General ephemerides of the solar system bodies

To observe the solar system bodies from the Earth at a given moment, it is necessary to know their positions on the celestial sphere. In a more general way, this implies to determine the considered body, Earth and Sun positions related to a given time. For that we use a planetary theories which provide (analytical or numerical) description of planets movement at the time of their revolution around the Sun.
In the same way there are natural satellites theories about their movements according to their central body. For the asteroids and other small bodies of the solar system, it is following a numerical integration of their movement that we can determine their orbit.

You can carry out calculations of positions ephemeris of any body of the solar system for one or more dates spread over an time span of which you will indicate the initial date, the number of dates and the step of calculation. The provided timescales are Terrestrial Time (TT) and the coordinated universal Time (UTC). The planetary theories suggested are upon choice INPOP06 [14], VSOP82 [2], DE200 [3], VSOP87 [4] and DE403 [5], DE405 and DE406 while natural satellites theories are NOE-MARS-06 [6] for Mars, L1 [7] for Jupiter, TASS 1.7 [8] for Saturn and GUST86 [9] for Uranus. For the Moon, the theory used is, according to case's, ELP2000-82 [13] or ELP2000-82B or LE200 [3] or LE403 [5] or LE405 or LE406.

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