These eclipse maps display local circumstances computed using the IQP eclipse computational method. This method is based on the precise 3D eclipse computational method designed in 2011 by John Irwin, from the UK. The IQP method is less computationally intense than the 3D method, but it aims to compute internal contact times (i.e. second and third contact) to within 0.1s of the ones computed with the 3D method.

The IQP method accounts for both the lunar limb and observer site topography, and it relies on an improved value for the eclipse solar radius (i.e. 959.95"), partly based on researches by the Besselian Elements Team. The eclipse centreline and the northern and southern limits of the umbral shadow path also accounts for these three factors. Hence, these lines are not smooth lines, as in most publicly available eclipse maps, but are noticeable jagged. Two lines are presented for both limits: they correspond to two values of the eclipse solar radius (i.e. 959.90" and 960.00") in order to create a region of uncertainty, instead than a simple line.