PARTIAL LUNAR ECLIPSE

Year 1751, on the afternoon of December 2nd.

A detailed astronomical broadsheet or plate depicting the partial lunar eclipse of December 2, 1751. It features a large decorative cartouche with calculation data, tables of local times for different cities, a diagram showing the Moon's path through the Earth's shadow, a detailed map of the lunar surface, and celestial projection charts with various measurement scales.

Under the Nuremberg meridian, this eclipse occurs as follows.

Moments of calculation.
True time of full moon, Nuremberg: 1751, Dec 2, p.m. 10^h 17' 23"
True longitude of the Sun: 10^s 10° 51' 4"
Place of the Moon in orbit: 4^s 10° 24' 5"
Longitude from ascending node: 4^s 11° 58' 8"
Increasing southern latitude: 38' 4"
Semidiameter of the Sun: 16' 20"
Semidiameter of the Moon: 16' 49"
Horizontal parallax: 0' 10"
Parallax of the Sun: 9"
Semidiameter of the shadow: 47' 7"
Hourly motion of the Sun: 2' 32"
True hourly motion of the Moon: 38' 32"
Hourly motion of the Moon from the Sun: 36' 0"
Inclination of the orbit to the ecliptic: 5° 11' 0"
From this are derived:
Total duration of the eclipse: 2^h 21' 44"
Magnitude: 10 Digits, 18 minutes

Dig:	h.	m.	s.	Surface spots (According to Hevelius)
1.	9.	13.	12.	Grimaldus.
2.	9.	21.	14.	Aristarchus & Keplerus.
3.	9.	25.	40.	Copernicus & Gassendus.
4.	9.	31.	1.	Reinholdus & Bulialdus.
5.	9.	38.	4.	Tycho & Hevelius.
6.	9.	46.	22.	Maurolycus & Maginus.
7.	9.	56.	22.	Clavius & Alphonsus.
8.	10.	11.	52.	Albategnius & Arzachel.
9.	10.	22.	54.	Thebit & Hipparchus.
10.	10.	33.	26.	Dionysius & Censorinus.
11.	10.	44.	58.	Langrenus & Petavius.

Under the noted meridians, the primary times will be as follows:

	Paris	Berlin	London
Beginning	8. 56. 2.	9. 21. 53.	8. 41. 55.
Middle	10. 6. 54.	10. 32. 45.	9. 52. 47.
End	11. 17. 46.	11. 43. 37.	11. 3. 39.

Magnitude everywhere: 10 Digits, 18 minutes

Duration everywhere: 2^h 21' 44"

Celestial projection showing the times of the phases for the Nuremberg meridian.

A small warning to observers.
This eclipse, since it occurs when the Moon is almost exactly at perigee, is useful for determining the equation of the apogee and, consequently, the equal motion of both luminaries. Therefore, we did not want to pass over recommending its observation to those who love astronomy.

At the top right, a diagram labeled "General diagram designed according to the most subtle measurement of the celestial projection" shows the circular shadow of the Earth and the Moon's path crossing the Ecliptic. The shadow is segmented to show the "eclipsed part" at various moments.

In the center bottom, a circular celestial projection chart shows intersecting arcs and lines with specific contact points labeled "Initial contact" and "Final contact".

In the bottom right, a detailed circular engraving of the Moon's surface displays topographical features like craters and lunar maria, set within a simple border.

Linear measurement scales at the bottom:
1. "Diameter of the Moon: 33' 38""
2. "Semidiameter of the Earth's shadow."
3. "Hourly motion: 1h of 36' 0" divided into minutes."
4. "Scale of scruples: one degree."