Exoplanets can be detected with various observational techniques. Among them, radial
velocity (RV) has the key advantages of revealing the architecture of planetary systems and …

Measured spectral shifts due to intrinsic stellar variability (eg, pulsations, granulation) and
activity (eg, spots, plages) are the largest source of error for extreme-precision radial-velocity …

We present an analysis of Sun-as-a-star observations from four different high-resolution,
stabilized spectrographs—HARPS, HARPS-N, EXPRES, and NEID. With simultaneous …

With dedicated exoplanet surveys underway for multiple extreme-precision radial velocity
(EPRV) instruments, the near-future prospects of RV exoplanet science are promising …

We study the properties of line bisectors in the spectrum of the Sun-as-a-star, as observed
using the Integrated Sunlight Spectrometer (ISS) of the SOLIS project. Our motivation is to …

Thousands of exoplanet detections have been made over the last 25 years using Doppler
observations, transit photometry, direct imaging, and astrometry. Each of these methods is …

We describe the data reduction pipeline (DRP) for the Palomar Radial Velocity instrument
(PARVI). PARVI is a fiber-fed, high-resolution J and H band spectrometer that targets cool …

For solar-type stars, spots and their associated magnetic regions induce radial velocity
perturbations through the Doppler rotation signal and the suppression of convective …

The signal induced by a temperate, terrestrial planet orbiting a Sun-like star is an order of
magnitude smaller than the host stars' intrinsic variability. Understanding stellar activity is …

Measuring periodic changes in the line-of-sight velocities of stars via spectroscopy (the
“radial velocity technique”) is a well-established method to detect planets orbiting stars other …