Ecliptic coordinate system
The ecliptic coordinate system is a celestial coordinate system commonly used for representing the positions and orbits of Solar System objects. Because most planets (except Mercury), and many small solar system bodies have orbits with small inclinations to the ecliptic, it is convenient to use it as the fundamental plane. The system's origin can be either the center of the Sun or the center of the Earth, its primary direction is towards the vernal equinox, and it has a right-handed convention. It may be implemented in spherical or rectangular coordinates.
Primary direction 
The celestial equator and the ecliptic are slowly moving due to perturbing forces on the Earth, therefore the orientation of the primary direction, their intersection at the Northern Hemisphere vernal equinox, is not quite fixed. A slow motion of Earth's axis, precession, causes a slow, continuous turning of the coordinate system westward about the poles of the ecliptic, completing one circuit in about 26,000 years. Superimposed on this is a smaller motion of the ecliptic, and a small oscillation of the Earth's axis, nutation.
In order to reference a coordinate system which can be considered as fixed in space, these motions require specification of the equinox of a particular date, known as an epoch, when giving a position in ecliptic coordinates. The three most commonly used are:
- Mean equinox of a standard epoch (usually J2000.0, but may include B1950.0, B1900.0, etc.)
- is a fixed standard direction, allowing positions established at various dates to be compared directly.
- Mean equinox of date
- is the intersection of the ecliptic of "date" (that is, the ecliptic in its position at "date") with the mean equator (that is, the equator rotated by precession to its position at "date", but free from the small periodic oscillations of nutation). Commonly used in planetary orbit calculation.
- True equinox of date
- is the intersection of the ecliptic of "date" with the true equator (that is, the mean equator plus nutation). This is the actual intersection of the two planes at any particular moment, with all motions accounted for.
A position in the ecliptic coordinate system is thus typically specified true equinox and ecliptic of date, mean equinox and ecliptic of J2000.0, or similar. Note that that there is no "mean ecliptic", as the ecliptic is not subject to small periodic oscillations.
Spherical coordinates 
|heliocentric||l||b||r||x, y, z[note 1]|
Ecliptic longitude or celestial longitude (symbols: heliocentric , geocentric ) measures the angular distance of an object along the ecliptic from the primary direction. Like right ascension in the equatorial coordinate system, the primary direction (0° ecliptic longitude) points from the Earth towards the Sun at the vernal equinox. Because it is a right-handed system, ecliptic longitude is measured positive eastwards in the fundamental plane (the ecliptic) from 0° to 360°.
Ecliptic latitude or celestial latitude (symbols: heliocentric , geocentric ), measures the angular distance of an object from the ecliptic towards the north (positive) or south (negative) ecliptic pole. For example, the north ecliptic pole has a celestial latitude of +90°.
Distance is also necessary for a complete spherical position (symbols: heliocentric , geocentric ). Different distance units are used for different objects. Within the Solar System, astronomical units are used, and for objects near the Earth, Earth radii or kilometers are used.
In ancient times 
Historically, ecliptic longitude was measured using twelve signs, each of 30° longitude, a legacy of astrology. The signs approximately corresponded to the constellations crossed by the ecliptic. Longitudes were specified in signs, degrees, minutes, and seconds; for instance a longitude of 19° 55' 58" was 19°.933 east of the start of the sign Leo, which was 120° from the equinox.
Rectangular coordinates 
There is a rectangular variant of ecliptic coordinates often used in orbital calculation. It has its origin at the center of the Sun, its fundamental plane in the plane of the ecliptic, its primary direction (the axis) toward the vernal equinox, that is, the place where the Sun crosses the celestial equator in a northward direction in its annual apparent circuit around the ecliptic, and a right-handed convention, specifying a axis 90° to the east in the fundamental plane and a axis perpendicular to the - plane in a right-handed sense.
These rectangular coordinates are related to the corresponding spherical coordinates by
Conversion between celestial coordinate systems 
Converting Cartesian vectors 
Conversion from ecliptic coordinates to equatorial coordinates 
Conversion from equatorial coordinates to ecliptic coordinates 
where is the obliquity of the ecliptic.
See also 
- The Ecliptic: the Sun's Annual Path on the Celestial Sphere Durham University Department of Physics
- MEASURING THE SKY A Quick Guide to the Celestial Sphere James B. Kaler, University of Illinois
Notes and references 
- Nautical Almanac Office, U.S. Naval Observatory; H.M. Nautical Almanac Office, Royal Greenwich Observatory (1961). Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and Nautical Almanac. H.M. Stationery Office, London. pp. 24–27.
- Explanatory Supplement (1961), pp. 20, 28
- U.S. Naval Observatory, Nautical Almanac Office (1992). In P. Kenneth Seidelmann. Explanatory Supplement to the Astronomical Almanac. University Science Books, Mill Valley, CA. pp. 11–13. ISBN 0-935702-68-7.
- Meeus, Jean (1991). Astronomical Algorithms. Willmann-Bell, Inc., Richmond, VA. p. 137. ISBN 0-943396-35-2.
- Explanatory Supplement (1961), sec. 1G
- Leadbetter, Charles (1742). "A Compleat System of Astronomy". J. Wilcox, London. p. 94., at Google books; numerous examples of this notation appear throughout the book.
- Explanatory Supplement (1961), pp. 20, 27
- Explanatory Supplement (1992), pp. 555-558