Stacked Periodograms as a Probe of Exoplanetary Populations

TL;DR

This paper introduces a novel method using stacked periodograms of radial velocity data to statistically detect exoplanet populations, even when individual planets are not directly detectable, aiding population-level studies.

Contribution

The paper proposes and demonstrates a new stacking periodogram technique to analyze existing RV datasets for exoplanet population detection, overcoming individual detection limitations.

Findings

Detected a marginally significant exoplanet population signal in existing data.

Method shows promise for identifying populations even when individual planets are not detectable.

Analysis suggests potential for future population studies with improved data.

Abstract

Ongoing, extreme-precision Doppler radial velocity surveys seek planets with masses less than several M$_\oplus$; population-level studies to determine the distribution of planetary masses, however, remain difficult due to the required observational time investment, as well as challenges associated with robustly detecting the lowest mass planets. We outline a novel approach that leverages extensive, existing RV datasets to constrain masses of exoplanet populations: stacking periodograms of RV timeseries across many targets. We show that an exoplanet population may be statistically identifiable in the stacked periodogram, even when individual planets do not pass the threshold of detection. We discuss analytical, statistical properties of the stacked periodogram, perform simulations to demonstrate the efficacy of the method, and investigate the influence of semi-structured window functions and stellar activity. Analysis of the Lick-Carnegie Exoplanet Survey data set reveals a marginally significant ($1.6\sigma$) signal consistent with a population of exoplanets occupying $3-7$ day periods with typical $K$ between $1.6-5.1$ m s$^{-1}$. More detailed investigation of signals associated with stellar activity and yearly systematics may be necessary to confirm this result or detect other underlying Keplerian contributions.