From Wikipedia, the free encyclopedia
|30.857×1012 km||30.857×1015 m|
|206.26×103 AU||3.26156 ly|
|US customary / Imperial units|
|19.174×1012 mi||101.24×1015 ft|
The name parsec is "an abbreviated form of 'a distance corresponding to a parallax of one arcsecond'." It was coined in 1913 at the suggestion of British astronomer Herbert Hall Turner. A parsec is the distance from the Sun to an astronomical object which has a parallax angle of one arcsecond (1⁄3,600 of a degree). In other words, imagine that a straight line is drawn from the object to the Earth, a second line is drawn from the Earth to the Sun, and a third line is drawn from the object to the Sun that is perpendicular to the line drawn from the Earth to the Sun. Now, if the angle formed between the line drawn from the object to the Earth and the line drawn from the object to the Sun is exactly one arcsecond, then the object's distance from the Sun would be exactly one parsec.
The angle can be measured by observing the object's precise location in the sky. It becomes quite convenient for astronomers to determine the object's distance by simply measuring its apparent motion in the sky over a 6-month interval. After six months, the Earth is at the opposite end of its orbit around the Sun, a distance equal to twice the base of the right triangle described above. In this case, the object's distance in parsecs is numerically (though not dimensionally) equal to the reciprocal of half the number of arcseconds by which its position appears to change ( ). The less an object appears to have moved, the farther it is from the Sun, and vice versa.
Equivalencies in other units 
1 parsec ≡ 648000 / π astronomical units
History and derivation 
The parsec is equal to the length of the adjacent side of an imaginary right triangle in space. The two dimensions on which this triangle is based are the angle (which is defined as 1 arcsecond), and the opposite side (which is defined as 1 astronomical unit, which is the distance from the Earth to the Sun). Using these two measurements, along with the rules of trigonometry, the length of the adjacent side (the parsec) can be found.
One of the oldest methods for astronomers to calculate the distance to a star was to record the difference in angle between two measurements of the position of the star in the sky. The first measurement was taken from the Earth on one side of the Sun, and the second was taken half a year later when the Earth was on the opposite side of the Sun. The distance between the two positions of the Earth for the measurements was known to be twice the distance between the Earth and the Sun. The difference in angle between the two measurements was known to be twice the parallax angle, which is formed by lines from the Sun and Earth to the star at the vertex. Then the distance to the star could be calculated using trigonometry. The first successful direct measurements of an object at interstellar distances were undertaken by German astronomer Friedrich Wilhelm Bessel in 1838, who used this approach to calculate the three and a half parsec distance of 61 Cygni.
The parallax of a star is taken to be half of the angular distance that a star appears to move relative to the celestial sphere as Earth orbits the Sun. Equivalently, it is the subtended angle, from that star's perspective, of the semi-major axis of Earth's orbit. The star, the sun and the earth form the corners of an imaginary right triangle in space: the right angle is the corner at the sun, and the corner at the star is the parallax angle. The length of the opposite side to the parallax angle is the distance from the Earth to the Sun (defined as 1 astronomical unit (AU)), and the length of the adjacent side gives the distance from the sun to the star. Therefore, given a measurement of the parallax angle, along with the rules of trigonometry, the distance from the sun to the star can be found. A parsec is defined as the length of the adjacent side of this right triangle in space when the parallax angle is 1 arcsecond.
The use of the parsec as a unit of distance follows naturally from Bessel's method, since distance in parsecs can be computed simply as the reciprocal of the parallax angle in arcseconds (i.e. if the parallax angle is 1 arcsecond, the object is 1 pc distant from the sun; If the parallax angle is 0.5 arcsecond, the object is 2 pc distant; etc.). No trigonometric functions are required in this relationship because the very small angles involved mean that the approximate solution of the skinny triangle can be applied.
Though it may have been used before, the term parsec was first mentioned in an astronomical publication in 1913. Astronomer Royal Frank Watson Dyson expressed his concern for the need of a name for that unit of distance. He proposed the name astron, but mentioned that Carl Charlier had suggested siriometer and Herbert Hall Turner had proposed parsec. It was Turner's proposal that stuck.
Calculating the value of a parsec 
In the diagram above (not to scale), S represents the Sun, and E the Earth at one point in its orbit. Thus the distance ES is one astronomical unit (AU). The angle SDE is one arcsecond (1/3600 of a degree) so by definition D is a point in space at a distance of one parsec from the Sun. By trigonometry, the distance SD is
Using the small-angle approximation, by which the sine (and, hence, the tangent) of an extremely small angle is essentially equal to the angle itself (in radians),
One AU ≈ 149597870700 metres, so 1 parsec ≈ 3.085678×1016 m ≈ 3.261564 ly.
A corollary is that 1 parsec is also the distance from which a disc with a diameter of 1 AU must be viewed for it to have an angular diameter of 1 arcsecond (by placing the observer at D and a diameter of the disc on ES).
Usage and measurement 
The parallax method is the fundamental calibration step for distance determination in astrophysics; however, the accuracy of ground-based telescope measurements of parallax angle is limited to about 0.01 arcseconds, and thus to stars no more than 100 pc distant. This is because the Earth’s atmosphere limits the sharpness of a star's image. Space-based telescopes are not limited by this effect and can accurately measure distances to objects beyond the limit of ground-based observations. Between 1989 and 1993, the Hipparcos satellite, launched by the European Space Agency (ESA), measured parallaxes for about 100,000 stars with an astrometric precision of about 0.97 milliarcseconds, and obtained accurate measurements for stellar distances of stars up to 1,000 pc away. NASA's FAME satellite was to have been launched in 2004, to measure parallaxes for about 40 million stars with sufficient precision to measure stellar distances of up to 2,000 pc. However, the mission's funding was withdrawn by NASA in January 2002. ESA's Gaia satellite, which was due to be launched in late 2012, but has been pushed to August 2013, is intended to measure one billion stellar distances to within 20 microarcseconds, producing errors of 10% in measurements as far as the Galactic Center, about 8,000 pc away in the constellation of Sagittarius.
Distances in parsecs 
Distances less than a parsec 
Distances measured in fractions of a parsec usually involve objects within a single star system. So, for example:
- One astronomical unit (AU), the distance from the Sun to the Earth, is just under 0.000005 parsecs (150,000,000 km; 96,000,000 mi).
- The most distant space probe, Voyager 1, was 0.0006 parsecs (0.002 ly) from Earth as of May 2013[update]. It took Voyager 35 years to cover that distance.
- The Oort cloud is estimated to be approximately 0.6 parsecs (2.0 ly) in diameter
Parsecs and kiloparsecs 
Distances measured in parsecs (pc) include distances between nearby stars, such as those in the same spiral arm or globular cluster. A distance of 1,000 parsecs (3,300 ly) is commonly denoted by the kiloparsec (kpc). Astronomers typically use kiloparsecs to measure distances between parts of a galaxy, or within groups of galaxies. So, for example:
- One parsec is approximately 3.26 lightyears.
- The nearest known star to the Earth, other than the Sun, Proxima Centauri, is 1.3 parsecs (4.24 ly) away.
- The distance to the open cluster Pleiades is 130 ± 10 pc (420 ± 33 ly).
- The center of the Milky Way is more than 8 kiloparsecs (26,000 ly) from the Earth, and the Milky Way is roughly 34 kpc (110,000 ly) across.
- The Andromeda Galaxy (M31) is ~780 kpc (2,500,000 ly) away from the Earth.
Megaparsecs and gigaparsecs 
A distance of one million parsecs (3.3 million light-years or 3.3 Mly) is commonly denoted by the megaparsec (Mpc). Astronomers typically measure the distances between neighbouring galaxies and galaxy clusters in megaparsecs.
Galactic distances are sometimes given in units of Mpc/h (as in "50/h Mpc"). h is a parameter in the range [0.5,0.75] reflecting the uncertainty in the value of the Hubble constant H for the rate of expansion of the universe: h = H / (100 km/s/Mpc). The Hubble constant becomes relevant when converting an observed redshift z into a distance d using the formula d ≈ (c / H) × z.
One gigaparsec (Gpc) is one billion parsecs — one of the largest distance measures commonly used. One gigaparsec is about 3.3 billion light-years (3.3 Gly), or roughly one fourteenth of the distance to the horizon of the observable universe (dictated by the cosmic background radiation). Astronomers typically use gigaparsecs to measure large-scale structures such as the size of, and distance to, the CfA2 Great Wall; the distances between galaxy clusters; and the distance to quasars.
- The Andromeda Galaxy is about 0.78 Mpc (2.5 Mly) from the Earth.
- The nearest large galaxy cluster, the Virgo Cluster, is about 16.5 Mpc (54 Mly) from the Earth.
- The galaxy RXJ1242-11, observed to have a supermassive black hole core similar to the Milky Way's, is about 200 Mpc (650 Mly) from the Earth.
- The particle horizon (the boundary of the observable universe) has a radius of about 14.0 Gpc (46 Gly).
Volume units 
To determine the number of stars in the Milky Way Galaxy, volumes in cubic kiloparsecs[a] (kpc3) are selected in various directions. All the stars in these volumes are counted and the total number of stars statistically determined. The number of globular clusters, dust clouds and interstellar gas is determined in a similar fashion. To determine the number of galaxies in superclusters, volumes in cubic megaparsecs[a] (Mpc3) are selected. All the galaxies in these volumes are classified and tallied. The total number of galaxies can then be determined statistically. The huge void in Boötes is measured in cubic megaparsecs. In cosmology, volumes of cubic gigaparsecs[a] (Gpc3) are selected to determine the distribution of matter in the visible universe and to determine the number of galaxies and quasars. The Sun is alone in its cubic parsec,[a] (pc3) but in globular clusters the stellar density per cubic parsec could be from 100 to 1,000.
See also 
1 pc3 ≈ 2.938×1049 m3 1 kpc3 ≈ 2.938×1058 m3 1 Mpc3 ≈ 2.938×1067 m3 1 Gpc3 ≈ 2.938×1076 m3
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