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M. Barczys, J. E. Larkin (UCLA), A. Quirrenbach (UCSD), J. R. Graham (UCB)
We present the design of OSIRIS (OH-Suppressing InfraRed Imaging Spectrograph), an adaptive optics (AO) optimized, near infrared integral-field spectrograph. The instrument uses a lenslet array to sample a small rectangular patch of the sky at resolutions approaching the diffraction limit of the 10-meter Keck Telescope. OSIRIS will provide moderate spectral resolution (R~3800), and full broadband (z, J, H, and K) spectral coverage at over 1000 spatial locations in the AO-corrected field. The integral field design makes optimal use of the new large-format (20482) infrared arrays, and is well matched to the compact nature of AO targets. Furthermore, the spectral resolution is high enough to isolate background OH emission lines. By summing spectral channels uncontaminated with OH emission, OSIRIS will also produce very deep near infrared images.
We hope to begin construction of OSIRIS by the end of 2000 in the UCLA Infrared Astrophysics Lab, with delivery to the telescope by the first half of 2003. OSIRIS's simple design (e.g. only four cryogenic mechanisms and a fixed grating) should allow rapid construction, using many off-the-shelf components.
With the extremely low backgrounds of an AO spectrograph, many new scientific problems can be investigated. Key projects driving the design of OSIRIS are High-Redshift Galaxies, Brown Dwarfs, and Active Galactic Nuclei. Other possible programs include Kuiper Belt Objects, Gamma-Ray Bursts, Radio Galaxies, Quasar Host Galaxies, Planetary Science, the Galactic Center, and dense Star Formation Regions.
This poster will present the overall design of OSIRIS and some of its science goals. We will also present results from our performance/feasibility testing of the lenslet array which have been carried out on the OSIRIS Test Bed Spectrograph in the UCLA Infrared Astrophysics Lab. Development of the instrument concept is supported by the Keck Science Steering Committee and the NSF Center for Adaptive Optics.
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The author(s) of this abstract have provided an email address for comments about the abstract: barczysm@astro.ucla.edu