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| [[File:poissonspot setup treisinger.jpg||400px|thumb|right|Arago spot experiment. A point source illuminates a circular object, casting a shadow on a screen. At the shadow's center a bright spot appears due to [[diffraction]], contradicting the prediction of [[geometric optics]].]]
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| In [[optics]], an '''Arago spot''', '''Fresnel bright spot''', or '''Poisson spot''' is a bright point that appears at the center of a circular object's [[shadow]] due to [[Fresnel diffraction]].<ref name="pedrotti2007" /><ref name="walker2008" /><ref name="ohanian1989" /><ref name="hecht2002" /> This spot played an important role in the discovery of the [[wave nature]] of [[light]] (see history section below) and is a common way to demonstrate that light behaves as a wave for example in undergraduate physics laboratory exercises. The basic experimental setup is shown in the figure on the right. The light must come from a "point source" such as an illuminated pinhole, or a diverging [[laser beam]]. The dimensions of the setup must comply with the requirements for [[Fresnel diffraction]]. Namely, the [[Fresnel number]] must satisfy
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| : <math>F = \frac{d^{2}}{l \lambda} \gtrsim 1</math>
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| where
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| : ''d'' is the diameter of the circular object
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| : ''l'' is the distance between the object and the screen
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| : ''λ'' the wavelength of the source
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| Finally, the edge of the circular object must be sufficiently smooth. These conditions together explain why the bright spot is not encountered in everyday life. However, with the abundance of [[laser|laser sources]] available today it is easy to perform an Arago spot experiment (see for example [http://www.princeton.edu/~rvdb/images/Questar/PoissonSpot.html here]). In [[astronomy]], the Arago spot can be also easily observed in the strongly defocussed image of a [[star]] in a [[Newtonian telescope]]. There the star provides an almost ideal [[point source]] at infinity and the [[secondary mirror]] of the telescope constitutes the circular obstacle.
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| The presence of the Arago spot can be easily understood. When light shines on a circular obstacle, [[Huygens' principle]] says that every point in the plane of the obstacle acts as a new point source of light. The light coming from points on the [[circumference]] of the obstacle, and going to the center of the shadow, travels exactly the same distance; so all the light passing close by the object arrives at the screen in [[phase (waves)|phase]] and constructively [[Interference (wave propagation)|interferes]]. This results in a bright spot at the shadow's center, where [[geometrical optics]] and [[particle theory of light|particle theories of light]] predict that there should be no light at all.
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| ==History==
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| The original Arago spot experiment was carried out in the beginning of the 19th century and was the deciding experiment on the question of whether light is a particle or a wave. It is thus a great example of a so-called ''[[experimentum crucis]]''. It only turned out much later (in one of [[Einstein]]'s [[Annus Mirabilis papers|''Annus Mirabilis'' papers]]) that light can be equally described as a particle ([[wave-particle duality]] of light).
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| At the beginning of the 19th century it became more and more evident that light does not simply propagate along straight lines ([[Thomas Young (scientist)|Thomas Young]] published his [[Young's Double Slit Interferometer|double-slit experiment]] in 1807 <ref name="young1807"/>).
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| However, many still favored Isaac Newton's corpuscular theory of light, among them the great theoretician [[Siméon Denis Poisson]].<ref name="newton1704"/> In 1818 the [[French Academy of Sciences]] launched therefore a competition to explain the properties of light, where Poisson was one of the members of the judging committee. The civil engineer [[Augustin-Jean Fresnel]] entered this competition by submitting a new [[wave theory of light]].<ref name="fresnel1868"/> Poisson studied Fresnel's theory in detail and of course looked for a way to prove it wrong being a supporter of the particle-theory of light. Poisson thought that he had found a flaw when he argued that a consequence of Fresnel’s theory was that there would exist an on-axis bright spot in the shadow of a circular obstacle, where there should be complete darkness according to the particle-theory of light. As mentioned before the Arago spot is not easily observed in every-day situations, so it was only natural for Poisson to interpret it as an absurd result and that it should disprove Fresnel's theory.
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| However, the head of the committee, [[François Arago|Dominique-François-Jean Arago]], and who incidentally later became Prime Minister of France, decided to perform the experiment in more detail. He molded a 2 mm metallic disk to a glass plate with wax.<ref name="fresnel1868_arago"/> To everyone's surprise he succeeded in observing the predicted spot, which convinced most scientists of the wave-nature of light. In the end Fresnel won the competition, much to Poisson's chagrin.
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| Arago later noted that the phenomenon (which was later to be
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| known as Poisson’s Spot or the Spot of Arago) had already
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| been observed by [[Joseph-Nicolas_Delisle|Delisle]] <ref name="delisle1715"/> and [[Giacomo_F._Maraldi|Maraldi]]<ref name="maraldi1723"/> a century earlier.
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| ==Theory==
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| [[File:huygensfresnelintegral.jpg||300px|thumb|right|Notation for calculating the wave amplitude at point P<sub>1</sub> from a spherical point source at P<sub>0</sub>.]]
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| At the heart of Fresnel's wave theory is the [[Huygens-Fresnel principle]], which states that every unobstructed point of a wavefront becomes the source of a secondary spherical [[wavelet]] and that the amplitude of the optical field ''E'' at a point on the screen is given by the superposition of all those secondary wavelets taking into account their relative phases.<ref name="sommerfeld"/> This means that the field at a point P<sub>1</sub> on the screen is given by a surface integral:
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| :<math>
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| U(P_1) = \frac{A e^{\mathbf{i} k r_0}}{r_0} \int_S \frac{e^{\mathbf{i} k r_1}}{r_1} K(\chi) dS,
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| </math>
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| where the inclination factor <math>K(\chi)</math> which ensures that the secondary wavelets do not propagate backwards is given by
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| :<math>
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| K(\chi) = \frac{\mathbf{i}}{2 \lambda} (1 + \cos(\chi))
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| </math>
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| and
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| : ''A'' is the amplitude of the source wave
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| : <math>k = \frac{2\pi}{\lambda}</math> is the [[wavenumber]]
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| : ''S'' is the unobstructed surface.
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| The first term outside of the integral represents the oscillations from the source wave at a distance ''r''<sub>0</sub>. Similarly, the term inside the integral represents the oscillations from the secondary wavelets at distances ''r''<sub>1</sub>.
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| In order to derive the intensity behind the circular obstacle using this integral one assumes that the experimental parameters fulfill the requirements of the [[Fresnel diffraction|near-field diffraction]] regime (the size of the circular obstacle is large compared to the wavelength and small compared to the distances ''g''=P<sub>0</sub>C and ''b''=CP<sub>1</sub>). Going to [[polar coordinates]] then yields the integral for a circular object of radius a (see for example Born and Wolf<ref name="bornwolf"/>):
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| :<math>
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| U(P_1) = - \frac{\mathbf{i}}{\lambda} \frac{A e^{\mathbf{i} k (g+b)}}{g b} 2\pi \int_a^{\infty} e^{\mathbf{i} k \frac{1}{2} (\frac{1}{g} + \frac{1}{b})r^2} r dr.
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| </math>
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| [[File:poissonspotintensity.jpg||300px|thumb|right|The on-axis intensity at the center of the shadow of a small circular obstacle converges to the unobstructed intensity.]]
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| This integral can be solved numerically (see below). If ''g'' is large and ''b'' is small so that the angle <math>\chi</math> is not negligible one can write the integral for the on-axis case (P<sub>1</sub> is at the center of the shadow) as (see <ref name="sommerfeldp186"/>):
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| :<math>
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| U(P_1) = \frac{A e^{\mathbf{i} k g}}{g} \frac{b}{\sqrt{b^2+a^2}} e^{\mathbf{i} k \sqrt{b^2+a^2}}.
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| </math>
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| The source [[Intensity (physics)|intensity]], which is the square of the field amplitude, is <math>I_0=\left|\frac{A e^{\mathbf{i} k g}}{g}\right|^2</math> and the intensity at the screen <math>I = \left | U(P_1) \right |^2</math>. The on-axis intensity as a function of the distance ''b'' is hence given by:
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| :<math>I = \frac{b^2}{b^2+a^2} I_0.</math>
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| This shows that the on-axis intensity at the center of the shadow tends to the source intensity, as if the circular object was not present at all. Furthermore, this means that the Arago spot is present even just a few obstacle diameters behind the disc.
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| ===Calculation of diffraction images===
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| To calculate the full diffraction image that is visible on the screen one has to consider the surface integral of the previous section. One cannot exploit circular symmetry anymore, since the line between the source and an arbitrary point on the screen does not pass through the center of the circular object. With the aperture function <math>g(r,\theta)</math> which is 1 for transparent parts of the object plane and 0 otherwise (i.e. It is 0 if the direct line between source and the point on the screen passes through the blocking circular object.) the integral that needs to be solved is given by:
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| :<math>
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| U(P_1) \propto \int_0^{2\pi} \int_0^{\infty} g(r,\theta) e^{\frac{\mathbf{i} \pi \rho^2}{\lambda} \left( \frac{1}{g} + \frac{1}{b} \right)} \rho d\rho d\theta.
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| </math>
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| Numerical calculation of the integral using the [[trapezoidal rule]] or [[Simpson's rule]] is not efficient and becomes numerically unstable especially for configurations with large [[Fresnel number]]. However, it is possible to solve the radial part of the integral so that only the integration over the azimuth angle remains to be done numerically.<ref name="dauger"/> For a particular angle one must solve the line integral for the ray with origin at the intersection point of the line P<sub>0</sub>P<sub>1</sub> with the circular object plane. The contribution for a particular ray with azimuth angle <math>\theta_1</math> and passing a transparent part of the object plane from <math>r=s</math> to <math>r=t</math> is:
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| :<math>
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| R(\theta_1) \propto e^{\pi \mathbf{i} s^2/2} - e^{\pi \mathbf{i} t^2/2}.
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| </math>
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| So for each angle one has to compute the intersection point(''s'') of the ray with the circular object and then sum the contributions <math>I(\theta_1)</math> for a certain number of angles between 0 and <math>2\pi</math>. Results of such a calculation are shown in the following images.
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| [[File:poissonspot simulation d4mm.jpg|200px]]
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| [[File:poissonspot simulation d2mm.jpg|200px]]
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| [[File:poissonspot simulation d1mm.jpg|200px]]
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| The images show simulated Arago spots in the shadow of a disc of varying diameter (4 mm, 2 mm, 1 mm – left to right) at a distance of 1 m from the disc. The point source has a wavelength of 633 nm (e.g. He-Ne Laser) and is located 1 m from the disc. The image width corresponds to 16 mm.
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| ==Experimental aspects==
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| Observation of the Arago spot with a conventional light source can be challenging. This section summarizes how the various experimental parameters affect the visibility of the Arago spot.
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| ===Intensity and size===
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| For an ideal [[point source]] the intensity of the Arago spot equals that of the undisturbed [[wave front]]. Only the width of the Arago spot intensity peak depends on the distances between source, circular object and screen, as well as the source's wavelength and the diameter of the circular object. This is clear from the simulation images above. <!--The shape of the Poisson spot's intensity distribution will in fact be similar for experimental setups with the same Fresnel number.--> This means that one can compensate for a reduction in the source's [[wavelength]] by increasing the distance l between circular object and screen or reducing the circular object's diameter.
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| The lateral intensity distribution on the screen has in fact the shape of a squared [[Bessel function|zeroth Bessel function of the first kind]] when close to the [[optical axis]] and using a [[plane wave|plane wave source]] (point source at infinity):<ref name="harvey1984"/>
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| :<math>
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| U(P_1,r) \propto J_0^2(\frac{\pi r d}{\lambda b})
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| </math>
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| where
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| : ''r'' is the distance of the point <math>P_1</math> on the screen from the optical axis
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| : ''d'' is the diameter of circular object
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| : <math>\lambda</math> is the wavelength
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| : ''b'' is the distance between circular object and screen.
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| The following images show the radial intensity distribution of the simulated Arago spot images above:
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| [[File:poissonspot simulation d4mm lateral.jpg|200px]]
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| [[File:poissonspot simulation d2mm lateral.jpg|200px]]
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| [[File:poissonspot simulation d1mm lateral.jpg|200px]]
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| The red lines in these three graphs correspond to the simulated images above, and the green lines were computed by applying the corresponding parameters to the squared Bessel function given above.
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| ===Finite source size and spatial coherence===
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| The main reason why the Arago spot is hard to observe in circular shadows from conventional light sources is that such light sources are bad approximations of point sources. If the wave source has a finite size ''S'' then the Arago spot will have an extent that is given by ''S''×''b''/''g'', as if the circular object acted like a lens.<ref name="sommerfeld"/> At the same time the intensity of the Arago spot is reduced with respect to the intensity of the undisturbed wave front.
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| ===Deviation from circularity===
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| If the cross-section of the circular object deviates slightly from its circular shape (but it still has a sharp edge on a smaller scale) the shape of the point-source Arago spot changes. In particular, if the object has an ellipsoidal cross-section the Arago spot has the shape of an [[evolute]].<ref name="coulson1922"/> Note that this is only the case if the source is close to an ideal point source. From an extended source the Arago spot is only affected marginally, since one can interpret the Arago spot as a [[point-spread function]]. And so the image of the extended source only becomes washed out due to the convolution with the point-spread function, but it does not decrease in over all intensity.
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| ===The circular object's surface roughness===
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| The Arago spot is very sensitive to small-scale deviations from the ideal circular cross-section. This means that a small amount of surface roughness of the circular object can completely cancel out the bright spot. This is shown in the following three diagrams which are simulations of the Arago spot from a 4 mm diameter disc (''g'' = ''b'' = 1 m):
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| [[File:poissonspot simulation d4mm lateral cor10.jpg|200px]]
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| [[File:poissonspot simulation d4mm lateral cor50.jpg|200px]]
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| [[File:poissonspot simulation d4mm lateral cor100.jpg|200px]]
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| The simulation includes a regular sinusoidal corrugation of the circular shape of amplitude 10 µm, 50 µm and 100 µm, respectively. Note, that the 100 µm edge corrugation almost completely removes the central bright spot.
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| This effect can be best understood using the [[Fresnel zone|Fresnel zone concept]]. The circular object blocks a certain number of Fresnel zones. The Fresnel zone that begins with the edge of the circular object is the only one that contributes to the Arago spot. All the Fresnel zones that are further out destructively [[interference (light)|interfere]] with each other and thus cancel. Random edge corrugation whose amplitude is of the same order as the width of that adjacent Fresnel zone reduces the Arago spot intensity. Contributions from the parts of the edge whose radius has been increased by the corrugation to about the width of the adjacent Fresnel zone now destructively interfere with those contributions from the parts which have not been affected by the corrugation.
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| The adjacent Fresnel zone is approximately given by:<ref name="reisinger2009"/>
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| :<math>
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| \Delta r \approx \sqrt{r^2 + \lambda \frac{g b}{g+b}} - r.
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| </math>
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| The edge corrugation should not be much more than 10% of this width to see a close to ideal Arago spot. In the above simulations with the 4 mm diameter disc the adjacent Fresnel zone has a width of about 77 µm.
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| ==Arago spot with matter waves==
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| Recently, the Arago spot experiment has been demonstrated with a supersonic expansion beam of [[deuterium]] molecules, so-called neutral [[matter waves]].<ref name="reisinger2009"/> Material particles behave like waves as is known from [[quantum mechanics]]. The wave-nature of particles actually dates back to [[Louis de Broglie|de Broglie's]] hypothesis<ref name="debroglie"/> as well as [[Davisson–Germer experiment|Davisson and Germer's experiments]].<ref name="davisson"/> An Arago spot of electrons, which also constitute matter waves, can be observed in [[transmission electron microscope]]s when examining circular structures of a certain size.
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| The observation of an Arago spot with large molecules, thus proving their wave-nature, is a topic of current research.<ref name="reisinger2009"/>
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| ==Other applications==
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| Beside the demonstration of wave-behavior the Arago spot also has a few other applications. One of the ideas is to use the Arago spot as a straight line reference in alignment systems (see [http://www.slac.stanford.edu/econf/C971013/papers/047.PDF Feier et al.]). Another is to use the spot's sensitvity to beam [[optical aberration|aberrations]] to probe aberrations in laser beams.<ref name="harvey1984"/>
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| <ref name="davisson">{{Citation
| |
| | last = Davisson | first = C.
| |
| | last2 = Germer | first2 = L.
| |
| | year = 1927
| |
| | title = Diffraction of Electrons by a Crystal of Nickel
| |
| | journal = Nature
| |
| | volume = 119
| |
| | pages = 558
| |
| |bibcode = 1927Natur.119..558D |doi = 10.1038/119558a0 }}</ref>
| |
| | |
| }}
| |
| | |
| [[Category:Diffraction]]
| |
| [[Category:History of physics]]
| |