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Objects in the Edgeworth-Kuiper belt and the main asteroid belt should emitmicrowaves that may give rise to extra anisotropy signals in the multipole ofthe cosmic microwave background (CMB) experiment. Constraints are derived fromthe absence of positive detection of such anisotropies for ell < 50, giving thetotal mass of Edgeworth-Kuiper belt objects to be smaller than 0.2 earth mass.This limit is consistent with the mass extrapolated from the observablepopulation with the size of a > 15 km, assuming that the small-objectpopulation follows the power law in size dN/da ~ a^{-q} with the canonicalindex expected for collisional equilibrium, q ~ 3.5, with which 23% of the massis ascribed to objects smaller than are observationally accessible down tograins. A similar argument applied to the main asteroid belt indicates that thegrain population should not increase faster than q ~ 3.6 towards smaller radii,if it follows the power law continued to observed asteroids with larger radii.It is underlined that both cases are at or only slightly above the limit thatcan be physically significant, implying the importance of tightening furtherthe CMB anisotropy limit, which may be attained with the observation at higherradio frequencies.

Microwave Emission from the Edgeworth-Kuiper Belt and the Asteroid Belt Constrained from WMAP