We Need to Resolve the Resolution Issue
Rather than arbitrarily increasing the rotational velocity parameters, we would like to quantify hydra's line widening so we can degrade our synthetic spectra accordingly. We're using a simple chi-square test to compare spectra, so its important to make the synthetic spectra look as much like the observed spectra as possible. Therefore, we need to mimic the processes and transformations that the observed spectra underwent (see the previous discussion of the rectification procedure). On a related note, I wonder if we need more information than just surface gravity to model the width of the lines before they reach the detector. Would we expect 9020's components to be fast rotators? Would they have especially turbulent photospheres? What other factors could significantly affect the line widths?