Aditya R. Sengupta, Jordan Diaz, Matthew DeMartino, Rebecca Jensen-Clem, Sylvain Cetre, Elinor Gates, Kevin Bundy, Daren Dillon, Philip Hinz, Maïssa Salama, Nour Skaf, Olivier Guyon, Tara Crowe, Caleb Dobias, Stephen S. Eikenberry, Rodrigo Amezcua-Correa, Stephanos Yerolatsitis

Ground-based direct imaging of exoplanets at high contrast requires precise correction of atmospheric turbulence using adaptive optics (AO). The planet-to-star contrast ratio at small angular separations from the host star is often limited by non-common-path aberrations (NCPAs) seen only in the science plane. The photonic lantern (PL) can be used to sense aberrations at the final science imaging plane. This enables a two-stage wavefront control architecture, in which the first-stage wavefront sensor senses atmospheric turbulence and the PL senses NCPAs and other aberrations not seen by the first stage. We demonstrate closed-loop control of residual wavefront errors using a non-dispersed PL after first-stage AO correction on the Shane 3m telescope at Lick Observatory. Our results show that non-dispersed PLs can be used for second-stage wavefront sensing, enabling performance improvements via minimally invasive retrofits to existing AO systems.