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My goal here is to make it easy for the amateur astronomer interested in stellar cartography (particularly 3D maps) and astrometry to do calculations. Unfortunately I can't avoid a lot of astronomical terminology and symbols, which might be a little confusing to the newcomer. If you're already comfortable with concepts such as right ascension, proper motion, absolute magnitude, and parallax, and know how to do calculations with them, you can safely skip this page. Otherwise, read on!
Just as locations on the spherical Earth can be specified with two numbers latitude and longitude  locations on the seemingly spherical sky can be given with a similar pair of numbers. There are many celestial coordinate systems  this site uses one called equatorial coordinates. In effect, equatorial coordinates take the lines of latitude and longitude and expand them off the Earth into space. Thus the celestial analog of latitude measures how far "north" or "south" a star is from the Earth's equatorial plane, and the analog of longitude measures how far around the sky the star is.
The two coordinates have special names:
In this web site, as in many other astronomical publications, the symbol for right ascension is (alpha) and the symbol for declination is (delta).
For most practical purposes, you'll be looking up the right ascension and declination of stars on a star chart or in a list. Most of the time you don't have to worry much more about the details behind them  just think of them as being like longitude and latitude and you'll be all right. There are two exceptions, which are really important only if you plan on doing a lot of calculations:
For historical reasons is normally expressed in hours, not degrees. One hour of right ascension equals 15 degrees, so right ascensions run from zero to 24 hours. Furthermore, hours of right ascension are often divided up into minutes and seconds, so you have to be careful in distinguishing seconds of angle (which come 3600 to a degree) from seconds of right ascension (which come 3600 to an hour).
and are often listed in degrees (hours for ), minutes, and seconds in many catalogs. For astronomical calculations, these units are awkward  it's much easier to work with "decimal" (ordinary floating point) values. Convert, if necessary, by:
Remember, you may need to convert (decimal hours) to degrees by multiplying by 15.
Since people can't perceive depth over the great distances of space, the stars appear to be imbedded in a flat, uniformly large sphere. Thus, for most purposes only two coordinates  right ascension and declination  are needed to locate a star. However, astronomers have figured out that stars are at different distances from the sun, and so describing their positions fully requires a third coordinate. In most cases, the distance to the star serves as that third coordinate.
Although this is easy to understand mathematically  three dimensions, three independent coordinates  actually measuring the distance is extremely difficult. Astronomers did not succeed until the 1830s  more than two centuries after the invention of the telescope  when they finally succeeded in measuring a quantity called parallax. Parallax is the result of motion  as seen from a moving object, nearby objects appear to shift with respect to farther ones. Since the Earth revolves around the Sun once per year, nearby stars show a small but measurable shift during that time.
Parallax is expressed as an angle, and given the symbol (totally unrelated to the symbol for 3.14159...). It depends on the radius of the Earth's orbit (a) and the star's distance (d). The usual formula for parallax is:
However, since it's true for all stars that d >> a, you can use a smallangle approximation (tan x ~ x) and write:
This formula gives in radians. Radians are awkward, though  the parallax angles are always much less than 1 radian, and so astronomers prefer to measure parallax in arcseconds (1/3600 degree, or roughly 1/200,000 radian). Astronomers also define a distance unit from parallax data, one specially chosen to be convenient for working with parallaxes. The parsec, abbreviated pc, is defined as the distance d at which the parallax equals exactly 1 arcsecond. If the distance to a star is given in parsecs, and the parallax is given in arcseconds, then:
To get the distance to a star in parsecs, just take the reciprocal of the parallax. Therefore, parsecs are a very convenient unit when using parallax data, and so I use parsecs rather than light years throughout this site. If you prefer working with light years, 1 pc = 3.262 light years.
The closest bright star to the sun, Alpha Centauri, has a parallax of 0.742 arcseconds and a distance of 1/0.742 = 1.35 pc. Only about 60 stars have distances under 5 pc, and many of the most famous bright stars, such as Betelgeuse in Orion, and Polaris the North Star, are many hundreds of parsecs away.
In addition to knowing where the stars are, it's important to know how bright they are. Astronomers use a system called magnitude to characterize the brightness of a star.
Apparent magnitude, V, is the brightness of the star as it appears from Earth. Most star catalogs give the apparent magnitude of a star along with its position. Larger magnitudes denote fainter stars  this seems a little weird initially, but if you think of "first class" versus "third rate" it will make more sense.
The magnitude scale is logarithmic, with a brightness ratio of 100 corresponding to a difference of 5 magnitude units. Naked eye stars typically have magnitudes from about 0 to +6; Sirius, the brightest star visible in the night sky, has a magnitude of 1.44. By contrast, stars dimmer than magnitude +10 can be seen only in binoculars or telescopes, and those dimmer than +20 require giant telescopes to be seen at all.
Since stars are at very different distances, stars of similar apparent magnitudes may be very different in total light output. Astronomers need a more fundamental measure of stellar energy output. The absolute magnitude M_{V} is defined as the apparent magnitude (V) a star would have if it were moved to a distance of 10 parsecs.
If a star's apparent magnitude V and distance d are known, you can find M_{V} from the following formula:
As an example, Sirius has an apparent magnitude of 1.44, and its distance is 2.64 parsecs. Thus the absolute magnitude of Sirius is:
Just as a 100fold difference in apparent brightness yields a 5 unit change in apparent magnitude, a 100fold difference in true luminosity, i.e., actual energy output, yields a 5 unit difference in absolute magnitude. Thus comparing two stars' absolute magnitudes shows which star is more luminous, and by how much.
The Sun's absolute magnitude is +4.85. The least luminous stars  small cool stars with low masses  have absolute magnitudes of about +18, whereas supernovas, stars undergoing colossal explosions, can have absolute magnitudes of 15 or brighter.
Although stars appear stationary, with the constellations keeping their shape and appearance, the stars are actually moving around rapidly. Only the great distances between stars keep us from noticing this readily. However, with modern equipment, astronomers can easily measure these motions.
A star that is moving through space will normally appear to move across our line of sight to it  that is, the star will appear to move sideways and hence shift with respect to other stars. This motion is called proper motion, because it is an intrinsic motion of the star, rather than an apparent motion caused by the motion of the Earth. Proper motion, denoted by , is expressed as an angular velocity (usually in arcseconds per year).
A star's proper motion can be in any direction. Usually, proper motion is decomposed into two components. One, (_{} ) corresponds to change in right ascension, and one (_{} ) to change in declination. These two components are what you'll normally find in catalogs.
In calculus terms, _{} = d / dt and _{} = d / dt (in appropriate units, of course).
Proper motion is an angular velocity. If the distance to a star is known, the proper motion can be turned into a linear velocity  one with units like kilometers per second. The linear velocity corresponding to proper motion is transverse velocity, V_{T}. Transverse velocity is important for calculating stellar motions over time  a calculation discussed in more detail in the LongTerm Stellar Motions page.
Stars can also move along our line of sight to them. The component of a star's motion towards or away from Earth is the radial velocity, V_{R}. Unlike proper motion, radial velocity is a linear velocity, and has units such as kilometers per second. Radial velocity can be measured accurately by analyzing a star's light in detail.
Finally, the star's total velocity, through space, is the vector sum of its radial and transverse velocities. The relationship between the star's total velocity, v, and its radial and transverse velocities v_{R} and v_{T}, is illustrated in the following diagram:
Here are some symbols widely used in this web site.
Symbol  Meaning 

Equatorial Coordinates 

Right ascension  
Declination  
d  Distance to star 
General Spherical Coordinates 

Azimuth (spherical coords)  
Altitude (spherical coords)  
r  Distance to star 
Angular Velocities 

_{}  Component of proper motion in right ascension 
_{}  Component of proper motion in declination 
Linear Velocities 

v_{R}  Radial velocity (negative = approaching) 
v_{TA}  Transverse velocity, component in right ascension 
v_{TD}  Transverse velocity, component in declination 
v_{x},v_{y}v_{z}  Cartesian velocity vectors 
Other Quantities 

t  Time (usually in years) 
Parallax  
V  Apparent visual magnitude 
M_{V}  Absolute visual magnitude 
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