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Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum
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dc.contributor.author | Cameron, A. Collier | |
dc.contributor.author | Mortier, A. | |
dc.contributor.author | Phillips, D. | |
dc.contributor.author | Dumusque, X. | |
dc.contributor.author | Haywood, R. D. | |
dc.contributor.author | Langellier, N. | |
dc.contributor.author | Watson, C. A. | |
dc.contributor.author | Cegla, H. M. | |
dc.contributor.author | Costes, J. | |
dc.contributor.author | Charbonneau, D. | |
dc.contributor.author | Coffinet, A. | |
dc.contributor.author | Latham, D. W. | |
dc.contributor.author | Lopez-Morales, M. | |
dc.contributor.author | Malavolta, L. | |
dc.contributor.author | Maldonado, J. | |
dc.contributor.author | Micela, G. | |
dc.contributor.author | Milbourne, T. | |
dc.contributor.author | Molinari, E. | |
dc.contributor.author | Saar, S. H. | |
dc.contributor.author | Thompson, S. | |
dc.contributor.author | Buchschacher, N. | |
dc.contributor.author | Cecconi, M. | |
dc.contributor.author | Cosentino, R. | |
dc.contributor.author | Ghedina, A. | |
dc.contributor.author | Glenday, A. | |
dc.contributor.author | Gonzalez, M. | |
dc.contributor.author | Li, C. -H. | |
dc.contributor.author | Lodi, M. | |
dc.contributor.author | Lovis, C. | |
dc.contributor.author | Pepe, F. | |
dc.contributor.author | Poretti, E. | |
dc.contributor.author | Rice, K. | |
dc.contributor.author | Sasselov, D. | |
dc.contributor.author | Sozzetti, A. | |
dc.contributor.author | Szentgyorgyi, A. | |
dc.contributor.author | Udry, S. | |
dc.contributor.author | Walsworth, R. | |
dc.date.accessioned | 2019-07-03T15:30:03Z | |
dc.date.available | 2019-07-03T15:30:03Z | |
dc.date.issued | 2019-07 | |
dc.identifier | 258803305 | |
dc.identifier | 112957bd-2942-4a7b-b995-f4bb85086e3e | |
dc.identifier | 000474907100084 | |
dc.identifier | 85087388588 | |
dc.identifier.citation | Cameron , 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/stz1215 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1904.12186v1 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/59222243 | |
dc.identifier.uri | https://hdl.handle.net/10023/18038 | |
dc.description.abstract | The 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.format.extent | 14810010 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Techniques: radial velocities | en |
dc.subject | Sun: activity | en |
dc.subject | Sun: faculae, plages | en |
dc.subject | Sun: granulation | en |
dc.subject | Sunspots | en |
dc.subject | Planets and satellites: detection | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | European Commission | 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 | 10.1093/mnras/stz1215 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/1904.12186 | en |
dc.identifier.grantnumber | ST/R00824/1 | en |
dc.identifier.grantnumber | ST/R003203/1 | en |
dc.identifier.grantnumber | en |
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