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The jets launched by actively accreting black holes are capable of launchingseveral of the massive (million or billion solar mass) molecular outflowsobserved in galaxies. These outflows could suppress or enhance star formationin galaxies. To investigate the stability of clouds capable to form stars inoutflows, we modeled CO and HCO+ ALMA data of the galaxy IC5063, in whichblack-hole jets impact molecular clouds. Using a radiative transfer code thatself-consistently performs astrochemical and thermal balance calculations basedon the available gas heating sources, we found that mechanical heating andcosmic ray (CR) heating are fully capable of individually reproducing the data.In our best-fit model, CRs provide about 1/3rd of the dense gas heating at theradio lobes, emphasizing the role of this often neglected mechanism in heatingthe gas and potentially generating outflows. The gas temperature and densityindicate that the jet passage leads to an increase of about 1 order ofmagnitude in the internal pressure Pi of molecular clouds (with Pi/k from8*10^5 up to 7*10^6 K cm^-3), irrespective of the excitation mechanism. Fromthe fluxes of [S II] and [N II] lines in VLT MUSE data, the external pressurePe of molecular clouds increases in several regions enough to exceed Pi. Thisresult leads us to conclude that we are observing the expansion of an ionizedoverpressurized cocoon that compresses molecular clouds and that could lead totheir collapse. Some jet-impacted clouds, nonetheless, near pathways that thejet cleared have increased Pi and decreased Pe. They are likely to undergoevaporation of their outer layers. Part of the evaporated layers could massload the outflow thanks to ram pressure from co-spatial ionized gas flows. Theobserved pressure changes thus suggest that both star formation enhancement andsuppression could simultaneously occur.

Linking pressure gradients with the stability of molecular clouds in galactic outflows