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Andrew W. Howard measures the physical properties and population of exoplanets. In the 2013 study with Erik A. Petigura and Geoffrey W. Marcy, the team searched Kepler space telescope photometry and inserted synthetic exoplanet transits into real observations to measure transit survey completeness.^[ref]

Correcting missed detections changed the question from “how many candidates were found?” to the underlying exoplanet occurrence rate. For the study's 5–50-day orbital periods, the rising distribution flattened below about twice Earth's radius.

Erik A. Petigura studies exoplanet occurrence rates using transit observations. His 2013 study with Geoffrey W. Marcy and Andrew W. Howard independently searched Kepler space telescope photometry for small planets with orbital periods of $5$–$50$ days.

To estimate how many planets the search missed, the team injected synthetic exoplanet transit signals into the observations and ran the detection procedure again. Correcting for this recovery rate changed the inference from a count of detected candidates to an estimate of the underlying population. Their inferred size distribution flattened below roughly twice Earth's radius.^[ref]

Geoffrey W. Marcy worked on the radial velocity method for finding exoplanets, including precision iodine-cell Doppler calibration. His paper with R. Paul Butler combined a wide recorded stellar radiation spectrum with reference absorption lines introduced directly into the stellar beam.

Measuring a small Doppler shift requires distinguishing real stellar motion from instrumental changes. The superimposed reference constrains the spectrograph's wavelength scale and point spread function during the exposure, allowing the stellar shift to be fitted with those effects included. The paper reported year-long tests of the technique on three solar-type stars.^[ref]

R. Paul Butler develops precise stellar radial velocity measurements for detecting orbiting companions. With Geoffrey W. Marcy, he developed iodine-cell Doppler calibration, superimposing a dense reference spectrum on the same light entering a stellar spectrograph.

The reference lines constrain both the wavelength scale and the instrumental point spread function during the observation. Modeling them together with the shifted stellar radiation spectrum reduces errors caused by changes in the instrument. Their 1992 tests obtained a velocity scatter below $25\mathrm{m}{\mathrm{s}}^{-1}$ over a year, providing a practical foundation for searches for low-mass companions.^[ref]