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\subsection{Fitting the SED}  %Blazar SEDs are dominated by two peaks. The lower energy features can be explained by radio synchrotron radiation from the relativistic electrons in a jet pointing at our line-of-sight and inverse Compton scattering off the synchrotron photons or photons from the originating environment. Massaro et al. (2006) and Tramacere et al. (2007) have shown that both emission processes can be modeled by log-parabolic distributions. In FRSQ blazars, the radio emission is weaker, and so other features, like the accretion disk surrounding the   Blazar SEDs are dominated by two peaks. It has been shown that the low-energy peak, due to radio synchrotron radiation, and the higher-energy bump, due to inverse Compton radiation, can be modeled by log-parabolic distributions \cite{http://adsabs.harvard.edu/abs/2006A&A...448..861M,http://adsabs.harvard.edu/abs/2009A&A...501..879T}. \cite{2006A&A...448..861M,2009A&A...501..879T}.  Also present in blazars are an accretion disk and a hot dusty torus surrounding the super-massive black hole, both of which can be modeled by blackbody distributions \cite{http://adsabs.harvard.edu/abs/2002ApJ...575..667D}. \cite{2002ApJ...575..667D}.  The user will linearly combine these four models to fit the multi-wavelength SED of PKS 1127-14. The user starts a fitting session by opening the Fitting Tool component on the Iris desktop. The SED Viewer updates with an overplotted, unfit powerlaw model, and a plot of the residuals shown below the data. The user removes the powerlaw component, and adds four models from the Preset Components provided by Sherpa: two logarithmic parabolas (\texttt{logparabola}s) for the radio synchrotron and inverse Compton radiation and two blackbodies (\texttt{blackbody}s) for the hot dust and accretion disk. The models are added to the Components field, where the model parameter values are displayed. Double-clicking a component allows you to edit the parameters, e.g. freeze and thaw parameters, reset their initial values, and set their minimum and maximum values.