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This paper investigates whether an isotropic zodiacal light from the outerSolar system can account for the detected background excess in near-infrared.Assuming that interplanetary dust particles are distributed in a thin sphericalshell at the outer Solar system (>200 AU), thermal emission from such cold (<30K) dust in the shell has a peak at far-infrared (~100 microns). By comparingthe calculated thermal emission from the dust shell with the observedbackground emissions at far-infrared, permissible dust amount in the outerSolar system is obtained. Even if the maximum dust amount is assumed, theisotropic zodiacal light as the reflected sunlight from the dust shell at theouter Solar system cannot explain the detected background excess atnear-infrared.

Is the Infrared Background Excess Explained by the Isotropic Zodiacal Light from the Outer Solar System?