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

Abstract

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.

27 pages, 12 figures, 2 tables. Accepted for publication by ApJ. Changes made to match the accepted version

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Cited by in corpus (15)

• The Simons Observatory: Galactic Science Goals and Forecasts
• Starlight-polarization-based tomography of the magnetized interstellar medium: PASIPHAE's line-of-sight inversion method
• Frequency dependence of the thermal dust $E/B$ ratio and $EB$ correlation: insights from the spin-moment expansion
• Full-sky Models of Galactic Microwave Emission and Polarization at Sub-arcminute Scales for the Python Sky Model
• Magnetic Misalignment of Interstellar Dust Filaments
• Non-Gaussian modelling and statistical denoising of Planck dust polarization full-sky maps using scattering transforms
• Modeling parity-violating spectra in Galactic dust polarization with filaments and its applications to cosmic birefringence searches
• Characterizing line-of-sight variability of polarized dust emission with future CMB experiments
• Impact of Galactic dust non-Gaussianity on searches for B-modes from inflation
• Generative Models of Multi-channel Data from a Single Example -- Application to Dust Emission
• The Simons Observatory: Assessing the Impact of Dust Complexity on the Recovery of Primordial $B$-modes
• The Galactic interstellar medium has a preferred handedness of magnetic misalignment
• ForSE+: Simulating non-Gaussian CMB foregrounds at 3 arcminutes in a stochastic way based on a generative adversarial network
• Impact of Galactic non-Gaussian foregrounds on CMB lensing measurements
• Forecasts of constraining isotropic cosmic birefringence on AliCPT-1