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The open SEDs are listed in the Science Tools frame. The user selects the SED they wish to analyze, and inputs the required information for a calculation.  \subsubsection{Redshifting}  Redshifting an SED in Iris refers to cosmological redshift. Because the apparent magnitude of a source is dimmer at high redshifts than low redshift, we correct the flux so that the area under the shifted SED equals that of the un-shifted SED [REFERENCES, astLib]. For the Sherpa implementation, astLib]:  \[\]  In sherpa-samp,  we extend astLib's astSED.redshift function astSED class for its implementation of redshifting SEDs  [REFERENCE]. From the user's perspective, he/she supplies the initial and final redshift of the SED and clicks "Create New SED." The returned SED has the same name of the unshifted SED, appended with _redshift. For example, if the final redshift is \textit{z}\(=0.0\) the shifted SED is named "Sed_0.0."  \subsubsection{Interpolation}  Users can interpolate an SED along the spectral axis. We provide three interpolation options: linear, linear spline, and nearest neighbor. Interpolation may be carried out on a linear or logarithmic scale. Users may choose the number of bins, the spectral range overwhich to interpolate, and may choose to smooth the resultant SED via a boxcar method.  \subsubsection{Integration}  From the user's perspective, he/she supplies the initial and final redshift of the SED and clicks "Create New SED." The returned SED has the same name of the unshifted SED, appended with _redshift. For example, if the final redshift is \textit{z}\(=0.0\) the shifted SED is named "Sed_0.0."