Speaker
Description
The knowledge of the coherent and turbulent magnetic field of our
Galaxy is of great importance for interpreting the arrival directions
of Ultrahigh Energy Cosmic Rays.
In this presentation, we augment our study of the coherent magnetic
field of the Galaxy (Unger&Farrar 2023) with Faraday rotation measures
(RMs) of pulsars. In contrast to the polarized synchrotron intensity
and extragalactic RMs previously used to tune our models, pulsar RMs
have the potential to provide a tomographic view of the Galactic
magnetic field. However the distances of only a small fraction of
pulsars have been directly measured, while for the vast majority of
pulsars the distances are model dependent. We provide, for the first
time, a methodology for quantitative use of pulsar RMs in modeling the
GMF, and discuss the implications of the data for the structure of the
disk field and the toroidal halo field.
We also present an estimate of the turbulent component of the
Galactic magnetic field based on the total synchrotron intensity
emission of cosmic-ray electrons in the Galaxy as measured by WMAP and
Planck.
