The Doppler method for the detection of exoplanets /

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"Version: 20191201"--Title page verso.Includes bibliographical references.1. Introduction -- 1.1. The dawn of Doppler measurements -- 1.2. Early work on stellar radial velocity measurements -- 1.3. Toward precise stellar radial velocity measurements -- 1.4. The early hints of exoplanets -- 1.5. The 51 Peg revolution -- 1.6. The Doppler method2. The instruments for Doppler measurements -- 2.1. Echelle spectrographs -- 2.2. Fourier transform spectrometers -- 2.3. Charge-coupled device detectors3. Factors influencing the radial velocity measurement -- 3.1. Instrumental characteristics -- 3.2. Stellar characteristics -- 3.3. RV precision across spectral types4. Simultaneous wavelength calibration -- 4.1. Instrumental shifts -- 4.2. Hollow cathode lamps -- 4.3. The telluric method -- 4.4. Gas absorption cells -- 4.5. Laser frequency combs -- 4.6. Fabry-P?erot etalons -- 4.7. The RV precision of modern spectrographs5. Calculating the Doppler shifts : the cross-correlation method -- 5.1. Mathematical Formalism -- 5.2. Choice of template -- 5.3. CCF detection of spectroscopic binaries -- 5.4. Fahlman-Glaspey shift detection6. 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 -- 6.5. Calculation of the Doppler shift -- 6.6. Construction of an iodine cell -- 6.7. Closing remarks7. Frequency analysis of time series data -- 7.1. Introduction -- 7.2. The discrete fourier transform -- 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 -- 7.11. Finding multiperiodic signals in your data -- 7.12. Required number of observations -- 7.13. Frequency versus period8. Keplerian orbits -- 8.1. Orbital parameters -- 8.2. Describing the orbital motion -- 8.3. The radial velocity curve -- 8.4. The mass function -- 8.5. Mean orbital inclination -- 8.6. Eccentric orbits -- 8.7. Calculating Keplerian orbits -- 8.8. Dynamical effects -- 8.9. Barycentric corrections9. Avoiding false planets : rotational modulation -- 9.1. Introduction -- 9.2. Spots -- 9.3. Plage and faculae -- 9.4. Granulation and convective blueshift -- 9.5. Testing for rotational modulation10. Avoiding false planets : indicators of stellar activity -- 10.1. Activity indicators -- 10.2. Line depth ratios -- 10.3. Spectral line shapes -- 10.4. Chromatic RV variations -- 10.5. Use of individual lines -- 10.6. Radial velocity jitter -- 10.7. Activity cycles -- 10.8. Concluding remarks11. Dealing with stellar activity -- 11.1. Fourier filtering -- 11.2. High pass filtering -- 11.3. Gaussian processes -- 11.4. A short comparison of filtering methods -- 11.5. The RV challenge -- 11.6. Toward earth analogs12. Contributions to the error budget -- 12.1. Guiding errors -- 12.2. Changes in the instrumental setup -- 12.3. Detector errors -- 12.4. Errors in the Barycentric correction -- 12.5. The secular acceleration -- 12.6. Telluric line contamination -- 12.7. Moonlight contamination13. The Rossiter-McLaughlin effect -- 13.1. Introduction -- 13.2. Origin of the Rossiter-McLaughlin effect -- 13.3. The Rossiter-McLaughlin effect in exoplanets -- 13.4. Spin axis of the star.The study of exoplanets is one of the most vibrant fields of astrophysics today. Precise radial velocity (RV, or Doppler) measurements created the field by discovering the first exoplanets. Although employed for more than 30 years, RV measurements are still relevant today; when used with the transit method it provides the first characterization of exoplanets in terms of its mass, radius, and bulk density. These provide the first clues as to the internal structure of the exoplanet. With this text, Hatzes provides a deep understanding of the Doppler method, including how to achieve RV measurement precision, as well as the challenges, limitations, and potential of the technique. It also covers other aspects of the method such instrumentation, wavelength calibration, finding periodic signals in RV time series, signal interpretation, and Keplerian orbits. It's an essential reference for researchers and graduate students in the field of exoplanets, and additionally stellar spectroscopists and instrumentalists.Researchers and graduate students in the field of exoplanets.Also available in print.Mode of access: World Wide Web.System requirements: Adobe Acrobat Reader, EPUB reader, or Kindle reader.A.P. Hatzes is one of the pioneers in searching for extrasolar planets with over 30 years' experience in the use of precise stellar radial velocity measurements. Besides searching for extrasolar planets, he has also extended the use of these types of measurements to the study of stellar oscillations in magnetic A-type and K giant stars. In 1988 he joined Bill Cochran at the University of Texas at Austin for the start of the McDonald Observatory Planet Search Program. He has been working exoplanets ever since. Hatzes is currently director of the Thuringian State Observatory and Professor of Physics and Astronomy at the Friedrich-Schiller-University in Germany.Title from PDF title page (viewed on January 6, 2020).

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: .,

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1 online resource (various pagings) :illustrations (some color).

Language

English

ISBN/ISSN

9780750316897

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523

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Subject(s)

SCIENCE / Astronomy.
Solar system - the Sun & planets.
Extrasolar planets
Astronomical spectroscopy.

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A.P. Hatzes.

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