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Published July 2015 | Published
Journal Article Open

Prime Focus Spectrograph for the Subaru telescope: massively multiplexed optical and near-infrared fiber spectrograph


The Prime Focus Spectrograph (PFS) is an optical/near-infrared multifiber spectrograph with 2394 science fibers distributed across a 1.3-deg diameter field of view at the Subaru 8.2-m telescope. The wide wavelength coverage from 0.38  μm to 1.26  μm, with a resolving power of 3000, simultaneously strengthens its ability to target three main survey programs: cosmology, galactic archaeology and galaxy/AGN evolution. A medium resolution mode with a resolving power of 5000 for 0.71  μm to 0.89  μm will also be available by simply exchanging dispersers. We highlight some of the technological aspects of the design. To transform the telescope focal ratio, a broad-band coated microlens is glued to each fiber tip. A higher transmission fiber is selected for the longest part of the cable system, optimizing overall throughput; a fiber with low focal ratio degradation is selected for the fiber-positioner and fiber-slit components, minimizing the effects of fiber movements and fiber bending. Fiber positioning will be performed by a positioner consisting of two stages of piezo-electric rotary motors. The positions of these motors are measured by taking an image of artificially back-illuminated fibers with the metrology camera located in the Cassegrain container; the fibers are placed in the proper location by iteratively measuring and then adjusting the positions of the motors. Target light reaches one of the four identical fast-Schmidt spectrograph modules, each with three arms. The PFS project has passed several project-wide design reviews and is now in the construction phase.

Additional Information

© 2015 Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Received Dec. 7, 2014; accepted for publication May 22, 2015; published online Jun. 23, 2015. We gratefully acknowledge support from the Funding Program for World-Leading Innovative R&D on Science and Technology (FIRST) program "Subaru Measurements of Images and Redshifts (SuMIRe)," CSTP, Japan, and Fundação de Amparo a Pesquisa do Estado de São Paulo (FAPESP), Brazil. We appreciate staff members at Subaru Telescope for continuously supporting our activities. We thank NAOJ ATC staff members, particularly Tetsuo Nishino, Norio Okada, and Yukiko Kamata, for preparing AlN pin bases, and Durham University staff members for their consultancy to IPMU on the fiber system. We also acknowledge the WFMOS-B team whose accumulated efforts of many years have inspired us. This paper has been revised and updated, for the purpose of journal publication, from the PFS overview paper presented in an SPIE conference.

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