Editing Latitude (section)

==Astronomical latitude==
[[File:Geoida.svg|thumb|{{olist
    |Ocean
    |Ellipsoid
    |Local plumb line
    |Continent
    |Geoid
}}]]
'''Astronomical latitude''' ({{math|Φ}}) is the angle between the equatorial plane and the true [[vertical direction]] at a point on the surface. The true vertical, the direction of a [[plumb line]], is also the [[gravity direction]] (the resultant of the [[gravitational acceleration]] (mass-based) and the [[centrifugal acceleration]]) at that latitude.<ref name=torge/> Astronomic latitude is calculated from angles measured between the [[zenith]] and stars whose [[declination]] is accurately known.

In general the true vertical at a point on the surface does not exactly coincide with either the normal to the reference ellipsoid or the normal to the geoid. The geoid is an idealized, theoretical shape "at mean sea level". Points on land do not lie precisely on the geoid, and the vertical at a point at a specific time is influenced by tidal forces which the theoretical geoid averages out. The angle between the astronomic and geodetic normals is called ''[[vertical deflection]]'' and is usually a few seconds of arc but it is important in geodesy.<ref name=torge/><ref name=wellenhofmoritz>{{cite book|last1=Hofmann-Wellenhof |first1=B. |last2=Moritz |first2=H. |date=2006 |title=Physical Geodesy |edition=2nd |isbn=3-211-33544-7}}</ref>

Astronomical latitude is not to be confused with [[declination]], the coordinate [[astronomer]]s use in a similar way to specify the angular position of stars north-south of the [[celestial equator]] (see [[equatorial coordinates]]), nor with [[ecliptic latitude]], the coordinate that astronomers use to specify the angular position of stars north-south of the [[ecliptic]] (see [[ecliptic coordinates]]).