MOSFIRE, the multi-object spectrometer for infra-red exploration at the Keck Observatory

Ian S. McLean; Charles C. Steidel; Harland W. Epps; Nicholas Konidaris; Keith Y. Matthews; Sean Adkins; Theodore Aliado; George Brims; John M. Canfield; John L. Cromer; Jason Fucik; Kristin Kulas; Greg Mace; Ken Magnone; Hector Rodriguez; Gwen Rudie; Ryan Trainor; Eric Wang; Bob Weber; Jason Weiss

doi:10.1117/12.924794

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27 September 2012 MOSFIRE, the multi-object spectrometer for infra-red exploration at the Keck Observatory

Ian S. McLean, Charles C. Steidel, Harland W. Epps, Nicholas Konidaris, Keith Y. Matthews, Sean Adkins, Theodore Aliado, George Brims, John M. Canfield, John L. Cromer, Jason Fucik, Kristin Kulas, Greg Mace, Ken Magnone, Hector Rodriguez, Gwen Rudie, Ryan Trainor, Eric Wang, Bob Weber, Jason Weiss

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Proceedings Volume 8446, Ground-based and Airborne Instrumentation for Astronomy IV; 84460J (2012) https://doi.org/10.1117/12.924794
Event: SPIE Astronomical Telescopes + Instrumentation, 2012, Amsterdam, Netherlands

Abstract

This paper describes the as-built performance of MOSFIRE, the multi-object spectrometer and imager for the Cassegrain focus of the 10-m Keck 1 telescope. MOSFIRE provides near-infrared (0.97 to 2.41 μm) multi-object spectroscopy over a 6.1' x 6.1' field of view with a resolving power of R~3,500 for a 0.7" (0.508 mm) slit (2.9 pixels in the dispersion direction), or imaging over a field of view of ~6.9' 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. Instead of fabricated focal plane masks requiring frequent cryo-cycling of the instrument, MOSFIRE is equipped with a cryogenic Configurable Slit Unit (CSU) developed in collaboration with the Swiss Center for Electronics and Microtechnology (CSEM). Under remote control the CSU can form masks containing up to 46 slits with ~0.007-0.014" precision. Reconfiguration time is < 6 minutes. Slits are formed by moving opposable bars from both sides of the focal plane. An individual slit has a length of 7.0" but bar positions can be aligned to make longer slits in increments of 7.5". When masking bars are retracted from the field of view and the grating is changed to a mirror, MOSFIRE becomes a wide-field imager. The detector is a 2K x 2K H2-RG HgCdTe array from Teledyne Imaging Sensors with low dark current and low noise. Results from integration and commissioning are presented.

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Ian S. McLean, Charles C. Steidel, Harland W. Epps, Nicholas Konidaris, Keith Y. Matthews, Sean Adkins, Theodore Aliado, George Brims, John M. Canfield, John L. Cromer, Jason Fucik, Kristin Kulas, Greg Mace, Ken Magnone, Hector Rodriguez, Gwen Rudie, Ryan Trainor, Eric Wang, Bob Weber, and Jason Weiss "MOSFIRE, the multi-object spectrometer for infra-red exploration at the Keck Observatory", Proc. SPIE 8446, Ground-based and Airborne Instrumentation for Astronomy IV, 84460J (27 September 2012); https://doi.org/10.1117/12.924794

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