Is the Infrared Background Excess Explained by the Isotropic Zodiacal Light from the Outer Solar System?
arXiv:1808.03424 · doi:10.1093/pasj/psy100
Abstract
This paper investigates whether an isotropic zodiacal light from the outer Solar system can account for the detected background excess in near-infrared. Assuming that interplanetary dust particles are distributed in a thin spherical shell at the outer Solar system (>200 AU), thermal emission from such cold (<30 K) dust in the shell has a peak at far-infrared (~100 microns). By comparing the calculated thermal emission from the dust shell with the observed background emissions at far-infrared, permissible dust amount in the outer Solar system is obtained. Even if the maximum dust amount is assumed, the isotropic zodiacal light as the reflected sunlight from the dust shell at the outer Solar system cannot explain the detected background excess at near-infrared.
6 pages, 2 figures, accepted by PASJ
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Cited by in corpus (3)
- JWST's PEARLS: Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
- Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER
- The isotropic interplanetary dust cloud and near-infrared extragalactic background light observed with COBE/DIRBE