2025MNRAS.539.3157V

This study examines the bilateral supernova remnant (SNR) G16.2-2.7 through an observational and theoretical analysis to better understand its evolution. We performed a statistical analysis of the magnetic field vectors based on linearly polarized data from the MeerKAT radio telescope. We found that the shocked magnetic field in the shell is mainly tangential, indicating that G16.2-2.7 is an evolved SNR, in the late Sedov-Taylor evolution stage. The pre-shock interstellar Galactic magnetic field (IGMF) is tilted $\sim 20^\circ$ with respect to the Galactic plane. We observe polarized filaments aligned with the IGMF in the interior of the SNR. We propose a scenario in which a Type Ia supernova occurred 8 kyr ago within a cavity created by its progenitor system. Under these assumptions, magnetohydrodynamic simulations successfully reproduced the size of G16.2-2.7, its bilateral morphology, and the presence of inner filaments.