Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorDumusque, X.
dc.contributor.authorCretignier, M.
dc.contributor.authorSosnowska, D.
dc.contributor.authorBuchschacher, N.
dc.contributor.authorLovis, C.
dc.contributor.authorPhillips, D.F.
dc.contributor.authorPepe, F.
dc.contributor.authorAlesina, F.
dc.contributor.authorBuchhave, L.A.
dc.contributor.authorBurnier, J.
dc.contributor.authorCecconi, M.
dc.contributor.authorCegla, H.M.
dc.contributor.authorCloutier, R.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorCosentino, R.
dc.contributor.authorGhedina, A.
dc.contributor.authorGonzález, M.
dc.contributor.authorHaywood, R.D.
dc.contributor.authorLatham, D.W.
dc.contributor.authorLodi, M.
dc.contributor.authorLópez-Morales, M.
dc.contributor.authorMaldonado, J.
dc.contributor.authorMalavolta, L.
dc.contributor.authorMicela, G.
dc.contributor.authorMolinari, E.
dc.contributor.authorMortier, A.
dc.contributor.authorPérez Ventura, H.
dc.contributor.authorPinamonti, M.
dc.contributor.authorPoretti, E.
dc.contributor.authorRice, K.
dc.contributor.authorRiverol, L.
dc.contributor.authorRiverol, C.
dc.contributor.authorSan Juan, J.
dc.contributor.authorSégransan, D.
dc.contributor.authorSozzetti, A.
dc.contributor.authorThompson, S.J.
dc.contributor.authorUdry, S.
dc.contributor.authorWilson, T.G.
dc.date.accessioned2021-05-11T10:30:05Z
dc.date.available2021-05-11T10:30:05Z
dc.date.issued2021-04
dc.identifier.citationDumusque , X , Cretignier , M , Sosnowska , D , Buchschacher , N , Lovis , C , Phillips , D F , Pepe , F , Alesina , F , Buchhave , L A , Burnier , J , Cecconi , M , Cegla , H M , Cloutier , R , Collier Cameron , A , Cosentino , R , Ghedina , A , González , M , Haywood , R D , Latham , D W , Lodi , M , López-Morales , M , Maldonado , J , Malavolta , L , Micela , G , Molinari , E , Mortier , A , Pérez Ventura , H , Pinamonti , M , Poretti , E , Rice , K , Riverol , L , Riverol , C , San Juan , J , Ségransan , D , Sozzetti , A , Thompson , S J , Udry , S & Wilson , T G 2021 , ' Three years of HARPS-N high-resolution spectroscopy and precise radial velocity data for the Sun ' , Astronomy and Astrophysics , vol. 648 , A103 . https://doi.org/10.1051/0004-6361/202039350en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 274091652
dc.identifier.otherPURE UUID: eea62093-0a4b-4574-96fe-7a74fd9344d5
dc.identifier.otherRIS: urn:DD0DD60E244C6E358EEA1B29B4C71E61
dc.identifier.otherScopus: 85104681159
dc.identifier.otherORCID: /0000-0002-8863-7828/work/93514395
dc.identifier.otherORCID: /0000-0001-8749-1962/work/93515204
dc.identifier.otherWOS: 000642516900001
dc.identifier.urihttps://hdl.handle.net/10023/23155
dc.descriptionFunding: XD is grateful to The Branco Weiss Fellowship-Society in Science for its financial support. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 851555/SCORE). ACC acknowledges support from the Science and Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. This work has been carried out in the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). AM acknowledges support from the senior Kavli Institute Fellowships. This research used the DACE platform developed in the frame of PlanetS (https://dace.unige.ch). This work was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute (RDH).en
dc.description.abstractContext. The solar telescope connected to HARPS-N has been observing the Sun since the summer of 2015. Such a high-cadence, long-baseline data set is crucial for understanding spurious radial-velocity signals induced by our Sun and by the instrument. On the instrumental side, this data set allowed us to detect sub- m s-1 systematics that needed to be corrected for. Aims. The goals of this manuscript are to (i) present a new data reduction software for HARPS-N, (ii) demonstrate the improvement brought by this new software during the first three years of the HARPS-N solar data set, and (iii) release all the obtained solar products, from extracted spectra to precise radial velocities. Methods. To correct for the instrumental systematics observed in the data reduced with the current version of the HARPS-N data reduction software (DRS version 3.7), we adapted the newly available ESPRESSO DRS (version 2.2.3) to HARPS-N and developed new optimised recipes for the spectrograph. We then compared the first three years of HARPS-N solar data reduced with the current and new DRS. Results. The most significant improvement brought by the new DRS is a strong decrease in the day-to-day radial-velocity scatter, from 1.27 to 1.07 m s-1; this is thanks to a more robust method to derive wavelength solutions, but also to the use of calibrations closer in time. The newly derived solar radial-velocities are also better correlated with the chromospheric activity level of the Sun in the long term, with a Pearson correlation coefficient of 0.93 compared to 0.77 before, which is expected from our understanding of stellar signals. Finally, we also discuss how HARPS-N spectral ghosts contaminate the measurement of the calcium activity index, and we present an efficient technique to derive an index free of instrumental systematics. Conclusions. This paper presents a new data reduction software for HARPS-N and demonstrates its improvements, mainly in terms of radial-velocity precision, when applied to the first three years of the HARPS-N solar data set. Those newly reduced solar data, representing an unprecedented time series of 34 550 high-resolution spectra and precise radial velocities, are released alongside this paper. Those data are crucial to understand stellar activity signals in solar-type stars further and develop the mitigating techniques that will allow us to detect other Earths.
dc.format.extent19
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysicsen
dc.rightsCopyright © ESO 2021. 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 final published version of the work, which was originally published at https://doi.org/10.1051/0004-6361/202039350.en
dc.subjectSun: activityen
dc.subjectTechniques: radial velocitiesen
dc.subjectMethods: data analysisen
dc.subjectInstrumentation: spectrographsen
dc.subjectAstronomical databases: miscellaneousen
dc.subjectPlanets and satellites: detectionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThree years of HARPS-N high-resolution spectroscopy and precise radial velocity data for the Sunen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
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/10.1051/0004-6361/202039350
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/R00824/1en


This item appears in the following Collection(s)

Show simple item record