What question did this study set out to answer?

This work aims to summarize advancements in radial velocity methods for measuring exoplanet masses and orbits.

June 29, 2026Annual Review of Astronomy and Astrophysics1 citationsOpen Access

Precise Radial Velocities

JBJennifer BurtCalifornia Institute of Technology XDX. DumusqueUniversity of Geneva SHSamuel HalversonJet Propulsion Laboratory

Key Points

This work aims to summarize advancements in radial velocity methods for measuring exoplanet masses and orbits.
Review of radial velocity methodologies over the past 20 years
Analysis of modern high-resolution optical and near-infrared spectrograph designs
Evaluation of data processing techniques to reduce instrument noise and stellar variability.
Enhanced calibration methods achieve stability of ≤50 cm s −1 over years
Increased accuracy in determining exoplanet mass measurements
Improved techniques for distinguishing planetary signals from stellar activity.

Abstract

Precise measurements of a star's radial velocity (RV) made using extremely stable, high-resolution, optical or near-infrared spectrographs can be used to determine the masses and orbital parameters of gravitationally bound extrasolar planets (exoplanets). Indeed, RV surveys and follow-up efforts have provided the vast majority of published exoplanet mass measurements and, in doing so, have enabled studies of exoplanet interior and atmospheric compositions. We review the current state of the RV field, with particular attention to: ▪ The evolution of precise RV methodologies over the past 2 decades. ▪ Modern RV spectrograph designs that can be calibrated to a stability level of ≤50 cm s −1 over timescales of years. ▪ RV data reduction and postprocessing techniques that minimize the impact of instrument systematics and stellar variability. ▪ Techniques for detecting exoplanets in RV data and disentangling planetary signals from stellar variability.

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