Interacción entre el RSN G359.1-0.5 y el medio interestelar

Abstract

G359.1-0.5 is a supernova remnant near the Galactic center region that belongs to the mixed morphology type, showing a radio continuum shell and diffuse thermal X-ray emission inside. Earlier molecular studies around the location of G359.1-0.5 revealed an annular CO structure in the velocity range from $-190$ to $-60~\rm{km} \rm{s}^{-1}$ with an H{\sc i} counterpart, both concentric with the remnant. Six OH masers at 1720~MHz along the edge of the radio-continuum shell were detected at velocities around $-5~\rm{km} \rm{s}^{-1}$, largely different from those found in previous molecular studies.In this work, we identify a molecular structure in the $^{12}$CO and $^{13}$CO J=1-0 lines between the velocities $-12.48$ and $+1.83~\rm{km} \rm{s}^{-1}$ which contains CO clumps apparently related to the OH masers. In addition, analyzing XMM-Newton archival data, we found evidence that part of the interior gas is not in ionization equilibrium. Finally, based on the collected data, we suggest a likely astrophysical scenario for G359.5-0.1.