Speaker
Description
Galaxies undergo significant evolution from the early Universe to the present day; feedback processes are vital ingredients needed to help untangle the details of this transformation. Powerful jets driven by active galactic nuclei (AGN) have a key role in suppressing gas cooling, thus modulating the cooling gas that infalls into the host galaxy's centre. These radio jets inflate large lobes and bubbles, which displace the hot atmosphere and are visible as cavities in X-ray surface brightness. In the central galaxy of Abell 1795, the powerful radio source has inflated two large bubbles, North (N) and South (S) of the AGN. These filaments of molecular gas are exclusively projected around the bubble rims and their smooth velocity gradients imply the gas flows are entrained by the bubbles (Russell et al. 2017). The interplay of molecular gas flows, jets and jet-inflated radio bubbles in AGN feedback remains unknown. Russell et al. (2017) found that the energy required to lift the North (N) filament ($10^9 M_\odot$) exceeds the N radio bubble's mechanical energy. This result was produced by assuming the Galactic value for the CO-to-H$_2$ conversion factor ($X_{CO,MW}$) to determine the filament's molecular mass. In this work we use recent observations of ${}^{13}$CO, made by the Atacama Large Millimeter Array (ALMA), along with earlier ${}^{12}$CO ALMA observations to investigate whether the molecular gas mass was previously overestimated. $X_{CO}$ will be measured in the N filament, and we will re-evaluate whether the radio bubble's mechanical energy is sufficient to lift and entrain the molecular gas mass of the N filament helping piece together the interplay of molecular gas and the jet-inflated bubbles.
