STUDY SUMMARY - IPMU

SUMMARY REPORT
WIDE FIELD FIBER-FED OPTICAL
MULTI-OBJECT SPECTROMETER (WFMOS)
6.0 Operations
We have designed the WFMOS instrument and science surveys for efficient, streamlined operation.
There are several components of operations that are necessary for realizing the scientific
return of WFMOS. The “Package A” data reduction pipeline is included in this construction proposal
and its associated costs. This pipeline produces calibrated spectra, and is described in Section
3. In this section, we summarize the additional components of operations required to complete
the Dark Energy and Galactic Archaeology surveys. Additional detail on the scientific
surveys and operational modes of the instrument appear in the OCDD; additional technical detail
on the instrument appears in the Detailed Technical Design. The components of operations fall
into the following categories:
• Construction of data reduction “Package B”
• Conducting the DE and GA science surveys
• Installation and removal of WFMOS from the Subaru Prime Focus.
We examine each of these categories in turn.
6.1 Data Reduction Package B
The Package B pipeline use the calibrated spectra from Package A and produces automated,
high level science products ready for further analysis. For the DE survey, this consists primarily
of extracting redshifts from the galaxy survey through the identification of the [OII] feature for
the low redshift survey, and through continuum fitting for the high-redshift survey. Galaxy typing
will be done for the better s:n targets. We will use a small team of scientists together with
professional programmers to produce the DE portion of Package B. Associated costs appear in
the Management and Cost volume. The PI delegates scientific management of the effort to Professor
John Peacock.
For the GA survey, Package B includes extraction of velocities and metallicities (low resolution)
and abundance determination (high resolution). Tasks include 1) automated estimation of
global stellar atmosphere parameters, 2) automated continuum estimation, multi-component line
fitting, and abundance analysis from line lists, 3) automated radial velocity estimation, and 4)
using optical plus near-IR photometry (and distances if available, e.g., from Gaia) to produce
model atmosphere fits to spectra. Associated costs appear in the Management and Cost volume.
The PI delegates scientific management of the effort to Prof. Mike Irwin.
Some of the Package B tasks have significant overlap between the DE and GA surveys.
These include:
• Optimizing sky subtraction methods.
• Scattered light modeling using blocked-off fibers.
The apportionment of these tasks will be made at the beginning of the Package B effort.
6.2 Conducting the Dark Energy and Galactic Archaeology Science Surveys
The two primary science surveys are described in detail in the OCDD. Each survey comprises
the following steps:
• Preparing observations.
• Monitoring survey progress.
• Analysis of results and publications.
Preparing observations involves selecting targets from existing catalogs, optimizing fiber al-
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