deletions | additions       diff --git a/subsubsection_Fitting_the_PSDs_With__.tex b/subsubsection_Fitting_the_PSDs_With__.tex  index 2b235b6..25e8a89 100644  --- a/subsubsection_Fitting_the_PSDs_With__.tex  +++ b/subsubsection_Fitting_the_PSDs_With__.tex 
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\end{equation}  $\alpha$ and $\beta$ are spectral indices, $A$ is just a normalization factor, and $\nu_b$ is the break frequency in the singly broken model. The goodness of fit from each model for each AGN will be compared to determine which model is correct. For all of the AGN where the singly broken model is the best fit we will have, for the first time, characteristic timescales in the 14--79 keV energy range.  \subsubsection{Case Study: 3C 273}  To test the viability of our method, we have downloaded the \nustar\ observation for 3C 273 as well as the 70 month \bat\ light curve. The \nustar\ observation was reduced using \textit{nupipeline} and \textit{nuproducts} contained in \textit{HEASOFT}. After binning the \swift/BAT and \nustar\ light curves to 5 day and 500 s bins respectively, the PSDs for each were measured using the innovative new technique presented in Zoghbi et al. (2013). Figure~\ref{fig:3C273}, shows the PSD power for 3C 273 derived from the \swift/BAT and \nustar\ light curves.