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Proceedings Paper

Design and development of MOSFIRE: the multi-object spectrometer for infrared exploration at the Keck Observatory
Author(s): Ian S. McLean; Charles C. Steidel; Harland Epps; Keith Matthews; Sean Adkins; Nicholas Konidaris; Bob Weber; Ted Aliado; George Brims; John Canfield; John Cromer; Jason Fucik; Kristin Kulas; Greg Mace; Ken Magnone; Hector Rodriguez; Eric Wang; Jason Weiss
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Paper Abstract

MOSFIRE is a unique multi-object spectrometer and imager for the Cassegrain focus of the 10 m Keck 1 telescope. A refractive optical design provides near-IR (0.97 to 2.45 μm) multi-object spectroscopy over a 6.14' x 6.14' field of view with a resolving power of R~3,270 for a 0.7" slit width (2.9 pixels in the dispersion direction), or imaging over a field of view of 6.8' diameter with 0.18" per pixel sampling. A single diffraction grating can be set at two fixed angles, and order-sorting filters provide spectra that cover the K, H, J or Y bands by selecting 3rd, 4th, 5th or 6th order respectively. A folding flat following the field lens is equipped with piezo transducers to provide tip/tilt control for flexure compensation at the 0.1 pixel level. A special feature of MOSFIRE is that its multiplex advantage of up to 46 slits is achieved using a cryogenic Configurable Slit Unit or CSU developed in collaboration with the Swiss Centre for Electronics and Micro Technology (CSEM). The CSU is reconfigurable under remote control in less than 5 minutes without any thermal cycling of the instrument. Slits are formed by moving opposable bars from both sides of the focal plane. An individual slit has a length of 7.1" but bar positions can be aligned to make longer slits. When masking bars are removed to their full extent and the grating is changed to a mirror, MOSFIRE becomes a wide-field imager. Using a single, ASIC-driven, 2K x 2K H2-RG HgCdTe array from Teledyne Imaging Sensors with exceptionally low dark current and low noise, MOSFIRE will be extremely sensitive and ideal for a wide range of science applications. This paper describes the design and testing of the instrument prior to delivery later in 2010.

Paper Details

Date Published: 20 July 2010
PDF: 12 pages
Proc. SPIE 7735, Ground-based and Airborne Instrumentation for Astronomy III, 77351E (20 July 2010); doi: 10.1117/12.856715
Show Author Affiliations
Ian S. McLean, Univ. of California, Los Angeles (United States)
Charles C. Steidel, California Institute of Technology (United States)
Harland Epps, UCO/Lick Observatory, Univ. of California, Santa Cruz (United States)
Keith Matthews, California Institute of Technology (United States)
Sean Adkins, W. M. Keck Observatory (United States)
Nicholas Konidaris, California Institute of Technology (United States)
Bob Weber, California Institute of Technology (United States)
Ted Aliado, Univ. of California, Los Angeles (United States)
George Brims, Univ. of California, Los Angeles (United States)
John Canfield, Univ. of California, Los Angeles (United States)
John Cromer, California Institute of Technology (United States)
Jason Fucik, California Institute of Technology (United States)
Kristin Kulas, Univ. of California, Los Angeles (United States)
Greg Mace, Univ. of California, Los Angeles (United States)
Ken Magnone, Univ. of California, Los Angeles (United States)
Hector Rodriguez, California Institute of Technology (United States)
Eric Wang, Univ. of California, Los Angeles (United States)
Jason Weiss, Univ. of California, Los Angeles (United States)


Published in SPIE Proceedings Vol. 7735:
Ground-based and Airborne Instrumentation for Astronomy III
Ian S. McLean; Suzanne K. Ramsay; Hideki Takami, Editor(s)

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