Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 1507.00725

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

Hajime Sugai·Naoyuki Tamura·Hiroshi Karoji·Atsushi Shimono·Naruhisa Takato·Masahiko Kimura·Youichi Ohyama·Akitoshi Ueda·Hrand Aghazarian·Marcio Vital de Arruda·Robert H. Barkhouser·Charles L. Bennett·Steve Bickerton·Alexandre Bozier·David F. Braun·Khanh Bui·Christopher M. Capocasale·Michael A. Carr·Bruno Castilho·Yin-Chang Chang·Hsin-Yo Chen·Richard C. Y. Chou·Olivia R. Dawson·Richard G. Dekany·Eric M. Ek·Richard S. Ellis·Robin J. English·Didier Ferrand·Décio Ferreira·Charles D. Fisher·Mirek Golebiowski·James E. Gunn·Murdock Hart·Timothy M. Heckman·Paul T. P. Ho·Stephen Hope·Larry E. Hovland·Shu-Fu Hsu·Yen-Shan Hu·Pin Jie Huang·Marc Jaquet·Jennifer E. Karr·Jason G. Kempenaar·Matthew E. King·Olivier Le Fèvre·David Le Mignant·Hung-Hsu Ling·Craig Loomis·Robert H. Lupton·Fabrice Madec·Peter Mao·Lucas Souza Marrara·Brice Ménard·Chaz Morantz·Hitoshi Murayama·Graham J. Murray·Antonio Cesar de Oliveira·Claudia Mendes de Oliveira·Ligia Souza de Oliveira·Joe D. Orndorff·Rodrigo de Paiva Vilaça·Eamon J. Partos·Sandrine Pascal·Thomas Pegot-Ogier·Daniel J. Reiley·Reed Riddle·Leandro Santos·Jesulino Bispo dos Santos·Mark A. Schwochert·Michael D. Seiffert·Stephen A. Smee·Roger M. Smith·Ronald E. Steinkraus·Laerte Sodré Jr·David N. Spergel·Christian Surace·Laurence Tresse·Clément Vidal·Sebastien Vives·Shiang-Yu Wang·Chih-Yi Wen·Amy C. Wu·Rosie Wyse·Chi-Hung Yan
View original source ↗Read source document ↗Export metadata ↓

Abstract

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 {\mu}m to 1.26 {\mu}m, 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 {\mu}m to 0.89 {\mu}m 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.

Explore related subjects

astro-ph.IM

Keep this discovery

BibTeXRIS

Hajime Sugai, Naoyuki Tamura, Hiroshi Karoji, Atsushi Shimono, Naruhisa Takato, Masahiko Kimura, Youichi Ohyama, Akitoshi Ueda, Hrand Aghazarian, Marcio Vital de Arruda, Robert H. Barkhouser, Charles L. Bennett, Steve Bickerton, Alexandre Bozier, David F. Braun, Khanh Bui, Christopher M. Capocasale, Michael A. Carr, Bruno Castilho, Yin-Chang Chang, Hsin-Yo Chen, Richard C. Y. Chou, Olivia R. Dawson, Richard G. Dekany, Eric M. Ek, Richard S. Ellis, Robin J. English, Didier Ferrand, Décio Ferreira, Charles D. Fisher, Mirek Golebiowski, James E. Gunn, Murdock Hart, Timothy M. Heckman, Paul T. P. Ho, Stephen Hope, Larry E. Hovland, Shu-Fu Hsu, Yen-Shan Hu, Pin Jie Huang, Marc Jaquet, Jennifer E. Karr, Jason G. Kempenaar, Matthew E. King, Olivier Le Fèvre, David Le Mignant, Hung-Hsu Ling, Craig Loomis, Robert H. Lupton, Fabrice Madec, Peter Mao, Lucas Souza Marrara, Brice Ménard, Chaz Morantz, Hitoshi Murayama, Graham J. Murray, Antonio Cesar de Oliveira, Claudia Mendes de Oliveira, Ligia Souza de Oliveira, Joe D. Orndorff, Rodrigo de Paiva Vilaça, Eamon J. Partos, Sandrine Pascal, Thomas Pegot-Ogier, Daniel J. Reiley, Reed Riddle, Leandro Santos, Jesulino Bispo dos Santos, Mark A. Schwochert, Michael D. Seiffert, Stephen A. Smee, Roger M. Smith, Ronald E. Steinkraus, Laerte Sodré Jr, David N. Spergel, Christian Surace, Laurence Tresse, Clément Vidal, Sebastien Vives, Shiang-Yu Wang, Chih-Yi Wen, Amy C. Wu, Rosie Wyse, Chi-Hung Yan. 2015-07-02. Prime Focus Spectrograph for the Subaru telescope: massively multiplexed optical and near-infrared fiber spectrograph. https://doi.org/10.1117/1.jatis.1.3.035001

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

The EDD Radio Astronomy Backend Framework

Modern digital radio astronomy receivers produce increasingly wide-bandwidth, high bit-rate data streams that necessitate the development of flexible, scalable, and maintainable backend processing and recording systems. Historically, such backend instrumentation has been tightly coupled to telescope observing modes, limiting reuse between observatories and science cases. We present the Effelsberg Direct Digitisation (EDD) backend framework, a software-defined architecture for constructing real-time radio astronomy backends on commodity off-the-shelf computing infrastructure. We describe its design, implementation, supported observing modes, and operational deployments. EDD separates a common core framework from plugin-provided observing capabilities. The core provides orchestration, telescope interfaces, pipeline lifecycle management, monitoring, and deployment tooling, while plugins implement processing pipelines for specific observing modes. The framework is designed to support both single-dish and interferometric instruments through site-specific configuration and plugin selection. EDD currently supports spectroscopy and spectropolarimetry, pulsar timing and searching, baseband recording, very long baseline interferometry, correlation, and beamforming. Operational deployments include the Effelsberg 100-m telescope, the SKA-MPI prototype dish, the Thai National Radio Telescope, and the ARGOS interferometric prototype array. By separating common services, observing-mode plugins, and site-specific configuration, it allows backend capabilities to be deployed across heterogeneous telescope environments and provides a community resource for broadband radio astronomy instrumentation.

astro-ph.IM↗
arXiv2026

Bayesian Superiority in On/Off analysis

We present a detailed comparison of Bayesian criteria with three non-informative priors - flat, Jeffreys, and scale-invariant - for testing a signal against an unknown background and compare them with the classical frequentist Li-Ma approach in the On/Off problem. We perform Monte Carlo simulations for various background levels and evaluate the Li-Ma and Bayesian criteria by their Type I error rates. We then simulate a nonzero signal and compare the criteria in terms of Type II error rates. We find that the Bayesian criterion with the Jeffreys prior yields lower Type I and Type II error rates than the Li-Ma criterion. In addition, we show that the Bayesian criteria are more robust than the Li-Ma criterion when the background distribution is overdispersed relative to the Poisson distribution.

astro-ph.IM↗
arXiv2026

An RFSoC-based Backend and Timing System for the Balloon-borne Very Long Baseline Interferometry Experiment

We present the design and performance characterization of the digital backend and precision-timing system for the Balloon-borne Very Long Baseline Interferometry Experiment (BVEX), a pathfinder for high-frequency stratospheric VLBI at 22 GHz. The backend uses one of the four 14-bit analog-to-digital converter inputs on an AMD-Xilinx RFSoC 4x2. Although the converters support sampling rates up to 5 GSPS, the flight configuration digitizes the 2-4 GHz intermediate frequency at 4.096 GSPS. CASPER firmware provides both a high-resolution spectrometer for pointing and receiver verification, and a VLBI acquisition chain with two-bit requantization that records at a rate of about 8.2 Gbps. The timestamped data packets are sent over 100 Gigabit Ethernet (GbE) to a 16 TB NVMe array in a storage computer that draws approximately 70-80 W. The timing chain uses a Rakon oven-controlled crystal oscillator as a timing reference while a time-interval counter measures its drift relative to a GPS reference with approximately 60 ps resolution. This is the first deployment of an RFSoC-based VLBI backend and precision-timing system on a stratospheric balloon. Ground tests validated the backend, spectrometer, and timing chain. The August 2025 CSA STRATOS flight ended before reaching the target float altitude because of a balloon failure, and as a result no science observations were obtained. For the planned 2027 reflight, we are developing a conduction-cooled data storage computer with 24 TB of NVMe capacity and a direct data path from the 100 GbE interface to the NVMe array.

astro-ph.IM↗