To the east of the nucleus there is a faint Ha cloud (circled red in figure above) located at the same location as a satellite dwarf galaxy candidate that was detected on deep images taken with the 6.5m Magellan telescope (Crnojevic et al, APJ 2016). This previously unreported Ha emission is likely to be the result of active star formation occurring within this dwarf galaxy.My image also reveals Ha emission to the south which is likely caused by the counter jet in this direction, and this is only one of a few images to detect this southern jet feature.
In addition to Ha emission, the jet also results in a smaller amount of OIII emission (see Morganti et al, MNRAS 2011). Prior OIII images have only focused on the inner filament and the first part of the outer filament. This image is the first to show the full extent of the OIII emission jet, including two faint ionised OIII clouds located in the outer segment (circled in figure below). There is diffuse OIII emission radiating from the nucleus which is likely related to starburst within the disc, and this creates a subtle violet halo on the RGBHO image.
On the wider view some extremely faint Ha clouds are visible scattered throughout the galactic cirrus. As the Ha has been processed using continuum subtraction these clouds represent true Ha emission rather than contamination from extended red emission, and in many areas are in different locations and morphology than the cirrus. These clouds likely represent Ha emission from the Milky Way that lie in our line of sight to Cen A.