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A new laboratory-generated chemical compound made from photodissociatedammonia (NH3) molecules reacting with acetylene (C2H2) was suggested as apossible coloring agent for Jupiter's Great Red Spot (GRS) by Carlson et al.(2016, Icarus 274, 106-115). Baines et al. (2016, Icarus, submitted) showedthat the GRS spectrum measured by the visual channels of the Cassini VIMSinstrument in 2000 could be accurately fit by a cloud model in which thechromophore appeared as a physically thin layer of small particles immediatelyabove the main cloud layer of the GRS. Here we show that the same chromophoreand same layer location can also provide close matches to the short wavespectra of many other cloud features on Jupiter, suggesting this material maybe a nearly universal chromophore that could explain the various degrees of redcoloration on Jupiter. This is a robust conclusion, even for 12% changes inVIMS calibration and large uncertainties in the refractive index of the maincloud layer due to uncertain fractions of NH4SH and NH3 in its cloud particles.The chromophore layer can account for color variations among north and southequatorial belts, equatorial zone, and the Great Red Spot, by varying particlesize from 0.12 microns to 0.29 microns and 1-micron optical depth from 0.06 to0.76. The total mass of the chromophore layer is much less variable, rangingfrom 18 to 30 micrograms/cm^2, except in the equatorial zone, where it is only10-13 micrograms/cm^2. We also found a depression of the ammonia volume mixingratio in the two belt regions, which averaged 0.4-0.5 X 10^{-4} immediatelybelow the ammonia condensation level, while the other regions averaged twicethat value.

A possibly universal red chromophore for modeling color variations on Jupiter