[OIII],Hα, and [NII] images of the central region demonstrating the inner, highly collimated jet; a PSF pattern was subtracted, but some faint PSF emission spikes remain visible on the Hα and [NII] images. The position of the adopted jet axis (white lines with arrows) is superimposed on the Hα and [NII] images, as has been shown in Fig. 2. [OIII] contour levels are given for three levels from 10⁻¹⁷ to 10⁻¹⁵ erg cm⁻² s⁻¹ Å⁻¹. The [OIII]image exhibits the fine helical structure of the inner, highly collimated jet, which consists of a wiggling continuous flow, loops (L1 and L2), and the chain of small knots (marked as N7–11 following the numeration for “N”-knots from Paresce & Hack 1994) This emission pattern can also be traced as loops on the Hα and [NII] images. The [OIII] and Hα images also show that whereas the starting position of the NE jet agrees well with the proposed location of R Aqr stellar system, the starting position of the SW emission is shifted relative to the adopted jet axis by 0.′′7.