Measuring precise radial velocities on individual spectral lines. I. Validation of the method and application to mitigate stellar activity

TL;DR

This paper introduces a novel spectral line-based method for measuring stellar radial velocities, effectively mitigating stellar activity effects and improving precision in exoplanet detection efforts.

Contribution

The study presents a new approach to derive RVs from individual spectral lines, demonstrating its effectiveness in reducing stellar activity noise and correcting systematic instrumental effects.

Findings

RVs derived from the new method are consistent with standard HARPS data reduction.

Systematic night-to-night RV offsets of 0.4 m/s are identified and corrected.

Selective analysis of spectral lines can significantly reduce stellar activity-induced noise.

Abstract

Stellar activity is the main limitation to the detection of Earth-twins using the RV technique. Despite many efforts in trying to mitigate the effect of stellar activity using empirical and statistical techniques, it seems that we are facing an obstacle that will be extremely difficult to overcome using current techniques. In this paper, we investigate a novel approach to derive precise RVs considering the wealth of information present in high-resolution spectra. This new method consists in building a master spectrum from all observations and measure the RVs of each spectral line in a spectrum relative to it. When analysing several spectra, the final product is the RVs of each line as a function of time. We demonstrate on three stars intensively observed with HARPS that our new method gives RVs that are extremely similar to the ones derived from the HARPS data reduction software. Our new approach to derive RVs demonstrates that the non-stability of daily HARPS wavelength solution induces night-to-night RV offsets with an standard deviation of 0.4 m/s, and we propose a solution to correct for this systematic. Finally, and this is probably the most astrophysically relevant result of this paper, we demonstrate that some spectral lines are strongly affected by stellar activity while others are not. By measuring the RVs on two carefully selected subsample of spectral lines, we demonstrate that we can boost by a factor of 2 or mitigate by a factor of 1.6 the red noise induced by stellar activity in the 2010 RVs of Alpha Cen B. By measuring the RVs of each spectral line, we are able to reach the same RV precision as other approved techniques. In addition, this new approach allows to demonstrate that each line is differently affected by stellar activity. Preliminary results show that studying in details the behaviour of each spectral line is probably the key to overcome stellar activity.