This is a proposal to search for particles in the outer Solar
 system, either small dust particles of the sort seen around nearby
 main sequence stars (e.g. Vega) and young stellar objects or
 larger bodies such as comets and meteorites within and beyond the
 Kuiper belt.  Such particles are commonly seen around nearby stars,

 The principle difficulty in detecting distant particles is
 foreground emission by the zodiacal light, although background
 emission from interstellar cirrus could also be a difficulty if its
 angular distribution is well-correlated with the ecliptic plane.
 The proposed observations include six wavelength bands chosen to
 provide maximum sensitivity to foreground and background radiation
 and to allow these to be subtracted from the emission in bands most
 sensitive to distant particles.

 We use two complementary methods to conduct this search.  The first
 is to observe 15 positions perpendicular to the ecliptic plane at 6
 wavelengths, starting at 0 deg latitude and progressing upwards to
 32 deg in logarithmically spaced intervals.  The 3 shortest bands
 will be used to model the zodiacal light, the longest to detect cold
 background emission, and the 2 intermediate wavelengths to detect
 distant particles in the Solar system.  The second method is to map
 small areas at three different latitudes to look for fluctuations
 caused by clumping of the distant emission caused by, for example,
 clusters of large bodies such as comets.

 Because we cannot determine apriori which method is likely to be
 the most successful, the observing time is split equally between
 the two.  This second part of the proposal describes the mapping of
 three regions to search for fluctuations.