Scripta clarissimi mathematici M. Ioannis Regiomontani, de torqueto, astrolabio armillari, regula magna ptolemaica, baculo[que] astronomico, & observationibus cometarum, aucta necessariis, Ioannis Schoneri ... additionibus. Item observationes motuum solis, ac stellarum tam fixarum [qua ...] erraticarum. Item libellus M. Georgii Purbachii de quadrato geometrico ...

Here, first of all, the configuration of the sky must be expressed, not as we did before by means of the Sun, for at night it is snatched under the horizon and cannot illuminate the holes of the larger ruler, while by day it obscures the other stars so that they cannot be seen by the eye of the observer. Instead, one must proceed by a different path: therefore, with the Sun situated near the West, shape the form of the sky as was taught previously, and learn the place of the Sun observed in the equinoctial signifer zodiac, and learn which equinoctial degree it lies next to. At the same time, arrange the weighted clock likely a water clock or similar time-measuring device, which also counts the small parts of equal hours, in such a way that you know the position of its index at the moment when you arranged the instrument through the inspection of the Sun. Then, after the sunset as the stars begin to shine, explore by means of the hour-index how much time has passed since the daytime observation, and for every four minutes of an hour, take individual degrees of the equinoctial from the mark observed earlier next to the place of the Sun; and to the end of such an equinoctial arc, apply the place of the Sun noted in the equinoctial signifer. For thus it is fitting to represent the position of the celestial ecliptic. While that trace remains, move the crest hither and thither until the center of the desired star is established in the plane of the circle of latitude, and at the same time the entire star is seen through the holes of the smaller, raised or lowered ruler, just as the thing itself requires. For then the ruler of longitude will show, with its end which extends toward the star, the place of the star in the ecliptic signifer according to longitude. The ruler of latitude, however, will reveal the latitude of the star, whether Northern or Southern, just as its end, turned toward the star, advises. But if it pleases you to work a little more curiously, it will be necessary to increase the motion of the Sun according to the quantity of mean time between the two observations, namely by adding two minutes and nearly half of one degree to the place of the Sun for each equal hour. Furthermore, if you wish to be content with a certain cruder observation without the help of the weighted clock, you will reach the proposed goal in this way: with the Sun leaning toward the sunset, collect the seen place of the Moon from the preceding [problem]. But afterward,