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The FLS extragalactic component
A. Science Goals
The extragalactic working group recommended a FLS program designed to
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detect enough extragalactic sources at unexplored sensitivity
levels to generate a representative sample and reduce the
uncertainties in the source counts,
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characterize the dominant source populations with both MIPS and
IRAC data from SIRTF plus ancillary surveys at optical,
near-infrared, and radio wavelengths, and
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explore the cirrus foreground at moderately high |b|, and its
effect on point-source detectability,
all in time to support the first SIRTF science users. Most existing
archival data at visible and radio wavelengths are not well matched to
supporting the FLS goals. For example, the HDF is too small, and existing
all-sky radio surveys are not sufficiently sensitive. New ancillary data
obtained well before the (uncertain) SIRTF launch date will significantly
enchance the scientific value of the FLS, so most of the extragalactic FLS
should be confined to the northern continuous viewing zone (CVZ) with
ecliptic latitudes greater than 80 deg.
Go back to Workshop Report or
FLS history page.
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