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A MCMC fit to the coronal line [Si VI]. Note that both the broad and narrow component are blueshifted to the systemic velocity of the galaxy.
An outflow is any bulk movement of gas or particles from a central source. These phenomena are typically seen in massive galaxies hosting supermassive black holes. However, there is growing evidence of black hole activity in lower mass dwarf galaxies, and this begs the question: can black holes in dwarf galaxies drive outflows that can disrupt star formation?
The JWST GO-3663 program aims to answer this question. The first paper of this program, Aravindan et al., 2026, ApJ, 1000, 230A, investigates the NIR coronal line emission of four dwarf galaxies. Coronal lines are highly ionized emission lines and their presence strongly indicates AGN activity. Not only do we find extended coronal line emission in these dwarfs but many show broad, asymmetric emission profiles, a tell-tale sign of outflowing gas. While the energtics of these outflow do not indicate the gas is completely expelled from the galaxy, the central regions are clearly disturbed. This discovery can have important ramifications on our view of feedback in dwarf galaxies, and the inclusion of AGN processes in modelling can help alleviate long standing tensions between simulations and observations.
(Top) Spatial flux, width, and velocity maps of broad, outflowing [OIII] emission in one of our dwarf galaxies. (Bottom) NIR coronal line flux and velocity maps of the same galaxy. The extended emission of these highly ionized lines indicates the outflows are of AGN-origin.
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