28 June 2006 OSIRIS: a diffraction limited integral field spectrograph for Keck
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We present an overview of the OSIRIS integral field spectrograph which was recently commissioned on the Keck II Telescope. OSIRIS works with the Keck Adaptive Optics system and utilizes an infrared transmissive lenslet array to sample a rectangular field of view at close to the Keck diffraction limit. By packing the spectra close together (2 pixel rows per spectrum) and using the Rockwell Hawaii-2 detector (wavelengths between 1 and 2.5 microns), we achieve a relatively large field of view (up to 6."4) while maintaining full broad-band spectral coverage at a resolution of 3800. Among the challenges of the instrument are: a fully cryogenic design (approximately 250 kg are brought down to 55K); four spatial scales from 0."02 to 0."10; extremely low wavefront error (approximately 25 nm of non-common path error); large all aluminum optics for the spectrograph; extremely repeatable spectral formats; and a sophisticated data reduction pipeline. OSIRIS also serves as a starting point for our design of IRIS which is a planned integral field spectrograph for the Thirty Meter Telescope.
© (2006) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
James Larkin, Matthew Barczys, Alfred Krabbe, Sean Adkins, Ted Aliado, Paola Amico, George Brims, Randy Campbell, John Canfield, Thomas Gasaway, Allan Honey, Christof Iserlohe, Christopher A. Johnson, Evan Kress, David LaFreniere, James Lyke, Ken Magnone, Nick Magnone, Michael McElwain, Juleen Moon, Andreas Quirrenbach, Gunnar Skulason, Inseok Song, Michael Spencer, Jason Weiss, Shelley Wright, "OSIRIS: a diffraction limited integral field spectrograph for Keck", Proc. SPIE 6269, Ground-based and Airborne Instrumentation for Astronomy, 62691A (28 June 2006); doi: 10.1117/12.672061; https://doi.org/10.1117/12.672061

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