Journal
EXPERIMENTAL ASTRONOMY
Volume 49, Issue 1-2, Pages 73-84Publisher
SPRINGER
DOI: 10.1007/s10686-020-09654-z
Keywords
Echelle spectroscopy; Cross-correlation function; M-type stars; Stellar activity indicators
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Funding
- INAF through the competitive project FRONTIERA-2016
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The HARPS/HARPS-N Data Reduction Software (DRS) relies on the crosscorrelation between the observed spectra and a suitable stellar mask to compute a cross-correlation function (CCF) to be used both for the radial velocity (RV) computation and as an indicator of stellar lines asymmetry, induced for example by the stellar activity. Unfortunately the M2 mask currently used by the HARPS/HARPSN DRS for M-type stars results in heavily distorted CCFs. We created several new stellar masks in order to decrease the errors in the RVs and to improve the reliability of the activity indicators as the bisector's span. We obtained very good results with a stellar mask created from the theoretical line list provided by the VALD3 database for an early M-type star (T-eff=3500 K and log g = 4.5). The CCF's shape and relative activity indicators improved and the RV time-series allowed us to recover known exoplanets with periods and amplitudes compatible with the results obtained with HARPS-TERRA.
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