Mid-Infrared spectrum of the zodiacal light
W. T. Reach, A. Abergel, F. Boulanger, F. X. Desert, M. Perault, J. P. Bernard, J. Blommaert, C. Cesarsky, D. Cesarsky, L. Metcalfe, J. L. Puget, F. Sibille, L. Vigroux;
AaA, 1996, 315, L381
ABSTRACT:Using the mid-infrared camera on the Infrared Space Observatory (ISO), the spectrum of a relatively empty piece of sky, dominated by zodiacal
light, was measured from 5 to 16.5{mu}m wavelength.
The spectrum has no
spectral features brighter than 15% of a blackbody fit to entire spectrum; the
temperature of the fit is 261.5+/-1.5K.
No galactic or cosmic background spectral
features are detected.
Comparison to models for three size distributions of
spherical grains composed of several different materials reveals acceptable
fits only for `astronomical silicate,' ruling out graphite, magnetite,
andesite, obsidian, glassy carbon, or water ice as the constituent of material
producing the zodiacal emission.
The size distribution is constrained to have
relatively fewer small particles compared to the coma of P/Halley.
There is a hint
of a 9-11{mu}m feature, which suggests that the particles producing the
zodiacal light are composed of silicates similar to those found in the coma of
P/Halley, collected interplanetary dust particles, and the dust around the
nearby star {beta} Pic.
KEYWORDS: interplanetary dust, background radiation, zodiacal light
CODE: reach96