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This work purports to model the far infrared gray-body emission in thespectra of high-Galactic-latitude clouds. Several carbonaceous laboratorymaterials are tested for their fitness as carriers of this modified-black-bodyemission which, according to data delivered by the Planck satellite, and othersbefore, is best fit with temperature 17.9 K and spectral index beta=1.78. Someof these materials were discarded for insufficient emissivity, others forinadequate beta. By contrast, CHONS clusters (beta=1.4, T=19 K) combine nicelywith magnesium silicate (beta=2, T=18.7 K) to give a spectrum which falls wellwithin the observational error bars (total emission cross-section at 250 mum:8.6 10^{-26} cm^{2} per H atom). Only 15 % of all Galactic carbon atoms areneeded for this purpose. The CHONS particles that were considered and describedhave a disordered (amorphous) structure but include a sizable fraction ofaromatic rings, although they are much less graphitized than a-C:H/HAC. Theycan be seen as one embodiment of ``astronomical graphite" deduced earlier onfrom the then available astronomical observations. Grain heating by H atomcapture is proposed as a contributor to the observed residual emissions that donot follow the dust/HI correlation.

The contribution of CHONS particles to the diffuse high Galactic latitude IR emission