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\subsection{Obsersation}  Images The data  provided were indata  cubes of edge length 256. with 256 pixels/channels on each dimension.  This represented an area of 0.26pc by 0.26pc, with a“depth” of spectrum of  20 km/s wide spectrum  centered at the 0-1 transition of 13CO and 12CO. Using CASA, these When processing the syntehtic  images were observed at a through casa, using simdata (or however it is called now), we assume  distance of ~450pc. 450 pc to the source.  This was chosen as it is the distance of HH46/47, a molecular outflow powered by a forming  star thatis forming and  has been recently  observed using ALMA. with ALMA (Arce et al. 2013).  CASA parameters were set as follows.  Indirection, the RA and Dec of the object to be observed, was set to be the same as that as HH46/47: J2000 8h25m44 -51d00m00  Incell, the angular width of a pixel at the desired distance was calculated using the small angle formula with a pixel size of ~0.001pc and ~0.001pc, assuming  a distance of 450pc. This gave an angle of approximately 0.5arcsec. Incenter specified the frequency on which the spectrum was centered. For 12CO, 13CO,  the 0-1 1-0  transition is at 110.201354GHz and for 13CO 12CO  it is at 115.271201GHz. (no need to give such high precission, you can quote 110.20 and 115.27 GHz in the text)  Inbright was chosen to be the brightest individual pixel in the data cube. This was calculated for each cube. As the cubes were provided in CGS units, this was converted to Janskys.  Noise was set to be tsys-atm which used CASA's pwc (perceptible water vapour) variable to calculate noise. noise (\textbf{Explain this better}.  0.5 (\textbf{what are the units for this number?}  was chosen for this (CASA default). Temperature on the ground and in the sky was set to be 269K (also the CASA default). Pointing time (CASA's 'integration') was chosen to be between 10s and 100s. The effects of this choice will be discussed.  Integration time was another variable tested, with various values between 300s and 10800s chosen for different setups. setups.\textbf{Need to explain better the difference between pointing time and integration time}  Various telescope configurations (antenna list variable in CASA) were used, ranging from the cycle0 cycle 0  compact configuration, two cycle 1 configurations and a configuration with the full array. The differences between these will also be discussed. \subsection{Analysis}