Abstract
The spectral data collected needs to be reduced to numbers and plots that are useful to astronomers, physicists, chemists, and scientists in general. Atlas plots of the spectrum of the radiation at both low and high dispersions are important. The former gives an overview of the intensity distribution, and the latter shows details such as line shapes and widths. Another need is for a line list that includes all lines evident on the high resolution atlas, and which incorporates accurate fitted line parameters, including frequency and wavelength, intensity, width, area, and damping, or an equivalent set of line parameters. The chapter discusses making of atlases and line lists. The examples are based on data taken on the McMath–Pierce Fourier transform spectrometer at the National Solar Observatory, Kitt Peak. With the “linelist” command and subsequent least square fitting, one can make a list of lines and their fitting parameters directly from an emission spectrum or an absorbance spectrum.
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