10.1.3 Na D
10.1.5 Hydroxyl 1.563 μm Absorption
10.5.2 Convective Blueshifts versus Line Strength
10.6.1 RV Jitter and Orbit Fitting
11 Dealing with Stellar Activity
11.1.1 The Pitfalls of Prewhitening
11.4 A Short Comparison of Filtering Methods
12 Contributions to the Error Budget
12.2 Changes in the Instrumental Setup
12.3.1 Electronic Noise Pickup
12.3.2 CCD Inhomogeneities and Discontinuities
12.3.3 Charge Transfer Effects
12.4 Errors in the Barycentric Correction
12.4.1 Inaccurate Time of Observations
12.4.2 Inaccurate Telescope Coordinates
12.4.3 Inaccurate Stellar Positions
12.4.4 Differential Barycentric Motion
12.6 Telluric Line Contamination
13 The Rossiter–McLaughlin Effect
13.1 Introduction
13.2 Origin of the Rossiter–McLaughlin Effect
13.3 The Rossiter–McLaughlin Effect in Exoplanets
13.3.1 The Radial Velocity Amplitude
13.3.2 The Spin–Orbit Alignment
To Gordon Walker and Bill Cochran, early pioneers in the radial velocity detection of exoplanets who inspired this work.
Preface
The first radial velocity (RV) measurements on a star using the Doppler method were made late in the 19th century. The discovery of the first exoplanet, found using the Doppler method, was made near the end of the 20th century. Why did the discovery of exoplanets take nearly one hundred years? In short, it is due to the spectacular improvement
