SKA1 AA* and AA4 will roughly double-to-triple the known pulsar population and supply thousands of new RMs, enabling detailed 3D mapping of Galactic disk and halo magnetic fields.
Comparison of algorithms for determination of rotation measure and Faraday structure I. 1100 - 1400 MHz
1 Pith paper cite this work. Polarity classification is still indexing.
abstract
(abridged) We run a Faraday structure determination data challenge to benchmark the currently available algorithms including Faraday synthesis (previously called RM synthesis in the literature), wavelet, compressive sampling and $QU$-fitting. The frequency set is similar to POSSUM/GALFACTS with a 300 MHz bandwidth from 1.1 to 1.4 GHz. We define three figures of merit motivated by the underlying science: a) an average RM weighted by polarized intensity, RMwtd, b) the separation $\Delta\phi$ of two Faraday components and c) the reduced chi-squared. Based on the current test data of signal to noise ratio of about 32, we find that: (1) When only one Faraday thin component is present, most methods perform as expected, with occasional failures where two components are incorrectly found; (2) For two Faraday thin components, QU-fitting routines perform the best, with errors close to the theoretical ones for RMwtd, but with significantly higher errors for $\Delta\phi$. All other methods including standard Faraday synthesis frequently identify only one component when $\Delta\phi$ is below or near the width of the Faraday point spread function; (3) No methods, as currently implemented, work well for Faraday thick components due to the narrow bandwidth; (4) There exist combinations of two Faraday components which produce a large range of acceptable fits and hence large uncertainties in the derived single RMs; in these cases, different RMs lead to the same Q, U behavior, so no method can recover a unique input model.
fields
astro-ph.HE 1years
2026 1verdicts
ACCEPT 1representative citing papers
citing papers explorer
-
Exploring the Magnetic Field Structure of the Milky Way with Pulsars in the SKA Era
SKA1 AA* and AA4 will roughly double-to-triple the known pulsar population and supply thousands of new RMs, enabling detailed 3D mapping of Galactic disk and halo magnetic fields.