Iris version 1.2 is not equipped with the full capabilities of the tool as set forth in the scientific requirements; many additional SED building, analysis, and visualization functions will be added in incremental releases. The features which will be added to Iris functionality in the near future are listed below, as well as plans for longer-term updates.
Short-term Additions to Iris
- Function to evaluate the effect of "de-redshifting" the observed SED
- Determination of the extinction for "de-reddening" the SED
- Complete Batch processing
Long-term Additions to Iris
- Users will be able to perform a bulk search and download of the SEDs associated with multiple sources, e.g., by searching for classes of sources in the archives ("AGNs", "brown dwarfs", etc.), or by supplying a list of source positions or a geometrical region of the sky.
- Iris will be able to ingest data in complex formats, such as spectral data cubes (three-dimensional data) and theoretical spectral models.
- Iris will support the conversion of an aggregate SED to a rebinned SED; i.e., it will be able to bin a raw collection of SED segments and/or photometric points and provide the flux as a function of equally spaced spectral coordinate points, on a linear scale.
- Users will be able calculate integrated fluxes in intervals of spectral coordinates of their choosing, defined from the functional curve generated by the best-fit model of the SED.
- Astrophysics features to be added to the tool include the evaluation of the bolometric luminosity for a source from the measured flux, and an estimate of the distance provided by the user; and the ability for the user to change the default values of the cosmological parameters.
- Iris will be equipped with a convolution tool for convolving a given SED with a generic function of the spectral coordinates; the user can define or be provided with a set of common analytical functions and instrumental profiles for this purpose.
Visualization and Interactive Editing
- Users will be able to perform simple mathematical operations on a selected subset of points or spectral segments, e.g., to average multiple fluxes or spectral segments or perform an aperture correction with a given spatial model of the source.
- Users will be able to "click and drag" a data point, set of points, or entire spectral segment to shift it along both the x and y axes, as well as to adjust the data in other ways, such as changing the curvature of a spectral segment or modifying the error bars.