ESO137-G034: Unveiling Coronal Structures and Feedback Mechanisms

Active galactic nuclei (AGN) are among the brightest objects in the Universe, emitting across the entire electromagnetic spectrum. The coupling of radiation from the central source with the inter stellar medium (ISM) generates feedback, capable of producing turbulence, outflows, and coronal line emission. This study focuses on the galaxy ESO137-G034, ideal for feedback studies due to a jet in strong interaction with the ISM. [O III] observations with HST reveal a conical structure and a 'Z'-shaped formation, while ATCA data show three radio lobes aligned with emitting regions, suggesting mechanical feedback. The objectives of this study include: characterizing the ionized gas morphology, quantifying nuclear and peripheral contributions, and performing multiband com parisons (near and mid-infrared) to map coronal gas. Data were obtained through integral field spectroscopy with the SINFONI (VLT) and MIRI-MRS (JWST). The analysis revealed, for the f irst time, the nucleus position, and MIRI-MRS maps indicate, for the first time, [Ne V] exten sions up to 1.1 kpc, with coronal emission lobes and filaments. [Si VI] emission shows a nuclear contribution of ∼1%, highlighting shocks as an additional energy mechanism. We conclude that 56 ESO137-G034 exhibits significant feedback, with filamentary coronal structures and lobes surpass ing the central region in flux, making it a peculiar case in the literature.