We present the radial velocity structure of the molecular hydrogen outflows associated to the star forming region Cepheus A .
This structure is derived from the doppler shift of the H _ { 2 } v =1–0 S ( 1 ) emission line obtained by Fabry–Pérot spectroscopy .
The East and West regions of emission , called Cep A ( E ) and Cep A ( W ) , show radial velocities in the range of -20 to 0 km s ^ { -1 } with respect to the molecular cloud .
Cep A ( W ) shows an increasing velocity with position offset from the core indicating the existence of a possible accelerating mechanism .
Cep A ( E ) has an almost constant mean radial velocity of -18 km s ^ { -1 } along the region although with a large dispersion in velocity , indicating the possibility of a turbulent outflow .
A detailed analysis of the Cep A ( E ) region shows evidence for the presence of a Mach disk on that outflow .
Also , we argue that the presence of a velocity gradient in Cep A ( W ) is indicative of a C-shock in this region .
Following Riera et al .
( 23 ) , we analyzed the data using wavelet analysis to study the line width and central radial velocity distributions .
We found that both outflows have complex spatial and velocity structure characteristic of a turbulent flow .