$Ab$ $initio$ modeling of Galactic dust polarized CMB foreground
Alexei G. Kritsuk, Ka Wai Ho, Ka Ho Yuen, Raphael Flauger
TLDR
This paper uses exascale simulations to model Galactic dust polarization, explaining E/B mode asymmetry and positive TE signals for CMB experiments.
Key contributions
- Generated high-resolution synthetic dust polarization maps using exascale simulations.
- Developed a turbulence model that accurately matches Planck's E- and B-mode spectra.
- Offers new insights into the physical origins of observed E/B asymmetry and positive TE signals.
- Enables development of advanced Galactic foreground models for future CMB experiments.
Why it matters
Understanding Galactic dust polarization is crucial for accurate Cosmic Microwave Background (CMB) measurements. This work provides a sophisticated model that explains key observed features like E/B asymmetry, improving foreground removal for current and future CMB experiments.
Original Abstract
We present the analysis of high-resolution synthetic dust polarization maps derived from large-scale simulations of magnetized multiphase interstellar turbulence carried out with the AthenaK code on the $Frontier$ exascale supercomputer at the Oak Ridge National Laboratory. Our turbulence model accurately captures spectral properties of the $E$- and $B$-modes measured by $Planck$ at 353 GHz. The simulations provide new insights into the physical origins of the observed $E/B$ asymmetry and positive $TE$ signal, facilitating the development of advanced models of Galactic foreground emission for current and future CMB experiments.
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