On-sky demonstration of second-stage wavefront control with a photonic lantern
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arXiv
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| Autores principales: | , , , , , , , , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866909924802428928 |
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| author | Sengupta, Aditya R. Diaz, Jordan DeMartino, Matthew Jensen-Clem, Rebecca Cetre, Sylvain Gates, Elinor Bundy, Kevin Dillon, Daren Hinz, Philip Salama, Maïssa Skaf, Nour Guyon, Olivier Crowe, Tara Dobias, Caleb Eikenberry, Stephen S. Amezcua-Correa, Rodrigo Yerolatsitis, Stephanos |
| author_facet | Sengupta, Aditya R. Diaz, Jordan DeMartino, Matthew Jensen-Clem, Rebecca Cetre, Sylvain Gates, Elinor Bundy, Kevin Dillon, Daren Hinz, Philip Salama, Maïssa Skaf, Nour Guyon, Olivier Crowe, Tara Dobias, Caleb Eikenberry, Stephen S. Amezcua-Correa, Rodrigo Yerolatsitis, Stephanos |
| contents | 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_20560 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | On-sky demonstration of second-stage wavefront control with a photonic lantern Sengupta, Aditya R. Diaz, Jordan DeMartino, Matthew Jensen-Clem, Rebecca Cetre, Sylvain Gates, Elinor Bundy, Kevin Dillon, Daren Hinz, Philip Salama, Maïssa Skaf, Nour Guyon, Olivier Crowe, Tara Dobias, Caleb Eikenberry, Stephen S. Amezcua-Correa, Rodrigo Yerolatsitis, Stephanos Instrumentation and Methods for Astrophysics 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. |
| title | On-sky demonstration of second-stage wavefront control with a photonic lantern |
| topic | Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2511.20560 |