Context : The region G24.78+0.08 , which is associated with a cluster of high-mass young stellar objects in different evolutionary stages , is one of the best laboratories to investigate massive star-formation .

Aims : We aim to image the molecular outflows towards G24.78+0.08 at high-angular resolution using SiO emission , which is considered the classical tracer of protostellar jets .
In this way we study the mass loss process in which we previously detected a hypercompact ionised region , as well as rotation and infall signatures .

Methods : We performed SiO observations with the VLA interferometer in the J = 1–0 v =0 transition and with the SMA array in the 5–4 transition .
A complementary IRAM 30-m single-dish survey in the ( 2–1 ) , ( 3–2 ) , ( 5–4 ) , and ( 6–5 ) SiO lines was also carried out .

Results : Two collimated SiO high-velocity ( up to 25 km s ^ { -1 } w.r.t .
the systemic velocity ) outflows driven by the A2 and C millimeter continuum massive cores have been imaged .
On the other hand , we detected no SiO outflow driven by the young stellar objects in more evolved evolutionary phases that are associated with ultracompact ( B ) or hypercompact ( A1 ) H ii regions .
The A2 outflow has also been traced using H _ { 2 } S. The LVG analysis of the SiO emission reveals high-density gas ( 10 ^ { 3 } –10 ^ { 4 } cm ^ { -3 } ) , with well constrained SiO column densities ( 0.5–1 10 ^ { 15 } cm ^ { -2 } ) .
The driving source of the A2 outflow is associated with typical hot core tracers such as CH _ { 3 } OCHO ( methyl formate ) , C _ { 2 } H _ { 3 } CN ( vinyl cyanide ) , HCC ^ { 13 } CN ( cyanoacetilene ) , and ( CH _ { 3 } ) _ { 2 } CO ( acetone ) .

Conclusions : The driving source of the main SiO outflow in G24 has an estimated luminosity of a few 10 ^ { 4 } L _ { \sun } ( typical of a late O-type star ) and is embedded in the 1.3 mm continuum core A2 , which in turn is located at the centre of a hot core that rotates on a plane perpendicular to the outflow main axis .
The present SiO images support a scenario similar to the low-mass case for massive star formation , where jets that are clearly traced by SiO emission , create outflows of swept-up ambient gas usually traced by CO .