Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega
Bin B. Ren, Nicole L. Wallack, Spencer A. Hurt, Dimitri Mawet, Aarynn, L. Carter, Daniel Echeverri, Jorge Llop-Sayson, Tiffany Meshkat, Rebecca, Oppenheimer, Jonathan Aguilar, Eric Cady, Elodie Choquet, Garreth Ruane,, Gautum Vasisht, Marie Ygouf

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 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…
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Taxonomy
TopicsStellar, planetary, and galactic studies · Astrophysics and Star Formation Studies · Astro and Planetary Science
