Public HARPS radial velocity database corrected for systematic errors

Abstract

Context. The High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph is mounted since 2003 at the ESO 3.6 m telescope in La Silla and provides state-of-the-art stellar radial velocity (RV) measurements with a precision down to ∼ 1 m s −1 . The spectra are extracted with a dedicated data-reduction software (DRS) and the RVs are computed by cross correlating with a numerical mask. Aims. The aim of this study is three-fold: (i) Create an easy access to the public HARPS RV data set. (ii) Apply the new public SpEctrum Radial Velocity AnaLyser (SERVAL) pipeline to the spectra, and produce a more precise RV data set. (iii) Check whether the precision of the RVs can be further improved by correcting for small nightly systematic effects. Methods. For each star observed with HARPS, we downloaded the publicly available spectra from the ESO archive, and recomputed the RVs with SERVAL. This was based on fitting each observed spectrum with a high signal-to-noise ratio template created by co-adding all the available spectra of that star. We then computed nightly zero points (NZPs) by averaging the RVs of quiet stars. Results. Analysing the RVs of the most RV-quiet stars, whose RV scatter is < 5 m s −1 , we find that SERVAL RVs are on average more precise than DRS RVs by a few percent. Investigating the NZP time series, we find three significant systematic effects, whose magnitude is independent of the software used for the RV derivation: (i) stochastic variations with a magnitude of ∼ 1 m s −1 ; (ii) longterm variations, with a magnitude of ∼ 1 m s −1 and a typical timescale of a few weeks; and (iii) 20-30 NZPs significantly deviating by few m s −1 . In addition, we find small ( 1 m s −1 ) but significant intra-night drifts in DRS RVs before the 2015 intervention, and in SERVAL RVs after it. We confirm that the fibre exchange in 2015 caused a discontinuous RV jump, which strongly depends on the spectral type of the observed star: from ∼ 14 m s −1 for late F-type stars, to ∼ −3 m s −1 for M dwarfs. The combined effect of extracting the RVs with SERVAL and correcting them for the systematics we find is an improved average RV precision: ∼ 5% improvement for spectra taken before the 2015 intervention, and ∼ 15% improvement for spectra taken after it. To demonstrate the quality of the new RV data set, we present an updated orbital solution of the GJ 253 two-planet system. Conclusions. Our NZP-corrected SERVAL RVs can be retrieved from a user-friendly, public database. It provides more than 212 000 RVs for about 3000 stars along with many auxiliary information, such as the NZP corrections, various activity indices, and DRS-CCF products.Differential RV from SERVAL corrected for BERV, SA, drift, (non-NZP corrected). (d) RV from DRS corrected for BERV, SA, drift, (non-NZP corrected). (e) Differential RV from SERVAL corrected for BERV, SA, drift, (non-NZP corrected, joint RV calculation with -pre and -post fibre upgrade data.) (f) Chromatic index from SERVAL. (g) Differential line width from SERVAL. (h) Hα index from SERV...

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