Magnetic fields in elliptical galaxies: Using the Laing-Garrington effect in radio galaxies and polarized emission from background radio sources

TL;DR

This study investigates magnetic fields in elliptical galaxies using polarization effects in radio galaxies and background sources, estimating field strengths and structures to inform galaxy evolution models.

Contribution

It introduces two novel methods to constrain magnetic fields in ellipticals, combining polarization asymmetry analysis and RM distribution studies.

Findings

Small-scale magnetic fields are 0.1-2.75 μG.

Large-scale fields are an order of magnitude weaker.

Estimated central fields around 6 μG.

Abstract

Magnetic fields in elliptical galaxies are poorly constrained due to a lack of significant synchrotron emission from them. This paper explores properties of magnetic fields in ellipticals via two methods. First, we exploit the Laing-Garrington effect (asymmetry in the observed polarization fraction between radio galaxy jets) for 57 galaxies with redshifts up to $0.5$. We use the differences in polarization fraction and rotation measure between the jet and counterjet to estimate the small- and large-scale magnetic fields in and around ellipticals (including their circumgalactic medium). We find that the small-scale field (at scales smaller than the driving scale of turbulence, approximately $300~{\rm pc}$) lies in the range $0.1~\text{--}~2.75~\mu{\rm G}$. The large-scale field (at scales of $100~{\rm kpc}$) is an order of magnitude smaller than the small-scale field. In the second method, we cross-match the Faraday rotation measures (RM) of a few hundred (out of $3098$) extragalactic radio sources with galaxy catalogs to explore the effect of the number and morphology of intervening galaxies on the observed RM distribution. We use both Gaussian and non-Gaussian functions to describe the RM distribution and derive its statistical properties. Finally, using the difference in the observed polarization fraction between the intervening spirals and ellipticals, we estimate the small-scale magnetic fields at the center of ellipticals to be $\sim6~\mu{\rm G}$. Both methods with different observations and analysis techniques give magnetic field strengths consistent with previous studies ($\leq10\mu{\rm G}$), and the results can be used to constrain dynamo theories and galaxy evolution simulations.