Grey and white contours show the 3.6 and 1.3 cm radio continuum emission from the ionized jet in this source. Note the elongated structure (SE-NW) in the dust and molecular gas perpendicular to the radio jet (SW- NE). From Patel et al. (2005).[]{data-label="fig:patel"}](patel_bw.ps){width="10cm"}

The direct observational evidence of accretion discs around massive young stars is now beginning to arrive. Millimetre interferometry had delivered convincing observations of compact flattened structures around the more luminous intermediate mass young stellar objects such as GL490 (Mundy & Adelman 1988) and G192.16-3.82 (Shepherd & Kurtz 1999). Now sub-millimetre interferometry has heralded the best example of a disc around a genuinely luminous object. Patel et al. (2005) have used the SMA to resolve an elongated dust and molecular structure 1000 AU in size that is perpendicular to the radio jet in Cep A2 (Fig \[fig:patel\]). The molecular line has a rotational kinematic signature which helps to confirm the disc interpretation. This is a taster of what ALMA will do for massive star formation studies.

We consider the alternative coalescence model by Bonnell et al. (1998) to be unnecessary, unrealistic and unsupported. Unnecessary since there was never really a fundamental problem with the accretion picture as described 