The Vector Vortex Coronagraph: Laboratory Results and First Light at Palomar Observatory

TL;DR

This paper presents laboratory results and first light observations of the vector vortex coronagraph, demonstrating its high contrast performance and potential for direct imaging of faint exoplanets and companions.

Contribution

It introduces the vector vortex coronagraph's laboratory performance and first on-sky detection, highlighting its efficiency and suitability for high-contrast exoplanet imaging.

Findings

Achieved contrast of ~1e-6 at 3 λ/D in lab tests.

Detected a brown dwarf companion 3000 times fainter than its host star.

Demonstrated the coronagraph's effectiveness in real observational conditions.

Abstract

High-contrast coronagraphy will be needed to image and characterize faint extra-solar planetary systems. Coronagraphy is a rapidly evolving field, and many enhanced alternatives to the classical Lyot coronagraph have been proposed in the past ten years. Here, we discuss the operation of the vector vortex coronagraph, which is one of the most efficient possible coronagraphs. We first present recent laboratory results, and then first light observations at the Palomar observatory. Our near-infrared H-band (centered at ~ 1.65 microns) and K-band (centered at ~ 2.2 microns) vector vortex devices demonstrated excellent contrast results in the lab, down to ~ 1e-6 at an angular separation of 3 lb/d. On sky, we detected a brown dwarf companion 3000 times fainter than its host star (HR 7672) in the Ks band (centered at ~2.15 microns), at an angular separation of ~ 2.5 lb/d. Current and next-generation high-contrast instruments can directly benefit from the demonstrated capabilities of such a vector vortex: simplicity, small inner working angle, high optical throughput (>90%), and maximal off-axis discovery space.