deletions | additions       diff --git a/subsection_Background_and_Motivation_Accretion__.tex b/subsection_Background_and_Motivation_Accretion__.tex  index bef990d..32b3edf 100644  --- a/subsection_Background_and_Motivation_Accretion__.tex  +++ b/subsection_Background_and_Motivation_Accretion__.tex 
...
In \citet{Shimizu_2013}, we took advantage of the $>5$ years of continuous monitoring of the ultra-hard X-ray sky to analyze the long-term light curves for 30 of the brightest AGN in the \textit{Swift}/BAT sample by constructing the PSD. We attempted to measure for the first time the break in the PSD at these high energies to determine if the same \citet{McHardy_2006} relationship exists. Further any evolution of the break timescale with energy would give insight into the geometry of the corona assuming the timescale is related to a radial distance away from the SMBH. Unfortunately, due to the relatively low sensitivity of \textit{Swift}/BAT, the time resolution of our light curves was limited to $\sim5$ days. The PSD was therefore limited to timescales $>10$ days given Nyquist sampling. We were successful in measuring the slopes of the low frequency PSD finding nearly all of the AGN were consistent with a slope of -1, very similar to the PSD in the 2--10 keV range.   \textit{NuSTAR}, launched in 2012, however provides a window to the shorter timescales necessary to measure the PSD breaks. Its high sensitivity (1000 times more sensitive than \textit{Swift}/BAT) and remarkable timing capabilities allow one to create high quality light curves that can cover timescales from several hundred to several hundred thousand seconds. \textit{NuSTAR} also has overlapping energy coverage with \bat\ between 14--75 keV. The PSD constructed from \nustar\ therefore can be combined with the \bat\ light curves and extend the PSD over nearly six orders of magnitude in temporal frequency.  In this proposal we will outline our plan for selecting \bat\ AGN from the \nustar\ archive, our method for constructing and analyzing the PSD using a new maximum likelihood technique, and the expected scientific goals and implications.