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Title: The DESI Fiber View Camera System

Journal Article · · Publications of the Astronomical Society of the Pacific
 [1];  [1];  [2];  [3];  [1]; ORCiD logo [2];  [3];  [4];  [4];  [1];  [2];  [1];  [2]
  1. Yale Univ., New Haven, CT (United States). Physics Dept.
  2. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  3. Yale Univ., New Haven, CT (United States). Astronomy Dept.
  4. Univ. of California, Berkeley, CA (United States). Space Sciences Lab.
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The Dark Energy Spectroscopic Instrument (DESI) is a 5000 fiber multi-object spectrometer now being installed at the prime focus of the 4 m Mayall telescope at Kitt Peak. Using DESI to measure ~35 million galaxy redshifts and using the Baryon Acoustic Oscillation (BAO) technique to measure distances, the results will probe the nature of the recently discovered mysterious component of our universe called dark energy. Computer controlled robotic positioners move the 120 μm diameter fibers to positions of galaxies whose location on the sky have been obtained in a previous target selection imaging survey. To achieve good throughput the fibers should be centered on the target position to within 3 μm. The robotic positioners however are only capable of a 50 μm precision on their first move. To achieve the desired precision, the Fiber View Camera (FVC) system has been implemented. The FVC, located near the hole in the primary mirror of the Mayall telescope, has been designed to take an exposure of the focal plane, located at the prime focus some 12 m above the FVC, after the robotic positioners have completed their first move. The FVC is intended to measure the fiber locations with a precision of 3 μm and issue a set of fiber coordinate corrections for the second move correcting the fiber positions by the robotic positioners. Tests show that after two iterations better than 99% of the fibers will be in their intended location to within the desired precision. This paper describes the design of the FVC system, the R&D program preceding the final design, and the tests that have been carried out to demonstrate that the FVC can achieve the required precision.

Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
Sponsoring Organization:
USDOE Office of Science (SC)
Grant/Contract Number:
FG02-92ER40704; AC02–05CH1123
OSTI ID:
1527002
Journal Information:
Publications of the Astronomical Society of the Pacific, Vol. 131, Issue 1000; ISSN 0004-6280
Publisher:
Astronomical Society of the Pacific (ASP)Copyright Statement
Country of Publication:
United States
Language:
English

References (11)

The DESI wide field corrector optics conference August 2014
ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument journal January 2018
The DESI fiber positioner system conference August 2016
The Dark Energy Spectroscopic Instrument (DESI) conference July 2014
Gemini planet imager observational calibrations VIII: characterization and role of satellite spots conference July 2014
Laser Interferometer Measurement System on the Yale PDS 2020G journal January 1986
Fabrication of the DESI Corrector Lenses text January 2018
Gemini Planet Imager Observational Calibrations VIII: Characterization and Role of Satellite Spots text January 2014
Theoretical studies of the effects of grain noise on photographic stellar astrometry and photometry journal November 1983
Fabrication of the DESI corrector lenses
  • Brooks, David; Miller, Timothy N.; Besuner, Robert W.
  • Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III https://doi.org/10.1117/12.2312949
conference July 2018
Non-axisymmetric Aberration Patterns from Wide-field Telescopes Using Spin-weighted Zernike Polynomials journal February 2018

Figures / Tables (13)

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Table 2(p. 3)table Table 2
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Figure 5(p. 5)figure Figure 5
Figure 6(p. 6)figure Figure 6
Table 3(p. 6)table Table 3
Figure 7(p. 7)figure Figure 7
Figure 8(p. 7)figure Figure 8
Figure 10(p. 8)figure Figure 10
Figure 9(p. 8)figure Figure 9

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79 ASTRONOMY AND ASTROPHYSICS
instrumentation: detectors
galaxies: statistics
(cosmology:) dark energy