The CHEOPS view of HD 95338b: refined transit parameters, and a search for exomoons

TL;DR

This paper refines the parameters of the HD 95338b exoplanet system using CHEOPS and TESS data, introduces a new methodology for exomoon detection, and sets constraints on potential exomoons in the system.

Contribution

It presents a novel exomoon search methodology applied to CHEOPS data, improving planetary parameters and establishing detection limits for exomoons.

Findings

Refined stellar and planetary parameters with reduced uncertainties.

Potential to detect exomoons as small as 0.8 Earth radii at 5 sigma.

Exclusion of exomoons around 0.6 Earth radii at 1 sigma.

Abstract

Despite the ever-increasing number of known exoplanets, no uncontested detections have been made of their satellites, known as exomoons. The quest to find exomoons is at the forefront of exoplanetary sciences. Certain space-born instruments are thought to be suitable for this purpose. We show the progress made with the CHaracterizing ExOPlanets Satellite (CHEOPS) in this field using the HD 95338 planetary system. We present a novel methodology as an important step in the quest to find exomoons. We utilize ground-based spectroscopic data in combination with Gaia observations to obtain precise stellar parameters. These are then used as input in the analysis of the planetary transits observed by CHEOPS and the Transiting Exoplanet Survey Satellite (TESS). In addition, we search for the signs of satellites primarily in the form of additional transits in the Hill sphere of the eccentric Neptune-sized planet HD 95338b in a sequential approach based on four CHEOPS visits. We also briefly explore the transit timing variations of the planet. We present refined stellar and planetary parameters, narrowing down the uncertainty on the planet-to-star radius ratio by a factor of $10$. We also pin down the ephemeris of HD 95338b. Using injection/retrieval tests, we show that a $5 \sigma$ detection of an exomoon would be possible at $R_{\rm Moon} = 0.8$~$R_\oplus$ with the methodology presented here. We exclude the transit of an exomoon in the system with $R_{\rm Moon} \approx 0.6$~$R_\oplus$ at the $1\sigma$ level. The algorithm used for finding the transit-like event can be used as a baseline for other similar targets, observed by CHEOPS or other missions.