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(If you can translate this graphic into another language, feel free to get in touch with the author.). Without text and bottom scale indicator Without English text Blank version Versión española 中文版 version française deutsche Version Nederlandse versie schwarzweiß deutsche Version 2018 version
A celestial map by the Dutch cartographer Frederik de Wit, 1670. A star chart is a celestial map of the night sky with astronomical objects laid out on a grid system. They are used to identify and locate constellations, stars, nebulae, galaxies, and planets. [1] They have been used for human navigation since time immemorial. [2]
The Harmonia Macrocosmica is a star atlas written by Andreas Cellarius and published in 1660 by Johannes Janssonius.The first part of the atlas contains copper plate prints depicting the world systems of Claudius Ptolemy, Nicolaus Copernicus, and Tycho Brahe.
The International Celestial Reference System (ICRS) is the current standard celestial reference system adopted by the International Astronomical Union (IAU). Its origin is at the barycenter of the Solar System , with axes that are intended to "show no global rotation with respect to a set of distant extragalactic objects".
1 Regions and celestial objects of the Solar System. ... Print/export Download as PDF; Printable version; In other projects
Diagram illustrating the definition of the hour circle of a star In astronomy , the hour circle is the great circle through a given object and the two celestial poles . [ 1 ] Together with declination and distance (from the planet's centre of mass ), it determines the location of any celestial object .
In astronomy, the rotation period or spin period [1] of a celestial object (e.g., star, planet, moon, asteroid) has two definitions. The first one corresponds to the sidereal rotation period (or sidereal day), i.e., the time that the object takes to complete a full rotation around its axis relative to the background stars (inertial space).
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A direct distance measurement of an astronomical object is possible only for those objects that are "close enough" (within about a thousand parsecs ) to Earth.