Predicting CMB dust foreground using galactic 21 cm data

Understand

Understanding large-angular-scale galactic foregrounds is crucial for future CMB experiments aiming to detect $B$-mode polarization from primordial gravitational waves.

• Traditionally, the dust component has been separated using its different frequency dependence.
• However, using non-CMB observations has potential to increase fidelity and decrease the reconstruction noise.
• In this exploratory paper we investigate the capability of galactic 21 cm observations to predict the dust foreground in intensity.