Slitless Solar Spectroscopy

Spectrographs have traditionally suffered from the inability to obtain line intensities, widths, and Doppler shifts over large spatial regions of the Sun quickly because of their narrow instantaneous field of view. This has limited the spectroscopic analysis of rapidly varying solar features like, flares, CME eruptions, coronal jets, and reconnection regions. Imagers, on the other hand, have provided high time resolution images of the full Sun with limited spectral resolution.In this paper we present recent advances in deconvolving spectrally dispersed images obtained through broad slits. We use this new theoretical formulation to examine the effectiveness of various potential observing scenarios, spatial and spectral resolutions, signal to noise ratio, and other instrument characteristics. We test this method on two specific observing scenarios.With the original method developed for the single spectral line case, we first analyze the effect of overlapping spectral lines on the resulting spectral parameters. Second, we determine how well the method performs when given dispersed image input with either three orders (0, +1, -1), or with two orders (0, +1). In both cases a more accurate Gauss error function calculation is employed on the dispersed images. This information will lay the foundation for a new generation of spectral imagers optimized for slitless spectral operation, enabling us to obtain spectral information in transient solar events.