En la Tierra son COORDENADAS GEOGRÁFICAS.

Fuera de la tierra son COORDENADAS ASTRONÓMICAS.

Dr Adelmo Enrique Romero Méndez thank you for your contribution to the discussion

This algorithm has been incorporated into a computer program called STELLA (System to Estimate Latitude and Longitude Astronomically), developed by the U.S. Naval Observatory for Navy shipboard use. This approach would be especially useful for high-accuracy automated observing systems. Practical celestial navigation usually requires a marine chronometer to measure time, a sextant to measure the angles, an almanac giving schedules of the coordinates of celestial objects, a set of sight reduction tables to help perform the height and azimuth computations, and a chart of the region. Observations are limited to a few Sun sights during the day and a few star sights during twilight. Because observations with hand-held sextants have typical uncertainties of about one arcminute, celestial fixes are rarely more accurate than several nautical miles.Both longitude and latitude are angles measured with the center of the earth as an origin. A longitude is an angle from the prime merdian, measured to the east (longitudes to the west are negative). Latitudes measure an angle up from the equator (latitudes to the south are negative). Imagine the lines of latitude and longitude ballooning outward from the Earth and printing them on the inside of the sky sphere, as shown at right. They are now called, respectively, declination and right ascension. Directly out from the Earth's equator, 0° latitude, is the celestial equator, 0° declination. The SE is a heliocentric coordinate system with the Z-axis normal to and northward from the ecliptic plane. The X-axis extends toward the first point of Aries (Vernal Equinox, i.e. to the Sun from Earth in the first day of Spring). The Y-axis completes the right handed set. The celestial coordinate system, which serves modern astronomy so well, is firmly grounded in the faulty world-view of the ancients. They believed the Earth was motionless and at the center of creation. The sky, they thought, was exactly what it looks like: a hollow hemisphere arching over the Earth like a great dome. A geographic coordinate system is a system that uses a three-dimensional spherical surface to determine locations on the Earth. Any location on Earth can be referenced by a point with longitude and latitude coordinates. The Universal Transverse Mercator (UTM) is a map projection system for assigning coordinates to locations on the surface of the Earth. Like the traditional method of latitude and longitude, it is a horizontal position representation, which means it ignores altitude and treats the earth surface as a perfect ellipsoid. India is a vast country. Lying entirely in the Northern hemisphere the main land extends between latitudes 8°4'N and 37°6'N and longitudes 68°7'E and 97°25'E.

The problem is the calculation of the latitude because there is a difference between geocentric (declination) and geodetic latitude. Also, there is a slight difference between the geoidal latitude that observations are based on (they follow the observer's vertical) and geodetic latitude, which is defined by the normal to the ECEF (WGS84) reference ellipsoid. Another matter to consider is the local datum where transverse Mercator projection is based and must be reduced to ECEF (WGS84). An interesting discussion is in the link:

https://www.quora.com/What-is-the-difference-among-astronomical-latitude-geocentric-latitude-and-geodetic-latitude

Dr John Hatzopoulos thank you for your contribution to the discussion

Astronomical (or celestial) coordinate systems are organized arrangements for specifying positions of satellites, planets, stars, galaxies, and other celestial objects relative to physical reference points available to a situated observer (e.g. the true horizon and north to an observer on Earth's surface). Celestial coordinates are the analogue of geographic longitude and latitude on Earth, projected into space on the sky. The plane of Earth's orbit represents for us the plane of the solar system, and in our sky we see its direction traced out by the path of the Sun over a year with respect to the stars. The Equatorial Coordinate System uses two measurements, right ascension and declination. Right ascension (abbreviated RA) is similar to longitude and is measured in hours, minutes and seconds eastward along the celestial equator. Lines of latitude and longitude form a global grid system. Any point on earth can be located by specifying its latitude and longitude, including Washington, DC, which is pictured here.Latitude and longitude make up the grid system that helps us identify absolute, or exact, locations on the Earth's surface. You can use latitude and longitude to identify specific locations. Latitude and longitude are also helpful in identifying landmarks. Just like Earth's lines of latitude and longitude, the celestial sphere is an extension of the coordinate system we use on Earth, but in our sky. In ancient times, sky watchers thought that the planets, Sun, Moon, and stars orbited around the Earth on glass spheres.The SE is a heliocentric coordinate system with the Z-axis normal to and northward from the ecliptic plane. The X-axis extends toward the first point of Aries (Vernal Equinox, i.e. to the Sun from Earth in the first day of spring). The Y-axis completes the right handed set. Practical celestial navigation usually requires a marine chronometer to measure time, a sextant to measure the angles, an almanac giving schedules of the coordinates of celestial objects, a set of sight reduction tables to help perform the height and azimuth computations, and a chart of the region. Observations are limited to a few Sun sights during the day and a few star sights during twilight. Because observations with hand-held sextants have typical uncertainties of about one arcminute, celestial fixes are rarely more accurate than several nautical miles.