The Doppler Method for the Detection of Exoplanets. Professor Artie Hatzes

Saturation and Blooming

       2.3.10 Fringing

       2.3.11 Persistence

       References

       3 Factors Influencing the Radial Velocity Measurement

       3.1 Instrumental Characteristics

       3.1.1 Wavelength Coverage

       3.1.2 Signal-to-noise Ratio

       3.1.3 Resolving Power

       3.2 Stellar Characteristics

       3.2.1 Stellar Rotational Velocity

       3.2.2 Spectral Line Strength

       3.2.3 Number Density of Spectral Lines

       3.3 RV Precision across Spectral Types

       3.3.1 Radial Velocities of High-mass Stars

       3.3.2 Radial Velocities of Low-mass Stars

       References

       4 Simultaneous Wavelength Calibration

       4.1 Instrumental Shifts

       4.2 Hollow Cathode Lamps

       4.2.1 Th–Ar

       4.2.2 HCL in the Infrared

       4.3 The Telluric Method

       4.4 Gas Absorption Cells

       4.4.1 The Hydrogen Fluoride Cell

       4.4.2 The Iodine Absorption Cell

       4.4.3 Absorption Cells at Infrared Wavelengths

       4.5 Laser Frequency Combs

       4.6 Fabry–Pérot Etalons

       4.7 The RV Precision of Modern Spectrographs

       References

       5 Calculating the Doppler Shifts: The Cross-correlation Method

       5.1 Mathematical Formalism

       5.2 Choice of Template

       5.2.1 Standard Stars

       5.2.2 Synthetic Masks

       5.2.3 Self-templates

       5.2.4 Mismatched Template and Stellar Spectra

       5.3 CCF Detection of Spectroscopic Binaries

       5.4 Fahlman–Glaspey Shift Detection

       References

       6 The Iodine Cell Method

       6.1 The Instrumental Profile

       6.2 Modeling the IP with the Iodine Cell Method

       6.3 Influence of Changes in the IP

       6.4 Ingredients for the Iodine Cell Method

       6.4.1 The Fiducial

       6.4.2 The Template

       6.5 Calculation of the Doppler Shift

       6.6 Construction of an Iodine Cell

       6.7 Closing Remarks

       References

       7 Frequency Analysis of Time Series Data

       7.1 Introduction

       7.2 The Discrete Fourier Transform

       7.2.1 Convolution

       7.2.2 Visualizing Fourier Transforms

       7.3 The Lomb–Scargle Periodogram

       7.4 The Generalized Lomb–Scargle Periodogram

       7.5 The Bayesian Generalized Lomb–Scargle Periodogram

       7.6 Comparison of the Types of Periodograms

       7.7 The Spectral Window

       7.8 The Nyquist Frequency and Aliasing

       7.9 Frequency Resolution

       7.10 Assessing the Statistical Significance