Measuring of the distance of two points is possible by making a line between them and by placing a measuring rod along it – supposed the distance is not too long between our points. As the distance becomes longer, this procedure starts to be complicated and expensive: distances of more than a several hundred meters are very hard to measure this way. If the terrain between our points is rough or inpassable, this method cannot be applied at all.

A new method was introduced at the end of the 16th, early 17th centuries. Measuring a longer distance can be made by measuring a shorter line and some angles. The first triangulation was proposed by Gemma Frisius (Fig. 11), then in 1615, another Dutchman, Snellius accomplished a distance measurement by triangulation between the towers of Alkmaar and Breda (true distance cca. 140 kilometers, throughout the Rhein-Maas delta swamps; Fig. 12). During the campaign, he set up triangles with church towers at the nodes and measured the angles of all triangles. Having these data, it was needed to measure only one triangle side to calculate all distances between the nodes.

The Snellius-measurements provided an interesting invention: the sum of the detected inner angles of a triangle occurred to be slightly more than 180 degrees (Fig. 13). This is the consequence of the non-planar, spheroid geometry of the surface of the Earth, and this is true at spherical triangles. It was the root of a new branch of the geometry: the spherical trigonometry.

Using triangulation networks, not only distances but also coordinates can be determined. For this, it is first needed to measure the geographic coordinates of one point of the network. That’s why there is in most cases an astronomical observatory at the starting point of a geodetic network: these measurements can be carried out there in most simple way. Also it is necessary a baseline: a shorter distance between two network points, whose distance is measured physically, and an azimuth: the measured angle between the true north and a triangle edge to a selected network point. Of course, the angles of all triangles should be measured together with the heights of the points. Using all of these data, and assuming an ellipsoid with a pre-set semi-major axis and flattening, the coordinates of all network points can be calculated. They are called triangulated coordinates. The longitude values in these coordinates are measured from the meridian of the astronomical observatory (Fig. 14).

To check the obtained coordinates of the base points, more baselines and –
which later brought a real revolution in the data processing – the
astronomical coordinates were observed at several triangulation points (at the
so-called Laplace-points) of the network. The *observed*
positions, however, differed from the ones, *computed* by the
trigonometry. The difference occurred in all cases and its magnitude was not
predictable. Its cause is the geoid shape of the Earth: the astronomic observations
are based on the knowledge of the local horizontal and vertical lines, which are
slightly different from the tangent and normal directions of the ellipsoid. As we
mentioned above, the whole body is not exactly an ellipsoid. It is almost that, but
not completely.

This problem became so important in the first half of the
19^{th} century that Gauss invented his famous method of
the least squares exactly to solve that. The goal is to ‘adjust’ the coordinates of
the base points in order to minimize the squares of the differences occurring at the
Laplace-points. The method is called *geodetic network
adjustment*, which is, in practical words, to homogenize the errors,
mostly caused by the geoid shape, in the whole network. The result of the adjustment
is a geodetic point set organized into a network, with their finalized coordinate
values.

What means the adjustment from geometric point of view? What is the geometric result? An ellipsoid whose

size and shape was pre-set during the adjustment;

semi-minor axis fits (as much as possible) to a parallel direction of the rotation axis;

surface part – the one set by the extents of the network – fits optimally to the same part of the geoid.

The geometric center of this ellipsoid is, of course, different from the mass center of the Earth (Fig. 15). This way, not only the size and shape of the ellipsoid is known but also its spatial location.

From the point of view of the ellipsoid location method in space, there are three types of them:

deliberate displacement: there is only one astronomical base-point, the network is not adjusted, the ellipsoid is fit to the geoid surface at only one point (usually the location of the astronomical observatory). This method is characteristic at the small islands in the ocean, with no continent on the horizon; the network names are often indicated by the ’ASTRO’ sign. Also, this is the usual method used at the old mapping works, having geodetic basis that was build before the invention of the adjustment method.

relative displacement: the network adjustment is accomplished, the ellipsoid is fit to a certain part of the geoid surface, practically to the extents of the survey.

absolute displacement: the geometric center of the ellipsoid is at the mass center of the planet, the semi-minor axis lies in the rotational axis. It cannot be realized just by surface geodesy or geophysics (as the exact direction of the mass center cannot be determined from the surface by geophysical methods). For its implementation, space geodesy (Doppler measurements, GPS) is needed. Prior to the space age, before to the 1960s, there were no ellipsoids with absolute displacement. The WGS84 is a typical example of this.