Table A.1
List of activity indicators used in the analysis.
| Chromospheric line indicators (d): | |||||||
|---|---|---|---|---|---|---|---|
| Indicator | Central [Å] | λ | Central Δλ(a) | Left Δλ(b) | Right Δλ(b) | Examined in (c) | Description |
| Hα | 6562.8 | ±40 km s−1 | −500 to −300 km s−1 | 300 to 500 km s−1 | Ze18, T-O18, Fu19, Sch19, La21, Je22, Sch22, Fu23 | Chromospheric lines can be characterised by their emission flux in the line core. This emission flux can be measured from the line’s pseudo-equivalent width (pEW) or line index, as defined in Sch19 and Ze18, respectively, for the data used here. The pEW is the equivalent width of the line with respect to a pseudo-continuum, with the spectrum of a similar non-active star subtracted from it to remove photospheric contributions. The line index is the ratio of mean flux around the line centre to the flux in reference bandpasses on either sides of the line, regions assumed to not be affected by stellar activity. Both pEW and line index measure the 0th moment of the line (i.e. depth, area, or integrated flux). We present the different lines of the Ca II infrared triplet and the Na I doublet in different rows. | |
| Ca IRTa | 8498.0 | ±15 km s−1 | ±40 km s−1 from 8492.0 Å | ±40 km s−1 from 8504.0 Å | " | ||
| Ca IRTb | 8542.1 | ±15 km s−1 | −300 to −200 km s−1 | 250 to 350 km s−1 | " | ||
| Ca IRTc | 8662.1 | ±15 km s−1 | −300 to −200 km s−1 | 200 to 300 km s−1 | " | ||
| Na D1 | 5895.9 | ±15 km s−1 | ±40 km s−1 from 5885.0 Å | ±40 km s−1 from 5892.9 Å | Ze18, Fu19, Sch19, Je22, Sch22 | ||
| Na D2 | 5889.9 | ±15 km s−1 | ±40 km s−1 from 5892.9 Å | ±40 km s−1 from 5905.0 Å | ″ | ||
| He I D3 | 5875.6 | ±2.5 Å | ±1.25 Å from 5871.1 Å | ±1.25 Å from 5881.1 Å | Sch19, Fu20, Je22, Sch22 | ||
| He I λ10 830 Å | 10830.3 | ±0.25 Å | ±1.00 Å from 10818.0 Å | ±1.00 Å from 10871.7 Å | " | ||
| Paβ | 12818.1 | ±0.25 Å | ±1.00 Å from 12813.5 Å | ±1.00 Å from 12822.5 Å | Sch19, Je22, Sch22 | ||
| Photospheric absorption band indices: | |||||||
| Indicator | Numerator Δλ [Å] | Denominator Δλ [Å] | Examined in (c) | Description | |||
| CaH 2 | 6815.1 − 6817.1 | 6811.1 − 6813.1 | Sch21, Je22 | Photospheric bands can cover multiple spectral orders and are blended with other spectral features, which challenges the measurement of their pEW or line index, as typically done with chromospheric lines. Instead, photospheric band indices can be defined as the ratio of mean fluxes in two different small ranges on either side of the band head (Sch19). Similarly to chromospheric line indicators, these indices measure the 0th moment of the band absorption lines. | |||
| CaH 3 | 6972.1 − 6975.1 | 7045.1 − 7048.1 | " | ||||
| TiO λ7048 Å | 7054.1 − 7058.1 | 7044.1 − 7048.1 | Sch19, Sch22, Je22, Fu23 | ||||
| TiO λ8428 Å | 8433.7 − 8437.7 | 8428.2 − 8432.2 | " | ||||
| TiO λ8858 Å | 8860.1 − 8862.1 | 8856.6 − 8858.6 | " | ||||
| VO λ7434 Å | 7433.9 − 7434.9 | 7432.3 − 7433.3 | Sch19, Sch22, Je22 | ||||
| VO λ7940 Å | 7939.5 − 7941.5 | 7933.8 − 7935.8 | ″ | ||||
| FeH WFB | 9895.3 − 9904.3 | 9884.3 − 9893.3 | Sch21, Je22 | ||||
| Diagnostic indicators: | |||||||
| Indicator | Examined in(c) | Description | |||||
| chromatic index (CRX) (e) | Ze18, T-O18, La21, Je22, Sch22 | The CRX measures wavelength-dependent changes in the RVs. It is defined as the slope between the order-wise RVs and the average logarithmic wavelength of the order (Ze18). | |||||
| differential line width (dLW) (e) | Ze18, T-O18, La21, Je22 | The dLW measures differential variations in the absorption line widths of the observed spectrum with respect to a spectral template when performing a template matching minimisation (Ze18). It traces similar variations as the CCF FWHM and measures the 2nd moment of the line profile (i.e. variance). | |||||
| CCF Full width at half maximum (CCF-FWHM) (f) | La20, La21, Je22, Sch22 | The CCF represents an average shape of the stellar absorption lines, hence, its profile can be used to trace activity effects. The FWHM and the contrast are typically derived from a Gaussian fit to the CCF. The FWHM measures changes in the average width of the absorption lines (2nd moment of the CCF). The contrast traces the 0th moment of the CCF. The BIS is the difference between the average RV of the top region of the CCF profile and the average RV of the bottom region, originally defined by Queloz et al. (2001). It traces asymmetries in the line profile, so it measures the 3rd moment of the profile (skewness). | |||||
| CCF bisector inverse slope (CCF-BIS) (f) | " | ||||||
| CCF-contrast (f) | " | ||||||
References. Ze18: Zechmeister et al. (2018); Sch19: Schöfer et al. (2019); Sch21: Schöfer (2021); La20: Lafarga et al. (2020); T-O18: Tal-Or et al. (2018); Fu19: Fuhrmeister et al. (2019); La21: Lafarga et al. (2021); Je22: Jeffers et al. (2022); Sch22: Schöfer et al. (2022); Fu23: Fuhrmeister et al. (2023).
Notes. (a) Passband Δλ used to integrate the flux coming from the central line, indicated in km s−1 from the central line, unless otherwise specified (i.e. indicated in Å for the indicators computed following Sch19). (b) Left and right bandpasses Δλ at either side of the central line used as continuum reference, indicated in km s−1 from the central line, unless otherwise specified (i.e. indicated in km s−1 from a different reference wavelength for the Na I doublet lines, and indicated in Å from a different reference wavelength for the indicators computed following Sch19). (c) Listing only works by the CARMENES consortium, where underline indicates the reference where the indicator is defined. Quote (") indicates that the references are the same as in the row above. (d) The indicators calculated following Zechmeister et al. (2018) are dimensionless indices, while the indicators from Sch 19, Sch22 are pEWs (in Å) calculated after subtracting an inactive reference star spectrum. (e) Calculated for the VIS and NIR channel. (f) Calculated only for the VIS channel.
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