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We present the DustFilaments code, a full sky model for the millimeterGalactic emission of thermal dust. Our model, composed of millions of filamentsthat are imperfectly aligned with the magnetic field, is able to reproduce themain features of the dust angular power spectra at 353 GHz as measured by thePlanck mission. Our model is made up of a population of filaments with sizesfollowing a Pareto distribution $\propto L_a^{-2.445}$, with an axis ratiobetween short and long semi-axes $\epsilon \sim 0.16$ and an angle of magneticfield misalignment with a dispersion RMS($\theta_{LH}$)$=10$ degree. On largescales our model follows a Planck-based template. On small scales, our modelproduces spectra that behave like power-laws up to $\ell \sim 4000$ or smallerscales by considering even smaller filaments, limited only by computing power.We can produce any number of Monte Carlo realizations of small-scale Galacticdust. Our model will allow tests of how the small-scale non-Gaussianity affectCMB weak lensing, and the consequences for the measurement of primordialgravitational waves or relativistic light relic species. Our model also cangenerate frequency decorrelation on the Modified Black Body (MBB) spectrum ofdust, and is freely adjustable to different levels of decorrelation. This canbe used to test the performance of component separation methods and the impactof frequency spectra residuals on primordial $B$-mode surveys. The filamentdensity we paint in the sky is also able to reproduce the general level ofnon-Gaussianities measured by Minkowski functionals in the Planck 353 GHzchannel map.

Full-sky, arcminute-scale, 3D models of Galactic microwave foreground dust emission based on filaments