Full-sky, arcminute-scale, 3D models of Galactic microwave foreground
  dust emission based on filaments
  We present the DustFilaments code, a full sky model for the millimeter
Galactic emission of thermal dust. Our model, composed of millions of filaments
that are imperfectly aligned with the magnetic field, is able to reproduce the
main features of the dust angular power spectra at 353 GHz as measured by the
Planck mission. Our model is made up of a population of filaments with sizes
following a Pareto distribution $\propto L_a^{-2.445}$, with an axis ratio
between short and long semi-axes $\epsilon \sim 0.16$ and an angle of magnetic
field misalignment with a dispersion RMS($\theta_{LH}$)$=10$ degree. On large
scales our model follows a Planck-based template. On small scales, our model
produces spectra that behave like power-laws up to $\ell \sim 4000$ or smaller
scales by considering even smaller filaments, limited only by computing power.
We can produce any number of Monte Carlo realizations of small-scale Galactic
dust. Our model will allow tests of how the small-scale non-Gaussianity affect
CMB weak lensing, and the consequences for the measurement of primordial
gravitational waves or relativistic light relic species. Our model also can
generate frequency decorrelation on the Modified Black Body (MBB) spectrum of
dust, and is freely adjustable to different levels of decorrelation. This can
be used to test the performance of component separation methods and the impact
of frequency spectra residuals on primordial $B$-mode surveys. The filament
density we paint in the sky is also able to reproduce the general level of
non-Gaussianities measured by Minkowski functionals in the Planck 353 GHz
channel map.
