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Our sample consists of 56 spectroscopically confirmed quasar light curves from the seventh data release of the Sloan Digital Sky Survey (Schneider et al. 2010). These quasars range in redshift from $z = 0.19$ to $z = 3.83$ and in luminosity from $L = 10^{15} L_{\odot}$ to $L = 10^{20} L_{\odot}$. %  These samples were taken from the Southern Equitorial Stripe known as Stripe 82. Stripe 82 is a $275^{2}$ degree area of sky with repeated sampling centered on the celestial equator. It reaches 2 magnitudes deeper than SDSS single pass data going as deep as magnitude 23.5 in the r-band for galaxies with median seeing of 1.1'' (Annis et al. 2014).  These samples were chosen because they exist in the field of the Kepler K2 mission's campaign 8. This will eventually give us K2 has  a muchdenser data set with  shorter cadence allowing than SDSS with observations approximately every 30 minutes. This increase in time sampling rate will allow  us to probe far deeper into the short-term variability properties of these objects than would be possible with SDSS alone. as compared to SDSS.  %Talk more about Kepler Each light curve contains photometric information from two bands (g and r) with as much as 10 years of data. The number of epochs of data range from 29 observations to 81 observations in all photometric bands with sampling intervals ranging from one day to two years. This inconsistent sampling will lead to issues with our analysis which will be discussed later. %  PSF magnitudes are calibrated using a set of standard stars (Ivezic et al 2007) to reduce the error in our data down to 1\%. We then convert these magnitudes to fluxes for our analysis and convert observed time sampling intervals to the rest frame of the quasar. %  We use asinh magnitudes (also referred to as "Luptitudes") for flux conversion (York et al. 2000) (Lupton, Gunn, \& Szalay 1999) as is standard for SDSS.  
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  $$ $$    *then the PSD  **then maybe a little bit on the structure function  *Then introduce the greens function  \section{The Kalman Filter}    \section{Fitting CARMA Models}  \section{Canonical Light Curves}  \subsection{SDSS J134342.5-004243.8 (sample 36 in r-band)}