system. Proper motion studies reveal velocities of 500 (Martí et al. 1998). Other examples are G35.2N (Gibb et al. 2003) and IRAS (Rodríguez et al. 2005) and possibly W3 IRS 5d2 (Wilson et al 2003), which are mostly much more knotty and have a more exaggerated point symmetry. In other cases we just resolve the base of the jet; the best example being Cep A2 as in Fig \[fig:patel\], and GL 2591 also falls in this category (Trinidad et al. 2003). The fast motion in the Cep A2 jet has recently been confirmed by proper motion studies (Curiel et al. 2006) (Figure \[fig:cepa2\]). One expects that such highly collimated flows are driven by MHD mechanisms in the star-disc system as for low-mass outflows.

![Series of VLA 3.6 cm continuum maps of the jet from the massive YSO Cep A2. Note the outward motion of the knots in the jet which corresponds to a speed of 480  on the sky and nearly 600  after correction of inclination. The filled circles mark the position of the knots in the 1999 epoch. From Curiel et al. (2006).[]{data-label="fig:cepa2"}](cepa_pm.ps){height="17cm"}

However, jets are not the only radio morphology seen in massive YSOs. The exciting source of 