FIGURE 3. Atmospheric model fits to the light-curve data.
From the following article:
Charon's radius and atmospheric constraints from observations of a stellar occultation
A. A. S. Gulbis, J. L. Elliot, M. J. Person, E. R. Adams, B. A. Babcock, M. Emilio, J. W. Gangestad, S. D. Kern, E. A. Kramer, D. J. Osip, J. M. Pasachoff, S. P. Souza and T. Tuvikene
Nature 439, 48-51 (5 January 2006)
doi:10.1038/nature04276
The segments of the Clay light curve shown here have been expanded such that individual data points are resolved, and the first diffraction fringe is clearly visible during immersion and emersion. A diffraction model with a tenuous atmosphere (solid line), from which our 3
upper limit is derived, is displayed. To illustrate the effect of a substantial atmosphere, a second model is also shown (dashed line), which represents a 50-km scale height and a 10% flux drop at the surface (b = 0.10). This model merges with the data baseline beyond the limits of the plot. The differential bending in the dashed-line model has been enhanced significantly with respect to our upper limit (b = 0.015).
