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'{{other uses}} In [[astronomy]], '''declination''' (abbreviated '''dec'''; symbol '''''δ''''') is one of the two angles that locate a point on the [[celestial sphere]] in the [[equatorial coordinate system]], the other being [[hour angle]]. Declination's angle is measured north or south of the [[celestial equator]], along FUCK SCIENCE the [[hour circle]] passing through the point in question.<ref> {{cite book | last1 = U.S. Naval Observatory | first1=Nautical Almanac Office | editor = P. Kenneth Seidelmann | title = Explanatory Supplement to the Astronomical Almanac | publisher = University Science Books, Mill Valley, CA | year = 1992 | isbn = 0-935702-68-7 |page=724}} </ref> [[File:Ra and dec demo animation small.gif|right|thumb|350px| [[Right ascension]] and '''declination''' as seen on the inside of the [[celestial sphere]]. The primary direction of the system is the [[equinox|vernal equinox]], the ascending node of the [[ecliptic]] (red) on the [[celestial equator]] (blue). Declination is measured northward or southward from the [[celestial equator]], along the [[hour circle]] passing through the point in question.]] The root of word the ''declination'' (Latin, ''declinatio'') means "a bending away" or "a bending down". It comes from the same root as the words ''incline'' ("bend toward") and ''recline'' ("bend backward").<ref> {{cite book |url=http://books.google.com/?id=a6MRAAAAIAAJ |title=A Complete and Universal English Dictionary |first=James |last=Barclay |year=1799 }}, entries for ''declination'', ''inclination'', ''incline'', ''recline'', at [http://books.google.com/books Google books] </ref> ==Explanation== {{main|Equatorial coordinate system}} Declination in astronomy is comparable to geographic [[latitude]], projected onto the [[celestial sphere]], and hour angle is likewise comparable to longitude.<ref> {{cite book |url=http://books.google.com/?id=PJoUAQAAMAAJ |title=An Introduction to Astronomy |last=Moulton |first=Forest Ray |year=1918 |publisher=Macmillan Co., New York |page=125, art. 66}} , at [http://books.google.com/books Google books] </ref> Points north of the [[celestial equator]] have positive declinations, while those south have negative declinations. Any units of angular measure can be used for declination, but it is customarily measured in the [[Degree (angle)|degrees]] ( ° ), [[Minute of arc|minutes]] ( ' ), and [[Minute of arc|seconds]] ( " ) of [[sexagesimal|sexagesimal measure]], with 90° equivalent to {{frac|1|4}} circle. Declinations with magnitudes greater than 90° do not occur, because the poles are the northernmost and southernmost points of the celestial sphere. An object at the * [[celestial equator]] has a declination of 0° * [[Celestial pole|north celestial pole]] has a declination of +90° * [[Celestial pole|south celestial pole]] has a declination of −90° The sign is customarily included whether positive or negative. == Effects of precession == [[File:Ra and dec on celestial sphere.png|thumb|300px|[[Right ascension]] (blue) and '''declination''' (green) as seen from outside the [[celestial sphere]].]] {{main|Axial precession}} The Earth's axis rotates slowly westward about the poles of the ecliptic, completing one circuit in about 26,000 years. This effect, known as [[Axial precession|precession]], causes the coordinates of stationary celestial objects to change continuously, if rather slowly. Therefore, [[Equatorial coordinate system|equatorial coordinates]] (including declination) are inherently relative to the year of their observation, and astronomers specify them with reference to a particular year, known as an [[Epoch (astronomy)|epoch]]. Coordinates from different epochs must be mathematically rotated to match each other, or to match a standard epoch.<ref> Moulton (1918), pp. 92–95.</ref> The currently used standard epoch is [[J2000.0]], which is January 1, 2000 at 12:00 [[Terrestrial Time|TT]]. The prefix "J" indicates that it is a [[Julian epoch]]. Prior to J2000.0, astronomers used the successive [[Epoch (astronomy)#Besselian epoch|Besselian Epochs]] B1875.0, B1900.0, and B1950.0.<ref> see, for instance, {{cite book | author = U.S. Naval Observatory Nautical Almanac Office | first =Nautical Almanac Office | coauthors = U.K. Hydrographic Office, H.M. Nautical Almanac Office | title = The Astronomical Almanac for the Year 2010 | publisher = U.S. Govt. Printing Office | year = 2008 |page=B2, |chapter=Time Scales and Coordinate Systems, 2010 | isbn = }}</ref> ==Stars== A [[star]]'s direction remains nearly fixed due to its vast distance, but its [[right ascension]] and declination do change gradually due to [[precession of the equinoxes]] and [[proper motion]], and cyclically due to [[Stellar parallax|annual parallax]]. The declinations of [[Solar System]] objects change very rapidly compared to those of stars, due to [[orbit|orbital motion]] and close proximity. As seen from locations in the Earth's [[Northern Hemisphere]], celestial objects with declinations greater than 90°&nbsp;−&nbsp;{{math|''φ''}} (where {{math|''φ''}} = observer's [[latitude]]) appear to circle daily around the [[celestial pole]] without dipping below the [[horizon]], and are therefore called [[circumpolar star]]s. This similarly occurs in the [[Southern Hemisphere]] for objects with declinations less (i.e. more negative) than −90°&nbsp;−&nbsp;{{math|''φ''}} (where {{math|''φ''}} is always a [[negative number]] for southern latitudes). An extreme example is the [[pole star]] which has a declination near to +90°, so is circumpolar as seen from anywhere in the Northern Hemisphere except very close to the equator. Circumpolar stars never dip below the horizon. Conversely, there are other stars that never rise above the horizon, as seen from any given point on the Earth's surface (except exactly on the [[equator]]). Generally, if a star whose declination is {{math|''δ''}} is circumpolar for some observer (where {{math|''δ''}} is either positive or negative), then a star whose declination is −{{math|''δ''}} never rises above the horizon, as seen by the same observer. (This neglects the effect of [[atmospheric refraction]].) Likewise, if a star is circumpolar for an observer at latitude {{math|''φ''}}, then it never rises above the horizon as seen by an observer at latitude −{{math|''φ''}}. Neglecting atmospheric refraction, declination is always 0° at east and west points of the [[horizon]]. At the north point, it is 90°&nbsp;−&nbsp;|{{math|''φ''}}|, and at the south point, −90° + |{{math|''φ''}}|. From the [[Geographical pole|poles]], declination is uniform around the entire horizon, approximately 0°. {|class="wikitable" |+ '''[[Star]]s visible by [[latitude]]''' | rowspan="3" style="background:#89cff0; text-align:center;" |'''Observer's [[latitude]] (°)''' | colspan="3" style="background:#f4c2c2; text-align:center;"| '''Declination''' |- align = "center" | style="background:#f4c2c2;" |'''of [[circumpolar star]]s (°)''' | style="background:#f4c2c2;" |'''of non-circumpolar stars (°)''' | style="background:#f4c2c2;" |'''of stars not visible (°)''' |- | style="background:#f4c2c2;" | + for north latitude, − for south | style="background:#f4c2c2;" | &nbsp; | style="background:#f4c2c2;" | − for north latitude, + for south |- style="text-align:center;" | 90 ([[Geographical pole|Pole]]) | 90 to 0 || <center>N/A</center> || 0 to 90 |- style="text-align:center;" | 66.5 ([[arctic circle|Arctic]]/[[antarctic circle|Antarctic]] Circle) | 90 to 23.5 || +23.5 to −23.5 || 23.5 to 90 |- style="text-align:center;" | 45 ([[45th parallel north|midpoint]]) | 90 to 45 || +45 to −45 || 45 to 90 |- style="text-align:center;" | 23.5 (Tropic of [[Tropic of Cancer|Cancer]]/[[Tropic of Capricorn|Capricorn]]) | 90 to 66.5 || +66.5 to −66.5 || 66.5 to 90 |- style="text-align:center;" | 0 ([[Equator]]) | <center>N/A</center> || +90 to −90 || <center>N/A</center> |- |} Non-circumpolar stars are visible only during certain days or [[season]]s of the year. [[File:Stars and dec.png|thumb|600px|center|The night sky, divided into two halves. '''Declination''' (green) begins at the [[celestial equator|equator]] (green) and is positive northward (towards the top), negative southward (towards the bottom). The lines of declination (green) divide the sky into [[small circle]]s, here 15° apart.]] ==Sun== {{main|Position of the Sun}} The Sun's declination varies with the [[season]]s. As seen from [[arctic]] or [[antarctic]] latitudes, the Sun is circumpolar near the local [[summer solstice]], leading to the phenomenon of it being above the [[horizon]] at [[midnight]], which is called [[midnight sun]]. Likewise, near the local winter solstice, the Sun remains below the horizon all day, which is called [[polar night]]. ==Relation to latitude== When an object is directly overhead its declination is almost always within 0.01 degree of the observer's latitude; it would be exactly equal except for two complications.{{citation needed|date=August 2012}} The first complication applies to all celestial objects: the object's declination equals the observer's astronomic latitude, but the term "latitude" ordinarily means geodetic latitude, which is the latitude on maps and GPS devices. In the continental United States and surrounding area the difference (the [[vertical deflection]]) is typically a few arcseconds (1 arcsecond = 1/3600 degree) but can be as great as 41 arcseconds.<ref>{{cite web |url = http://www.ngs.noaa.gov/GEOID/USDOV2009/ |title = USDOV2009 |year = 2011 |publisher = [[U.S. National Geodetic Survey]] |location = Silver Spring, Maryland }}</ref> The second complication is that assuming no deflection of the vertical, "overhead" means perpendicular to the ellipsoid at observer's location, but the perpendicular line does not pass through the center of the earth; almanacs give declinations measured at the center of the Earth. (An ellipsoid is an approximation to sea level that is mathematically manageable).<ref>{{cite book |editor = P. Kenneth Seidelmann |title = Explanatory Supplement to the Astronomical Almanac |publisher = University Science Books |location = Sausalito, CA |year = 1992 |pages = 200–5}}</ref> For the moon this discrepancy can reach 0.003 degree; the Sun and planets are hundreds of times more distant and for them the discrepancy is proportionately smaller (and for the stars is unmeasurable). ==See also== {{Div col|cols=3}} * [[Celestial coordinate system]] * [[Ecliptic]] * [[Equatorial coordinate system]] * [[Geographic coordinates]] * [[Lunar standstill]] * [[Right ascension]] * [[Setting circles]] * [[Position of the Sun]] {{Div col end}} ==Notes and references== {{reflist}} == External links == * [http://stars.astro.illinois.edu/celsph.html MEASURING THE SKY A Quick Guide to the Celestial Sphere] James B. Kaler, University of Illinois * [http://astro.unl.edu/naap/motion1/cec_units.html Celestial Equatorial Coordinate System] University of Nebraska-Lincoln * [http://astro.unl.edu/naap/motion1/cec_both.html Celestial Equatorial Coordinate Explorers] University of Nebraska-Lincoln * {{cite web|last=Merrifield|first=Michael|title=(α,δ) – Right Ascension & Declination|url=http://www.sixtysymbols.com/videos/declination.htm|work=Sixty Symbols|publisher=[[Brady Haran]] for the [[University of Nottingham]]}} [[Category:Celestial coordinate system]] [[Category:Angle]] [[Category:Technical factors of astrology]]'