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Table A.1.
Description of the time series available for the HARPS-N solar data.
| Name | Description | Unit | Type |
|---|---|---|---|
| Filename | Name of the observation | – | STRING |
| Date BJD | Barycentric Julian Date minus 2 400 000 | days | FLOAT |
| RV raw | RV of the Sun in the Solar System barycentric rest frame | m s−1 | FLOAT |
| RV | RV of the Sun in the heliocentric rest frame, corrected for differential extinction. This value is obtained by subtracting Berv bary to helio and RV diff extinction to RV raw | m s−1 | FLOAT |
| RV err | RV error | m s−1 | FLOAT |
| Rhk | log( ) calcium activity index |
dex | FLOAT |
| Rhk err | log( ) calcium activity index error |
dex | FLOAT |
| Smw | S Mount Wilson calcium activity index | – | FLOAT |
| Smw err | S Mount Wilson calcium activity index error | – | FLOAT |
| Bis Span | Bisector span of the CCF | m s−1 | FLOAT |
| Bis Span err | Bisector span error of the CCF | m s−1 | FLOAT |
| FWHM raw | Raw FWHM of the CCF | m s−1 | FLOAT |
| FWHM | FWHM of the CCF, corrected for the solar ecliptic obliquity and Earth orbit eccentricity. See Sect. 3.2 in Collier Cameron et al. (2019) for more information. We note that in that paper, the authors have to optimise the value of γ corresponding to the fraction of the observed v sin i. They found a value of 1.04 for the old DRS solar data. Performing the same optimisation for the new DRS data lead to a value of 1.15. | m s−1 | FLOAT |
| FWHM err | FWHM error of the CCF | m s−1 | FLOAT |
| Contrast raw | Raw contrast of the CCF | % | FLOAT |
| Contrast | Contrast of the CCF, corrected for the FWHM correction so that the equivalent width of the CCF is conserved. See Sect. 3.2 in Collier Cameron et al. (2019) for more information | % | FLOAT |
| Contrast err | Contrast error of the CCF | % | FLOAT |
| Berv | Barycentric Earth RV correction | m s−1 | FLOAT |
| Berv bary to helio | Correction to change from the Solar System barycentric to heliocentric rest frame. To change from the heliocentric to barycentric rest frame, just add this term to RV | m s−1 | FLOAT |
| RV diff extinction | Estimation of the RV effect induced by differential extinction. See Sect. 2.4 in Collier Cameron et al. (2019) for more information. To include the effect of differential extinction, just add this value to RV | m s−1 | FLOAT |
| Airmass | Sun airmass | – | FLOAT |
| Coordinates | Sun coordinates | hms / dms | STRING |
| Texp | Exposure time | s | FLOAT |
| Sn order 10 | Signal to noise in order 10 | – | FLOAT |
| Sn order 20 | Signal to noise in order 20 | – | FLOAT |
| Sn order 30 | Signal to noise in order 30 | – | FLOAT |
| Sn order 40 | Signal to noise in order 40 | – | FLOAT |
| Sn order 50 | Signal to noise in order 50 | – | FLOAT |
| Sn order 60 | Signal to noise in order 60 | – | FLOAT |
| Obs quality | Quality flag to assess the observation’s quality (no clouds, no calima). Data with values ≥0.99 are all excellent. See Sect. 2.3 in Collier Cameron et al. (2019) for more information. | – | FLOAT |
| DRS quality | Quality flag of the data reduction software (true for good, false for bad) | – | BOOLEAN |
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