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In geometry, the **stereographic projection** is a particular mapping (function) that projects a sphere onto a plane. The projection is defined on the entire sphere, except at one point: the projection point. Where it is defined, the mapping is smooth and bijective. It is conformal, meaning that it preserves angles at which curves meet. It is neither isometric nor area-preserving: that is, it preserves neither distances nor the areas of figures.

- History
- Definition
- First formulation
- Other conventions
- Generalizations
- Properties
- Wulff net
- Applications within mathematics
- Complex analysis
- Visualization of lines and planes
- Other visualization
- Arithmetic geometry
- Tangent half-angle substitution
- Applications to other disciplines
- Cartography
- Planetary science
- Crystallography
- Geology
- Photography
- See also
- References
- Sources
- External links
- Videos
- Software
- Miniplanet panoramas

Intuitively, then, the stereographic projection is a way of picturing the sphere as the plane, with some inevitable compromises. Because the sphere and the plane appear in many areas of mathematics and its applications, so does the stereographic projection; it finds use in diverse fields including complex analysis, cartography, geology, and photography. In practice, the projection is carried out by computer or by hand using a special kind of graph paper called a **stereographic net**, shortened to **stereonet**, or **Wulff net**.

The stereographic projection was known to Hipparchus, Ptolemy and probably earlier to the Egyptians. It was originally known as the planisphere projection.^{ [1] }* Planisphaerium * by Ptolemy is the oldest surviving document that describes it. One of its most important uses was the representation of celestial charts.^{ [1] } The term * planisphere * is still used to refer to such charts.

In the 16th and 17th century, the equatorial aspect of the stereographic projection was commonly used for maps of the Eastern and Western Hemispheres. It is believed that already the map created in 1507 by Gualterius Lud ^{ [2] } was in stereographic projection, as were later the maps of Jean Roze (1542), Rumold Mercator (1595), and many others.^{ [3] } In star charts, even this equatorial aspect had been utilised already by the ancient astronomers like Ptolemy.^{ [4] }

François d'Aguilon gave the stereographic projection its current name in his 1613 work *Opticorum libri sex philosophis juxta ac mathematicis utiles* (Six Books of Optics, useful for philosophers and mathematicians alike).^{ [5] }

In the late 16th century, Thomas Harriot proved that the stereographic projection is conformal; however, this proof was never published and sat among his papers in a box for more than three centuries.^{ [6] } In 1695, Edmond Halley, motivated by his interest in star charts, was the first to publish a proof.^{ [7] } He used the recently established tools of calculus, invented by his friend Isaac Newton.

The unit sphere *S*^{2} in three-dimensional space **R**^{3} is the set of points (*x*, *y*, *z*) such that *x*^{2} + *y*^{2} + *z*^{2} = 1. Let *N* = (0, 0, 1) be the "north pole", and let *M* be the rest of the sphere. The plane *z* = 0 runs through the center of the sphere; the "equator" is the intersection of the sphere with this plane.

For any point *P* on *M*, there is a unique line through *N* and *P*, and this line intersects the plane *z* = 0 in exactly one point *P′*, known as the **stereographic projection** of *P* onto the plane.

In Cartesian coordinates (*x*, *y*, *z*) on the sphere and (*X*, *Y*) on the plane, the projection and its inverse are given by the formulas

In spherical coordinates (*φ*, *θ*) on the sphere (with *φ* the zenith angle, 0 ≤ *φ* ≤ π, and *θ* the azimuth, 0 ≤ *θ* ≤ 2π) and polar coordinates (*R*, *Θ*) on the plane, the projection and its inverse are

Here, *φ* is understood to have value π when *R* = 0. Also, there are many ways to rewrite these formulas using trigonometric identities. In cylindrical coordinates (*r*, *θ*, *z*) on the sphere and polar coordinates (*R*, *Θ*) on the plane, the projection and its inverse are

Some authors^{ [8] } define stereographic projection from the north pole (0, 0, 1) onto the plane *z* = −1, which is tangent to the unit sphere at the south pole (0, 0, −1). The values *X* and *Y* produced by this projection are exactly twice those produced by the equatorial projection described in the preceding section. For example, this projection sends the equator to the circle of radius 2 centered at the origin. While the equatorial projection produces no infinitesimal area distortion along the equator, this pole-tangent projection instead produces no infinitesimal area distortion at the south pole.

Other authors^{ [9] } use a sphere of radius 1/2 and the plane *z* = −1/2. In this case the formulae become

In general, one can define a stereographic projection from any point *Q* on the sphere onto any plane *E* such that

*E*is perpendicular to the diameter through*Q*, and*E*does not contain*Q*.

As long as *E* meets these conditions, then for any point *P* other than *Q* the line through *P* and *Q* meets *E* in exactly one point *P′*, which is defined to be the stereographic projection of *P* onto *E*.^{ [10] }

More generally, stereographic projection may be applied to the unit *n*-sphere *S*^{n} in (*n* + 1)-dimensional Euclidean space **E**^{n+1}. If *Q* is a point of *S*^{n} and *E* a hyperplane in **E**^{n+1}, then the stereographic projection of a point *P* ∈ *S*^{n} − {*Q*} is the point *P′* of intersection of the line *QP* with *E*. In Cartesian coordinates (*x*_{i}, *i* from 0 to *n*) on *S*^{n} and (*X*_{i}, *i* from 1 to *n*) on *E*, the projection from *Q* = (1, 0, 0, ..., 0) ∈ *S*^{n} is given by

Defining

the inverse is given by

Still more generally, suppose that *S* is a (nonsingular) quadric hypersurface in the projective space **P**^{n+1}. In other words, *S* is the locus of zeros of a non-singular quadratic form *f*(*x*_{0}, ..., *x*_{n+1}) in the homogeneous coordinates *x*_{i}. Fix any point *Q* on *S* and a hyperplane *E* in **P**^{n+1} not containing *Q*. Then the stereographic projection of a point *P* in *S* − {*Q*} is the unique point of intersection of *QP* with *E*. As before, the stereographic projection is conformal and invertible outside of a "small" set. The stereographic projection presents the quadric hypersurface as a rational hypersurface.^{ [11] } This construction plays a role in algebraic geometry and conformal geometry.

The first stereographic projection defined in the preceding section sends the "south pole" (0, 0, −1) of the unit sphere to (0, 0), the equator to the unit circle, the southern hemisphere to the region inside the circle, and the northern hemisphere to the region outside the circle.

The projection is not defined at the projection point *N* = (0, 0, 1). Small neighborhoods of this point are sent to subsets of the plane far away from (0, 0). The closer *P* is to (0, 0, 1), the more distant its image is from (0, 0) in the plane. For this reason it is common to speak of (0, 0, 1) as mapping to "infinity" in the plane, and of the sphere as completing the plane by adding a point at infinity. This notion finds utility in projective geometry and complex analysis. On a merely topological level, it illustrates how the sphere is homeomorphic to the one-point compactification of the plane.

In Cartesian coordinates a point *P*(*x*, *y*, *z*) on the sphere and its image *P′*(*X*, *Y*) on the plane either both are rational points or none of them:

Stereographic projection is conformal, meaning that it preserves the angles at which curves cross each other (see figures). On the other hand, stereographic projection does not preserve area; in general, the area of a region of the sphere does not equal the area of its projection onto the plane. The area element is given in (*X*, *Y*) coordinates by

Along the unit circle, where *X*^{2} + *Y*^{2} = 1, there is no inflation of area in the limit, giving a scale factor of 1. Near (0, 0) areas are inflated by a factor of 4, and near infinity areas are inflated by arbitrarily small factors.

The metric is given in (*X*, *Y*) coordinates by

and is the unique formula found in Bernhard Riemann's *Habilitationsschrift* on the foundations of geometry, delivered at Göttingen in 1854, and entitled *Über die Hypothesen welche der Geometrie zu Grunde liegen*.

No map from the sphere to the plane can be both conformal and area-preserving. If it were, then it would be a local isometry and would preserve Gaussian curvature. The sphere and the plane have different Gaussian curvatures, so this is impossible.

Circles on the sphere that do *not* pass through the point of projection are projected to circles on the plane.^{ [12] }^{ [13] } Circles on the sphere that *do* pass through the point of projection are projected to straight lines on the plane. These lines are sometimes thought of as circles through the point at infinity, or circles of infinite radius. These properties can be verified by using the expressions of in terms of given in § First formulation: using these expressions for a substitution in the equation of the plane containing a circle on the sphere, and clearing denominators, one gets the equation of a circle, that is, a second-degree equation with as its quadratic part. The equation becomes linear if that is, if the plane passes through the point of projection.

All lines in the plane, when transformed to circles on the sphere by the inverse of stereographic projection, meet at the projection point. Parallel lines, which do not intersect in the plane, are transformed to circles tangent at projection point. Intersecting lines are transformed to circles that intersect transversally at two points in the sphere, one of which is the projection point. (Similar remarks hold about the real projective plane, but the intersection relationships are different there.)

The loxodromes of the sphere map to curves on the plane of the form

where the parameter *a* measures the "tightness" of the loxodrome. Thus loxodromes correspond to logarithmic spirals. These spirals intersect radial lines in the plane at equal angles, just as the loxodromes intersect meridians on the sphere at equal angles.

The stereographic projection relates to the plane inversion in a simple way. Let *P* and *Q* be two points on the sphere with projections *P′* and *Q′* on the plane. Then *P′* and *Q′* are inversive images of each other in the image of the equatorial circle if and only if *P* and *Q* are reflections of each other in the equatorial plane.

In other words, if:

*P*is a point on the sphere, but not a 'north pole'*N*and not its antipode, the 'south pole'*S*,*P′*is the image of*P*in a stereographic projection with the projection point*N*and*P″*is the image of*P*in a stereographic projection with the projection point*S*,

then *P′* and *P″* are inversive images of each other in the unit circle.

Stereographic projection plots can be carried out by a computer using the explicit formulas given above. However, for graphing by hand these formulas are unwieldy. Instead, it is common to use graph paper designed specifically for the task. This special graph paper is called a **stereonet** or **Wulff net**, after the Russian mineralogist George (Yuri Viktorovich) Wulff.^{ [14] }

The Wulff net shown here is the stereographic projection of the grid of parallels and meridians of a hemisphere centred at a point on the equator (such as the Eastern or Western hemisphere of a planet).

In the figure, the area-distorting property of the stereographic projection can be seen by comparing a grid sector near the center of the net with one at the far right or left. The two sectors have equal areas on the sphere. On the disk, the latter has nearly four times the area of the former. If the grid is made finer, this ratio approaches exactly 4.

On the Wulff net, the images of the parallels and meridians intersect at right angles. This orthogonality property is a consequence of the angle-preserving property of the stereoscopic projection. (However, the angle-preserving property is stronger than this property. Not all projections that preserve the orthogonality of parallels and meridians are angle-preserving.)

For an example of the use of the Wulff net, imagine two copies of it on thin paper, one atop the other, aligned and tacked at their mutual center. Let *P* be the point on the lower unit hemisphere whose spherical coordinates are (140°, 60°) and whose Cartesian coordinates are (0.321, 0.557, −0.766). This point lies on a line oriented 60° counterclockwise from the positive *x*-axis (or 30° clockwise from the positive *y*-axis) and 50° below the horizontal plane *z* = 0. Once these angles are known, there are four steps to plotting *P*:

- Using the grid lines, which are spaced 10° apart in the figures here, mark the point on the edge of the net that is 60° counterclockwise from the point (1, 0) (or 30° clockwise from the point (0, 1)).
- Rotate the top net until this point is aligned with (1, 0) on the bottom net.
- Using the grid lines on the bottom net, mark the point that is 50° toward the center from that point.
- Rotate the top net oppositely to how it was oriented before, to bring it back into alignment with the bottom net. The point marked in step 3 is then the projection that we wanted.

To plot other points, whose angles are not such round numbers as 60° and 50°, one must visually interpolate between the nearest grid lines. It is helpful to have a net with finer spacing than 10°. Spacings of 2° are common.

To find the central angle between two points on the sphere based on their stereographic plot, overlay the plot on a Wulff net and rotate the plot about the center until the two points lie on or near a meridian. Then measure the angle between them by counting grid lines along that meridian.

- Two points
*P*_{1}and*P*_{2}are drawn on a transparent sheet tacked at the origin of a Wulff net. - The transparent sheet is rotated and the central angle is read along the common meridian to both points
*P*_{1}and*P*_{2}.

Although any stereographic projection misses one point on the sphere (the projection point), the entire sphere can be mapped using two projections from distinct projection points. In other words, the sphere can be covered by two stereographic parametrizations (the inverses of the projections) from the plane. The parametrizations can be chosen to induce the same orientation on the sphere. Together, they describe the sphere as an oriented surface (or two-dimensional manifold).

This construction has special significance in complex analysis. The point (*X*, *Y*) in the real plane can be identified with the complex number *ζ* = *X* + i*Y*. The stereographic projection from the north pole onto the equatorial plane is then

Similarly, letting *ξ* = *X* − i*Y* be another complex coordinate, the functions

define a stereographic projection from the south pole onto the equatorial plane. The transition maps between the *ζ*- and *ξ*-coordinates are then *ζ* = 1/*ξ* and *ξ* = 1/*ζ*, with *ζ* approaching 0 as *ξ* goes to infinity, and *vice versa*. This facilitates an elegant and useful notion of infinity for the complex numbers and indeed an entire theory of meromorphic functions mapping to the Riemann sphere. The standard metric on the unit sphere agrees with the Fubini–Study metric on the Riemann sphere.

The set of all lines through the origin in three-dimensional space forms a space called the real projective plane. This plane is difficult to visualize, because it cannot be embedded in three-dimensional space.

However, one can visualize it as a disk, as follows. Any line through the origin intersects the southern hemisphere *z* ≤ 0 in a point, which can then be stereographically projected to a point on a disk in the XY plane. Horizontal lines through the origin intersect the southern hemisphere in two antipodal points along the equator, which project to the boundary of the disk. Either of the two projected points can be considered part of the disk; it is understood that antipodal points on the equator represent a single line in 3 space and a single point on the boundary of the projected disk (see quotient topology). So any set of lines through the origin can be pictured as a set of points in the projected disk. But the boundary points behave differently from the boundary points of an ordinary 2-dimensional disk, in that any one of them is simultaneously close to interior points on opposite sides of the disk (just as two nearly horizontal lines through the origin can project to points on opposite sides of the disk).

Also, every plane through the origin intersects the unit sphere in a great circle, called the *trace* of the plane. This circle maps to a circle under stereographic projection. So the projection lets us visualize planes as circular arcs in the disk. Prior to the availability of computers, stereographic projections with great circles often involved drawing large-radius arcs that required use of a beam compass. Computers now make this task much easier.

Further associated with each plane is a unique line, called the plane's *pole*, that passes through the origin and is perpendicular to the plane. This line can be plotted as a point on the disk just as any line through the origin can. So the stereographic projection also lets us visualize planes as points in the disk. For plots involving many planes, plotting their poles produces a less-cluttered picture than plotting their traces.

This construction is used to visualize directional data in crystallography and geology, as described below.

Stereographic projection is also applied to the visualization of polytopes. In a Schlegel diagram, an *n*-dimensional polytope in **R**^{n+1} is projected onto an *n*-dimensional sphere, which is then stereographically projected onto **R**^{n}. The reduction from **R**^{n+1} to **R**^{n} can make the polytope easier to visualize and understand.

In elementary arithmetic geometry, stereographic projection from the unit circle provides a means to describe all primitive Pythagorean triples. Specifically, stereographic projection from the north pole (0,1) onto the *x*-axis gives a one-to-one correspondence between the rational number points (*x*, *y*) on the unit circle (with *y* ≠ 1) and the rational points of the *x*-axis. If (*m*/*n*, 0) is a rational point on the *x*-axis, then its inverse stereographic projection is the point

which gives Euclid's formula for a Pythagorean triple.

The pair of trigonometric functions (sin *x*, cos *x*) can be thought of as parametrizing the unit circle. The stereographic projection gives an alternative parametrization of the unit circle:

Under this reparametrization, the length element *dx* of the unit circle goes over to

This substitution can sometimes simplify integrals involving trigonometric functions.

The fundamental problem of cartography is that no map from the sphere to the plane can accurately represent both angles and areas. In general, area-preserving map projections are preferred for statistical applications, while angle-preserving (conformal) map projections are preferred for navigation.

Stereographic projection falls into the second category. When the projection is centered at the Earth's north or south pole, it has additional desirable properties: It sends meridians to rays emanating from the origin and parallels to circles centered at the origin.

- Stereographic projection of the world north of 30°S. 15° graticule.
- The stereographic projection with Tissot's indicatrix of deformation.

The stereographic is the only projection that maps all circles on a sphere to circles on a plane. This property is valuable in planetary mapping where craters are typical features. The set of circles passing through the point of projection have unbounded radius, and therefore degenerate into lines.

In crystallography, the orientations of crystal axes and faces in three-dimensional space are a central geometric concern, for example in the interpretation of X-ray and electron diffraction patterns. These orientations can be visualized as in the section Visualization of lines and planes above. That is, crystal axes and poles to crystal planes are intersected with the northern hemisphere and then plotted using stereographic projection. A plot of poles is called a **pole figure**.

In electron diffraction, Kikuchi line pairs appear as bands decorating the intersection between lattice plane traces and the Ewald sphere thus providing *experimental access* to a crystal's stereographic projection. Model Kikuchi maps in reciprocal space,^{ [15] } and fringe visibility maps for use with bend contours in direct space,^{ [16] } thus act as road maps for exploring orientation space with crystals in the transmission electron microscope.

Researchers in structural geology are concerned with the orientations of planes and lines for a number of reasons. The foliation of a rock is a planar feature that often contains a linear feature called lineation. Similarly, a fault plane is a planar feature that may contain linear features such as slickensides.

These orientations of lines and planes at various scales can be plotted using the methods of the Visualization of lines and planes section above. As in crystallography, planes are typically plotted by their poles. Unlike crystallography, the southern hemisphere is used instead of the northern one (because the geological features in question lie below the Earth's surface). In this context the stereographic projection is often referred to as the **equal-angle lower-hemisphere projection**. The equal-area lower-hemisphere projection defined by the Lambert azimuthal equal-area projection is also used, especially when the plot is to be subjected to subsequent statistical analysis such as density contouring.

Some fisheye lenses use a stereographic projection to capture a wide-angle view.^{ [17] } Compared to more traditional fisheye lenses which use an equal-area projection, areas close to the edge retain their shape, and straight lines are less curved. However, stereographic fisheye lenses are typically more expensive to manufacture.^{ [18] } Image remapping software, such as Panotools, allows the automatic remapping of photos from an equal-area fisheye to a stereographic projection.

The stereographic projection has been used to map spherical panoramas, starting with Horace Bénédict de Saussure's in 1779. This results in effects known as a *little planet* (when the center of projection is the nadir) and a *tube* (when the center of projection is the zenith).^{ [19] }

The popularity of using stereographic projections to map panoramas over other azimuthal projections is attributed to the shape preservation that results from the conformality of the projection.^{ [19] }

- List of map projections
- Astrolabe
- Astronomical clock
- Poincaré disk model, the analogous mapping of the hyperbolic plane
- Stereographic projection in cartography

In geography, **latitude** is a geographic coordinate that specifies the north–south position of a point on the Earth's surface. Latitude is an angle which ranges from 0° at the Equator to 90° at the poles. Lines of constant latitude, or *parallels*, run east–west as circles parallel to the equator. Latitude is used together with longitude to specify the precise location of features on the surface of the Earth. On its own, the term latitude should be taken to be the *geodetic latitude* as defined below. Briefly, geodetic latitude at a point is the angle formed by the vector perpendicular to the ellipsoidal surface from that point, and the equatorial plane. Also defined are six *auxiliary latitudes* that are used in special applications.

A **sphere** is a geometrical object that is a three-dimensional analogue to a two-dimensional circle. A sphere is the set of points that are all at the same distance *r* from a given point in three-dimensional space. That given point is the centre of the sphere, and *r* is the sphere's radius. The earliest known mentions of spheres appear in the work of the ancient Greek mathematicians.

In mathematics, a **3-sphere** is a higher-dimensional analogue of a sphere. It may be embedded in 4-dimensional Euclidean space as the set of points equidistant from a fixed central point. Analogous to how the boundary of a ball in three dimensions is an ordinary sphere, the boundary of a ball in four dimensions is a 3-sphere. A 3-sphere is an example of a 3-manifold and an *n*-sphere.

The **equatorial coordinate system** is a celestial coordinate system widely used to specify the positions of celestial objects. It may be implemented in spherical or rectangular coordinates, both defined by an origin at the centre of Earth, a fundamental plane consisting of the projection of Earth's equator onto the celestial sphere, a primary direction towards the vernal equinox, and a right-handed convention.

In mechanics and geometry, the **3D rotation group**, often denoted **SO(3)**, is the group of all rotations about the origin of three-dimensional Euclidean space under the operation of composition.

In mathematics, the **complex plane** is the plane formed by the complex numbers, with a Cartesian coordinate system such that the x-axis, called **real axis**, is formed by the real numbers, and the y-axis, called **imaginary axis**, is formed by the imaginary numbers.

In physics and mathematics, the **Lorentz group** is the group of all Lorentz transformations of Minkowski spacetime, the classical and quantum setting for all (non-gravitational) physical phenomena. The Lorentz group is named for the Dutch physicist Hendrik Lorentz.

**Elliptic geometry** is an example of a geometry in which Euclid's parallel postulate does not hold. Instead, as in spherical geometry, there are no parallel lines since any two lines must intersect. However, unlike in spherical geometry, two lines are usually assumed to intersect at a single point. Because of this, the elliptic geometry described in this article is sometimes referred to as *single elliptic geometry* whereas spherical geometry is sometimes referred to as *double elliptic geometry*.

In mathematics, the **open unit disk** around *P*, is the set of points whose distance from *P* is less than 1:

In geometry, **inversive geometry** is the study of *inversion*, a transformation of the Euclidean plane that maps circles or lines to other circles or lines and that preserves the angles between crossing curves. Many difficult problems in geometry become much more tractable when an inversion is applied.

In geometry and complex analysis, a **Möbius transformation** of the complex plane is a rational function of the form

In the mathematical field of differential topology, the **Hopf fibration** describes a 3-sphere in terms of circles and an ordinary sphere. Discovered by Heinz Hopf in 1931, it is an influential early example of a fiber bundle. Technically, Hopf found a many-to-one continuous function from the 3-sphere onto the 2-sphere such that each distinct *point* of the 2-sphere is mapped from a distinct great circle of the 3-sphere. Thus the 3-sphere is composed of fibers, where each fiber is a circle — one for each point of the 2-sphere.

In mathematics, and specifically in potential theory, the **Poisson kernel** is an integral kernel, used for solving the two-dimensional Laplace equation, given Dirichlet boundary conditions on the unit disk. The kernel can be understood as the derivative of the Green's function for the Laplace equation. It is named for Siméon Poisson.

In mathematics, the group of **rotations about a fixed point in four-dimensional Euclidean space** is denoted **SO(4)**. The name comes from the fact that it is the special orthogonal group of order 4.

The **Lambert azimuthal equal-area projection** is a particular mapping from a sphere to a disk. It accurately represents area in all regions of the sphere, but it does not accurately represent angles. It is named for the Swiss mathematician Johann Heinrich Lambert, who announced it in 1772. "Zenithal" being synonymous with "azimuthal", the projection is also known as the **Lambert zenithal equal-area projection**.

In geometry, the **Beltrami–Klein model**, also called the **projective model**, **Klein disk model**, and the **Cayley–Klein model**, is a model of hyperbolic geometry in which points are represented by the points in the interior of the unit disk and lines are represented by the chords, straight line segments with ideal endpoints on the boundary sphere.

**Oblate spheroidal coordinates** are a three-dimensional orthogonal coordinate system that results from rotating the two-dimensional elliptic coordinate system about the non-focal axis of the ellipse, i.e., the symmetry axis that separates the foci. Thus, the two foci are transformed into a ring of radius in the *x*-*y* plane. Oblate spheroidal coordinates can also be considered as a limiting case of ellipsoidal coordinates in which the two largest semi-axes are equal in length.

In general relativity, a point mass deflects a light ray with impact parameter by an angle approximately equal to

In geometry, the **Poincaré disk model**, also called the **conformal disk model**, is a model of 2-dimensional hyperbolic geometry in which all points are inside the unit disk, and straight lines are either circular arcs contained within the disk that are orthogonal to the unit circle or diameters of the unit circle.

In mathematics, the **Riemann sphere**, named after Bernhard Riemann, is a model of the **extended complex plane**: the complex plane plus one point at infinity. This extended plane represents the **extended complex numbers**, that is, the complex numbers plus a value for infinity. With the Riemann model, the point is near to very large numbers, just as the point is near to very small numbers.

- 1 2 Snyder (1993).
- ↑ According to (Snyder 1993), although he acknowledges he did not personally see it
- ↑ Snyder (1989).
- ↑ Brown, Lloyd Arnold :
*The story of maps*, p.59. - ↑ According to (Elkins, 1988) who references Eckert, "Die Kartenwissenschaft", Berlin 1921, pp 121–123
- ↑ Lohne, John (1979). "Essays on Thomas Harriot".
*Archive for History of Exact Sciences*.**20**(3/4): 189–312. doi:10.1007/BF00327737. - ↑ Timothy Feeman. 2002. "Portraits of the Earth: A Mathematician Looks at Maps". American Mathematical Society.
- ↑ Cf. Apostol (1974) p. 17.
- ↑ Gelfand, Minlos & Shapiro 1963
- ↑ Cf. Pedoe (1988).
- ↑ Cf. Shafarevich (1995).
- ↑ Ahlfors, Lars (1966).
*Complex Analysis*. McGraw-Hill, Inc. p. 19. - ↑ Conway, John; Doyle, Peter; Gilman, Jane; Thurston, Bill (1994-04-12), "Stereographic Projection",
*Geometry and the Imagination in Minneapolis*, Minnesota University, archived from the original on 2021-04-19, retrieved 2022-04-26 - ↑ Wulff, George, Untersuchungen im Gebiete der optischen Eigenschaften isomorpher Kristalle: Zeits. Krist.,36, 1–28 (1902)
- ↑ M. von Heimendahl, W. Bell and G. Thomas (1964) Applications of Kikuchi line analyses in electron microscopy,
*J. Appl. Phys.***35**:12, 3614–3616. - ↑ P. Fraundorf, Wentao Qin, P. Moeck and Eric Mandell (2005) Making sense of nanocrystal lattice fringes,
*J. Appl. Phys.***98**:114308. - ↑ Samyang 8 mm f/3.5 Fisheye CS Archived 2011-06-29 at the Wayback Machine
- ↑ "Samyang 8 mm f/3.5 Aspherical IF MC Fish-eye". lenstip.com. Retrieved 2011-07-07.
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*A comprehensive introduction to differential geometry, Volume IV*. Houston, Texas: Publish or Perish. ISBN 0-914098-73-X.

Wikimedia Commons has media related to Stereographic projection .

- Weisstein, Eric W. "Stereographic projection".
*MathWorld*. - Stereographic Projection Archived 2013-03-10 at the Wayback Machine on PlanetMath
- Stereographic Projection and Inversion from Cut-the-Knot
- DoITPoMS Teaching and Learning Package - "The Stereographic Projection"

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