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Iris provides 1D interpolation along the spectral axis. There are 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}  The Integration tool was developed to make estimating integrated fluxes of a SED quick and painless. Iris provides two methods of integration: (1) through a user-defined passband, and (2) through a photometric filter. The first option lets the user specify the spectral range in wavelength, frequency, or energy units (Angstroms, Hz, and keV, respectively) to integrate under. The second estimates the integrated flux measured through any of the photometric filters provided by the Spanish Virtual Observatory's (SVO's) Filter Profile Service ([REFERENCE]). Service\footnote{http://svo2.cab.inta-csic.es/theory/fps/index.php} \cite{http://adsabs.harvard.edu/abs/2013arXiv1312.3249S}.  We chose the SVO's Filter Profile Service because of its extensive collection (over 1000 filters at IR, optical and UV instruments) and of its VO-compliancy. The user chooses from a list of filters which can be searched by double-clicking on an instrument name, or by searching for a string in the browser. The user sees the min, max and effective wavelengths of the filters before applying the filter to the SED. How does it work in the background??  Both methods return the effective wavelength of the passband in Angstroms and the calculated flux in Janskys. The user can export the data to a new SED or save the results to a FITS or VOTable file.