Fitting of the dust model with the observations. Left panel: comparison of the observed (black contours) and modeled (red contours) tail brightness isophotes. The innermost contour corresponds to 8 × 10⁻¹⁴ solar disk units, and the brightness decreases in factors of two outward. One solar disk intensity unit corresponds to 2.4 × 10⁶ erg s⁻¹ cm⁻² sr⁻¹ Å⁻¹. The images are rotated to the conventional orientation (north up, east to the left). The x- and y-axes are labeled in kilometers projected on the sky at the object distance. The blob observed to the right of the comet optocenter is a bright star. Right panel: comparison of observed (black line) and modeled (red line) tail brightness along the direction described by the blue dotted line in the left panel.