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The Aberdare constituency came into being at the 1918 election. The first representative was Charles Butt Stanton, who had been elected at a by-election following Hardie's death in 1915. However, in 1922, Stanton was defeated by a Labour candidate, and Labour has held the seat ever since. The only significant challenge came from Plaid Cymru at the 1970 and February 1974 General Elections, but these performances have not since been repeated. From 1984 until 2019 the parliamentary seat, now known as Cynon Valley, was held by Ann Clwyd of Labour.
Local government.
Aberdare was an ancient parish within Glamorgan. Until the mid-19th century the local government of Aberdare and its locality remained in the hands of traditional structures such as the parish vestry and the High Constable, who was chosen annually. However, with the rapid industrial development of the parish, these traditional bodies could not cope with the realities of an urbanised, industrial community which had developed without any planning or facilities. During the early decades of the 19th century the ironmasters gradually imposed their influence over local affairs, and this remained the case following the formation of the Merthyr Board of Guardians in 1836. During the 1850s and early 1860s, however, as coal displaced iron as the main industry in the valley, the ironmasters were displaced as the dominant group in local government and administration by an alliance between mostly indigenous coal owners, shopkeepers and tradesmen, professional men and dissenting ministers. A central figure in this development was the Rev Thomas Price. The growth of this alliance was rooted in the reaction to the 1847 Education Reports and the subsequent efforts to establish a British School at Aberdare.
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In the 1840s there were no adequate sanitary facilities or water supply, and mortality rates were high. Outbreaks of cholera and typhus were commonplace. Against this background, Thomas Webster Rammell prepared a report for the General Board of Health on the sanitary condition of the parish, which recommended that a local board of health be established. The whole parish of Aberdare was formally declared a local board district on 31 July 1854, to be governed by the Aberdare Local Board of Health. Its first chairman was Richard Fothergill and the members included David Davis, Blaengwawr, David Williams ("Alaw Goch"), Rees Hopkin Rhys and the Rev. Thomas Price. It was followed by the Aberdare School Board in 1871. The Old Town Hall was erected in 1831 although it was not converted for municipal use until the second half of the century.
By 1889, the Local Board of Health had initiated a number of developments: these included the purchase of local reservoirs from the Aberdare Waterworks Company for £97,000, a sewerage scheme costing £35,000, as well as the opening of Aberdare Public Park and a local fever hospital. The lack of a Free Library, however, remained a concern.
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Later, the formation of the Glamorgan County Council (upon which Aberdare had five elected members) in 1889, followed by the Aberdare Urban District Council, which replaced the Local Board in 1894, transformed the local politics of the Aberdare valley.
At the 1889 Glamorgan County Council Elections most of the elected representatives were coalowners and industrialists, and the only exception in the earlier period was the miners' agent David Morgan (Dai o'r Nant), elected in 1892 as a labour representative. From the early 1900s, however, Labour candidates began to gain ground and dominated local government from the 1920s onwards. The same pattern was seen on the Aberdare UDC.
Aberdare Urban District was abolished in 1974 under the Local Government Act 1972. The area became part of the borough of Cynon Valley within the new county of Mid Glamorgan. The area of the former urban district was made a community, later being subdivided in 1982 into five communities: Aberaman, Cwmbach, Llwydcoed, Penywaun, and a smaller Aberdare community. The Aberdare community was further divided in 2017 into two communities called Aberdare East and Aberdare West. Aberdare East includes Aberdare town centre and the village of Abernant. Aberdare West includes Cwmdare, Cwm Sian and Trecynon. No community council exists for either of the Aberdare communities.
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Cynon Valley Borough Council and Mid Glamorgan County Council were both abolished in 1996, since when Aberdare has been governed by Rhondda Cynon Taf County Borough Council. The town lies mainly in the Aberdare East ward, represented by two county councillors. Nearby Cwmdare, Llwydcoed and Trecynon are represented by the Aberdare West/Llwydcoed ward. Both wards have been represented by the Labour Party since 2012.
Culture.
Aberdare, during its boom years, was considered a centre of Welsh culture: it hosted the first National Eisteddfod in 1861, with which David Williams (Alaw Goch) was closely associated. The town erected a monument in the local park to commemorate the occasion. A number of local eisteddfodau had long been held in the locality, associated with figures such as William Williams (Carw Coch) The Eisteddfod was again held in Aberdare in 1885, and also in 1956 at Aberdare Park, where the Gorsedd standing stones still exist. At the last National Eisteddfod held in Aberdare in 1956 Mathonwy Hughes won the chair. From the mid 19th century, Aberdare was an important publishing centre where a large number of books and journals were produced, the majority of which were in the Welsh language. A newspaper entitled Y Gwladgarwr (the Patriot) was published at Aberdare from 1856 until 1882 and was circulated widely throughout the South Wales valleys. From 1875 a more successful newspaper, Tarian y Gweithiwr (the Workman's Shield) was published at Aberdare by John Mills. "Y Darian", as it was known, strongly supported the trade union movements among the miners and ironworkers of the valleys. The miners' leader, William Abraham, derived support from the newspaper, which was also aligned with radical nonconformist liberalism. The rise of the political labour movement and the subsequent decline of the Welsh language in the valleys, ultimately led to its decline and closure in 1934.
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The Coliseum Theatre is Aberdare's main arts venue, containing a 600-seat auditorium and cinema. It is situated in nearby Trecynon and was built in 1938 using miners' subscriptions.
The Second World War poet Alun Lewis was born near Aberdare in the village of Cwmaman; there is a plaque commemorating him, including a quotation from his poem "The Mountain over Aberdare".
The founding members of the rock band Stereophonics originated from Cwmaman. It is also the hometown of guitarist Mark Parry of Vancouver rock band The Manvils. Famed anarchist-punk band Crass played their last live show for striking miners in Aberdare during the UK miners' strike.
Griffith Rhys Jones − or Caradog as he was commonly known − was the conductor of the famous 'Côr Mawr' ("great choir") of some 460 voices (the South Wales Choral Union), which twice won first prize at Crystal Palace choral competitions in London in the 1870s. He is depicted in the town's most prominent statue by sculptor Goscombe John, unveiled on Victoria Square in 1920.
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Aberdare was culturally twinned with the German town of Ravensburg.
Religion.
Anglican Church.
The original parish church of St John the Baptist was originally built in 1189. Some of its original architecture is still intact.
With the development of Aberdare as an industrial centre in the nineteenth century it became increasingly apparent that the ancient church was far too small to service the perceived spiritual needs of an urban community, particularly in view of the rapid growth of nonconformity from the 1830s onwards. Eventually, John Griffith, the rector of Aberdare, undertook to raise funds to build a new church, leading to the rapid construction of St Elvan's Church in the town centre between 1851 and 1852. This Church in Wales church still stands the heart of the parish of Aberdare and has had extensive work since it was built. The church has a modern electrical, two-manual and pedal board pipe organ, that is still used in services.
John Griffith, vicar of Aberdare, who built St Elvan's, transformed the role of the Anglican church in the valley by building a number of other churches, including St Fagan's, Trecynon. Other churches in the parish are St Luke's (Cwmdare), St James's (Llwydcoed) and St Matthew's (1891) (Abernant).
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In the parish of Aberaman and Cwmaman is St Margaret's Church, with a beautiful old pipe organ with two manuals and a pedal board. Also in this parish is St Joseph's Church, Cwmaman. St Joseph's has recently undergone much recreational work, almost converting the church into a community centre, surrounded by a beautiful floral garden and leading to the Cwmaman Sculpture Trail. However, regular church services still take place. Here, there is a two-manual and pedal board electric organ, with speakers at the front and sides of the church.
In 1910 there were 34 Anglican churches in the Urban District of Aberdare. A survey of the attendance at places of worship on a particular Sunday in that year recorded that 17.8% of worshippers attended church services, with the remainder attending nonconformist chapels.
Nonconformity.
The Aberdare Valley was a stronghold of Nonconformity from the mid-nineteenth century until the inter-war years. In the aftermath of the 1847 Education Reports nonconformists became increasingly active in the political and educational life of Wales and in few places was this as prevalent as at Aberdare. The leading figure was Thomas Price, minister of Calfaria, Aberdare.
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Aberdare was a major centre of the 1904–05 Religious Revival, which had begun at Loughor near Swansea. The revival aroused alarm among ministers for the revolutionary, even anarchistic, impact it had upon chapel congregations and denominational organisation. In particular, it was seen as drawing attention away from pulpit preaching and the role of the minister. The local newspaper, the "Aberdare Leader", regarded the revival with suspicion from the outset, objecting to the 'abnormal heat' which it engendered. Trecynon was particularly affected by the revival, and the meetings held there were said to have aroused more emotion and excitement than the more restrained meetings in Aberdare itself. The impact of the revival was significant in the short term, but in the longer term was fairly transient.
Once the immediate impact of the revival had faded, it was clear from the early 20th century that there was a gradual decline in the influence of the chapels. This can be explained by several factors, including the rise of socialism and the process of linguistic change which saw the younger generation increasingly turn to the English language. There were also theological controversies such as that over the New Theology propounded by R.J. Campbell.
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Of the many chapels, few are still used for their original purpose and a number have closed since the turn of the millennium. Many have been converted for housing or other purposes (including one at Robertstown which has become a mosque), and others demolished. Among the notable chapels were Calfaria, Aberdare and Seion, Cwmaman (Baptist); Saron, Aberaman and Siloa, Aberdare (Independent); and Bethania, Aberdare (Calvinistic Methodist).
Independents.
The earliest Welsh Independent, or Congregationalist chapel in the Aberdare area was Ebenezer, Trecynon, although meetings had been held from the late 18th century in dwelling houses in the locality, for example at Hirwaun. During the 19th century, the Independents showed the biggest increases in terms of places of worship: from two in 1837 to twenty-five (four of them being English causes), in 1897. By 1910 there were 35 Independent chapels, with a total membership of 8,612. Siloa Chapel was the largest of the Independent chapels in Aberdare and is one of the few that remain open today, having been 're-established' as a Welsh language chapel. The Independent ministers of nineteenth-century Aberdare included some powerful personalities, but none had the kind of wider social authority which Thomas Price enjoyed amongst the Baptists.
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Of the other Independent chapels in the valley, Saron, in Davis Street, Aberaman, was used for regular services by a small group of members until 2011. For many years, these were held in a small side-room, and not the chapel itself. The chapel has a large vestry comprising rows of two-way-facing wooden benches and a stage, with a side entrance onto Beddoe Street and back entrance to Lewis Street. Although the building is not in good repair, the interior, including pulpit and balcony seating area (back and sides), was in good order but the chapel eventually closed due to the very small number of members remaining. In February 1999, Saron became a Grade II Listed Building.
Baptists.
The Baptists were the most influential of the nonconformist denominations in Aberdare and their development was led by the Rev. Thomas Price who came to Aberdare in the early 1840s as minister of Calfaria Chapel. In 1837 the Baptists had three chapels, but in 1897 there were twenty, seventeen of them being Welsh. By 1910 the number of chapels had increased to 30, with a total membership of 7,422. Most of these Baptist chapels were established under the influence of Thomas Price who encouraged members to establish branch chapels to attract migrants who flocked to the town and locality from rural Wales. The chapels came together for regular gatherings, including baptismal services which were held in the River Cynon As a result, Price exerted an influence in the religious life of the locality which was far greater than that of any other minister.
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Calvinistic Methodists.
By 1910 there were 24 Calvinistic Methodist chapels in the Aberdare Urban District with a total membership of 4,879. The most prominent of these was Bethania, Aberdare, once the largest chapel in Aberdare. Derelict for many years, it was demolished in 2015. The Methodists were numerically powerful and while some of their ministers such as William James of Bethania served on the Aberdare School Board and other public bodies, their constitution militated against the sort of active political action which came more naturally to the Baptists and Independents.
Other denominations.
In 1878 Mother Shepherd, a native Welsh speaker, was sent to Aberdare by the Salvation Army at the start of a period of growth for their mission. After five years she had created seven new stations before she was recalled to London. Shepherd would return to Aberdare working for the community. In 1930 she was given a public funeral.
The Wesleyan Methodists had 14 places of worship by 1910. There was also a significant Unitarian tradition in the valley and three places of worship by 1910. Highland Place Unitarian Church celebrated its 150th anniversary in 2010, with a number of lectures on its history and the history of Unitarianism in Wales taking place there. The church has a two-manual pipe organ with pedal board that is used to accompany all services. The current organist is Grace Jones, the sister of the former organist Jacob Jones. The connected schoolroom is used for post-service meetings and socialising.
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Judaism.
Seymour Street was once home to a synagogue which opened its doors in the late 1800s but closed in 1957. The site now has a blue plaque.
Education.
The state of education in the parish was a cause for concern during the early industrial period, as is illustrated by the reaction to the 1847 Education Reports. Initially, there was an outcry, led by the Rev Thomas Price against the comments made by the vicar of Aberdare in his submission to the commissioners. However, on closer reflection, the reports related the deficiencies of educational provision, not only in Aberdare itself but also in the communities of the valleys generally. In so doing they not only criticised the ironmasters for their failure to provide schools for workers' children but also the nonconformists for not establishing British Schools. At the ten schools in Aberdare there was accommodation for only 1,317 children, a small proportion of the population. Largely as a result of these criticisms, the main nonconformist denominations worked together to establish a British School, known locally as Ysgol y Comin, which was opened in 1848, accommodating 200 pupils. Funds were raised which largely cleared the debts and the opening of the school was marked by a public meeting addressed by Price and David Williams ("Alaw Goch").
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Much energy was expended during this period on conflicts between Anglicans and nonconformists over education. The establishment of the Aberdare School Board in 1871 brought about an extension of educational provision but also intensified religious rivalries. School Board elections were invariably fought on religious grounds. Despite these tensions the Board took over a number of existing schools and established new ones. By 1889, fourteen schools were operated by the Board but truancy and lack of attendance remained a problem, as in many industrial districts.
In common with other public bodies at the time (see 'Local Government' above), membership of the School Board was dominated by coal owners and colliery officials, nonconformist ministers, professional men and tradesmen. Only occasionally was an Anglican clergyman elected and, with the exception of David Morgan ("Dai o'r Nant"), no working class candidates were elected for more than one term.
Transport.
The town is served by Aberdare railway station and Aberdare bus station, opposite each other in the town centre. The town has also been subject to an extensive redevelopment scheme during 2012–13.
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Sports.
Aberdare was noted as "very remarkable" for its traditions of "Taplasau Hâf" (summer games/dances), races and "gwrolgampau" ("manly sports") which were said to have been a feature of the area since at least the 1640s. The town is also home to "Yr Ynys", an historic sports ground which has the distinction of hosting the first Rugby League international, a professional Rugby League team, a football League side and an All Blacks' tour match. Today the Ynys hosts the town's Rugby union and cricket teams, as well as the Sobell Leisure Centre and the Ron Jones Athletics Stadium, a 263-seat stadium with crumb rubber track and field sports facilities, home to Aberdare Valley AAC.
Cricket.
A cricket club was re-established at the Ynys in 1968 and was named Riverside Cricket Club in reference to its location near the banks of the river. The club would later be renamed Dare Valley CC, before finally changing its name to Aberdare CC. In 2008 the club was granted a 25-year lease on the land outside the boundary of the Ynys' pitch 1, where a club house and training nets were soon constructed. This was followed by the building of a Community Hub and Café in the 2010s. Today, the club runs 3 adult teams and 4 junior sides.
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Rugby League.
The Northern Union hired the Ynys on 1 January 1908 to host what would be the first ever international rugby league match. Played on a near frozen pitch, the match between Wales and the New Zealand All Golds proved to be a close and exciting game. The decisive score came from local star and former Aberdare RFC player, Dai "Tarw" Jones, who scored a try just minutes before the final whistle, giving Wales a 9–8 victory.
The match attracted 15,000 paying spectators, with the gate receipts of £560 highlighting the commercial potential of rugby league at the Ynys. This took place at a time when the Northern Union was looking to establish professional teams across south Wales and just months after the Welsh Rugby Union had sanctioned Aberdare RFC for professionalism (banning Jones for life). As such, discussions on the establishment of a Rugby League club in Aberdare advanced quickly and on 21 July 1908, Aberdare RLFC were admitted to the Northern Union's Rugby League. On 5 September 1908 the new team played their first match against Wigan in front of a crowd of 3,000 at the Ynys.
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The potential for crowd support was again demonstrated on 10 November 1908, when the Ynys hosted its second international side as 5,000 spectators watched Aberdare take on the first touring Australian team. However the Aberdare club side could not replicate the heroics of the Welsh team, losing the match 10–37. Indeed, Aberdare struggled under Northern Union rules and initially high crowd numbers deteriorated with the poor results, which saw Aberdare finishing their only season in the Rugby Football League as the bottom club. Finally on 10 July 1909, Aberdare reported 'unexpected difficulties' in its finances and resigned from the Northern Rugby League.
Rugby Union.
A rugby club representing Aberdare was recorded as early as 1876, but the modern Aberdare RFC traces its history back to a foundation of 1890. The club had great success in the early twentieth century with local star Dai 'Tarw' Jones captaining the club from 1905 to 1907. Jones gained recognition as a player in club, representative and international games. Most notably, Jones played an important part in the "Match of the century", when Wales defeated the New Zealand All Blacks. In 1907, Jones and the Aberdare club played a pivotal role in the professionalism scandal, with the Welsh Rugby Union permanently suspending the club's entire committee and a number of players (including a lifetime ban for Jones). These events would quickly lead to many of the town's players and fans switching to rugby league, with the first ever rugby league international and the founding of Aberdare RLFC in 1908.
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Despite the suspensions, rugby union continued in the town as the club (renamed Aberaman RFC) moved to Aberaman Park. The Ynys Stadium would host its first international rugby union side on 12 December 1935, when the 1935-36 All Blacks played a tour match against a Mid-Districts side. The All Blacks won the match 31–10 in front of a crowd of 6,000.
Aberaman RFC returned to the Ynys in the 1960s. In February 1971, a clubhouse was opened at the old Crown Hotel in Gloucester Street, this was followed by the construction of a grand stand at the Ynys costing £20,000. Following the advent of professionalism in rugby union, the WRU sanctions against Aberdare were no longer applicable. As such, the club took the name Aberdare RUFC once again. Aberdare is also home to Abercwmboi RFC and Hirwaun RFC.
Association Football.
The Ynys stadium was also home to Aberdare Athletic F.C., members of the Football League between 1921 and 1927. Aberdare finished bottom in their final season and folded in 1928 after failing to be re-elected to the league.
Aberaman Athletic F.C. continued to play until World War II, and was succeeded by Aberdare & Aberaman Athletic in 1945 and Aberdare Town F.C. in 1947. The club continue to play in the Welsh Football League. Today, Aberdare Town plays in the South Wales Alliance League and are based at Aberaman Park.
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Aberration
An aberration is something that deviates from the normal way.
Aberration may also refer to:
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Aberration (astronomy)
In astronomy, aberration (also referred to as astronomical aberration, stellar aberration, or velocity aberration) is a phenomenon where celestial objects exhibit an apparent motion about their true positions based on the velocity of the observer: It causes objects to appear to be displaced towards the observer's direction of motion. The change in angle is of the order of where is the speed of light and the velocity of the observer. In the case of "stellar" or "annual" aberration, the apparent position of a star to an observer on Earth varies periodically over the course of a year as the Earth's velocity changes as it revolves around the Sun, by a maximum angle of approximately 20 arcseconds in right ascension or declination.
The term "aberration" has historically been used to refer to a number of related phenomena concerning the propagation of light in moving bodies.
Aberration is distinct from parallax, which is a change in the apparent position of a relatively nearby object, as measured by a moving observer, relative to more distant objects that define a reference frame. The amount of parallax depends on the distance of the object from the observer, whereas aberration does not. Aberration is also related to light-time correction and relativistic beaming, although it is often considered separately from these effects.
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Aberration is historically significant because of its role in the development of the theories of light, electromagnetism and, ultimately, the theory of special relativity. It was first observed in the late 1600s by astronomers searching for stellar parallax in order to confirm the heliocentric model of the Solar System. However, it was not understood at the time to be a different phenomenon.
In 1727, James Bradley provided a classical explanation for it in terms of the finite speed of light relative to the motion of the Earth in its orbit around the Sun,
which he used to make one of the earliest measurements of the speed of light. However, Bradley's theory was incompatible with 19th-century theories of light, and aberration became a major motivation for the aether drag theories of Augustin Fresnel (in 1818) and G. G. Stokes (in 1845), and for Hendrik Lorentz's aether theory of electromagnetism in 1892. The aberration of light, together with Lorentz's elaboration of Maxwell's electrodynamics, the moving magnet and conductor problem, the negative aether drift experiments, as well as the Fizeau experiment, led Albert Einstein to develop the theory of special relativity in 1905, which presents a general form of the equation for aberration in terms of such theory.
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Explanation.
Aberration may be explained as the difference in angle of a beam of light in different inertial frames of reference. A common analogy is to consider the apparent direction of falling rain. If rain is falling vertically in the frame of reference of a person standing still, then to a person moving forwards the rain will appear to arrive at an angle, requiring the moving observer to tilt their umbrella forwards. The faster the observer moves, the more tilt is needed.
The net effect is that light rays striking the moving observer from the sides in a stationary frame will come angled from ahead in the moving observer's frame. This effect is sometimes called the "searchlight" or "headlight" effect.
In the case of annual aberration of starlight, the direction of incoming starlight as seen in the Earth's moving frame is tilted relative to the angle observed in the Sun's frame. Since the direction of motion of the Earth changes during its orbit, the direction of this tilting changes during the course of the year, and causes the apparent position of the star to differ from its true position as measured in the inertial frame of the Sun.
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While classical reasoning gives intuition for aberration, it leads to a number of physical paradoxes observable even at the classical level (see history). The theory of special relativity is required to correctly account for aberration. The relativistic explanation is very similar to the classical one however, and in both theories aberration may be understood as a case of addition of velocities.
Classical explanation.
In the Sun's frame, consider a beam of light with velocity equal to the speed of light formula_1, with x and y velocity components formula_2 and formula_3, and thus at an angle formula_4 such that formula_5. If the Earth is moving at velocity formula_6 in the x direction relative to the Sun, then by velocity addition the x component of the beam's velocity in the Earth's frame of reference is formula_7, and the y velocity is unchanged, formula_8. Thus the angle of the light in the Earth's frame in terms of the angle in the Sun's frame is
In the case of formula_10, this result reduces to formula_11, which in the limit formula_12 may be approximated by formula_13.
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Relativistic explanation.
The reasoning in the relativistic case is the same except that the relativistic velocity addition formulas must be used, which can be derived from Lorentz transformations between different frames of reference. These formulas are
where formula_16, giving the components of the light beam in the Earth's frame in terms of the components in the Sun's frame. The angle of the beam in the Earth's frame is thus
or
In the case of formula_10, this result reduces to formula_20, and in the limit formula_12 this may be approximated by formula_13. This relativistic derivation keeps the speed of light formula_23 constant in all frames of reference, unlike the classical derivation above.
Relationship to light-time correction and relativistic beaming.
Aberration is related to two other phenomena, light-time correction, which is due to the motion of an observed object during the time taken by its light to reach an observer, and relativistic beaming, which is an angling of the light emitted by a moving light source. It can be considered equivalent to them but in a different inertial frame of reference. In aberration, the observer is considered to be moving relative to a (for the sake of simplicity) stationary light source, while in light-time correction and relativistic beaming the light source is considered to be moving relative to a stationary observer.
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Consider the case of an observer and a light source moving relative to each other at constant velocity, with a light beam moving from the source to the observer. At the moment of emission, the beam in the observer's rest frame is tilted compared to the one in the source's rest frame, as understood through relativistic beaming. During the time it takes the light beam to reach the observer the light source moves in the observer's frame, and the 'true position' of the light source is displaced relative to the apparent position the observer sees, as explained by light-time correction. Finally, the beam in the observer's frame at the moment of observation is tilted compared to the beam in source's frame, which can be understood as an aberrational effect. Thus, a person in the light source's frame would describe the apparent tilting of the beam in terms of aberration, while a person in the observer's frame would describe it as a light-time effect.
The relationship between these phenomena is only valid if the observer and source's frames are inertial frames. In practice, because the Earth is not an inertial rest frame but experiences centripetal acceleration towards the Sun, many aberrational effects such as annual aberration on Earth cannot be considered light-time corrections. However, if the time between emission and detection of the light is short compared to the orbital period of the Earth, the Earth may be approximated as an inertial frame and aberrational effects are equivalent to light-time corrections.
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Types.
The "Astronomical Almanac" describes several different types of aberration, arising from differing components of the Earth's and observed object's motion:
Annual aberration.
Annual aberration is caused by the motion of an observer on Earth as the planet revolves around the Sun. Due to orbital eccentricity, the orbital velocity formula_6 of Earth (in the Sun's rest frame) varies periodically during the year as the planet traverses its elliptic orbit and consequently the aberration also varies periodically, typically causing stars to appear to move in small ellipses.
Approximating Earth's orbit as circular, the maximum displacement of a star due to annual aberration is known as the "constant of aberration", conventionally represented by formula_25. It may be calculated using the relation formula_26 substituting the Earth's average speed in the Sun's frame for formula_6 and the speed of light formula_1. Its accepted value is 20.49552 arcseconds (sec) or 0.000099365 radians (rad) (at J2000).
Assuming a circular orbit, annual aberration causes stars exactly on the ecliptic (the plane of Earth's orbit) to appear to move back and forth along a straight line, varying by formula_25 on either side of their position in the Sun's frame. A star that is precisely at one of the ecliptic poles (at 90° from the ecliptic plane) will appear to move in a circle of radius formula_25 about its true position, and stars at intermediate ecliptic latitudes will appear to move along a small ellipse.
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For illustration, consider a star at the northern ecliptic pole viewed by an observer at a point on the Arctic Circle. Such an observer will see the star transit at the zenith, once every day (strictly speaking sidereal day). At the time of the March equinox, Earth's orbit carries the observer in a southwards direction, and the star's apparent declination is therefore displaced to the south by an angle of formula_25. On the September equinox, the star's position is displaced to the north by an equal and opposite amount. On either solstice, the displacement in declination is 0. Conversely, the amount of displacement in right ascension is 0 on either equinox and at maximum on either solstice.
In actuality, Earth's orbit is slightly elliptic rather than circular, and its speed varies somewhat over the course of its orbit, which means the description above is only approximate. Aberration is more accurately calculated using Earth's instantaneous velocity relative to the barycenter of the Solar System.
Note that the displacement due to aberration is orthogonal to any displacement due to parallax. If parallax is detectable, the maximum displacement to the south would occur in December, and the maximum displacement to the north in June. It is this apparently anomalous motion that so mystified early astronomers.
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Solar annual aberration.
A special case of annual aberration is the nearly constant deflection of the Sun from its position in the Sun's rest frame by formula_25 towards the "west" (as viewed from Earth), opposite to the apparent motion of the Sun along the ecliptic (which is from west to east, as seen from Earth). The deflection thus makes the Sun appear to be behind (or retarded) from its rest-frame position on the ecliptic by a position or angle formula_25.
This deflection may equivalently be described as a light-time effect due to motion of the Earth during the 8.3 minutes that it takes light to travel from the Sun to Earth. The relation with formula_25 is : [0.000099365 rad / 2 π rad] x [365.25 d x 24 h/d x 60 min/h] = 8.3167 min ≈ 8 min 19 sec = 499 sec. This is possible since the transit time of sunlight is short relative to the orbital period of the Earth, so the Earth's frame may be approximated as inertial. In the Earth's frame, the Sun moves, at a mean velocity v = 29.789 km/s, by a distance formula_35 ≈ 14,864.7 km in the time it takes light to reach Earth, formula_36 ≈ 499 sec for the orbit of mean radius formula_37 = 1 AU = 149,597,870.7 km. This gives an angular correction formula_38 ≈ 0.000099364 rad = 20.49539 sec, which can be solved to give formula_39 ≈ 0.000099365 rad = 20.49559 sec, very nearly the same as the aberrational correction (here formula_25 is in radian and not in arcsecond).
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Diurnal aberration.
Diurnal aberration is caused by the velocity of the observer on the surface of the rotating Earth. It is therefore dependent not only on the time of the observation, but also the latitude and longitude of the observer. Its effect is much smaller than that of annual aberration, and is only 0.32 arcseconds in the case of an observer at the Equator, where the rotational velocity is greatest.
Secular aberration.
The secular component of aberration, caused by the motion of the Solar System in space, has been further subdivided into several components: aberration resulting from the motion of the solar system barycenter around the center of our Galaxy, aberration resulting from the motion of the Galaxy relative to the Local Group, and aberration resulting from the motion of the Local Group relative to the cosmic microwave background. Secular aberration affects the apparent positions of stars and extragalactic objects. The large, constant part of secular aberration cannot be directly observed and "It has been standard practice to absorb this large, nearly constant effect into the reported" positions of stars.
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In about 200 million years, the Sun circles the galactic center, whose measured location is near right ascension (α = 266.4°) and declination (δ = −29.0°). The constant, unobservable, effect of the solar system's motion around the galactic center has been computed variously as 150 or 165 arcseconds. The other, observable, part is an acceleration toward the galactic center of approximately 2.5 × 10−10 m/s2, which yields a change of aberration of about 5 μas/yr. Highly precise measurements extending over several years can observe this change in secular aberration, often called the secular aberration drift or the acceleration of the Solar System, as a small apparent proper motion.
Recently, highly precise astrometry of extragalactic objects using both Very Long Baseline Interferometry and the "Gaia" space observatory have successfully measured this small effect. The first VLBI measurement of the apparent motion, over a period of 20 years, of 555 extragalactic objects towards the center of our galaxy at equatorial coordinates of α = 263° and δ = −20° indicated a secular aberration drift 6.4 ±1.5 μas/yr.
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The first VLBI measurement of the apparent motion, over a period of 20 years, of 555 extragalactic objects towards the center of our galaxy at equatorial coordinates of α = 263° and δ = −20° indicated a secular aberration drift 6.4 ±1.5 μas/yr. Later determinations using a series of VLBI measurements extending over almost 40 years determined the secular aberration drift to be 5.83 ± 0.23 μas/yr in the direction α = 270.2 ± 2.3° and δ = −20.2° ± 3.6°. Optical observations using only 33 months of "Gaia" satellite data of 1.6 million extragalactic sources indicated an acceleration of the solar system of 2.32 ± 0.16 × 10−10 m/s2 and a corresponding secular aberration drift of 5.05 ± 0.35 μas/yr in the direction of α = 269.1° ± 5.4°, δ = −31.6° ± 4.1°. It is expected that later "Gaia" data releases, incorporating about 66 and 120 months of data, will reduce the random errors of these results by factors of 0.35 and 0.15. The latest edition of the International Celestial Reference Frame (ICRF3) adopted a recommended galactocentric aberration constant of 5.8 μas/yr and recommended a correction for secular aberration to obtain the highest positional accuracy for times other than the reference epoch 2015.0.
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Planetary aberration.
Planetary aberration is the combination of the aberration of light (due to Earth's velocity) and light-time correction (due to the object's motion and distance), as calculated in the rest frame of the Solar System. Both are determined at the instant when the moving object's light reaches the moving observer on Earth. It is so called because it is usually applied to planets and other objects in the Solar System whose motion and distance are accurately known.
Discovery and first observations.
The discovery of the aberration of light was totally unexpected, and it was only by considerable perseverance and perspicacity that James Bradley was able to explain it in 1727. It originated from attempts to discover whether stars possessed appreciable parallaxes.
Search for stellar parallax.
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James Bradley's observations.
Consequently, when Bradley and Samuel Molyneux entered this sphere of research in 1725, there was still considerable uncertainty as to whether stellar parallaxes had been observed or not, and it was with the intention of definitely answering this question that they erected a large telescope at Molyneux's house at Kew. They decided to reinvestigate the motion of γ Draconis with a telescope constructed by George Graham (1675–1751), a celebrated instrument-maker. This was fixed to a vertical chimney stack in such manner as to permit a small oscillation of the eyepiece, the amount of which (i.e. the deviation from the vertical) was regulated and measured by the introduction of a screw and a plumb line.
The instrument was set up in November 1725, and observations on γ Draconis were made starting in December. The star was observed to move 40 southwards between September and March, and then reversed its course from March to September. At the same time, 35 Camelopardalis, a star with a right ascension nearly exactly opposite to that of γ Draconis, was 19" more northerly at the beginning of March than in September. The asymmetry of these results, which were expected to be mirror images of each other, were completely unexpected and inexplicable by existing theories.
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Early hypotheses.
Bradley and Molyneux discussed several hypotheses in the hope of finding the solution. Since the apparent motion was evidently caused neither by parallax nor observational errors, Bradley first hypothesized that it could be due to oscillations in the orientation of the Earth's axis relative to the celestial sphere – a phenomenon known as nutation. 35 Camelopardalis was seen to possess an apparent motion which could be consistent with nutation, but since its declination varied only one half as much as that of γ Draconis, it was obvious that nutation did not supply the answer (however, Bradley later went on to discover that the Earth does indeed nutate). He also investigated the possibility that the motion was due to an irregular distribution of the Earth's atmosphere, thus involving abnormal variations in the refractive index, but again obtained negative results.
On August 19, 1727, Bradley embarked upon a further series of observations using a telescope of his own erected at the Rectory, Wanstead. This instrument had the advantage of a larger field of view and he was able to obtain precise positions of a large number of stars over the course of about twenty years. During his first two years at Wanstead, he established the existence of the phenomenon of aberration beyond all doubt, and this also enabled him to formulate a set of rules that would allow the calculation of the effect on any given star at a specified date.
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Development of the theory of aberration.
Bradley eventually developed his explanation of aberration in about September 1728 and this theory was presented to the Royal Society in mid January the following year. One well-known story was that he saw the change of direction of a wind vane on a boat on the Thames, caused not by an alteration of the wind itself, but by a change of course of the boat relative to the wind direction.
However, there is no record of this incident in Bradley's own account of the discovery, and it may therefore be apocryphal.
The following table shows the magnitude of deviation from true declination for γ Draconis and the direction, on the planes of the solstitial colure and ecliptic prime meridian, of the tangent of the velocity of the Earth in its orbit for each of the four months where the extremes are found, as well as expected deviation from true ecliptic longitude if Bradley had measured its deviation from right ascension:
Bradley proposed that the aberration of light not only affected declination, but right ascension as well, so that a star in the pole of the ecliptic would describe a little ellipse with a diameter of about 40", but for simplicity, he assumed it to be a circle. Since he only observed the deviation in declination, and not in right ascension, his calculations for the maximum deviation of a star in the pole of the ecliptic are for its declination only, which will coincide with the diameter of the little circle described by such star. For eight different stars, his calculations are as follows:
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Based on these calculations, Bradley was able to estimate the constant of aberration at 20.2", which is equal to 0.00009793 radians, and with this was able to estimate the speed of light at per second. By projecting the little circle for a star in the pole of the ecliptic, he could simplify the calculation of the relationship between the speed of light and the speed of the Earth's annual motion in its orbit as follows:
Thus, the speed of light to the speed of the Earth's annual motion in its orbit is 10,210 to one, from whence it would follow, that light moves, or is propagated as far as from the Sun to the Earth in 8 minutes 12 seconds.
The original motivation of the search for stellar parallax was to test the Copernican theory that the Earth revolves around the Sun. The change of aberration in the course of the year demonstrates the relative motion of the Earth and the stars.
Retrodiction on Descartes' lightspeed argument.
In the prior century, René Descartes argued that if light were not instantaneous, then shadows of moving objects would lag; and if propagation delays over short terrestrial distances (as in experiments proposed by others at the time) were large enough to be humanly perceptible, then during a lunar eclipse the Sun, Earth, and Moon would be out of alignment by more than an hour's motion, contrary to observation. Huygens commented that, on Rømer's lightspeed data (implying an earth-moon round-trip time of only a few seconds), the lag angle would be undetectably small. What they both overlooked is that for observers being carried along by Earth's orbital motion, velocity aberration (as understood only later) would exactly counteract and perfectly conceal the lag even if large, leaving such eclipse-alignment analysis completely unrevealing about light speed. (Otherwise, shadow lag detection could be employed to sense absolute translational motion, contrary to a basic principle of relativity.)
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Historical theories of aberration.
The phenomenon of aberration became a driving force for many physical theories during the 200 years between its observation and the explanation by Albert Einstein.
The first classical explanation was provided in 1729, by James Bradley as described above, who attributed it to the finite speed of light and the motion of Earth in its orbit around the Sun. However, this explanation proved inaccurate once the wave nature of light was better understood, and correcting it became a major goal of the 19th century theories of luminiferous aether. Augustin-Jean Fresnel proposed a correction due to the motion of a medium (the aether) through which light propagated, known as "partial aether drag". He proposed that objects partially drag the aether along with them as they move, and this became the accepted explanation for aberration for some time. George Stokes proposed a similar theory, explaining that aberration occurs due to the flow of aether induced by the motion of the Earth. Accumulated evidence against these explanations, combined with new understanding of the electromagnetic nature of light, led Hendrik Lorentz to develop an electron theory which featured an immobile aether, and he explained that objects contract in length as they move through the aether. Motivated by these previous theories, Albert Einstein then developed the theory of special relativity in 1905, which provides the modern account of aberration.
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Bradley's classical explanation.
Bradley conceived of an explanation in terms of a corpuscular theory of light in which light is made of particles. His classical explanation appeals to the motion of the earth relative to a beam of light-particles moving at a finite velocity, and is developed in the Sun's frame of reference, unlike the classical derivation given above.
Consider the case where a distant star is motionless relative to the Sun, and the star is extremely far away, so that parallax may be ignored. In the rest frame of the Sun, this means light from the star travels in parallel paths to the Earth observer, and arrives at the same angle regardless of where the Earth is in its orbit. Suppose the star is observed on Earth with a telescope, idealized as a narrow tube. The light enters the tube from the star at angle formula_4 and travels at speed formula_1 taking a time formula_44 to reach the bottom of the tube, where it is detected. Suppose observations are made from Earth, which is moving with a speed formula_6. During the transit of the light, the tube moves a distance formula_46. Consequently, for the particles of light to reach the bottom of the tube, the tube must be inclined at an angle formula_47 different from formula_4, resulting in an "apparent" position of the star at angle formula_47. As the Earth proceeds in its orbit it changes direction, so formula_47 changes with the time of year the observation is made. The apparent angle and true angle are related using trigonometry as:
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In the case of formula_10, this gives formula_11. While this is different from the more accurate relativistic result described above, in the limit of small angle and low velocity they are approximately the same, within the error of the measurements of Bradley's day. These results allowed Bradley to make one of the earliest measurements of the speed of light.
Luminiferous aether.
In the early nineteenth century the wave theory of light was being rediscovered, and in 1804 Thomas Young adapted Bradley's explanation for corpuscular light to wavelike light traveling through a medium known as the luminiferous aether. His reasoning was the same as Bradley's, but it required that this medium be immobile in the Sun's reference frame and must pass through the earth unaffected, otherwise the medium (and therefore the light) would move along with the earth and no aberration would be observed.
He wrote:
However, it soon became clear Young's theory could not account for aberration when materials with a non-vacuum refractive index were present. An important example is of a telescope filled with water. The speed of light in such a telescope will be slower than in vacuum, and is given by formula_54 rather than formula_1 where formula_56 is the refractive index of the water. Thus, by Bradley and Young's reasoning the aberration angle is given by
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which predicts a medium-dependent angle of aberration. When refraction at the telescope's objective is taken into account this result deviates even more from the vacuum result. In 1810 François Arago performed a similar experiment and found that the aberration was unaffected by the medium in the telescope, providing solid evidence against Young's theory. This experiment was subsequently verified by many others in the following decades, most accurately by Airy in 1871, with the same result.
Aether drag models.
Fresnel's aether drag.
In 1818, Augustin Fresnel developed a modified explanation to account for the water telescope and for other aberration phenomena. He explained that the aether is generally at rest in the Sun's frame of reference, but objects partially drag the aether along with them as they move. That is, the aether in an object of index of refraction formula_56 moving at velocity formula_6 is partially dragged with a velocity formula_60 bringing the light along with it. This factor is known as "Fresnel's dragging coefficient". This dragging effect, along with refraction at the telescope's objective, compensates for the slower speed of light in the water telescope in Bradley's explanation. With this modification Fresnel obtained Bradley's vacuum result even for non-vacuum telescopes, and was also able to predict many other phenomena related to the propagation of light in moving bodies. Fresnel's dragging coefficient became the dominant explanation of aberration for the next decades.
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Stokes' aether drag.
However, the fact that light is polarized (discovered by Fresnel himself) led scientists such as Cauchy and Green to believe that the aether was a totally immobile elastic solid as opposed to Fresnel's fluid aether. There was thus renewed need for an explanation of aberration consistent both with Fresnel's predictions (and Arago's observations) as well as polarization.
In 1845, Stokes proposed a 'putty-like' aether which acts as a liquid on large scales but as a solid on small scales, thus supporting both the transverse vibrations required for polarized light and the aether flow required to explain aberration. Making only the assumptions that the fluid is irrotational and that the boundary conditions of the flow are such that the aether has zero velocity far from the Earth, but moves at the Earth's velocity at its surface and within it, he was able to completely account for aberration.
The velocity of the aether outside of the Earth would decrease as a function of distance from the Earth so light rays from stars would be progressively dragged as they approached the surface of the Earth. The Earth's motion would be unaffected by the aether due to D'Alembert's paradox.
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Both Fresnel and Stokes' theories were popular. However, the question of aberration was put aside during much of the second half of the 19th century as focus of inquiry turned to the electromagnetic properties of aether.
Lorentz' length contraction.
In the 1880s once electromagnetism was better understood, interest turned again to the problem of aberration. By this time flaws were known to both Fresnel's and Stokes' theories. Fresnel's theory required that the relative velocity of aether and matter to be different for light of different colors, and it was shown that the boundary conditions Stokes had assumed in his theory were inconsistent with his assumption of irrotational flow. At the same time, the modern theories of electromagnetic aether could not account for aberration at all. Many scientists such as Maxwell, Heaviside and Hertz unsuccessfully attempted to solve these problems by incorporating either Fresnel or Stokes' theories into Maxwell's new electromagnetic laws.
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Special relativity.
Lorentz' theory matched experiment well, but it was complicated and made many unsubstantiated physical assumptions about the microscopic nature of electromagnetic media. In his 1905 theory of special relativity, Albert Einstein reinterpreted the results of Lorentz' theory in a much simpler and more natural conceptual framework which disposed of the idea of an aether. His derivation is given above, and is now the accepted explanation. Robert S. Shankland reported some conversations with Einstein, in which Einstein emphasized the importance of aberration:
Other important motivations for Einstein's development of relativity were the moving magnet and conductor problem and (indirectly) the negative aether drift experiments, already mentioned by him in the introduction of his first relativity paper. Einstein wrote in a note in 1952:
While Einstein's result is the same as Bradley's original equation except for an extra factor of formula_62, Bradley's result does not merely give the classical limit of the relativistic case, in the sense that it gives incorrect predictions even at low relative velocities. Bradley's explanation cannot account for situations such as the water telescope, nor for many other optical effects (such as interference) that might occur within the telescope. This is because in the Earth's frame it predicts that the direction of propagation of the light beam in the telescope is not normal to the wavefronts of the beam, in contradiction with Maxwell's theory of electromagnetism. It also does not preserve the speed of light "c" between frames. However, Bradley did correctly infer that the effect was due to relative velocities.
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Optical aberration
In optics, aberration is a property of optical systems, such as lenses and mirrors, that causes the "image" created by the optical system to not be a faithful reproduction of the "object" being observed. Aberrations cause the image formed by a lens to be blurred, distorted in shape or have color fringing or other effects not seen in the object, with the nature of the distortion depending on the type of aberration.
Aberration can be defined as a departure of the performance of an optical system from the predictions of paraxial optics. In an imaging system, it occurs when light from one point of an object does not converge into (or does not diverge from) a single point after transmission through the system. Aberrations occur because the simple paraxial theory is not a completely accurate model of the effect of an optical system on light, rather than due to flaws in the optical elements.
An image-forming optical system with aberration will produce an image which is not sharp. Makers of optical instruments need to correct optical systems to compensate for aberration.
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Aberration can be analyzed with the techniques of geometrical optics. The articles on reflection, refraction and caustics discuss the general features of reflected and refracted rays.
Overview.
With an ideal lens, light from any given point on an object would pass through the lens and come together at a single point in the "image plane" (or, more generally, the "image surface"). Real lenses, even when they are perfectly made, do not however focus light exactly to a single point. These deviations from the idealized lens performance are called "aberrations" of the lens.
Aberrations fall into two classes: "monochromatic" and "chromatic". Monochromatic aberrations are caused by the geometry of the lens or mirror and occur both when light is reflected and when it is refracted. They appear even when using monochromatic light, hence the name.
Chromatic aberrations are caused by dispersion, the variation of a lens's refractive index with wavelength. Because of dispersion, different wavelengths of light come to focus at different points. Chromatic aberration does not appear when monochromatic light is used.
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Monochromatic aberrations.
The most common monochromatic aberrations are:
Although defocus is technically the lowest-order of the optical aberrations, it is usually not considered as a lens aberration, since it can be corrected by moving the lens (or the image plane) to bring the image plane to the optical focus of the lens.
In addition to these aberrations, piston and tilt are effects which shift the position of the focal point. Piston and tilt are not true optical aberrations, since when an otherwise perfect wavefront is altered by piston and tilt, it will still form a perfect, aberration-free image, only shifted to a different position.
Chromatic aberrations.
Chromatic aberration occurs when different wavelengths are not focussed to the same point. Types of chromatic aberration are:
Theory of monochromatic aberration.
In a perfect optical system in the classical theory of optics, rays of light proceeding from any "object point" unite in an "image point"; and therefore the "object space" is reproduced in an "image space." The introduction of simple auxiliary terms, due to Gauss, named the focal lengths and focal planes, permits the determination of the image of any object for any system. The Gaussian theory, however, is only true so long as the angles made by all rays with the optical axis (the symmetrical axis of the system) are infinitely small, i.e., with infinitesimal objects, images and lenses; in practice these conditions may not be realized, and the images projected by uncorrected systems are, in general, ill-defined and often blurred if the aperture or field of view exceeds certain limits.
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The investigations of James Clerk Maxwell and Ernst Abbe showed that the properties of these reproductions, i.e., the relative position and magnitude of the images, are not special properties of optical systems, but necessary consequences of the supposition (per Abbe) of the reproduction of all points of a space in image points, and are independent of the manner in which the reproduction is effected. These authors showed, however, that no optical system can justify these suppositions, since they are contradictory to the fundamental laws of reflection and refraction. Consequently, the Gaussian theory only supplies a convenient method of approximating reality; realistic optical systems fall short of this unattainable ideal. Currently, all that can be accomplished is the projection of a single plane onto another plane; but even in this, aberrations always occurs and it may be unlikely that these will ever be entirely corrected.
Aberration of axial points (spherical aberration in the restricted sense).
Let (Figure 1) be any optical system, rays proceeding from an axis point under an angle will unite in the axis point ; and those under an angle in the axis point . If there is refraction at a collective spherical surface, or through a thin positive lens, will lie in front of so long as the angle is greater than ("under correction"); and conversely with a dispersive surface or lenses ("over correction"). The caustic, in the first case, resembles the sign '>' (greater than); in the second '<' (less than). If the angle is very small, is the Gaussian image; and is termed the "longitudinal aberration", and the "lateral aberration" of the pencils with aperture . If the pencil with the angle is that of the maximum aberration of all the pencils transmitted, then in a plane perpendicular to the axis at there is a circular "disk of confusion" of radius , and in a parallel plane at another one of radius ; between these two is situated the "disk of least confusion".
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The largest opening of the pencils, which take part in the reproduction of , i.e., the angle , is generally determined by the margin of one of the lenses or by a hole in a thin plate placed between, before, or behind the lenses of the system. This hole is termed the "stop" or "diaphragm"; Abbe used the term "aperture stop" for both the hole and the limiting margin of the lens. The component of the system, situated between the aperture stop and the object , projects an image of the diaphragm, termed by Abbe the "entrance pupil"; the "exit pupil" is the image formed by the component , which is placed behind the aperture stop. All rays which issue from O and pass through the aperture stop also pass through the entrance and exit pupils, since these are images of the aperture stop. Since the maximum aperture of the pencils issuing from is the angle u subtended by the entrance pupil at this point, the magnitude of the aberration will be determined by the position and diameter of the entrance pupil. If the system be entirely behind the aperture stop, then this is itself the entrance pupil ("front stop"); if entirely in front, it is the exit pupil ("back stop").
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If the object point be infinitely distant, all rays received by the first member of the system are parallel, and their intersections, after traversing the system, vary according to their "perpendicular height of incidence," i.e. their distance from the axis. This distance replaces the angle in the preceding considerations; and the aperture, i.e., the radius of the entrance pupil, is its maximum value.
Aberration of elements, i.e. smallest objects at right angles to the axis.
If rays issuing from (Figure 1) are concurrent, it does not follow that points in a portion of a plane perpendicular at to the axis will be also concurrent, even if the part of the plane be very small. As the diameter of the lens increases (i.e., with increasing aperture), the neighboring point will be reproduced, but attended by aberrations comparable in magnitude to . These aberrations are avoided if, according to Abbe, the "sine condition", , holds for all rays reproducing the point . If the object point is infinitely distant, and are to be replaced by and , the perpendicular heights of incidence; the "sine condition" then becomes . A system fulfilling this condition and free from spherical aberration is called "aplanatic" (Greek , privative; , a wandering). This word was first used by Robert Blair to characterize a superior achromatism, and, subsequently, by many writers to denote freedom from spherical aberration as well.
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Since the aberration increases with the distance of the ray from the center of the lens, the aberration increases as the lens diameter increases (or, correspondingly, with the diameter of the aperture), and hence can be minimized by reducing the aperture, at the cost of also reducing the amount of light reaching the image plane.
Aberration of lateral object points (points beyond the axis) with narrow pencils — astigmatism.
A point (Figure 2) at a finite distance from the axis (or with an infinitely distant object, a point which subtends a finite angle at the system) is, in general, even then not sharply reproduced if the pencil of rays issuing from it and traversing the system is made infinitely narrow by reducing the aperture stop; such a pencil consists of the rays which can pass from the object point through the now infinitely small entrance pupil.
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such a pencil consists of the rays which can pass from the object point through the now infinitely small entrance pupil. in the "first principal section" or "meridional section", and the other at right angles to it, i.e. in the second principal section or sagittal section. We receive, therefore, in no single intercepting plane behind the system, as, for example, a focusing screen, an image of the object point; on the other hand, in each of two planes lines and are separately formed (in neighboring planes ellipses are formed), and in a plane between and a circle of least confusion. The interval , termed the astigmatic difference, increases, in general, with the angle made by the principal ray with the axis of the system, i.e. with the field of view. Two "astigmatic image surfaces" correspond to one object plane; and these are in contact at the axis point; on the one lie the focal lines of the first kind, on the other those of the second. Systems in which the two astigmatic surfaces coincide are termed anastigmatic or stigmatic.
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Sir Isaac Newton was probably the discoverer of astigmation; the position of the astigmatic image lines was determined by Thomas Young; and the theory was developed by Allvar Gullstrand. A bibliography by P. Culmann is given in Moritz von Rohr's "Die Bilderzeugung in optischen Instrumenten".
Aberration of lateral object points with broad pencils — coma.
By opening the stop wider, similar deviations arise for lateral points as have been already discussed for axial points; but in this case they are much more complicated. The course of the rays in the meridional section is no longer symmetrical to the principal ray of the pencil; and on an intercepting plane there appears, instead of a luminous point, a patch of light, not symmetrical about a point, and often exhibiting a resemblance to a comet having its tail directed towards or away from the axis. From this appearance it takes its name. The unsymmetrical form of the meridional pencil formerly the only one considered is coma in the narrower sense only; other errors of coma have been treated by Arthur König and Moritz von Rohr, and later by Allvar Gullstrand.
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Curvature of the field of the image.
If the above errors be eliminated, the two astigmatic surfaces united, and a sharp image obtained with a wide aperture—there remains the necessity to correct the curvature of the image surface, especially when the image is to be received upon a plane surface, e.g. in photography. In most cases the surface is concave towards the system.
Distortion of the image.
Even if the image is sharp, it may be distorted compared to ideal pinhole projection. In pinhole projection, the magnification of an object is inversely proportional to its distance to the camera along the optical axis so that a camera pointing directly at a flat surface reproduces that flat surface. Distortion can be thought of as stretching the image non-uniformly, or, equivalently, as a variation in magnification across the field. While "distortion" can include arbitrary deformation of an image, the most pronounced modes of distortion produced by conventional imaging optics is "barrel distortion", in which the center of the image is magnified more than the perimeter (Figure 3a). The reverse, in which the perimeter is magnified more than the center, is known as "pincushion distortion" (Figure 3b). This effect is called lens distortion or image distortion, and there are algorithms to correct it.
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Systems free of distortion are called "orthoscopic" (, right; , to look) or "rectilinear" (straight lines).
This aberration is quite distinct from that of the sharpness of reproduction; in unsharp, reproduction, the question of distortion arises if only parts of the object can be recognized in the figure. If, in an unsharp image, a patch of light corresponds to an object point, the "center of gravity" of the patch may be regarded as the image point, this being the point where the plane receiving the image, e.g., a focusing screen, intersects the ray passing through the middle of the stop. This assumption is justified if a poor image on the focusing screen remains stationary when the aperture is diminished; in practice, this generally occurs. This ray, named by Abbe a "principal ray" (not to be confused with the "principal rays" of the Gaussian theory), passes through the center of the entrance pupil before the first refraction, and the center of the exit pupil after the last refraction. From this it follows that correctness of drawing depends solely upon the principal rays; and is independent of the sharpness or curvature of the image field. Referring to Figure 4, we have , where is the "scale" or magnification of the image. For to be constant for all values of , must also be constant. If the ratio be sufficiently constant, as is often the case, the above relation reduces to the "condition of Airy," i.e. is a constant. This simple relation is fulfilled in all systems which are symmetrical with respect to their diaphragm (briefly named "symmetrical or holosymmetrical objectives"), or which consist of two like, but different-sized, components, placed from the diaphragm in the ratio of their size, and presenting the same curvature to it (hemisymmetrical objectives); in these systems .
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The constancy of necessary for this relation to hold was pointed out by R. H. Bow (Brit. Journ. Photog., 1861), and Thomas Sutton (Photographic Notes, 1862); it has been treated by O. Lummer and by M. von Rohr (Zeit. f. Instrumentenk., 1897, 17, and 1898, 18, p. 4). It requires the middle of the aperture stop to be reproduced in the centers of the entrance and exit pupils without spherical aberration. M. von Rohr showed that for systems fulfilling neither the Airy nor the Bow-Sutton condition, the ratio will be constant for one distance of the object. This combined condition is exactly fulfilled by holosymmetrical objectives reproducing with the scale 1, and by hemisymmetrical, if the scale of reproduction be equal to the ratio of the sizes of the two components.
Zernike model of aberrations.
Circular wavefront profiles associated with aberrations may be mathematically modeled using Zernike polynomials. Developed by Frits Zernike in the 1930s, Zernike's polynomials are orthogonal over a circle of unit radius. A complex, aberrated wavefront profile may be curve-fitted with Zernike polynomials to yield a set of fitting coefficients that individually represent different types of aberrations. These Zernike coefficients are linearly independent, thus individual aberration contributions to an overall wavefront may be isolated and quantified separately.
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There are even and odd Zernike polynomials. The even Zernike polynomials are defined as
formula_1
and the odd Zernike polynomials as
formula_2
where and are nonnegative integers with , is the azimuthal angle in radians, and is the normalized radial distance. The radial polynomials formula_3 have no azimuthal dependence, and are defined as
formula_4
The first few Zernike polynomials, multiplied by their respective fitting coefficients, are:
where is the normalized pupil radius with , is the azimuthal angle around the pupil with , and the fitting coefficients are the wavefront errors in wavelengths.
As in Fourier synthesis using sines and cosines, a wavefront may be perfectly represented by a sufficiently large number of higher-order Zernike polynomials. However, wavefronts with very steep gradients or very high spatial frequency structure, such as produced by propagation through atmospheric turbulence or aerodynamic flowfields, are not well modeled by Zernike polynomials, which tend to low-pass filter fine spatial definition in the wavefront. In this case, other fitting methods such as fractals or singular value decomposition may yield improved fitting results.
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The circle polynomials were introduced by Frits Zernike to evaluate the point image of an aberrated optical system taking into account the effects of diffraction. The perfect point image in the presence of diffraction had already been described by Airy, as early as 1835. It took almost hundred years to arrive at a comprehensive theory and modeling of the point image of aberrated systems (Zernike and Nijboer). The analysis by Nijboer and Zernike describes the intensity distribution close to the optimum focal plane. An extended theory that allows the calculation of the point image amplitude and intensity over a much larger volume in the focal region was recently developed (Extended Nijboer-Zernike theory). This Extended Nijboer-Zernike theory of point image or 'point-spread function' formation has found applications in general research on image formation, especially for systems with a high numerical aperture, and in characterizing optical systems with respect to their aberrations.
Analytic treatment of aberrations.
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The preceding review of the several errors of reproduction belongs to the "Abbe theory of aberrations," in which definite aberrations are discussed separately; it is well suited to practical needs, for in the construction of an optical instrument certain errors are sought to be eliminated, the selection of which is justified by experience. In the mathematical sense, however, this selection is arbitrary; the reproduction of a finite object with a finite aperture entails, in all probability, an infinite number of aberrations. This number is only finite if the object and aperture are assumed to be "infinitely small of a certain order"; and with each order of infinite smallness, i.e. with each degree of approximation to reality (to finite objects and apertures), a certain number of aberrations is associated. This connection is only supplied by theories which treat aberrations generally and analytically by means of indefinite series.
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The nature of the reproduction consists in the rays proceeding from a point being united in another point ; in general, this will not be the case, for , vary if , be constant, but , variable. It may be assumed that the planes and are drawn where the images of the planes and are formed by rays near the axis by the ordinary Gaussian rules; and by an extension of these rules, not, however, corresponding to reality, the Gauss image point , with coordinates , , of the point at some distance from the axis could be constructed. Writing and , then and are the aberrations belonging to , and , , and are functions of these magnitudes which, when expanded in series, contain only odd powers, for the same reasons as given above. On account of the aberrations of all rays which pass through , a patch of light, depending in size on the lowest powers of , , , which the aberrations contain, will be formed in the plane . These degrees, named by J. Petzval "the numerical orders of the image", are consequently only odd powers; the condition for the formation of an image of the th order is that in the series for and the coefficients of the powers of the 3rd, 5th, ... (2)th degrees must vanish. The images of the Gauss theory being of the third order, the next problem is to obtain an image of 5th order, or to make the coefficients of the powers of 3rd degree zero. This necessitates the satisfying of five equations; in other words, there are five alterations of the 3rd order, the vanishing of which produces an image of the 5th order.
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The expression for these coefficients in terms of the constants of the optical system, i.e. the radii, thicknesses, refractive indices and distances between the lenses, was solved by L. von Seidel; in 1840, J. Petzval constructed his portrait objective, from similar calculations which have never been published. The theory was elaborated by S. Finterswalder, who also published a posthumous paper of Seidel containing a short view of his work; a simpler form was given by A. Kerber. A. Konig and M. von Rohr have represented Kerber's method, and have deduced the Seidel formulae from geometrical considerations based on the Abbe method, and have interpreted the analytical results geometrically.
The aberrations can also be expressed by means of the "characteristic function" of the system and its differential coefficients, instead of by the radii, etc., of the lenses; these formulae are not immediately applicable, but give, however, the relation between the number of aberrations and the order. Sir William Rowan Hamilton thus derived the aberrations of the third order; and in later times the method was pursued by Clerk Maxwell ("Proc. London Math. Soc.," 1874–1875; (see also the treatises of R. S. Heath and L. A. Herman), M. Thiesen ("Berlin. Akad. Sitzber.," 1890, 35, p. 804), H. Bruns ("Leipzig. Math. Phys. Ber.," 1895, 21, p. 410), and particularly successfully by K. Schwarzschild ("Göttingen. Akad. Abhandl.," 1905, 4, No. 1), who thus discovered the aberrations of the 5th order (of which there are nine), and possibly the shortest proof of the practical (Seidel) formulae. A. Gullstrand (vide supra, and "Ann. d. Phys.," 1905, 18, p. 941) founded his theory of aberrations on the differential geometry of surfaces.
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The aberrations of the third order are: (1) aberration of the axis point; (2) aberration of points whose distance from the axis is very small, less than of the third order — the deviation from the sine condition and coma here fall together in one class; (3) astigmatism; (4) curvature of the field; (5) distortion.
Practical elimination of aberrations.
The classical imaging problem is to reproduce perfectly a finite plane (the object) onto another plane (the image) through a finite aperture. It is impossible to do so perfectly for "more than one" such pair of planes (this was proven with increasing generality by Maxwell in 1858, by Bruns in 1895, and by Carathéodory in 1926, see summary in Walther, A., J. Opt. Soc. Am. A 6, 415–422 (1989)). For a single pair of planes (e.g. for a single focus setting of an objective), however, the problem can in principle be solved perfectly. Examples of such a theoretically perfect system include the Luneburg lens and the Maxwell fish-eye.
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In order to render spherical aberration and the deviation from the sine condition small throughout the whole aperture, there is given to a ray with a finite angle of aperture u* (width infinitely distant objects: with a finite height of incidence h*) the same distance of intersection, and the same sine ratio as to one neighboring the axis (u* or h* may not be much smaller than the largest aperture U or H to be used in the system). The rays with an angle of aperture smaller than u* would not have the same distance of intersection and the same sine ratio; these deviations are called "zones," and the constructor endeavors to reduce these to a minimum. The same holds for the errors depending upon the angle of the field of view, w: astigmatism, curvature of field and distortion are eliminated for a definite value, w*, "zones of astigmatism, curvature of field and distortion," attend smaller values of w. The practical optician names such systems: "corrected for the angle of aperture u* (the height of incidence h*) or the angle of field of view w*." Spherical aberration and changes of the sine ratios are often represented graphically as functions of the aperture, in the same way as the deviations of two astigmatic image surfaces of the image plane of the axis point are represented as functions of the angles of the field of view.
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The final form of a practical system consequently rests on compromise; enlargement of the aperture results in a diminution of the available field of view, and vice versa. But the larger aperture will give the larger resolution. The following may be regarded as typical:
Chromatic or color aberration.
In optical systems composed of lenses, the position, magnitude and errors of the image depend upon the refractive indices of the glass employed (see Lens (optics) and Monochromatic aberration, above). Since the index of refraction varies with the color or wavelength of the light (see dispersion), it follows that a system of lenses (uncorrected) projects images of different colors in somewhat different places and sizes and with different aberrations; i.e. there are "chromatic differences" of the distances of intersection, of magnifications, and of monochromatic aberrations. If mixed light be employed (e.g. white light) all these images are formed and they cause a confusion, named chromatic aberration; for instance, instead of a white margin on a dark background, there is perceived a colored margin, or narrow spectrum. The absence of this error is termed achromatism, and an optical system so corrected is termed achromatic. A system is said to be "chromatically under-corrected" when it shows the same kind of chromatic error as a thin positive lens, otherwise it is said to be "overcorrected."
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If, in the first place, monochromatic aberrations be neglected — in other words, the Gaussian theory be accepted — then every reproduction is determined by the positions of the focal planes, and the magnitude of the focal lengths, or if the focal lengths, as ordinarily happens, be equal, by three constants of reproduction. These constants are determined by the data of the system (radii, thicknesses, distances, indices, etc., of the lenses); therefore their dependence on the refractive index, and consequently on the color, are calculable. The refractive indices for different wavelengths must be known for each kind of glass made use of. In this manner the conditions are maintained that any one constant of reproduction is equal for two different colors, i.e. this constant is achromatized. For example, it is possible, with one thick lens in air, to achromatize the position of a focal plane of the magnitude of the focal length. If all three constants of reproduction be achromatized, then the Gaussian image for all distances of objects is the same for the two colors, and the system is said to be in "stable achromatism."
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In practice it is more advantageous (after Abbe) to determine the chromatic aberration (for instance, that of the distance of intersection) for a fixed position of the object, and express it by a sum in which each component conlins the amount due to each refracting surface. In a plane containing the image point of one color, another colour produces a disk of confusion; this is similar to the confusion caused by two "zones" in spherical aberration. For infinitely distant objects the radius Of the chromatic disk of confusion is proportional to the linear aperture, and independent of the focal length ("vide supra", "Monochromatic Aberration of the Axis Point"); and since this disk becomes the less harmful with an increasing image of a given object, or with increasing focal length, it follows that the deterioration of the image is proportional to the ratio of the aperture to the focal length, i.e. the "relative aperture." (This explains the gigantic focal lengths in vogue before the discovery of achromatism.)
Examples:
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Newton failed to perceive the existence of media of different dispersive powers required by achromatism; consequently he constructed large reflectors instead of refractors. James Gregory and Leonhard Euler arrived at the correct view from a false conception of the achromatism of the eye; this was determined by Chester More Hall in 1728, Klingenstierna in 1754 and by Dollond in 1757, who constructed the celebrated achromatic telescopes. (See telescope.)
Glass with weaker dispersive power (greater formula_5) is named "crown glass"; that with greater dispersive power, "flint glass". For the construction of an achromatic collective lens (formula_6 positive) it follows, by means of equation (4), that a collective lens I. of crown glass and a dispersive lens II. of flint glass must be chosen; the latter, although the weaker, corrects the other chromatically by its greater dispersive power. For an achromatic dispersive lens the converse must be adopted.
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of flint glass must be chosen; the latter, although the weaker, corrects the other chromatically by its greater dispersive power. For an achromatic dispersive lens the converse must be adopted. equal radii. According to P. Rudolph (Eder's Jahrb. f. Photog., 1891, 5, p. 225; 1893, 7, p. 221), cemented objectives of thin lenses permit the elimination of spherical aberration on the axis, if, as above, the collective lens has a smaller refractive index; on the other hand, they permit the elimination of astigmatism and curvature of the field, if the collective lens has a greater refractive index (this follows from the Petzval equation; see L. Seidel, Astr. Nachr., 1856, p. 289). Should the cemented system be positive, then the more powerful lens must be positive; and, according to (4), to the greater power belongs the weaker dispersive power (greater formula_5), that is to say, crown glass; consequently the crown glass must have the greater refractive index for astigmatic and plane images. In all earlier kinds of glass, however, the dispersive power increased with the refractive index; that is, formula_5 decreased as formula_9 increased; but some of the Jena glasses by E.
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In all earlier kinds of glass, however, the dispersive power increased with the refractive index; that is, formula_5 decreased as formula_9 increased; but some of the Jena glasses by E. Abbe and O. Schott were crown glasses of high refractive index, and achromatic systems from such crown glasses, with flint glasses of lower refractive index, are called the "new achromats," and were employed by P. Rudolph in the first "anastigmats" (photographic objectives).
Instead of making formula_10 vanish, a certain value can be assigned to it which will produce, by the addition of the two lenses, any desired chromatic deviation, e.g. sufficient to eliminate one present in other parts of the system. If the lenses I. and II. be cemented and have the same refractive index for one color, then its effect for that one color is that of a lens of one piece; by such decomposition of a lens it can be made chromatic or achromatic at will, without altering its spherical effect. If its chromatic effect (formula_11) be greater than that of the same lens, this being made of the more dispersive of the two glasses employed, it is termed "hyper-chromatic."
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For two thin lenses separated by a distance formula_12 the condition for achromatism is formula_13; if formula_14 (e.g. if the lenses be made of the same glass), this reduces to formula_15, known as the "condition for oculars."
If a constant of reproduction, for instance the focal length, be made equal for two colors, then it is not the same for other colors, if two different glasses are employed. For example, the condition for achromatism (4) for two thin lenses in contact is fulfilled in only one part of the spectrum, since formula_16 varies within the spectrum. This fact was first ascertained by J. Fraunhofer, who defined the colors by means of the dark lines in the solar spectrum; and showed that the ratio of the dispersion of two glasses varied about 20% from the red to the violet (the variation for glass and water is about 50%). If, therefore, for two colors, a and b, formula_17, then for a third color, c, the focal length is different; that is, if c lies between a and b, then formula_18, and vice versa; these algebraic results follow from the fact that towards the red the dispersion of the positive crown glass preponderates, towards the violet that of the negative flint. These chromatic errors of systems, which are achromatic for two colors, are called the "secondary spectrum," and depend upon the aperture and focal length in the same manner as the primary chromatic errors do.
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In Figure 6, taken from M. von Rohr's "Theorie und Geschichte des photographischen Objectivs", the abscissae are focal lengths, and the ordinates wavelengths. The Fraunhofer lines used are shown in adjacent table.
The focal lengths are made equal for the lines C and F. In the neighborhood of 550 nm the tangent to the curve is parallel to the axis of wavelengths; and the focal length varies least over a fairly large range of color, therefore in this neighborhood the color union is at its best. Moreover, this region of the spectrum is that which appears brightest to the human eye, and consequently this curve of the secondary on spectrum, obtained by making formula_19, is, according to the experiments of Sir G. G. Stokes (Proc. Roy. Soc., 1878), the most suitable for visual instruments ("optical achromatism,"). In a similar manner, for systems used in photography, the vertex of the color curve must be placed in the position of the maximum sensibility of the plates; this is generally supposed to be at G'; and to accomplish this the F and violet mercury lines are united. This artifice is specially adopted in objectives for astronomical photography ("pure actinic achromatism"). For ordinary photography, however, there is this disadvantage: the image on the focusing-screen and the correct adjustment of the photographic sensitive plate are not in register; in astronomical photography this difference is constant, but in other kinds it depends on the distance of the objects. On this account the lines D and G' are united for ordinary photographic objectives; the optical as well as the actinic image is chromatically inferior, but both lie in the same place; and consequently the best correction lies in F (this is known as the "actinic correction" or "freedom from chemical focus").
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Should there be in two lenses in contact the same focal lengths for three colours a, b, and c, i.e. formula_20, then the relative partial dispersion formula_21 must be equal for the two kinds of glass employed. This follows by considering equation (4) for the two pairs of colors ac and bc. Until recently no glasses were known with a proportional degree of absorption; but R. Blair (Trans. Edin. Soc., 1791, 3, p. 3), P. Barlow, and F. S. Archer overcame the difficulty by constructing fluid lenses between glass walls. Fraunhofer prepared glasses which reduced the secondary spectrum; but permanent success was only assured on the introduction of the Jena glasses by E. Abbe and O. Schott. In using glasses not having proportional dispersion, the deviation of a third colour can be eliminated by two lenses, if an interval be allowed between them; or by three lenses in contact, which may not all consist of the old glasses. In uniting three colors an "achromatism of a higher order" is derived; there is yet a residual "tertiary spectrum," but it can always be neglected.
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The Gaussian theory is only an approximation; monochromatic or spherical aberrations still occur, which will be different for different colors; and should they be compensated for one color, the image of another color would prove disturbing. The most important is the chromatic difference of aberration of the axis point, which is still present to disturb the image, after par-axial rays of different colors are united by an appropriate combination of glasses. If a collective system be corrected for the axis point for a definite wavelength, then, on account of the greater dispersion in the negative components — the flint glasses, — overcorrection will arise for the shorter wavelengths (this being the error of the negative components), and under-correction for the longer wavelengths (the error of crown glass lenses preponderating in the red). This error was treated by Jean le Rond d'Alembert, and, in special detail, by C. F. Gauss. It increases rapidly with the aperture, and is more important with medium apertures than the secondary spectrum of par-axial rays; consequently, spherical aberration must be eliminated for two colors, and if this be impossible, then it must be eliminated for those particular wavelengths which are most effectual for the instrument in question (a graphical representation of this error is given in M. von Rohr, "Theorie und Geschichte des photographischen Objectivs").
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The condition for the reproduction of a surface element in the place of a sharply reproduced point — the constant of the sine relationship must also be fulfilled with large apertures for several colors. E. Abbe succeeded in computing microscope objectives free from error of the axis point and satisfying the sine condition for several colors, which therefore, according to his definition, were "aplanatic for several colors"; such systems he termed "apochromatic". While, however, the magnification of the individual zones is the same, it is not the same for red as for blue; and there is a chromatic difference of magnification. This is produced in the same amount, but in the opposite sense, by the oculars, which Abbe used with these objectives ("compensating oculars"), so that it is eliminated in the image of the whole microscope. The best telescope objectives, and photographic objectives intended for three-color work, are also apochromatic, even if they do not possess quite the same quality of correction as microscope objectives do. The chromatic differences of other errors of reproduction seldom have practical importance.
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Amy Grant
Amy Lee Grant (born November 25, 1960) is an American singer-songwriter and musician. She began her music career in contemporary Christian music (CCM) before crossing over to pop music in the mid-1980s. Grant has been referred to as "The Queen of Christian Pop".
Grant made her debut as a teenager, gaining fame in Christian music during the 1980s with hits such as "Father's Eyes", "El Shaddai", and "Angels". In the mid-1980s, she began broadening her audience and soon became one of the first CCM artists to cross over into mainstream pop on the heels of her successful albums "Unguarded" and "Lead Me On". In 1986, she scored her first "Billboard" Hot 100 no. 1 song in a duet with Peter Cetera, "The Next Time I Fall". In 1991, she released the album "Heart in Motion", which became her best-selling album, topping the "Billboard" Christian album chart for 32 weeks. It sold five million copies in the U.S. and produced her second no. 1 pop single "Baby Baby", as well as another three top 10 hits on the "Billboard" Hot 100: "That's What Love Is For", "Every Heartbeat" and "Good for Me".
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Grant had sold more than 30 million albums worldwide, won six Grammy Awards, 22 Gospel Music Association Dove Awards, and had the first Christian album to go platinum. She was honored with a star on the Hollywood Walk of Fame in 2006 for her contributions to the entertainment industry, and in 2022 she was announced as a recipient of the Kennedy Center Honors. Grant is the author of several books, including a memoir, "Mosaic: Pieces of My Life So Far", and a book based on the popular Christmas song "Breath of Heaven (Mary's Song)" that she co-wrote.
Background.
Early life and career.
Born in Augusta, Georgia, Grant is the youngest of four sisters. Her family settled in Nashville in 1967. She is a great-granddaughter of Nashville philanthropist A. M. Burton (founder of Life and Casualty Insurance Company, eponym of Nashville's Life & Casualty Tower, WLAC Radio, and WLAC-TV) and Lillie Burton. She has acknowledged the influence of the Burtons on her development as a musician, starting with their common membership in Nashville's Ashwood Church of Christ. According to the Singing Carrots website, based on her recorded songs, Grant has a mezzo-soprano voice type, also able to perform in the soprano and contralto ranges.
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In 1976, Grant wrote her first song ("Mountain Top"), performed in public for the first time at Harpeth Hall School, the all-girls school she attended in Nashville. She recorded a demo tape for her parents with church youth-leader Brown Bannister. While Bannister was dubbing a copy of the tape, Chris Christian, the owner of the recording studio, heard the demo and called Word Records. He played it over the phone, and she was offered a recording contract five weeks before her 16th birthday.
In 1977, she recorded her first album, "Amy Grant", produced by Bannister, who also produced her next 11 albums. It was released in early 1978, one month before her high-school graduation. Toward the end of 1978 she performed her first ticketed concert after beginning her first year at Furman University.
In May 1979, while at the album-release party for her second album, "My Father's Eyes", Grant met Gary Chapman, who had written the title track. Grant and Chapman toured together in mid-1979. In late 1980, she transferred to Vanderbilt University where she was a member of the sorority Kappa Alpha Theta. Grant made a few more albums before dropping out of college to pursue a career in music—"Never Alone", followed by a pair of live albums in 1981 ("In Concert" and "In Concert Volume Two"), both backed by an augmented edition of the DeGarmo & Key band. It was during these early shows that Grant also established one of her concert trademarks: performing barefoot. Grant continues to take off her shoes midway through performances, as she has said, "it is just more comfortable."
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In 1982 she released her breakthrough album "Age to Age". The album contains the signature track, "El Shaddai" (written by Michael Card) and the Grant-Chapman penned song, "In a Little While". "El Shaddai" was later awarded one of the "Songs of the Century" by the RIAA in 2001. Grant received her first Grammy Award for Best Contemporary Gospel Performance, as well as two GMA Dove Awards for Gospel Artist of the Year and Pop/Contemporary Album of the Year. "Age to Age" became the first Christian album by a solo artist to be certified gold (1983) and the first Christian album to be certified platinum (1985).
In the mid-1980s, Grant began touring and recording with young up-and-coming songwriter Michael W. Smith. Grant and Smith continue to have a strong friendship and creative relationship, often writing songs for or contributing vocals to each other's albums, and as of 2019, often touring together annually during November and December putting on Christmas concerts. During the 1980s, Grant was also a backup singer for Bill Gaither.
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Grant followed this album with the first of her Christmas albums, which was later the basis for her holiday shows. In 1984, she released another pop-oriented Christian hit, "Straight Ahead", earning Grant her first appearance at the Grammy Awards show in 1985. The head of NBC took notice of Grant's performance and called her manager to book her for her own Christmas special.
Widening audience.
Shortly after Grant established herself as the "Queen of Christian Pop" she changed directions to widen her fan base. Her goal was to become the first Christian singer-songwriter who was also successful as a contemporary pop singer. "Unguarded" (1985) surprised some fans for its very mainstream sound. "Find a Way", from "Unguarded", became one of the few non-Christmas Christian songs to hit the "Billboard" Top 40 list, also reaching No. 7 on the Adult Contemporary chart. She also scored No. 18 on "Billboard" AC in 1986 with "Stay for Awhile". Grant scored her first "Billboard" No. 1 song in 1986 with "The Next Time I Fall", a duet with former Chicago singer/bassist Peter Cetera. That year, she also recorded a duet with singer Randy Stonehill for his "Love Beyond Reason" album, titled "I Could Never Say Goodbye", and recorded "The Animals' Christmas" with Art Garfunkel.
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"Lead Me On" (1988) contained many songs which were about Christianity and love relationships, but some interpreted it as not being enough of a "Christian" record. Years later "Lead Me On" would be chosen as the greatest Contemporary Christian album of all time by "CCM Magazine". The mainstream song "Saved by Love" was a minor hit, receiving airplay on radio stations featuring the newly emerging Adult Contemporary format. The album's title song received some pop radio airplay and crossed over to No. 96 on the "Billboard" Hot 100, and "1974 (We Were Young)" and "Saved By Love" also charted as Adult Contemporary songs. In 1989, she appeared in a Target ad campaign, performing songs from the album.
In the mainstream.
When "Heart in Motion" was released in 1991, many fans were surprised that the album was of contemporary pop music. Grant's desire to widen her audience was frowned upon by the confines of the popular definitions of ministry at the time. The track "Baby Baby" written for Grant's newborn daughter Millie, of whom Grant wrote, her "six-week-old face was my inspiration", became a pop hit (hitting No. 1 on the "Billboard" Hot 100), and Grant was established as a name in the mainstream music world. "Baby Baby" received Grammy nominations for Best Female Pop Vocal Performance, and Record and Song of the Year (although it failed to win in any of those categories).
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Four other hits from the album made the Pop top 20: "Every Heartbeat" (No. 2), "That's What Love Is For" (No. 7), "Good for Me" (No. 8), and "I Will Remember You" (No. 20). On the Adult Contemporary chart, all five songs were top 10 hits, with two of the five ("Baby Baby" and "That's What Love Is For") reaching No. 1. Many Christian fans remained loyal, putting the album atop "Billboard" Contemporary Christian Chart for 32 weeks. "Heart in Motion" is Grant's best-selling album, having sold over five million copies according to the RIAA. Grant followed the album with her second Christmas album, "Home For Christmas" in 1992, which included the song "Breath of Heaven (Mary's Song)", written by Chris Eaton and Grant, and would later be covered by many artists, including Donna Summer, Jessica Simpson (who acknowledged Grant as one of her favorite artists), Vince Gill, Sara Groves, Point of Grace, Gladys Knight, and Broadway star Barbara Cook.
"House of Love" in 1994 continued in the same vein, containing pop songs mingled with spiritual lyrics. The album was a multi-platinum success and produced the pop hit "Lucky One" (No. 18 pop and No. 2 AC; No. 1 on Radio & Records) as well as the title track (a duet with country music star and future husband Vince Gill) (No. 37 pop) and a cover of Joni Mitchell's frequently covered "Big Yellow Taxi" (No. 67 pop) (in which she changed the line "And they charged the people "a dollar and a half" just to see'em" to "And then they charged the people "25 bucks" just to see'em").
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After she covered the 10cc song "The Things We Do for Love" for the "Mr. Wrong" soundtrack, "Behind the Eyes" was released in September 1997. The album struck a much darker note, leaning more towards downtempo, acoustic soft-rock songs, with more mature (yet still optimistic) lyrics. She called it her "razor blades and Prozac" album. Although "Takes a Little Time" was a moderate hit single, the album failed to sell like the previous two albums, which had both gone multi-platinum. "Behind The Eyes" was eventually certified Gold by the RIAA. The video for "Takes a Little Time" was a new direction for Grant; with a blue light filter, acoustic guitar, the streets and characters of New York City, and a plot, Grant was re-cast as an adult light rocker. She followed up "Behind The Eyes" with "A Christmas To Remember", her third Christmas album, in 1999. The album was certified gold in 2000.
Following the 9/11 attacks Grant's "I Will Remember You" saw a resurgence in popularity as many radio DJs mixed a special tribute version of the song. In the same year Grant won $125,000 for charity on the "Rock Star Edition" of "Who Wants to Be a Millionaire?"
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Return to Gospel Roots.
Grant returned to Christian pop with the 2002 release of an album of hymns titled "Legacy... Hymns and Faith". The album featured a Vince Gill-influenced mix of bluegrass and pop and marked Grant's 25th anniversary in the music industry. Grant followed this up with "Simple Things" in 2003. The album did not have the success of her previous pop or gospel efforts. Soon after "Simple Things", Grant and Interscope/A&M parted ways. The same year, Grant was inducted into the Gospel Music Hall of Fame by the Gospel Music Association, an industry trade organization of which she is a longstanding member, in her first year of eligibility. Grant released a sequel in 2005 titled "Rock of Ages...Hymns and Faith".
Grant joined the reality television phenomenon by hosting "Three Wishes", a show in which she and a team of helpers make wishes come true for small-town residents. The show debuted on NBC in the fall of 2005; however it was canceled at the end of its first season due to high production costs. After "Three Wishes" was canceled, Grant won her 6th Grammy Award for "Rock of Ages... Hymns & Faith". In a February 2006 webchat, Grant said she believes her "best music is still ahead".
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In April 2006, a live CD/DVD titled "Time Again... Amy Grant Live" was recorded in Fort Worth, Texas, at Bass Performance Hall. (Grant's first paid public performance was at the Will Rogers Auditorium in Fort Worth.) The concert was released on September 26, 2006. In addition to receiving a star on the Hollywood Walk of Fame, media appearances included write-ups in "CCM Magazine", and a performance on "The View".
In a February 2007 web chat on her web site, Grant discussed a book she was working on titled "Mosaic: Pieces of My Life So Far", saying, "It's not an autobiography, but more a collection of memories, song lyrics, poetry and a few pictures." The book was released on October 16, 2007. In November, it debuted at No. 35 on the "New York Times" Best Seller list. In the same web chat, Grant noted that she is "anxious to get back in the studio after the book is finished, and reinvent myself as an almost-50 performing woman".
2007 was Grant's 30th year in music. She left Word/Warner, and contracted with EMI CMG who re-released her regular studio albums as remastered versions on August 14, 2007. Marking the start of Grant's new contract is a career-spanning greatest hits album, with all the songs digitally remastered. The album was released as both a single-disc CD edition, and a two-disc CD/DVD Special Edition, the DVD featuring music videos and interviews. Grant appeared with Gill on "The Oprah Winfrey Show" for a holiday special in December 2007.
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In February 2008, Grant joined the writing team from Compassionart as a guest vocalist at the Abbey Road studios, London, to record a song called "Highly Favoured", which was included on the album "CompassionArt". On June 24, 2008, Grant re-released her 1988 album, "Lead Me On", in honor of its 20th anniversary. The two-disc release includes the original album and a second disc with new acoustic recordings, live performances from 1989, and interviews with Amy. Grant recreated the "Lead Me On" tour in the fall of 2008. On June 27, 2008, at Creation Festival Northeast she performed "Lead Me On" and a few other songs backed by Hawk Nelson. At the end of the concert, Grant returned to the stage and sang "Thy Word". She appeared on the 2008 album "" singing "Could I Have This Dance".
On May 5, 2009, Grant released an EP containing two new songs, "She Colors My Day", and "Unafraid", as well as the previously released songs "Baby Baby" and "Oh How the Years Go By". The EP, exclusively through iTunes, benefited the Entertainment Industry Foundation's (EIF) Women's Cancer Research Fund. In 2010, Grant released "Somewhere Down the Road", featuring the hit single "Better Than a Hallelujah", which peaked at No. 8 on "Billboard" Top Christian Songs chart. When asked about the new album during an interview with CBN.com, Grant says, "... my hope is just for those songs to provide companionship, remind myself and whoever else is listening what's important. I feel like songs have the ability to connect us to ourselves and to each other, and to our faith, to the love of Jesus, in a way that conversation doesn't do. Songs kind of slip in and move you before you realize it." In September 2012, Grant took part in a campaign called "30 Songs / 30 Days" to support "", a multi-platform media project inspired by Nicholas Kristof and Sheryl WuDunn's book.
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Grant's next album, "How Mercy Looks from Here", was released on May 14, 2013, and was produced by Marshall Altman. The album reached No. 12 on the "Billboard" 200 chart, making it her highest-charting album since 1997's "Behind the Eyes". Two singles were released from the album: "Don't Try So Hard" and "If I Could See", both of which charted on the US "Billboard" Hot Christian Songs chart. On August 19, 2014, she released an album of hits remixed by well known engineers and DJs. The album was titled "". It charted at 110 on the US "Billboard" 200 chart and at No. 5 on the US Dance chart. To promote the album, several new remix EPs were released on iTunes the following month including "Find a Way, "Stay for Awhile", "Baby Baby, "Every Heartbeat" and "That's What Love Is For". Due to club play of the remixes of "Baby Baby" and "Every Heartbeat", they charted at No. 3 and 13, respectively on the U.S. Dance Chart. This marked her first appearance on that chart in 23 years. On September 30, 2014, Grant released a new single titled "Welcome Yourself". In honor of Breast Cancer Awareness Month, proceeds of the single go to breast cancer research.
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On February 12, 2015, she announced a new compilation album titled "Be Still and Know... Hymns & Faith", to be released. The album was released on April 14, 2015, and charted at No. 7 in the U.S. on the "Billboard" Christian Albums chart. . Grant released a Christmas album on October 21, 2016, "Tennessee Christmas", which is a combination of classic Christmas songs and original material. It charted in the U.S. at No. 31 on the "Billboard" 200 and at No. 3 on the "Billboard" Top Holiday Albums chart. The single from the album, "To Be Together", reached No. 32 on the Hot Christian Songs chart and No. 19 on the Holiday Digital Song Sales chart. She supported the album with a series of Christmas concerts with Vince Gill at the Ryman Auditorium. She also toured the U.S. and Canada with Christmas concerts accompanied by Michael W. Smith and season 9 winner of "The Voice", Jordan Smith. In February 2017, she released a new song, "Say It With a Kiss", with accompanying video. During November and December 2017, Grant performed another series of Christmas concerts with Vince Gill at the Ryman and embarked on another U.S. and Canada Christmas tour with Michael W. Smith and Jordan Smith. Grant has been a guest narrator for Disney's Candlelight Processional at Walt Disney World in 2012, 2013, and 2015.
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Personal life.
On June 19, 1982, Grant married fellow Christian musician Gary Chapman. Their marriage produced three children. In March 1999 she filed for divorce from Chapman. On March 10, 2000, Grant married country singer-songwriter Vince Gill, who had been previously married to country singer Janis Oliver of Sweethearts of the Rodeo. Grant and Gill have one daughter together, Corrina Grant Gill, born March 12, 2001.
In the November 1999 "CCM Magazine", Grant explained why she left Chapman and married Gill:
In June 2020, Grant had an open-heart surgery to repair partial anomalous pulmonary venous return (PAPVR), a congenital heart condition.
Public views and perception.
Along with praise for her contributions to the contemporary Christian genre, Grant has also generated controversy within the Christian community, from "complaints that she was too worldly and too sexy" to a "barrage of condemnation" following her divorce and remarriage.
In an interview early in her career, Grant stated, "I have a healthy sense of right and wrong, but sometimes, for example, using foul, exclamation-point words among friends can be good for a laugh." The article which was based on that interview was constructed in such a manner so as to make it appear as though Grant condoned premarital sex. Later Grant reflected on how the article misrepresented her views, stating: "We probably talked for two hours about sexual purity, but when the interview finally came out he worded it in such a way that it sounded like I condoned premarital sex. So I picked up that article and thought, 'You've made me say something I've never said, and you've totally disregarded two hours of Bible put in one flippant comment that I made about a moan.
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Arthur William à Beckett
Arthur William à Beckett (25 October 1844 – 14 January 1909) was an English journalist and intellectual.
Biography.
He was a younger son of Gilbert Abbott à Beckett and Mary Anne à Beckett, brother of Gilbert Arthur à Beckett and educated at Felsted School. Besides fulfilling other journalistic engagements, Beckett founded The Tomahawk which ran from 1867 to 1870Beckett was on the staff of "Punch" from 1874 to 1902, edited the "Sunday Times" 1891–1895, and the "Naval and Military Magazine" in 1896.
He gave an account of his father and his own reminiscences in "The à Becketts of Punch" (1903). A childhood friend (and distant relative) of W. S. Gilbert, Beckett briefly feuded with Gilbert in 1869, but the two patched up the friendship, and Gilbert even later collaborated on projects with Beckett's brother.
He was married to Suzanne Frances Winslow, daughter of the noted psychiatrist Forbes Benignus Winslow. He is buried in the churchyard at St Mary Magdalen, Mortlake.
Works.
He published:
He wrote for the theatre two three-act comedies:
and
External links.
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Aberdeen, South Dakota
Aberdeen () is a city in and the county seat of Brown County, South Dakota, United States. As of the 2020 census, its population was 28,495. making it the third-most populous city in the state. Aberdeen is home of Northern State University.
History.
Settlement.
Before Aberdeen or Brown County was inhabited by European settlers, it was inhabited by the Sioux Indians from approximately 1700 to 1879. Europeans entered the region for business, founding fur trading posts during the 1820s; these trading posts operated until the mid-1830s. The first "settlers" of this region were the Arikara Indians, but they would later be joined by others.
The first group of Euro-American settlers to reach the area that is now Brown County was a party of four people, three horses, two mules, fifteen cattle, and two wagons. This group of settlers was later joined by another group the following spring, and, eventually, more settlers migrated toward this general area, currently known as Columbia, South Dakota. This town was established on June 15, 1879, was settled in 1880, and was incorporated in 1882.
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Creation of the town.
Aberdeen, like many towns of the Midwest, was built around the newly developing railroad systems. Aberdeen was first officially plotted as a town site on January 3, 1881, by Charles Prior, the superintendent of the Minneapolis office of the Chicago, Milwaukee, and St. Paul Railroad, or the Milwaukee Road for short, which was presided over by Alexander Mitchell, Charles Prior's boss, who was responsible for the choice of town names. He was born in Aberdeen, Scotland, after which the town of Aberdeen was named. Aberdeen was officially founded on July 6, 1881, the date of the first arrival of a Milwaukee Railroad train. Aberdeen then operated under a city charter granted by the Territorial Legislature in March 1883.
As Aberdeen grew, many businesses and buildings were constructed along the town's Main Street. However, this soon became a problem due to Aberdeen's periodic flooding, which led to it being referred to as "The Town in the Frog Pond". At first, this unique condition presented no problem to the newly constructed buildings because it had not rained very much but, when heavy rains fell, the Pond reappeared and flooded the basements of every building on Main Street, causing many business owners and home owners much turmoil. When this flooding happened, the city had one steam-powered pump that had to be used to dry out the entire area that had been flooded, which would take days, if not weeks – and more often than not, it would have rained again in this time period and caused even more flooding, even in the basements that had already been emptied of the water. When the water was gone from the basements, the city still had to deal with the mud that also resulted from the heavy rains.
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The city decided in 1882 to build an artesian ditch to control the "Frog Pond" effects; the plan was later upgraded and developed into an artesian well in 1884 to combat the heavy rains and keep the basements from flooding. The artesian well was designed by the city engineers to prevent flooding and develop a water system. However, during the digging of the well, the water stream that was found underground was too powerful to be contained. The water came blasting out with violent force and had the entire Main Street submerged in up to four feet of water. The engineers realized the previous flaws of the artesian well plan and soon added a gate valve to the well to control the flow of water, giving Aberdeen its first working water supply.
Aberdeen had four different railroad companies with depots built in the newly developing town. With these four railroads intersecting here, Aberdeen soon became known as the "Hub City of the Dakotas". When looking down on Aberdeen from above, the railroad tracks converging in Aberdeen resembled the spokes of a wheel converging at a hub, hence the name "Hub City of the Dakotas". These four railroad companies are the reason why Aberdeen was able to grow and flourish as it did. The only railroad still running through Aberdeen is the BNSF Railway.
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L. Frank Baum, who was later author of the book "The Wonderful Wizard of Oz" and its many sequels, lived here with his wife and children from 1888 to 1891. He ran a fancy goods store, Baum's Bazaar, for over a year, which failed. He later published one of the city's then nine newspapers, where he used his editorials to campaign for women's suffrage (a suffrage amendment to the new South Dakota constitution was on the ballot at the time). The city's small amusement park has some features reflective of the Oz series. After his sojourn in Aberdeen, he moved to Chicago in 1892.
Five sitting Presidents of the United States have visited Aberdeen: William McKinley in 1899, Theodore Roosevelt in 1903, William Howard Taft in 1911, Franklin D. Roosevelt in 1936, and George W. Bush in 2002.
Geography.
Aberdeen is located in northeastern South Dakota, in the James River valley, approximately west of the river. The James River enters northeastern South Dakota in Brown County, where it is dammed to form two reservoirs northeast of Aberdeen. The city is bisected by "Moccasin Creek", a slow-moving waterway which flows south and then northeast to the James River.
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According to the United States Census Bureau, the city has a total area of , of which is land and is water.
Climate.
Aberdeen experiences a humid continental climate (Köppen "Dfa") influenced by its position far from moderating bodies of water. This brings four distinct seasons, a phenomenon that is characterized by hot, relatively humid summers and cold, dry winters, and it lies in USDA Hardiness Zone 4b. The monthly daily average temperature ranges from in January to in July, while there are 16 days of + highs and 38 days with sub- lows annually. Snowfall occurs mostly in light to moderate amounts during the winter, totaling . Precipitation, at annually, is concentrated in the warmer months. Extreme temperatures have ranged from on January 12, 1912, and February 8, 1895, to on July 6 and 15, 1936, although a reading occurred as recently as January 15, 2009.
Demographics.
Aberdeen is the principal city of the Aberdeen Micropolitan Statistical Area, which includes all of Brown and Edmunds counties and has a population of 42,287 in 2020.
2020 census.
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As of the census of 2020, there were 28,495 people and 12,114 households in the city.
2010 census.
As of the census of 2010, there were 26,091 people, 11,418 households and 6,354 families residing in the city. The population density was . There were 12,158 housing units at an average density of . The racial make-up was 91.8% White, 0.7% African American, 3.6% Native American, 1.3% Asian, 0.2% Pacific Islander, 0.5% from other races and 2.0% from two or more races. Hispanic or Latino of any race were 1.6% of the population.
There were 11,418 households, of which 27.1% had children under the age of 18 living with them, 42.1% were married couples living together, 9.5% had a female householder with no husband present, 4.0% had a male householder with no wife present, and 44.4% were non-families. 36.9% of all households were made up of individuals, and 13.1% had someone living alone who was 65 years of age or older. The average household size was 2.18 and the average family size was 2.86.
The median age was 36.4 years. 22.2% of residents were under the age of 18; 12.8% were between the ages of 18 and 24; 24.1% were from 25 to 44; 24.4% were from 45 to 64; and 16.4% were 65 years of age or older. The gender make-up of the city was 47.6% male and 52.4% female.
2000 census.
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As of the census of 2000, there were 24,658 people, 10,553 households and 6,184 families residing in the city. The population density was . There were 11,259 housing units at an average density of . The racial make-up of the city was 94.61% White, 0.37% Black or African American, 3.17% Native American, 0.54% Asian, 0.13% Pacific Islander, 0.19% from other races and 0.99% from two or more races. 0.79% of the population were Hispanic or Latino of any race. 53.7% were of German, 15% Norwegian and 8.5% Irish ancestry.
There were 10,553 households, of which 27.3% had children under the age of 18 living with them, 47.0% were married couples living together, 8.9% had a female householder with no husband present, and 41.4% were non-families. 34.9% of all households were made up of individuals, and 13.6% had someone living alone who was 65 years of age or older. The average household size was 2.21 and the average family size was 2.86.
21.8% of the population were under the age of 18, 14.1% from 18 to 24, 26.4% from 25 to 44, 20.4% from 45 to 64, and 17.2% were 65 years of age or older. The median age was 36 years. For every 100 females, there were 89.2 males. For every 100 females age 18 and over, there were 85.3 males.
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The median household income was $33,276 and the median family income was $43,882. Males had a median income of $30,355 and females $20,092. The per capita income was $17,923. About 7.6% of families and 10.5% of the population were below the poverty line, including 10.6% of those under age 18 and 10.1% of those age 65 or over.
Religion.
There are several Roman Catholic, Baptist, Presbyterian, Methodist, Pentecostal, Lutheran, Church of Jesus Christ of Latter-day Saints, Nazarere, and Non-denominational churches in the area, as well as one synagogue.
Economy.
Super 8 Motels.
Super 8 Motels was founded in 1972 by Dennis Brown and Ron Rivett as a motel referral system, which was replaced with a franchise operation in 1973. The first Super 8, with 60 rooms, was opened in 1974 in Aberdeen and still operates today as the Super 8 Aberdeen East.
Arts and culture.
The Aberdeen Area Arts Council publishes a small monthly newspaper, "ARTiFACTS", with information on area events.
The Aberdeen Community Theatre was created in 1979 and performs at the Capitol Theatre in downtown Aberdeen. The Capitol Theatre opened in 1927 and donated to the Aberdeen Community Theatre in 1991; since then more than $963,000 has been spent on renovating and preserving the historical aspect of the Capitol Theatre. Today, the Aberdeen Community Theatre performs five mainstage productions and three youth productions per year.
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The South Dakota Film Festival established in 2007 is held annually in the fall. The festival has been host to Kevin Costner, Graham Greene, Adam Greenberg, CSA and many more stars of film and television. The festival's first feature film screened was "Into The Wild", shot partially in SD. The festival is held at the historic Capitol Theatre.
The Northern State University Theater Department puts on plays during the school year.
There are four galleries in Aberdeen: Presentation College's Wein Gallery, Northern State University's Lincoln Gallery, the Aberdeen Recreation & Cultural Center (ARCC) Gallery and the ArtWorks Cooperative Gallery located in The Aberdeen Mall.
Sports.
Bowling.
The Village Bowl in Aberdeen is a modern bowling center with multiple lanes. Located at 1314 8th Ave NW.
Minor league baseball.
Aberdeen has had three minor league baseball teams since 1920. The Aberdeen Boosters, a class D league team, played in 1920, the Aberdeen Grays, also a class D team, played from 1921 to 1923. The class C Aberdeen Pheasants from 1946 to 1971, and 1995 to 1997. The Pheasants were the affiliate of the former St. Louis Browns (and current Baltimore Orioles). Aberdeen was a stop to the majors for such notable players as Don Larsen (perfect game in the World Series), Lou Piniella (AL rookie of the year with Kansas City Royals in 1969), and Jim Palmer, Baseball Hall of Fame pitcher for the Baltimore Orioles. In the 1960's, the Pheasants were Coached by Cal Ripken, Sr, who later ended up being a Major League Coach and had two sons Cal, Jr. and Billy that also played for the Orioles organization.
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On June 8, 2024, the first SABR Historical Marker in the state of South Dakota was revealed on the campus of Northern State University. It was the 60th anniversary to the day when the Baltimore Orioles played an exhibition game at the ballpark.
Tennis.
Aberdeen has 19 public tennis courts throughout the city – Melgaard Park (4), Northern State University (6), and Holgate Middle School (8).
Golf.
Aberdeen has three golf courses: Lee Park Municipal Golf Course, Moccasin Creek Country Club and Rolling Hills Country Club. Lee Park and Moccasin Creek are both 18-hole courses. Rolling Hills is a combined nine-hole course and housing development which opened in 2005.
Hockey/ice skating.
Aberdeen has several outdoor skating rinks and hockey rinks open to the public during winter months. Aberdeen is also home to the NAHL team, Aberdeen Wings.
Skateboarding/rollerblading.
Aberdeen has a skate park located between East Melgaard Road and 17th Ave SE at Melgaard Park. The equipment installed includes a quarter pipe, penalty box with half pyramid, bank ramp, spine, kinked rail and a ground rail.
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Disc golf.
Aberdeen has two disc golf courses, Melgaard Park, and the Richmond Lake Disc Golf Course.
Roller Derby.
Aberdeen has an All-women's Roller Derby league "A-Town Roller Girlz" established in 2011, also bringing Junior Roller Derby to the area.
Parks and recreation.
Aberdeen Family YMCA.
The full service YMCA includes an aquatic center with a competitive size lap pool, zero depth entry recreation pool with play features and hot tub. There are three gyms one of which has a climbing wall. There are two racquetball courts. Saunas and steam rooms are in the men's and women's locker rooms. Over 100 group fitness classes are offered each week with child watch available (short term childcare). A wellness center that has cardio equipment, weight machines and free weights.
Family Aquatic Center.
Completed in the summer of 2007, this complex includes a zero entry pool, competition lap pool, lazy river, numerous water slides, play sand area, and a concession area.
Wylie Park Recreation Area.
Wylie Park Recreation Area features go-kart racing, sand volleyball courts, access to Wylie Lake, camping area, picnic areas, and is connected to Storybook Land. Wylie Lake is a small man-made lake, open in the summer months for swimming, lying on the beach, and paddle boating.
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Storybook Land.
Storybook Land is a park with attractions from several different children's storybooks. The park contains a castle, as well as a train that takes visitors through the park. There are two barns which contain petting zoos. Humpty Dumpty's Great Fall Roller Coaster was added to the park, summer 2015. Newly added is the Land of Oz, that features characters and attractions from L. Frank Baum's "The Wonderful Wizard of Oz". Baum was a resident of Aberdeen in the 1880s. He left after a severe drought led to the failure first of his variety store Baum's Bazaar, and then to his newspaper "The Aberdeen Saturday Pioneer", where he wrote an opinion column titled "Our Landlady".
Kuhnert Arboretum.
The Kuhnert Arboretum provides many new learning experiences for the residents of the Aberdeen area, including school-aged children. The Arboretum offers environmental education, a children's area, rose garden collection, recreational trails and much more.
Richmond Lake Recreation Area.
The Richmond Lake Recreation Area is used by all types of outdoors enthusiasts. Three separate areas in this park cater to the needs of campers, swimmers, naturalists, boaters and anglers. Campers stay in the South Unit, while the Forest Drive Unit is a great place for wildlife viewing. The Boat Ramp Unit provides access to the more than lake.
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Richmond Lake Recreation Area's small campground offers a quiet camping experience. The park also features a wheelchair accessible camping cabin.
The park's extensive trail system features over of trails, including both accessible and interpretive trails. Hikers, bikers, and horseback riders can observe the abundance of prairie plants and wildlife of the area up-close.
The park has multiple private and public boat ramps as well as an accessible fishing dock. Richmond Lake has a population of walleye, northern pike, bass, perch, crappie, bluegill, catfish, and bullheads within its waters. An entrance fee is required to gain access to the water and park itself.
Government.
Aberdeen is the center of government for Brown County. City government is overseen by a City Manager/Council form of government with a mayor and eight council members. The City Manager is Robin Bobzien, and the City Council is composed of Mayor Travis Shaunaman and Council Members Char Liebelt, Rich Ward, Erin Fouberg, Rob Ronayne, Alan Johnson, Tiffany Langer, David Novstup and Justin Reinbold. Each council member serves a five-year term.
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