationen
dc.subjectSunspotsen
dc.subjectPlanets and satellites: detectionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThree years of Sun-as-a-star radial-velocity observations on the approach to solar minimumen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz1215
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1904.12186en


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