# Physical conditions in Centaurus A's northern filaments I: APEX mid-J CO observations of CO-bright regions

## TL;DR

This study uses APEX observations to analyze molecular gas properties in Centaurus A's northern filaments, revealing new CO detections and physical conditions indicative of shock excitation and star formation influence.

## Contribution

First detection of CO(3-2) and CO(4-3) in Centaurus A's northern filaments, providing insights into the physical state of molecular gas influenced by AGN feedback.

## Key findings

- Detected CO(3-2) and CO(4-3) for the first time in the region.
- Molecular gas temperature estimated at 55-70 K.
- Gas densities found to be 200-600 cm^-3.

## Abstract

NGC 5128 (Centaurus A) is one of the best targets to study AGN-feedback in the local Universe. Optical filaments located at 16 kpc from the galaxy along the radio jet direction show recent star formation, likely triggered by the interaction of the jet with an HI shell. A large reservoir of molecular gas has been discovered outside the HI. In this reservoir, lies the Horseshoe complex: a filamentary structure seen in CO with ALMA and in Halpha with MUSE. The ionised gas is mostly excited by shocks, with only a minor contribution of star formation. We used the Atacama Pathfinder EXperiment (APEX) to observe the 12CO(3-2) and 12CO(4-3) transitions, as well as dense gas tracers in the Horseshoe complex. 12CO(3-2) and 12CO(4-3) are detected for the first time in the northern filaments of Centaurus A, with integrated intensity line ratios R32~0.2 and R43~0.1, compared to the 12CO(1-0) emission. We also derived a line ratio R21~0.6, based on the previous 12CO(2-1) observations of Salom\'e et al. (2016). We used the non-LTE radiative transfer code RADEX and determined that the molecular gas in this region has a temperature of 55-70 K and densities between 2-6x10^2 cm^-3. Such densities are also in agreement with results from the Paris-Durham shock code that predicts a post-shock density of a few 100 cm^-3. However, we need more observations of emission lines at a better angular resolution in order to place tighter constraints on our radiative models, whether they are used as a stand-alone tool (LVG codes) or combined with a shock model.