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\subsection{Inteferometry Modelling}  The simulation data provided were in data cubes with 256 pixels/channels on each dimension. This represented an area of 0.26pc by 0.26pc, with a 20 km/s wide spectrum centered at the 0-1 transition of ^{13}CO and ^{12}CO.  The We use the  Common Astronomy Software Applications (CASA)is a software package that allows us to simulate observations with various interferometers and single dish telescopes. It also has tools that allow us  toanalyse this data.  We will be running two tasks in CASA. The first, simobserve, will  simulatean  observation withvarious specified parameters. The second, simanalyze, will deconvolve and clean  the observation.  \subsection{CASA Parameters}  Simobserve parameters were set as follows.  The data cube was set as the skymodel, and we assume task simobserve. We assumed  a distance of 450 pc to thesource. This was chosen as it is the distance of HH46/47, a molecular outflow powered by a forming star that has been recently observed with ALMA (Arce et al. 2013). The location of the  source(simobserve's "Indirection") was set to be the same as the location of HH46/47: J2000 8h25m44 -51d00m00.  Incell, the angular size of a pixel at the desired distance was calculated using the small angle formula. With a pixel width of ~0.001pc,  and a calculated other CASA settings from this  distanceto the source of 450pc the angular size of a pixle is ~0.5".  Incenter specified the frequency on which the spectrum was centered. For 13CO, the 1-0 transition is at 110.20GHz  andfor 12CO it is at 115.27GHz.  Inbright was chosen to be  the brightest individual pixel in dimensions of  the data cube. This was calculated for each cube. As simulation. We set  the cubes were provided in CGS units, this was converted to Janskys.  Noise was chosen noise  to be tsys-atm which uses CASA's the  pwc (Precipitable (precipitable  Water Vapor)variable and temperature to calculate noise \textbf{still might need more explaination}. Both Temperature  and pwc temperature. These  were kept at their default values. These were CASA defaults of  0.5mm of water anda  ground temperature of 269K. This reflects 269K which reflect  good observing  conditions at \href{http://almascience.eso.org/about-alma/weather/atmosphere-model}{ALMA}. The total observations time (CASA's 'totaltime' variable) was generally chosen to be between 3600s and 7200s. However, some shorter observations were also made to test We examined  the usefullness of snapshots. Each observation is made up of a number of pointings or samplings (CASA's 'integration' variable) which was generally chosen to be 10s. Longer pointings were also tested.  The ALMA configuration (CASA's 'antennalist' variable) used for most effects  of changing  the trials was total integration time,  the 3rd configuration of pointing time and  the full array. However, various other configurations were compared. ALMA array used.  \subsection{Analysis}  The paramters We  used for CASA's analysis were also considered.  The number of cleaning iterations (CASA's 'niter' variable) was chosen the CASA task simanalyze  to be 10 000. deconvolve and clean the observed images.  We will show determined  that increasing the number of 10 000  cleaning iterations beyond this is ineffective.  The cycles were optimal and that we never terminated the clean early with the  thresholdat which cleaning stops (CASA's 'threshold' variable) was  set at 0.1mJy.Tests showed that changing this had little effect of the data.  \subsection{All Runs}  \begin{center}