|
|
The FLS extragalactic component
B. Observational Definition
The recommended extragalactic FLS consists of a shallow survey covering 5
square deg of sky and a "confirmation and verification" survey covering
about 1/4 square deg with both MIPS and IRAC. In comparison to the shallow
survey, the confirmation survey should attempt eight to ten times more
integration time per point on the sky. The extensive IRAC surveys improve
MIPS source positions (needed for position-coincidence identifications with
optical objects as faint as V~25 mag) and aid source classification (e.g.,
revealing the presence of an AGN, yielding rough redshift estimates,
characterizing the stellar populations). No IRS observations are
recommended because obtaining spectra for a statistically useful subset of
FLS sources would require too much observing time.
The shallow survey is broken up into two areas. The larger covers 4 square
degrees in that part of the CVZ with the lowest cirrus background (1 to 2
MJy/sr at 100 microns) near RA=17h, DEC=+61d (J2000), and not containing
any strong radio sources (see below). The final square deg is centered on
the ELAIS N1 field: RA=16h10m, DEC=+54d30' (J2000). This field is
attractive because it has the lowest cirrus background (0.4 MJy/sr at 100
microns) of any region near the northern CVZ, it is continuously visible
from the earliest possible SIRTF launch date until September 2002, and it
has been covered by a deep ISO survey at 15 and 175 microns. The
confirmation survey should be contained within the two shallow survey
areas.
Even at 24 microns, the combined surveys are large enough to characterize
the extragalactic source populations and determine source counts over 1.5
decades in flux density, after binning sources in six bins of width 0.25 in
log flux density.
Go back to Workshop Report or
FLS history page.
|
