English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We compare two rotationally invariant decomposition techniques on linearpolarisation data: the spin-2 spherical harmonic decomposition in two oppositeparities, the $E$- and $B$-mode, and the multiscale analysis of the gradient oflinear polarisation, $|\nabla \mathbf{P}|$. We demonstrate that bothdecompositions have similar properties in the image domain and the spatialfrequency domain. They can be used as complementary tools for turbulenceanalysis of interstellar magnetic fields in order to develop a betterunderstanding of the origin of energy sources for the turbulence, the origin ofpeculiar magnetic field structures and their underlying physics. We alsointroduce a new quantity $|\nabla EB|$ based on the $E$- and $B$-modes and weshow that in the intermediate and small scales limit $|\nabla EB| \simeq|\nabla \mathbf{P}|$. Analysis of the 2.3 GHz S-band Polarization All SkySurvey (S -PASS) shows many extended coherent filament-like features appearingas 'double-jumps' in the $|\nabla \mathbf{P}|$ map that are correlated withnegative and positive filaments of $B$-type polarisation. These localasymmetries between the two polarisation types, $E$ and $B$, of the non-thermalGalactic synchrotron emission have an influence on the $E$- and $B$-mode powerspectra analyses. The wavelet-based formalism of the polarisation gradientanalysis allows us to locate the position of $E$- or $B$-mode featuresresponsible for the local asymmetries between the two polarisation types. Inanalysed subregions, the perturbations of the magnetic field are trigged bystar clusters associated with HII regions, the Orion-Eridanus superbubble andthe North Polar Spur at low Galactic latitude.

A new perspective on turbulent Galactic magnetic fields through comparison of linear polarisation decomposition techniques