Many of the techniques used on optical data to convert broadband photometry to flux, including creating spectral energy distributions and integrating the pseudobolometric flux, don't work very well in the ultraviolet. After struggling with these issues for years, I wrote the following paper to demonstrate the difficulties and quantify the effects. It is now on astro-ph and published in the Astronomical Journal.
The figures in the paper were designed to compare effects with a consistent wavelength range within the confines of a two column article. So many of the figures are tall and hard to read if you are reading or projecting the paper onto a typical wide screen (like for many astro-ph/astrocoffee style discussions). I have created a pdf with most of the figures reproduced as single panels. That version is here.
Comments are welcome.
