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\subsection{Custom Python Functions}  Iris accepts custom models written as Python functions saved in *.py files. Any number of functions can be written in the file. The function must take two parameters: the first is an iterable of the model parameters, the second is a placeholder for the spectral axis, 'x.' One caveat is that the spectral data (x) must be in terms of Angstroms. For example, a model file for a modified black body  \(B_{\nu}(T) \left(\frac{\nu}{\nu_{0}}\right)^{\beta}\)  could be defined as in Figure \ref{fig:user_model_example}. \ref{subsec:user_model_example}.  User models can be arbitrarily combined with other custom or preset model functions. \subsection{Table Models}  A table model is a single template, having just the x and y coordiantes. Iris accepts two-columned ASCII files as table models, following the convention where the first column is the spectral values (in Angstroms) and the second contains the fluxes (in photons/s/cm^{2}/\AA). The fit returns the normalization constant (or amplitude) of the model.