Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega

TL;DR

This study uses the Keck/NIRC2 vortex coronagraph in Ms-band to set new, deeper limits on the presence of exoplanets around Vega, improving detection thresholds and ruling out certain planetary companions.

Contribution

It provides the deepest direct imaging detection limits for planets around Vega to date, combining imaging and radial velocity data for comprehensive constraints.

Findings

3 Jupiter mass detection limit beyond 12 au

Ruling out companions >8 Jupiter mass from 0.1 to 22 au

Detection limits of 2-3 Jupiter mass inside 4 au

Abstract

Gaps in circumstellar disks can signal the existence of planetary perturbers, making such systems preferred targets for direct imaging observations of exoplanets. Being one of the brightest and closest stars to the Sun, the photometric standard star Vega hosts a two-belt debris disk structure. Together with the fact that its planetary system is being viewed nearly face-on, Vega has been one of the prime targets for planet imaging efforts. Using the vector vortex coronagraph on Keck/NIRC2 in Ms-band at 4.67 $\mu$m, we report the planet detection limits from 1 au to 22 au for Vega with an on-target time of 1.8 h. We reach a 3 Jupiter mass limit exterior to 12 au, which is nearly an order of magnitude deeper than existing studies. Combining with existing radial velocity studies, we can confidently rule out the existence of companions more than ~8 Jupiter mass from 22 au down to 0.1 au for Vega. Interior and exterior to ~4 au, this combined approach reaches planet detection limits down to ~2-3 Jupiter mass using radial velocity and direct imaging, respectively. By reaching multi-Jupiter mass detection limits, our results are expected to be complemented by the planet imaging of Vega in the upcoming observations using the James Webb Space Telescope to obtain a more holistic understanding of the planetary system configuration around Vega.