These eclipse maps display local circumstances computed using the IQP eclipse computational method. This method is based on an accurate 3D numerical technique devised in 2011 by team member John Irwin. The IQP method is less computationally demanding than the 3D one but it aims to compute internal contact times (i.e. second and third contact) to within 0.1 seconds of the times derived from the 3D method.

The IQP method accounts for the topography on both the lunar limb and at the observer site, as well as relying on an improved value for the eclipse solar radius (959.95" ± 0.05", based on research by the Besselian Elements Team). The eclipse centreline and the northern and southern limits of the umbral shadow path also account for these three factors. Hence, these lines are not smooth lines, as in most publicly-available eclipse maps, but are noticeably jagged. Two lines are presented at each path limit corresponding to two values of the eclipse solar radius (959.90" and 960.00") in order to display a region of uncertainty rather than a simple line.

The shadows shown on the map are calculated based on the azimuth and altitude of the Sun's centre at maximum eclipse for every location. A correction for refraction is applied based on Sæmundsson's formula.

The red line appearing after clicking on the observer's location shows the direction of the Sun at maximum eclipse. The 3 dots along the line correspond to the location of eclipse-blocking low, medium and high clouds: if clouds at a certain reference height were present at the vertical of the corresponding dot, they would be in the direct line of sight of the eclipsed Sun as seen from the observer's location. On eclipse day, low/medium/high clouds weather forecasts should be checked for the locations indicated by those three dot rather than for the observer's location.

The following table summarises technical aspects of the computations. The map will be updated a couple of months before the eclipse when accurate EOP predictions become available.

Planetary ephemeris	JPL/DE440.
Astrometric method	Light-time + gravitational light deflection + planetary aberration.
Astrometric origin	Hybrid (topocentric & geocentric).
Earth orientation model	IAU2006A-EQX + EOP (TT–UT1 = +69.1840 s).
Earth orientation parameters	TAI–UTC = +37 s, UT1–UTC = +0.0000 s, polar motion = (+0.000, +0.000)".
Moon orientation model	ME421 (relative to PA440).
Mean solar radius	(696221 ± 36) km or (959.95 ± 0.05)" at one au.
Mean lunar radius	1738.091 km.
Terrestrial radii	6378.137 km, 6356.752 km (WGS84).
Lunar DEM	SLDEM2015/LDEM128 (256/128 pixels per degree).
Terrestrial DEM	SRTM3 (1200 pixels per degree) + EGM96 geoid undulation.
Software	EclipseView, LimbView & SkyWare (proprietary).