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| DEIMOS (Keck) | |
|---|---|
| Name | DEIMOS |
| Telescope | Keck II |
| Wavelength | Optical |
| Type | Multi-object spectrograph |
| First light | 1999 |
| Detectors | CCD mosaic |
| Resolution | R~1000–6000 |
DEIMOS (Keck)
DEIMOS is a multi‑object optical spectrograph on the Keck II telescope at W. M. Keck Observatory on Mauna Kea, designed for wide‑field deep spectroscopy. It enabled large redshift surveys and resolved kinematics studies by combining a large focal plane with high throughput optics and a precision slitmask system developed by teams from California Institute of Technology, University of California, Santa Cruz, and Carnegie Institution for Science. DEIMOS has been central to projects connected to Hubble Deep Field, Sloan Digital Sky Survey, and follow‑up programs for surveys by Subaru Telescope and the Very Large Telescope.
DEIMOS was commissioned to exploit the 10‑meter aperture of Keck II for deep extragalactic spectroscopy, addressing questions tied to the Hubble Space Telescope deep imaging campaigns and surveys such as the DEEP2 Galaxy Redshift Survey and programs related to GOODS and COSMOS. The instrument supports multiplexed observations analogous to those undertaken by Anglo‑Australian Telescope instruments and complements fiber spectroscopy from Sloan Digital Sky Survey and integral field work at European Southern Observatory. Its design emphasis on high throughput, spectral resolution, and a large field of view made it suitable for programs involving teams from University of California, Berkeley, California Institute of Technology, NASA, and international collaborators including Max Planck Society groups.
DEIMOS employs a refractive collimator and a large volume phase holographic grating system paired with a focal plane containing a mosaic of CCDs supplied by Lawrence Berkeley National Laboratory engineers and fabricated by vendors used by MIT and STScI. The instrument mount interfaces with the Keck II cassegrain rotator and includes a slitmask cassette system built with machining and metrology contributions from Jet Propulsion Laboratory and Carnegie Institution for Science. Specifications include a field of view comparable to those used on Subaru Telescope prime focus instruments, spectral resolving powers configurable across ranges used by instruments at Palomar Observatory and W. M. Keck Observatory staff, and a CCD mosaic cooled using cryogenic systems similar to those at European Southern Observatory facilities. DEIMOS optics and coatings draw on developments used by Gemini Observatory and Large Binocular Telescope projects.
DEIMOS supports multi‑object slitmask spectroscopy, long‑slit mode, and specialized configurations for faint object work, paralleling modes available on FORS instruments at VLT and the LRIS instrument at Keck I. The slitmask design process utilizes software workflows and astrometric catalogs from Hubble Space Telescope programs and survey catalogs from Sloan Digital Sky Survey and Pan-STARRS1 to optimize target selection. Data reduction pipelines were developed drawing on heritage from IRAF-based and modern Python toolkits employed by teams at Space Telescope Science Institute and University of Washington, incorporating wavelength calibration with arc lamps similar to those used at Anglo-Australian Observatory and flux calibration tied to standards from Cerro Tololo Inter-American Observatory. The pipeline supports sky subtraction strategies comparable to methods used at European Southern Observatory and artifact mitigation routines influenced by Hubble Space Telescope data processing.
DEIMOS enabled the DEEP2 Galaxy Redshift Survey, which produced redshift catalogs and large‑scale structure measurements in the manner of 2dF Galaxy Redshift Survey and Sloan Digital Sky Survey cosmological studies, contributing to constraints on galaxy evolution invoked in work by teams affiliated with Princeton University and Harvard University. Observations with DEIMOS have been used to measure rotation curves and dynamical masses of distant galaxies comparable to studies at VLT and Subaru Telescope, to characterize Lyman‑alpha emitters investigated in programs associated with Keck Observatory and Hubble Space Telescope deep fields, and to follow up transients discovered by surveys like Pan-STARRS and Palomar Transient Factory. DEIMOS data have underpinned analyses of galaxy stellar populations akin to studies from Caltech and Max Planck Institute for Astrophysics, contributed to measurements of baryon acoustic oscillations in conjunction with projects at Lawrence Berkeley National Laboratory, and supported slitmask campaigns targeting high‑redshift quasars similar to efforts at European Southern Observatory.
Since first light, DEIMOS has received detector upgrades and software improvements in concert with efforts at Lawrence Berkeley National Laboratory and instrumentation groups at University of California, Santa Cruz. Improvements in CCD cosmetics, read noise, and controller electronics paralleled upgrades undertaken at Keck Observatory and by teams at NOIRLab; grating and coating maintenance followed heritage from Gemini Observatory instrument programs. Performance metrics—throughput, spectral resolution, and stability—have been benchmarked against instruments at Subaru Telescope, Very Large Telescope, and Magellan Telescopes, and instrument teams have implemented pipeline enhancements inspired by practices at Space Telescope Science Institute and European Southern Observatory to maintain competitiveness for large surveys and PI programs.
The DEIMOS project has been managed by scientists and engineers from California Institute of Technology, University of California, Santa Cruz, Carnegie Institution for Science, and staff at W. M. Keck Observatory, with operational coordination involving observatory instrument scientists and support from technical groups at Jet Propulsion Laboratory and Lawrence Berkeley National Laboratory. Key operational roles mirror those at Keck Observatory instruments such as LRIS and NIRSPEC, including instrument scientists, software engineers, and mask fabrication technicians drawn from the broader community of institutions like Stanford University and University of California, Berkeley. The instrument has been supported through time allocation by committees associated with W. M. Keck Observatory partner institutions, and continues to serve international collaborations conducting cosmology, galaxy evolution, and transient follow‑up programs.
Category:Astronomical instruments