Status of the Integral Field Spectrograph for the Gemini Planet Imager

Details Status of the Integral Field Spectrograph for the Gemini Planet Imager Status of the Integral Field Spectrograph for the Gemini Planet Imager

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21544115c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #441.15; Bulletin of the American Astronomical Society, Vol. 42, p.403

Physics

Optics

Scientific paper

We present the status of construction and testing of the Integral Field Spectrograph (IFS) for the Gemini Planet Imager (GPI). The IFS is being constructed in the UCLA Infrared Laboratory as the science instrument. GPI is a facility class instrument for the Gemini Observatory being led by Bruce Macintosh at LLNL and involving eight institutions. The goals of GPI are to detect and characterize young, Jovian-mass planetary companions by distinguishing them from PSF speckle noise, to detect and measure debris disks through polarization, and to record low-resolution spectra from 0.98-2.4 microns. The IFS design is similar to the OSIRIS instrument at Keck and utilizes an infrared transmissive lenslet array to sample a rectangular field of view behind the "extreme” adaptive optics system. The IFS uses a Hawaii-2RG detector to produce a field of view greater than 2.8 x 2.8 arcseconds, with a spectral resolution in H band of R 45. The all transmissive powered optics of the IFS uses a prism instead of a grating. A cryogenic Wollaston prism can be inserted into the reimaging optic path to produce two images of orthogonal polarization states. The IFS is currently scheduled to be integrated into GPI in mid 2010, with first light expected in 2011. We will present the current status of the IFS and early test results.

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