Simulation results for Robo-AO-2 using HAPA: a wavefront sensing technique for improving the adaptive optics correction of fainter stars

TL;DR

This paper presents simulated results of a hybrid wavefront sensing technique called HAPA, combining laser and natural guide stars to improve adaptive optics correction for fainter stars, enabling better exoplanet imaging from the ground.

Contribution

It introduces HAPA, a novel hybrid wavefront sensing method, and demonstrates its potential through simulations for Robo-AO-2, aiming to extend adaptive optics correction to fainter stars.

Findings

HAPA improves wavefront correction for fainter guide stars.

Simulations show effective correction with various NGS configurations.

Potential to increase observable exoplanet targets from ground-based telescopes.

Abstract

Direct imaging of exoplanets allows us to measure positions and chemical signatures of exoplanets. Given the limited resources for space observations where the atmosphere is absent, we want to make these measurements from the ground. However, it is difficult from the ground because it requires an adaptive optics system to provide an extremely well corrected wavefront to enable coronographic techniques. Currently only natural guide star AO systems have demonstrated the necessary wavefront correction for direct imaging of exoplanets. However, using a stellar source as the guide star for wavefront sensing limits the number of exoplanet systems we can directly image because it requires a relatively bright V~10 mag star. To increase the number of observable targets, we need to push the limit of natural guide stars to fainter magnitudes with high Strehl ratio correction. We propose to combine laser guide star (LGS) and natural guide star (NGS) wavefront sensing to achieve the high Strehl correction with fainter natural guide stars. We call this approach Hybrid Atmospheric Phase Analysis (HAPA); 'hapa' in Hawaiian means 'half' or 'of mixed ethnic heritage'. The relatively bright LGS is used for higher order correction, whereas the NGS is used for high accuracy lower order correction. We focus on demonstrating this approach using Robo-AO-2 at the UH 2.2m telescope on Maunakea with a UV Rayleigh laser at 355 nm. The laser focuses at 10 km altitude and has an equivalent magnitude of m_U~8. In this report specifically, we present simulated results of HAPA employed at Robo-AO-2, with the LGS system having a single configuration of 16x16 subaperture Shack-Hartmann wavefront sensor and the NGS system having 6 different configurations -- 16x16, 8x8, 5x5, 4x4, 2x2 and 1x1. We also discuss the on-sky experiments we plan to carry out with HAPA at the UH 2.2m telescope.