Statistical signatures of interstellar turbulence in dust polarization maps

Ka Wai Ho; Ka Ho Yuen; Raphael Flauger; Alexei G. Kritsuk

doi:10.1103/vhhn-33jw

Letter

Statistical signatures of interstellar turbulence in dust polarization maps

Ka Wai Ho ^1,2,3,*, Ka Ho Yuen ^2,†,‡, Raphael Flauger ^4,§, and Alexei G. Kritsuk ^4,∥

¹Department of Astronomy, University of Wisconsin-Madison, Madison, Wisconsin 53715, USA
²Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
³Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA
⁴Physics Department, University of California, San Diego, La Jolla, California 92093, USA

^*Contact author: kawaiho@kitp.ucsb.edu
^†Contact author: kyuen@nju.edu.cn
^‡Present address: Nanjing University, Suzhou, Jiangsu Province, People’s Republic of China.
^§Contact author: flauger@ucsd.edu
^∥Contact author: akritsuk@ucsd.edu

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Phys. Rev. D 112, L101302 – Published 7 November, 2025

DOI: https://doi.org/10.1103/vhhn-33jw

Abstract

We present results from a high-resolution interstellar turbulence simulation and show that it closely reproduces recent Planck measurements. Our model captures the scaling of $E E$ and $B B$ spectra and the $E E / B B$ ratio in the inertial range. The probability density function of the dust polarization fraction is also consistent with observations. The $T E$ cross-correlation is in broad agreement with the Planck sky. This simulation provides new insights into the physical origins of the observed $E / B$ asymmetry and positive $T E$ signal, facilitating the development of advanced Galactic dust emission models for current and future cosmic microwave background experiments.

Physical Review D

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Statistical signatures of interstellar turbulence in dust polarization maps

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Statistical signatures of interstellar turbulence in dust polarization maps

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