deletions | additions       diff --git a/Temperature [1].tex b/Temperature [1].tex  index 90d63c7..145eca5 100644  --- a/Temperature [1].tex  +++ b/Temperature [1].tex 
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\begin{equation} %\label{eqn:J(T)}  J(T) = \frac{hv}{k(e ^ {\frac{hv}{kT}} - 1)}  \end{equation}  $M$ is the total  mass, $[{\rm H}_2/^{12}{\rm CO}]$ the mass ratio between $H_2$ and $^{12}CO$ (assumed to be $1/(8.6 ($1/(8.6  * 10 ^{-5})$, $\mu_m$ the mean molecular mass of $H_2$, $H_2$ ($2 * 1.6733 * 10 ^{-24}g$),  $A$ the area of emission (1 pixel), $T_{ex}$ the assumed temperature of excitation, $T_{bg}$ the background temperature (assumed to be 0K), ($0K$),  $T_B$ the brightness temperature, temperature calculated using the Rayleigh Jeans law,  $\Delta v$ the velocity resolution, k $k$  the Boltzman constant, $v$ the frequency of observation (115.3Ghz for $^{12}CO$, 110.2Ghz for $^{13}CO$). $^{13}CO$), $h$ Planck's constant.  (Bourke et al. 1997)  {\bf Every symbol here must be defined. What is v, what is alpha, A, etc? Explain it to yourself a year ago. If that you wouldn't understand, the reader probably won't either. State what this equation assumes. Also how do you get $T_B$ from the datacube I gave you? Give the equation you use. } Edit: I think that this has been dealt with, though not 100\% sure I have explained everything. Have checked the code and these are the equations. Should I include the fact that mass is the integral/sum over all pixels or is that implied?}  To ontain the momentum and energy, we used the calculated mass for each voxel as well as its known velocity. The data had velocity resolution of 0.08 km/s and included mass with $|v| < 10 km/s$.  {\bf need to add a couple sentences on how you derive the momentum and energy: "To obtain the momentum..."}  {\bf Before discussing excitation temperature, need a general paragraph on the basic trends, i.e. what does the raw simulation show, what are the general trends with time. I can write this if you want.} want.  Edit: I feel that there is a lot to add to this - this description just came from watching the video a couple of times.}  The simulation shows the gas cloud collpasing and the protostar forming at t=0.17Myr. The outflow begins to form immediately and is well extablished by t=0.22Myr with a significant mass of dense, high velocity gas. However, the outflow dissapates and by t=0.35Myr its structure is no longer visible. The free gas is low density and moving at a low velocity.  \section{Results}  \subsection{Excitation Temperature} 
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\begin{equation}  \bar T = \frac{ \Sigma \rho_i T_i }{\Sigma \rho_i}  \end{equation}  {\bf update if this is not what you did} did - Edit this is slightly complicated as T average was actually really high, even when accounting for mass. However if you looked at a graph of the temperatures you saw two spikes - one somewhere between 100K - 1000K (which was low density gas) and another at ~10K. I took the average of this lower spike. Should I call of T_{avg} high density gas?}  \begin{center}  \begin{tabular}{c | c} \label{tab_texcit}