AO4ELT5 Proceedings
Getting ready for GeMS 2.0: A workhorse AO facility
Sivo, Gaetano (Gemini South Observatory), Marin, Eduardo (Gemini South Observatory), Garrel, Vincent (Max Planck Institut fuer Extraterrestrische Physik), Neichel, Benoit (LAM), van Dam, Marcos (Flat Wavefront), Rigaut, Francois (Australian National University), Moreno, Cristian (Gemini South Observatory), Chirre, Emmanuel (Gemini South Observatory), Perez, Gabriel (Gemini South Observatory), Ebbers, Angelic (Gemini North Observatory), Collins, Paul (Gemini South Observatory), Vergara, Vicente (Gemini South Observatory), Toro, Eduardo (Gemini South Observatory), Diaz, Pablo (Gemini South Observatory), Chinn, Brian (Gemini South Observatory), Figueroa, Carlos (Gemini South Observatory), Donahue, Jeff (Gemini North Observatory), Gigoux, Pedro (Gemini South Observatory), Price, Ian (Australian National University), Herrald, Nick (Australian National University), Bennet, Francis (Australian National University), Carrasco, Rodrigo (Gemini South Observatory), Andersen, Morten (Gemini South Observatory), Angeloni, Rodolfo (Universidad de La Serena), Lazo, Manuel (Gemini South Observatory), Montes, Vanessa (Gemini South Observatory), Rutten, Rene (Gemini South Observatory)
AO systems aim at detecting and correcting for optical distortions induced by atmospheric turbulences. The Gemini South telescope has currently two main AO systems: the Gemini Multi Conjugated AO System GeMS and the Gemini Planet Imager GPI. GeMS is operational and regularly used for science observation delivering close to diffraction limit resolution over a large field of view (85×85 arcsec2). We first review the performance obtained this past year. Then we will go in the details of the strong modifications GeMS is currently having. We are integrating a new laser system in the laser guide star facility module. We are also advancing in the development of the new Natural Guide Star wavefront sensor. We present as well in this paper the preliminary results obtained with our new installed NGS mask that allows us better astrometric precision.
DOI: 10.26698/AO4ELT5.0093- Proceeding PDF
