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    • 专利摘要:
    The invention relates to an anastigmat telescope with three aspherical mirrors comprising: - means (5) linear displacement of the third mirror (M3) on the optical axis of the telescope (O) so as to vary the focal length of the telescope in a plurality of focal lengths (fi) between at least a minimum focal length (fmin) and a maximum focal length (fmax), - a plurality of aspheric optical components (CAi) associated respectively with the plurality of focal lengths (fi), -the third mirror presenting a new conicity (c'3) determined from an initial conicity (c3), the new conicity (c'3) being determined so that the telescope has, without the presence of said aspherical components and for the minimum and maximum focal lengths, compensable aberrations by said aspherical components, - the position (PCAi) and the shape of the surface (Si) of each aspherical component being determined so as to correct said compensating aberrations dudi t telescope for the associated focal (fi) and to optimize the image quality in the first focal plane of the telescope according to a predetermined criterion.
    公开号:FR3060136A1
    申请号:FR1700254
    申请日:2017-03-09
    公开日:2018-06-15
    发明作者:Nicolas TETAZ
    申请人:Thales SA；
    IPC主号:
    专利说明:

    The field of the invention is that of telescopes, in particular that of observation telescopes embedded in satellites. More specifically, the field of the invention relates to catoptric systems with large focal lengths.
    STATE OF THE ART
    Current space telescopes are single focal length. A known type of telescope is the Korsh type telescope. The Korsch type telescope, also known as TMA (acronym for the English expression “Three Mirors Anastigmat”) is an anastigmat telescope with three aspherical mirrors (either of the Concave-Convex-Concave type) which comprises at least one first M1 mirror concave, a second convex mirror M2 and a third concave mirror M3. The three mirrors being aspherical and of classical shape for such a telescope. The first, second and third mirrors M1, M2 and M3 are aspherical, of fixed shapes, each mirror being characterized by at least two parameters, a radius of curvature R and a conic c.
    This optical system has an optical axis O well known to those skilled in the art, defined by the radius passing through the center of the entrance pupil Pe and perpendicular to this pupil.
    The three mirrors M1, M2 and M3 are arranged so that the first mirror and the second mirror form an object at infinity of an intermediate image arranged in an intermediate focal plane P F i located between the second mirror and the third mirror , the third mirror forming from this intermediate image a final image in the focal plane P F of the telescope in which a detector D is placed. By applying Korsch equations well known to those skilled in the art, the positions are easily calculated and respective parameters of the three mirrors. The theoretical solution is of very good quality, which makes all the interest of this type of telescope.
    The quality of an optical system is evaluated by comparison between the ideal light wave limited by diffraction and the real light wave at the output of the optical system taking into account the defects of the optical system crossed. The analysis of the difference between theoretical wave and real wave makes it possible to identify the types of defects or aberrations of the optical system.
    It is known that the main geometric aberrations are: spherical aberration, astigmatism, coma, field curvature (defocus in the field) and distortion.
    Polynomials, and more particularly Zernike polynomials, are conventionally used to more easily qualify the different types of aberrations of a wavefront (ie a surface) at the output of an optical system.
    Zernike surfaces are the most commonly used. A Zernike surface is defined in polar coordinates in a space (ρ, Θ, z), and if z (p, Θ) represents the z coordinate of a point on this surface, we have the relation:
    __ + 7l- (l + ^) c 2 p 2 (1)
    Zj being a Zernike polynomial of order j and Cj being the constant associated with this polynomial, j being an index varying between 0 and an integer respectively, k being the conicity constant and c the curvature of the surface.
    Any surface decomposed according to polynomials is called φ-polynomial surface. This surface is therefore characterized by values of the coefficients of these polynomials.
    The interest in decomposing waveforms into orthogonal Zernicke polynomials is that each polynomial of the base considered corresponds to a different geometric aberration category. It is then possible to know the nature of the aberrations present in a wavefront.
    Table I below illustrates the different "Fringe Zernike" polynomials according to their order (here 1 to 16), as well as the corresponding aberration type.
    Order Polynomial Aberration (s) 1 1 Piston 2 p Cos [0] Tilt in x 3 p Sin [0] Inclination in y 4 -1 + 2 p 2 Focus 5 p 2 Cos [2 Θ] 0 ° astigmatism 6 p 2 Sin [2 θ] Astigmatism at 45 ° 7 p (-2 + 3 p 2 ) Cos [0] Coma in x 8 p (-2 + 3 p 2 ) Sin [0] Coma in y 9 1- 6p 2 + 6 p 4 Sphericity and focus 10 p 3 Cos [3 Θ] Sort sheet 11 p 3 Sin [3 Θ] Sort sheet 12 p 2 (-3 + 4 p 2 ) Cos [2 Θ] Astigmatism order 2 13 p 2 (-3 + 4 p 2 ) Sin [2 Θ] Astigmatism order 2 14 p (3 - 12 p 4 + 10 p 4 ) Cos [0] Coma in x order 2 15 p (3 - 12 p 2 + 10 p 4 ) SinlO] Coma in order 2 16 -1 + 12 p 2 - 30 p 4 + 20 p e Sphericity order 2
    Table I
    By adopting the definition of Fringe Zernike polynomials, the different types of aberration correspond to:
    -the focus corresponds to the term Z4,
    - astigmatism corresponds to terms Z5 and Z6,
    -the coma in terms Z7 and Z8 and
    - the first order spherical aberration at Z9.
    - the second order spherical aberration at Z16
    Conventionally, it is known to improve the quality of the image of optical instruments by adding a deformable mirror MD as an exit pupil, commonly known as a “free form” or free form surface, as illustrated in FIG. 1. a monofocal TMA.
    But the theoretical solution of the Korsch 3-mirror telescope being of very good quality, this one does not intervene in the optical combination of the telescope and is used only to compensate for the defects due to the imperfection of realization of the real system compared to the theoretical solution (atmospheric turbulence, defects in the M1 mirror). Thus, a deformable mirror in exit pupil is generally used to correct the constant aberrations in the field. When positioned in the pupil of an instrument, the deformation of the deformable mirror by adding a Zernike polynomial introduces constant aberrations into the field. For example, if we introduce a non-zero value for the polynomial Z5 on the deformable mirror, each point of the field will be impacted by astigmatism.
    In the general case, the surface S to be given to the deformable mirror to allow the correction of defects is called the "free form" surface, meaning that it has no symmetry of revolution (see general formula (1) and table I).
    The formulation (1) is a mathematical base of orthogonal polynomials allowing to define a surface with symmetry of revolution or not.
    An aspherical surface is a surface with symmetry of revolution which cannot be described by a single radius of curvature (like a sphere) because the local curvature changes along the surface.
    The classic definition of an aspherical surface defined in a space (p, z) is:
    P_
    R + À-p 4 + BP 6 + Cp 8 + ...
    (2)
    R is the radius of curvature, k constant taper, the terms A, B, C the aspheric coefficients of 4 th, and 8 th order 6®.
    By comparing with formula (1) and table I with formula (2), we notice that an aspheric surface decomposed in the form of Zernike polynomials has Z4, Z9 and Z16 (Fringe Zernicke polynomials function of p only, that is to say only with symmetry of revolution) and not of Z5, Z6, Z7, Z8, Z10 to Z15 (coefficients function of Θ), the latter coefficients therefore being detrimental for this type of surface.
    When a deformable and controllable MD mirror is used to compensate for the aberrations of a system, any desired surface can be obtained by controlling the mirror, the desired surface of the MD being calculated so as to compensate for the defects of the real system. We decompose the desired surface using polynomials, and we generate this surface by applying the correct coefficients in a controlled manner via the mirror control system. We can then change the shape of the surface by modifying the values of the coefficients.
    It is thus possible by directly controlling the value of the coefficients Cj to introduce the desired aberrations into the design.
    In addition it can be interesting to be able to change the focal length in flight. Indeed, changing the focal length in flight makes it possible to change the field of view and / or the resolution of the image with a single instrument.
    There are currently two families of telescopes:
    bifocal telescopes which make it possible to take a high resolution image but on a narrow field or an image on a wide field but at lower resolution, and
    - telescopes with continuous reflective zoom allowing a change of focal length in flight.
    As examples of bifocal telescopes, we can cite those which rest on a separation of a common channel into two different focal length channels. The separation can be done spectrally: the same field is separated by a dichroic plate if the wavelength domain allows this spectral separation (ex: visible and infrared). It can be done by separating the received flux into reflected flux and transmitted flux, by means of an optical density if it is a non-disjoint wavelength domain (ex: 50% of the flux is reflected, 50% transmitted).
    Advantages of these bifocal solutions with common channel separation:
    - Simultaneous bifocal function,
    - Observation of a common field of view.
    Disadvantages of these solutions:
    - Addition of optical elements (dichroic blade / density + mirrors / lenses specific to each channel),
    - Detectors specific to each channel,
    - If the spectral range of the channels is not disjoint, this requires losing a significant part of the flux,
    - Only bifocal.
    We can also cite the separation telescopes in the field of view: the two channels do not have the same field of view.
    Advantage of these bifocal separation solutions in the field of view:
    - simultaneous bifocal function.
    Disadvantages of these solutions:
    - Addition of optical elements: mirrors / lenses specific to each channel,
    - Detectors specific to each channel,
    - Observation of a different field of view,
    - Only bifocal.
    Another bifocal solution described in US Pat. No. 6,084,727 makes it possible to change the focal length of the telescope by inserting reflective elements on the optical path.
    Advantages of this solution for inserting reflective elements:
    - A single detector,
    - Observation of a common field.
    Disadvantages of this solution:
    - Addition of optical elements: mirrors specific to one of the channels,
    - Only bifocal,
    - Non-simultaneous bifocal function.
    As an example of a continuous reflective zoom telescope, mention may be made of the telescope described in US Pat. No. 6,333,811; it is based on a Cassegrain type telescope with image recovery, the magnification of which is variable, which makes it possible to obtain a continuous zoom.
    Advantages of this solution:
    - A single detector,
    - Continuous zoom,
    - Observation of a common field,
    - No modification of the shape of the mirrors.
    Disadvantages of this solution:
    - The number of mirrors: 7 mirrors including 3 aspherical, 2 "freeform" and 1 plane mirror,
    - Moving two freeform mirrors whose positioning can be sensitive,
    - Cassegrain type telescope, therefore with limited field.
    There are also zooms using mirrors with deformable curvature radii, an example of which is illustrated in the publication by Kristof Seidl et al. : "Wide field-of-view all-reflective objectives designed for multispectral image acquisition in photogrammetric applications".
    Advantages of this solution:
    - A single detector,
    - Continuous zoom,
    - Observation of a common field,
    - No moving of the mirrors.
    Disadvantages of this solution:
    - Too bulky for long focal lengths, for example greater than 10m,
    - Deformable mirrors only work for spherical mirrors with small diameters of the order of a few cm: they are therefore not compatible with pupil sizes of space telescopes typically greater than 0.5m.
    Thus, there is currently no multifocal TMA type telescope with very high optical quality for all focal lengths and which does not use expensive components such as a deformable mirror.
    An object of the present invention is to overcome the aforementioned drawbacks by proposing a telescope with three aspherical multifocal mirrors, mono detector and compact, operating for large pupil diameters, with a larger field of view than that of a Cassegrain (> 1), having a very high image quality for all focal lengths, being compensated with aspheric "classic" components that do not have a deformable "free-form" function.
    DESCRIPTION OF THE INVENTION
    The subject of the present invention is an anastigmat telescope with three aspherical mirrors comprising at least a first concave mirror, a second convex mirror, a third concave mirror and a first detector, and having an optical axis,
    the three mirrors being arranged so that the first mirror and the second mirror form from an object to infinity an intermediate image situated between the second mirror and the third mirror, the third mirror forming from this intermediate image a final image in a first focal plane of the telescope in which the first detector is placed, the first, second and third mirrors being of fixed shape characterized by at least one radius of curvature and a taper, the telescope further comprising:
    means of linear displacement of the third mirror on the optical axis of the telescope so as to vary the focal length of the telescope according to a plurality of focal lengths between at least a minimum focal length and a maximum focal length, the telescope at the minimum focal length having a first exit pupil at a first position, and the telescope at maximum focal length having a second exit pupil at a second position,
    a plurality of aspheric optical components associated respectively with the plurality of focal lengths, respectively disposed at a plurality of positions located between the first and the second position, each aspheric component being arranged on an optical path of a beam corresponding to said associated focal length when the telescope operates at said associated focal length, and outside the optical path associated with another focal length when the telescope operates at said other focal length,
    means for varying the optical path arranged between the aspherical components and the first detector, and configured so that the detector remains positioned in the first focal plane of the telescope,
    the third mirror having a new conicity determined from an initial conicity, the initial conicity being determined from the Korsch equations, the new conicity being determined so that the telescope presents, without the presence of said aspherical components and for the minimum and maximum focal lengths, aberrations compensated by said aspherical components,
    - the position and shape of the surface of each aspherical component being determined so as to correct said compensable aberrations of said telescope for the associated focal and to optimize the image quality in the first focal plane of the telescope according to a predetermined criterion.
    Preferably, the shape of the surface of each aspheric component includes first-order spherical aberration and focus. Preferably, the shape of the surface of each aspheric component further comprises a second order spherical aberration to further improve the image quality according to said criterion.
    Advantageously, the new taper deviates from the initial taper by more than 5% and less than 30%
    According to one embodiment, a new conicity of the first mirror and a new conicity of the second mirror are determined from an initial conicity of the first mirror and an initial conicity of the second mirror respectively, the initial conicities being determined from the equations of Korsch, the new conicities being determined so as to further improve the image quality of said telescope according to said criterion.
    Preferably each surface of an aspherical component is defined from the coefficients of the Fringe Zernike polynomials Z4, Z9 and if necessary Z16.
    According to one embodiment, we define:
    -a positive astigmatism such as an astigmatism for which a tangential focus is located before a sagittal focus,
    -a negative astigmatism such as an astigmatism for which a sagittal focus is located before a tangential focus,
    -a positive coma like a coma for which a shape of the spot image of a source point is a "comet" whose tail moves away from the optical axis and,
    -a negative coma like a coma for which a form of the spot image of a source point is a "comet" whose tail is directed towards the optical axis, the compensable aberrations being of positive astigmatism and positive coma for maximum focal length, positive astigmatism and negative coma for minimum focal length.
    Preferably, the new conicity of the third mirror is defined is determined so as to modify the sign of the telescope's astigmatism for the minimum focal length, without the presence of an aspherical component. Preferably, the predetermined criterion consists in minimizing a waveform error.
    Preferably, said positions of the aspherical components are separated from each other by a maximum of 50 mm.
    According to one embodiment, at least one aspherical component is retractable so as to be disposed on the optical path of the beam corresponding to the associated focal length when the telescope operates at said associated focal length, and outside the optical paths associated with the other focal lengths when the telescope works at one of these other focal lengths.
    Advantageously, the aspherical optical components are retractable mirrors.
    Advantageously, the retractable mirrors are mounted on a single support, the positions of the retractable mirrors then being substantially identical.
    According to one embodiment, the aspherical components are retractable mirrors mounted on a single support, the support further comprising a position for which no retractable mirror appears on the optical path of the incident beam on said support, the beam then passing through the support according to a secondary optical path, the telescope further comprising:
    an optical device disposed on the secondary optical path, configured to generate a second focal plane of the telescope corresponding to a chosen focal length, said optical device being further configured to correct said compensable aberrations of said telescope and to optimize the image quality in the second focal plane of the telescope according to said predetermined criterion and,
    a second detector arranged in the second focal plane of the telescope, and sensitive in a second spectral band different from a first spectral band of sensitivity of the first detector.
    Advantageously, the optical device is adapted to operate in transmission in the second spectral band, the first spectral band is included in the visible range and the second spectral band is included in the infrared region, and the focal length chosen has a value less than the minimum focal length.
    According to another embodiment, at least one aspherical component is a blade operating in transmission.
    According to a variant, the telescope according to the invention comprises only two focal lengths, the minimum focal length and the maximum focal length.
    Other characteristics, objects and advantages of the present invention will appear on reading the detailed description which follows and with reference to the appended drawings given by way of nonlimiting examples and in which:
    FIG. 1, already cited, illustrates a monofocal Korsch type telescope having a deformable mirror placed at the level of the exit pupil of the telescope.
    FIG. 2 illustrates a multifocal Korsch type telescope seen in a YZ plane, the focal length being made variable by deglazing the third mirror on the optical axis. Figure 2a describes the optical system for maximum focal length and Figure 2b describes the optical system for minimum focal length.
    Figure 3 illustrates the telescope of Figure 2 seen in the XZ plane, Figure 3a describes the optical system for maximum focal length and Figure 3b describes the optical system for minimum focal length.
    FIG. 4a describes a first variant of means for varying the optical path between the third mirror and the detector D.
    FIG. 4b illustrates a second variant of means for varying the optical path between the third mirror and the detector D in which the detector D is fixed, the means for varying the optical path comprising two mirrors T1 and T2 in the form of a roof, for a position of mirror T2.
    FIG. 4c illustrates the second variant of means for varying the optical path between the third mirror and the detector D in which the detector D is fixed, the means for varying the optical path comprising two mirrors T1 and T2 in the form of a roof, for a other position of the T2 mirror.
    FIG. 4d illustrates a third variant in which the means for varying the optical path between the third mirror and the detector D comprise conventional fixed mirrors and at least one conventional retractable mirror ...
    FIG. 5 illustrates the aberrations present in the focal plane for the bifocal telescope whose aspherical mirrors M1, M2 and M3 have the initial parameters obtained by solving the Korsch equations. Figure 5a illustrates these aberrations when the telescope operates at maximum focal length, and Figure 5b illustrates these aberrations when the telescope operates at minimum focal length.
    Figure 6 describes the sign convention used for certain categories of aberrations.
    Figure 7 shows schematically a Korsh type telescope according to the invention.
    FIG. 8 illustrates a first variant of the telescope according to the invention in which all the aspherical components CAi are retractable aspheric mirrors.
    FIG. 9 illustrates an example of a bifocal telescope according to the first variant of the invention.
    FIG. 9a illustrates an example of support for the retractable mirrors 10 of a bifocal telescope according to the invention.
    FIG. 10 illustrates a second variant of the telescope according to the invention in which at least one aspherical component is a blade operating in transmission.
    FIG. 11 illustrates, for the initial system, the resulting aberrations following the introduction of spherical aberration Z9 C a on an aspherical component CA as a function of its relative position relative to the effective exit pupil, when CA is arranged downstream of the effective exit pupil. Figure 11a corresponds to Z9ca <0 and Figure 8b corresponds to Z9ca> 0.
    FIG. 12 illustrates, for the initial system, the resulting aberrations following the introduction of Z9ca spherical aberration on an aspherical component CA as a function of its relative position relative to the effective exit pupil, when CA is arranged upstream of the effective exit pupil. The figure
    9a corresponds to Z9ca <0 and figure 9b to Z9ca> 0 ·
    FIG. 13 describes the evolution of the mean value of the telescope's astigmatism as a function of the taper value of the M3.
    Figure 14 illustrates the different aberrations present in the first focal plane of the telescope, with M3 having a taper c’3 = -0.52, Figure 14a for the max focal and Figure 14b for the min focal.
    Figure 15 illustrates the evolution of I quadratic mean value of the WFE RMS waveform error as a function of the taper value u M3.
    FIG. 16 illustrates the different aberrations in the first focal plane of a telescope according to the invention, the telescope having a new conicity c'3 of the mirror M3, and for the deformable mirror, a middle position Pm and Values of Z9md and of Z4md (Z9 | viD / max and Z9 | viD / min; Z4 | / | D / max and Z4 | viD / min) optimized. Figure 16a illustrates the different aberrations for the max focal length and Figure 16b for the min focal length.
    Figure 17 describes the variation of the average focus <Z4> of the 3-Mirror telescope without aspherical component as a function of the value of the cone of M3.
    Figure 18 illustrates the evolution of the main aberrations according to the value of the conicity of M2, for the min and max focal lengths.
    Figure 19 illustrates the evolution of the main aberrations as a function of the value of the taper of M1 for the min and max focal lengths.
    FIG. 20 illustrates the different aberrations in the first focal plane of a telescope according to the invention, the telescope having new conicities c'1, c'2 and c'3 respectively of the mirrors M1, M2 and M3, and for the aspherical mirror-like components, an identical position Pm and optimized values of Z9 M d, Z4 M d and Z16 M d. Figure 20a illustrates the different aberrations for the max focal length and Figure 20b for the min focal length. FIG. 21 illustrates a multi-channel embodiment of the telescope according to the invention.
    FIG. 22 illustrates an aspherical mirror support adapted to the multi-channel embodiment.
    FIG. 23 illustrates the method for determining the parameters of an anastigmat telescope according to the invention
    Figure 24 illustrates the evolution of the WFE averaged over the different focal lengths, after each step of the process.
    DETAILED DESCRIPTION OF THE INVENTION
    We will first describe a Korsch type telescope rendered multifocal. FIGS. 2 and 3 describe a Korsch type telescope 20 with 3 multifocal mirrors, the focal length being made variable by displacement of the third mirror M3 on the optical axis of the telescope O using means 5 of linear displacement. Document US 4993818 briefly describes the principle of such a system.
    The displacement of the mirror M3 between two extreme positions Pmin and Pmax makes it possible to produce a variable focal length between respectively a minimum focal length fmin and a maximum focal length fmax. The instrument comprises at least two focal lengths fmin and fmax and is capable of operating for intermediate focal lengths, by displacement of the mirror M3.
    FIG. 2 illustrates the telescope seen from the side in a YZ plane, FIG. 2a illustrates the telescope operating with the maximum focal length and FIG. 2b with the minimum focal length. FIG. 3 illustrates the telescope seen from the side in an XZ plane, FIG. 3a illustrates the telescope operating with the maximum focal length and FIG. 3b with the minimum focal length.
    For M3 at one of the extreme positions Pmin, the telescope has the minimum focal length fmin, a first exit pupil PS1 at a first position P1 and a focal plane PFmin (FIGS. 2b, 3b). For M3 at the other extreme position Pmax, the telescope has the maximum focal length fmax, a second exit pupil PS2 at a second position P2 and a focal plane PFmax (FIGS. 2a, 3a).
    Since the position of the focal plane of the telescope varies with the focal length, it is necessary to integrate means for varying the optical path between the third mirror M3 and the detector D configured so that the detector remains positioned in the focal plane of the telescope. These means are described below for the case of a standard multifocal 20 telescope, and will be applied later to a telescope according to the invention.
    According to a first variant, the means for varying the optical path between the third mirror M3 and the detector D comprise means of translation 10 of the detector D along the optical axis O, as illustrated in FIG. 4a. A plane mirror MO allows the beam to be folded back for better compactness of the overall optical system and / or to solve a problem of congestion.
    According to a second variant illustrated in FIGS. 4b and 4c, the detector D is fixed and the means for varying the optical path comprise two mirrors T1, T2 in the form of a roof (that is to say having two faces at approximately 90 ° one on the other) located between the third mirror M3 and the detector D, and means
    10 ’of linear translation of one of the two roof-shaped mirrors, T2 in the example, the other remaining fixed, along an axis not parallel to the optical axis, so as to vary the optical path. The slopes of T1 preferably at 45 ° are not necessarily parallel to those of T2. FIG. 4b illustrates a first position of the roof mirror T2 corresponding to a first position of the mirror M3 (short focal length), and FIG. 4c illustrates a second position of the roof mirror T2 corresponding to a second position of the mirror M3 (longer focal length) ). A plane mirror MO allows the beam to be folded back for better compactness of the overall optical system and / or to solve a problem of congestion.
    A third variant illustrated in FIG. 4d is particularly suitable when the telescope is bifocal, that is to say that it operates for only two focal lengths, the focal length fmin and the focal length fmax. The light beam corresponding to an operation at fmin is in dark gray, and the light beam corresponding to an operation at fmax is in lighter gray. The means of variation of the optical path include conventional fixed mirrors Mf, Mf and Mf ”and at least one conventional retractable mirror Mesc. The mirror Mf is arranged on the optical paths of the two beams. The retractable mirror is retracted when the telescope is operating at fmin and is positioned in the optical path of the beam when the telescope is operating at fmax. The fallback mirrors Mf ’and Mf” positioned in the optical path of the beam reflected by Mesc make it possible to obtain a focal plane PFmax at the same location as PFmin, or the detector D is positioned.
    In order to understand the path that led to the invention, we will first describe how to calculate a Korsch type telescope with multiple focal lengths fi, i index from 1 to n. The focal length fmin corresponds to f1 and the focal length fmax corresponds to fn. For a bifocal telescope, n = 2, operating only at fmin = f1 and fmax = f2.
    Parameters called initial parameters of the first, second and third mirrors compatible with both the minimum focal length fmin and the maximum focal length fmax are determined, using optical optimization software known in the prior art.
    Using the Korsch equations, we determine the radii of curvature and initial conics for the two extreme focal lengths of our zoom.
    For example, it is possible to answer the Korsch equations simultaneously for the two focal lengths fmin and fmax by having an identical radius of curvature M1 for the 2 focal lengths.
    The starting point is therefore constituted by the values: R1, R2_fmax, R2_fmin, R3_fmax, R3_fmin, C1_fmax, C1_fmin, C2_fmax, C2_fmin, C3_fmax, C3_fmin.
    The continuation of the optimization consists in constraining the radii of curvature and the conicities to be identical for the 2 extreme focal lengths fmin and fmax. Optimization is carried out conventionally using optical calculation software (CodeV, Zemax, Oslo, ...). This software works on the principle of minimizing an error function. Typically the error function includes image quality at the focal plane and the constraint of the focal lengths fmin and fmax.
    Thus, with a first optimization of the image quality in the focal plane of the telescope according to a predetermined criterion, we arrive at the initial parameters:
    Initial radii of curvature: R1, R2, R3 for M1, M2 and M3 respectively Conic initials: C1, C2, C3 for M1, M2 and M3 respectively.
    The predetermined criterion consists for example of minimizing a waveform error or WFE for "Wave Front Error" in English, averaged over a plurality of points of the field, well known to those skilled in the art. Typically one seeks to minimize the mean square value or WFE RMS.
    In this type of solution the forms of the mirrors M1, M2 and M3, characterized by the parameters radius of curvature R and constant of conicity c (we choose here not to take into account the terms of higher orders which do not bring d 'improvement), respond to the equations established by M. Korsch in order to obtain an aplanatic and anastigmate solution, without field curvature. However, these equations cannot be rigorously solved simultaneously for the two focal lengths fmin and fmax.
    This is a compromise and the image quality is affected. The image quality remains acceptable for telescopes with little volume constraint (that is to say for which the rays are incident on the mirrors with small angles). In the space domain, the volume constraint is essential. This solution is therefore not conceivable for spatial instruments of focal length and large pupil size in which the rays are incident on the mirrors with high angles.
    An illustrative example is a bifocal telescope with:
    Max focal length = 37.5 m
    Min focal length: 15 m
    Zoom Ratio: 2.5
    Mirror diameter M1: 1.1 m
    Distance between M1 and M2: 1600 mm
    Distances between the two extreme positions of M3: 250 mm
    Distances between PS1 and PS2: 250 mm
    Distance between PFmax and PFmin: 1600 mm (PF: focal plane).
    The step of determining the initial parameters by a first optimization as described above results in an initial configuration of the telescope with the following values:
    R1 = 4000 R2 = 1000 R3 = 1200
    mm c1 = -1 mm c2 = -2.1 mm c3 = -0.61
    Figure 5 illustrates the aberrations present in the focal plane P F (detector position) for the bifocal telescope whose three aspherical mirrors M1, M2 and M3 have the initial parameters obtained by solving the Korsch equations as explained above .
    Figure 5a illustrates the aberrations for the maximum focal length fmax, and Figure 5b for the minimum focal length fmin.
    As a reminder, the focus corresponds to Z4, the astigmatism to Z5 and Z6 (Z5 / 6), the coma to Z7 and Z8 (Z7 / 8) and the spherical aberration (first order) to Z9.
    In order to characterize more precisely the different categories of aberrations studied we will adopt a sign convention illustrated in Figure 6.
    We will name:
    - "radial" astigmatism: astigmatism for which the tangential focus is located before the sagittal focus. In the following this astigmatism will be considered by convention as positive and noted A + ;
    - "tangential" astigmatism: astigmatism for which the sagittal focus is located before the tangential focus. In the following this astigmatism will be considered by convention as negative and noted A '.
    -coma "external": coma for which the shape of the spot image of a source point is a "comet" whose tail (widest part) moves away from the optical axis. It is the coma created by a bifocal lens. In the following this coma will be considered by convention as positive, and noted C + ;
    - "internal" coma: coma for which the shape of the image spot of a source point is a "comet" whose tail is directed towards the optical axis. In the following this coma will be considered by convention as negative and noted C '
    It can be seen in FIG. 5 that these aberrations, with the exception of the spherical aberration Z9, are variable in the field (X, Y) of the telescope. The dominant aberrations for this initial configuration of the telescope are: Initial dominant aberrations for the maximum focal length (Figure 5a): Astigmatism (Z5 / 6)> 0 denoted A + , and Coma (Z7 / 8)> 0 denoted C +
    Initial dominant aberrations for a minimal focal length (figure 5b): Astigmatism (Z5 / 6) <0 noted A and Coma (Z7 / 8) <0 noted C '
    The telescope as it is cannot be used due to excessive aberrations.
    The Korsh 30 type telescope according to the invention, illustrated in FIG. 7, is based on a telescope 20 as illustrated in FIGS. 2 to comprising the three mirrors M1, M2 and M3 as described above, and a first detector D placed in a first focal plane Pf (we denote D and Pf respectively first detector and first focal plane because a second detector and a second focal plane will be introduced later in a variant of the invention).
    The telescope 30 according to the invention further comprises a plurality of aspherical optical components CAi, i index comprised between 1 and n, associated respectively with the plurality of focal lengths fi, and disposed respectively with a plurality of positions PCAi located between the first position P1 of the exit pupil PS1 and the second position P2 of the exit pupil PS2. It is between these two positions that the size of the aspherical components is minimized. These aspherical components have the role of compensating for the aberrations of the system, focal length by focal length, their calculation is described below.
    Preferably, the respective positions of the aspherical components are separated from each other by a maximum of 50 mm, preferably by a maximum of 20 mm. This facilitates the optimization calculations described below.
    The telescope 30 can comprise a plurality of n focal lengths with n> 2, or only two focal lengths fmin and fmax (bifocal telescope).
    The telescope 30 further comprises means 50 for varying the optical path, arranged between the aspherical components CAi and the first detector D, and configured so that the first detector remains positioned in the first focal plane of the telescope. The means 50 are typically the means 10 described in FIG. 4a, or the assembly [T1, T2, 10 '] described in FIGS. 4b and 4c, or an assembly comprising fixed mirrors and at least one retractable mirror, such as for example the assembly [MOesc, Mf ', Mf ”] describes figure 4d.
    Each aspherical component CAi is arranged on an optical path of a beam corresponding to the associated focal length fi when the telescope is operating at said associated focal length fi, and outside the optical path associated with another focal length when the telescope operates at this other focal length. Thus a given aspherical component CAi 0 is "seen" (reflected or traversed) by the light beam passing through the telescope only when the telescope operates at the corresponding focal length fio. To obtain this property, according to a preferred embodiment at least one aspherical component is retractable, via an adhoc mechanism, so as to be disposed on the optical path of the beam corresponding to said associated focal length when the telescope is operating at this associated focal length, and outside the optical path associated with the operating focal length, when the telescope is to one of the other focal lengths.
    Different combinations of aspherical component CAi and of means 50 are possible to obtain the above-mentioned property.
    According to a first variant, the aspherical components CAi are all retractable aspheric mirrors MAi, as illustrated in FIG. 8. They are placed on the optical path common to all the focal lengths, and positioned or not in the optical path depending on the focal length used. . Typically the simplest solution in terms of manufacture and adjustment is that all of the retractable mirrors are mounted on a single displacement mechanism 80. In this case the positions of the retractable mirrors PCAi are then substantially identical, within 10 mm, see 5mm gap.
    For a focal number at least equal to 3, an example of a mechanism is a barrel wheel, as illustrated in FIG. 8. The means 50 for allowing positioning of the first detector D in the first focal plane Pf are for example mirrors on the roof with a translation mechanism 10 'as described in Figures 4b and 4c.
    For a bifocal telescope, a translation mechanism 90 can be used to position MA1 or MA2 in the path of the optical beams common to the two focal lengths as illustrated in FIG. 9. When the telescope 30 operates with the long focal length fmax (dark gray), the MOesc retractable mirror is positioned in the optical path, the fixed mirrors Mf and Mf ”returning the beam to the first detector D, as described in Figure 4d and Figure 9. When the telescope operates with the focal length fmin (light gray), we retract MOesc mirror with a 95 mechanism. This avoids the complex mechanism of moving roof mirrors.
    For a bifocal telescope with two retractable aspherical mirrors MA1 and MA2, one can also use a support 80 for which the switching from one aspherical mirror to the other is done by tilting around an axis of rotation, mechanism called "flip / flop ”.
    This first variant of a telescope 30 composed entirely of mirrors has the advantage of (independent operation of the wavelength, the mirrors having no chromatism. The operating spectral band is then determined by the nature of the material reflecting mirrors and the spectral sensitivity band of the first detector.
    According to a second variant, at least one aspheric component is an LA aspheric blade operating in transmission. An example for a bifocal telescope is illustrated in FIG. 10. The retractable aspherical mirror MA is positioned in the path of the beams when the telescope operates at the focal length fmax, and is retracted (by a mechanism 105) when the telescope operates at the focal length fmin, the aspherical blade LA then finding itself in the path of the beam. The displacement mechanism 95 is then removed.
    In the case of a telescope 30 according to the invention, the exit pupil is not fixed according to the focal length of the zoom. The exit pupil moves (order of magnitude ~ 200mm) according to the chosen focal length. CAi aspherical mirrors. therefore work in the field. This has a very significant impact on the aberrations brought to the system by the aspherical mirrors.
    For a mirror arranged as an exit pupil, a beam corresponding to a point in the field illuminates this mirror in its entirety, and therefore the reflected beam will be impacted by spherical aberration if the mirror in question has spherical aberration.
    For a mirror positioned outside the exit pupil, each beam corresponding to a point in the field illuminates different areas of the mirror (and not all). The wavefronts reflected by different areas of the mirror will therefore have different aberrations. For example as explained below, the introduction of spherical aberration on CAi whose position does not coincide with the exit pupil, introduced into the telescope of astigmatism and coma in much larger proportions than l spherical aberration.
    Now let’s study which aberrations can be corrected by an aspherical component placed in the interpupillary area, i.e. between PS1 and PS2, for the initial telescope optimized with Korsh equations.
    For the following, the aberrations of the telescope, corresponding to the defects of the telescope as an optical system, should not be confused with the aberrations introduced in the form of the aspherical component, noted with the index CA.
    The following analysis uses aspherical components of the mirror type as an example, the calculations being able to be easily adapted to the use of at least one blade instead of a mirror.
    Figure 11 illustrates, for the initial system, the resulting aberrations following the introduction of spherical aberration on an aspherical component Z9ca (Z9ca> O for Figure 11a and Z9ca <0 for Figure 11b), depending on its position relative to the effective exit pupil PS, when it is located downstream of PS with respect to the mirror M3.
    Figure 12 illustrates, for the initial system, the resulting aberrations following the introduction of spherical aberration Z9ca on an aspherical component, with Z9ca> 0 for figure 12a and Z9ca <0 for figure 12b, according to its position relative to the effective exit pupil PS, when it is located upstream of PS with respect to the mirror M3.
    The aspherical component being placed between P1 and P2, it is located according to FIG. 11 for the maximum focal length (downstream of PS2 relative to M3) and according to FIG. 12 for the minimum focal length (upstream of PS1 relative to M3) .
    We see in Figures 11 and 12 that the introduction of Z9ca spherical aberration on an aspherical component CA introduces aberrations such as astigmatism and coma in the telescope. This means that an aspherical component can compensate for the inverse aberrations of those created by Z9caOn deduced from Figure 11 that for the max focal length fmax:
    -introducing Z9 C a> 0 creates astigmatism <0 and coma <0, which makes it possible to correct astigmatism> 0 and coma> 0 -introducing Z9ca <0 creates astigmatism > 0 and coma> 0, which allows to correct astigmatism <0 and coma <0
    We deduce from Figure 12 that for the focal length min fmin:
    -introducing Z9ca> 0 creates astigmatism <0 and coma> 0, which makes it possible to correct astigmatism> 0 and coma <0 -introducing Z9qa <0 creates astigmatism> 0 and coma <0 which allows to correct astigmatism <0 and coma> 0
    Thus, by placing an aspherical component per focal length between P1 and P2, the Z9ca of a given sign makes it possible to simultaneously correct for the two extreme focal lengths the astigmatism of the same given sign and the coma of opposite sign.
    For example Z9ca> 0 corrects A + and C + for fmax and A + and C for fmin.
    This correction capacity is not compatible with the initial system whose aberrations to be corrected are illustrated in FIG. 5.
    So by applying to the bifocal telescope a classic method of optimizing its parameters using the Korsch equations (initial configuration of the 3-mirror telescope) and by trying to compensate for aberrations using an aspherical component, at an impasse: An AC component per focal length placed in the interpupillary area cannot simultaneously correct astigmatism and coma present in the system operating at minimum focal length and at maximum focal length
    After numerous calculations, the inventors identified a way of making a Korsch type telescope with a plurality of focal lengths having a very good image quality.
    In the telescope 30 according to the invention, the third mirror M3 has a new conicity c’3 determined from the initial conicity c3 (calculated from the Korsch equations during the first optimization as explained above).
    The new conicity c’3 is determined so that the anastigmat telescope with three aspherical mirrors presents, without the presence of an aspherical component, and for the minimum and maximum focal lengths, aberrations compensable by adding this aspherical component.
    Taking into account the teaching of FIGS. 11 and 12, we seek to obtain a configuration of the M1 / M2 / M3 telescope (without CAi) having the following compensable aberrations:
    For maximum focal length: positive astigmatism A + and positive coma C + .
    For the minimum focal: positive astigmatism A + and negative coma C '.
    In Figure 5 we see that the astigmatism for the minimum focal length is negative.
    The new conicity c'3 is therefore determined so as to modify the sign of the telescope astigmatism without the presence of an aspherical component, for the minimum focal length, that is to say so as to transform the negative astigmatism of the system into a positive astigmatism for the minimum focal length.
    Figure 13 describes the evolution of the average value of the astigmatism of the 3-mirror telescope (without the CAi) <Z5 / 6> according to an arbitrary unit, for the min focal (curve 11) and the max focal (curve 12 ), depending on the taper value of M3. We find for the initial taper c3 = -0.61 a positive astigmatism for fmax and negative for fmin.
    This figure highlights the existence of a value of c’3inf for which the sign of the astigmatism for the focal min reverses, here c’3inf = -0.56. For a new conicity c’3 greater than or equal to c’3inf, the astigmatism of the focal min changes its sign. The new value of c’3 also cannot stray too far from the initial value c3 in order to maintain the convergence of the optical system.
    A second optimization of the image quality, starting from the value c'3inf is then carried out, in order to determine the new conicity c'3, and each position PCAi of the CAi, as well as each shape of the surface Si allowing obtain the best image quality according to the predetermined criterion.
    Preferably when all the aspherical components are mirrors, it is considered that they are positioned in the same place, that is to say that all the PCAi are equal to a single position Pm, which simplifies the optimization. We then calculate and S1 for fmin and Sn for fmax, and we deduce the intermediate Si from S1 and S2.
    According to another embodiment, PCA1 and S1 and PCAn and Sn are first calculated, and PCAi and Si intermediate are deduced from these values.
    With a priori knowledge of the aberrations capable of being compensated for by an aspherical component, as illustrated in FIGS. 11 and 12, it is known that the shape of the surface Si of a CAi capable of compensating for the aberrations of the optical system with focal length fi comprising M1, M2, and M3 of conicity c'3, must include first order spherical aberration Z9ca, and more particularly positive Z9ca.
    Thus the exact value of the new conicity c'3, the positrons PCAi, where appropriate the middle position Pm of the CAi, and the forms S1 for fmin, Sn for fmax, and Si for fi, are determined by a second optimization of the paths optics in the instrument, so as to correct the aberrations of the 3 mirror telescope having a new conicity c'3 and to optimize the image quality in the first focal plane of the telescope according to the predetermined criterion, typically the minimization of an error WFE wavefront.
    The modification of the conicity of M3 makes it possible to reverse the sign of the astigmatism of the focal min, and thus to introduce into the optical system aberrations such that the resulting aberrations of the optical system are compensable by an aspherical component positioned in the interpupillary area.
    Figure 14 illustrates the different aberrations present in the first focal plane of the 3-mirror telescope whose M3 has the new conicity c’3 = 0.52
    The new value c’3 of the conic of M3 makes it possible to obtain positive astigmatism for all focal lengths and opposite comas for extreme focal lengths.
    In the example the new conicity c’3 deviates by about 20% from the value of the initial conic c3 (equal to -0.61). Preferably the new conicity c’3 deviates from the initial conicity c3 by more than 5% and less than 30%.
    FIG. 15 illustrates the evolution of the mean square value of the WFE RMS waveform error as a function of the taper value of the M3, for the min focal lengths (curve 15) and the maximum focal lengths (curve 16). It can be seen that the initial conicity c3 corresponded to the optimized image quality value, a new conicity value c'3 greater than -0.56 causing an increase in the WFE, that is to say a decrease in the quality d 'picture. The change in value of the conic section of M3 does not meet a need for image quality, but makes it possible to obtain aberrations compensable by a CA. We are moving away from the optimum image quality in order to allow correction of aberrations.
    The introduction of spherical aberration Z9 C a at the level of each aspherical component CAi makes it possible to greatly reduce the Z7 / 8 (coma) and. Z5 / 6 (astigmatism) of the system, but does not reduce focus Z4. On the contrary, Z9ca will also cause an increase in the Z4 of the telescope as illustrated in Figure 17, which describes the variation of the average focus <Z4> of the system (3 Mirrors telescope without CAi) as a function of the value of the cone of M3, for the min focal (curve 17) and max focal (curve 18): it can be seen that the focus Z4 increases appreciably, particularly for the min focal.
    Focus Z4 CA should be introduced in the form of each CAi to compensate for the system Z4 (the one initially present and the one introduced by Z9 ca ).
    The introduction of Z4ca also makes it possible to balance the values of astigmatism and coma, that is to say to bring close the values of the respective coefficients, which makes it possible to improve the compensation by Z9ca From the range identified for c'3, the determination of the final value of c'3, of Z9ca (î) and Z4ca (î) for S1, Sn and all the intermediate Si, as well as the different positions (or the unique position Pm) CAi is performed by a second optimization.
    FIG. 16 illustrates the various aberrations in the first focal plane of a telescope 30 according to the invention, the telescope having a new conicity c'3 of the mirror M3, and CAi having a single median position Pm and values of Z9 C a (1), Ζ9οα (π), and Z4 CA (1), Ζ4 0 α (Π) (i.e. Z9 C A / max and Z9cA / min ; Z4cA / max and Z4cA / min) optimized. Figure 16a illustrates the different aberrations for the max focal length and Figure 16b for the min focal length.
    The shape of the surface for the max focal Sn therefore therefore comprises Z9ca (n) and Z4ca (n). The surface shape for the min focal length S1 includes Z9 C a (1) and Z4 CA (1).
    In the example c’3 = -0.52, the CAi are all positioned 110 mm after the PS1 and 140mm before the PS2.
    It can be seen by comparing this FIG. 16 with FIG. 5 (see the change of scale), that the quality of the telescope is greatly improved.
    According to one embodiment, to further improve the image quality, the taper of the mirrors M2 and M1 of the telescope 30 according to the invention is slightly modified.
    In the example, the performance of the telescope can be further improved, the Z7 / 8 and the Z9 being compensated only by the Z9ca. Changing the conicity of M2 (new value c’2) precisely allows to play on these two aberrations. However, this new conicity c’2 also provides significant amounts of Z4. This excess of Z4 is offset by the modification of the taper of the M1 (new value c’1), which also plays on the Z9.
    Thus a new conicity of the first mirror c'1 and a new conicity of the second mirror c'2 are determined respectively from a first initial conicity c1 of the first mirror and from a second initial conicity c2 of the second mirror, so as to further improve the image quality of the telescope according to the predetermined criterion.
    For the example, these modifications are illustrated in FIGS. 18 and 19.
    FIG. 18 illustrates the evolution of the main aberrations as a function of the value of the conicity of M2, for the min and max focal lengths, and FIG. 19 the evolution of the main aberrations as a function of the value of the conicity of M1.
    By a third optimization we determine the new taper values c’2 and c’1, illustrated in Figures 18 and 19:
    C’1 = -0.98
    C’2 = -2.1
    By comparing them to the initial values c1 = -1 and c2 = -2, we note that these variations in conicity are small (less than 10%, see less than 5% for c1), but nevertheless allow the quality of d to be further improved. 'picture.
    As a variant, Z16ca is also added, ie spherical aberration of the second order, which influences Z16, Z9, Z4 Z5 / 6 and Z7 / 8 and makes it possible to further increase the image quality.
    FIG. 20 illustrates the different aberrations in the first focal plane of a telescope 30 according to the invention, the telescope having new conicities c'1, c'2 and c'3 respectively mirrors M1, M2 and M3, and for CA1 and CAn, a middle position Pm and optimized values of Z9ca, Z4ca and Z16ca. Figure 20a illustrates the different aberrations for the max focal length and Figure 20b for the min focal length.
    As a reminder, we have c’3 = -0.52, c’1 = -0.98 and c’2 = -2.1.
    Table 2 below illustrates the values of the parameters (R, k, A, B) as well as the equivalent Zernicke coefficients Z4, Z9 and Z16 allowing to characterize the surface Sn of the aspherical mirror MAn corresponding to fmax = 37.5m.
    Z4 -2.89E-02 mm Z5 0 Z6 0 R -34500 Z7 0 k 0 = Z8 0 AT -3.43E-10 Z9 -7.21 E-04 B 4.27E-15 Z10 0 Z11 0 Z12 0
    Z13 0
    Z14 0
    Z15 0
    Z16 1.06E-05
    Table 2
    Table 3 below illustrates the values of the parameters (R, k, A, B) as well as the equivalent Zernicke coefficients Z4, Z9 and Z16 used to characterize the surface S1 of the aspheric mirror MA1 corresponding to fmin = 15m.
    Z4 -2.72E-02 Z5 0 Z6 0 R -46500 Z7 0 k 0 = Z8 0 AT -5.40E-10 Z9 -1.31E-03 B 1.67E-14 Z10 0 Z11 0 Z12 0 Z13 0 Z14 0 Z15 0 Z16 6.50E-05
    Table 3
    The optimization of each surface can be performed on the parameters (R, k 15, A, B) or on the equivalent Zernicke coefficients Z4, Z9, Z16, depending on the chosen option of the software used.
    We can also develop the optimization further in the higher orders by refining the surface by parameters C, D ... or their equivalent in Zernicke coefficients.
    It can be seen by comparing FIG. 20 with FIG. 16 (see change of scale) that the quality of the telescope is further improved. The final image quality obtained is compatible with the constraint of a WFE RMS <λ / 15, which for the visible corresponds to a WFE RMS <50 nm. (see figure 22 below).
    In the telescope 30 according to the invention the aspherical components CAi form an integral part of the optical combination of the instrument.
    Preferably, when the telescope according to the invention has a plurality of intermediate focal lengths with n> 2, the shape Si of each CAi associated with the intermediate focal lengths is calculated from the shape of the surface for the minimum focal length values S1 and maximum Sn , in order to apply the correct correction for each focal length;
    Thus, once the aberrations Z9ca, Z4ca and Z16ca are optimized for fmin and fmax, i.e. values of coefficients of the Fringe Zernike polynomials determined for fmin and fmax, the values of the coefficients of polynomials are calculated for each value of intermediate focal length, from the values of coefficients of the Fringe Zernike polynomials determined for fmin and fmax.
    According to one embodiment, the telescope 30 according to the invention has an additional channel operating in a wavelength range different from the operating range of the main channel of the telescope, an example of architecture of which is illustrated in FIG. 21.
    The main channel operates over a first wavelength range SB1, typically visible between 400 and 800 nm, and the first detector D has a sensitivity adapted to SB1. The additional channel operates for a second spectral band SB2 different from SB1, typically included in the infrared band.
    In this embodiment, the aspherical components associated with the different focal lengths are preferably retractable mirrors MAi mounted on a single support 80. This support also has a neutral position for which no retractable mirror appears on the optical path of the optical beam incident on the support (simple "hole without optical function). The beam then passes through the support 80 along a secondary optical path 86.
    For a bifocal telescope, an exemplary embodiment of such a three-position support 80 is illustrated in FIG. 22. It comprises three positions, respectively obtained by pivoting around an axis of rotation 40, the two aspherical mirrors MA1 and MA2 being mounted around of a hollow structure. In a first position MA1 reflects the incident beam, in a second position it is MA2 which reflects the incident beam, and in a third neutral position the incident beam passes through the support. Other designs are of course possible, such as a barrel wheel.
    This multi-channel telescope 30 further comprises an optical device 85 disposed on the secondary optical path 86 and configured to generate a second focal plane of the telescope P'f corresponding to a chosen focal length f '. The optical device 85 preferably operates in transmission, so as to be compatible with a chosen focal value f 'much less than fmin, typically 10 times lower. The device 85 is further configured to correct the compensable aberrations of the telescope and to optimize the image quality in the second focal plane of the telescope P ' F according to the predetermined criterion. It fulfills the same compensating function as aspherical mirrors. It is typically a dioptric objective made up of several lenses. Due to the flexibility of design, the lenses can be spherical while performing the compensation function. any other clarification to add
    A second detector D 'is arranged in the second focal plane of the telescope P' F , and has a sensitivity in the second spectral band SB2. A spectral filter is preferably placed on the secondary optical path, between the support 80 and the second detector D'to select the spectral band SB2.
    An additional path is thus produced with low mechanical complexification.
    An exemplary embodiment is a telescope having a main bifocal channel in the visible and an additional monofocal infrared channel. For the on-board optics on satellites, it is sought to obtain an infrared channel of lower resolution than the visible channel, but of larger field, which is obtained with a lower focal length f, typically by a factor of 10, compared to fmin. For example, a visible focal length of the order of ten meters and an IR focal length of the order of one meter.
    The position of the mirror M3 for infrared operation is preferably (but not necessarily) equal to one of the positions corresponding to the focal lengths of the visible main channel. For this focal length, simultaneous visible / IR measurement is possible.
    According to a variant, the telescope according to the invention comprises an aperture diaphragm placed in the interpupillary zone and adjustable in aperture to keep a numerical aperture substantially constant when the focal length varies.
    According to another aspect, the invention relates to a method 60 for determining parameters of an anastigmat telescope illustrated in FIG. 23.
    The telescope includes:
    - three aspherical mirrors, a first concave M1 mirror, a second convex M2 mirror, a third concave M3 mirror,
    a first detector D,
    a plurality of aspherical components CAi (i index from 1 to n) and,
    means 5 for linear displacement of the third mirror on the optical axis O of the telescope so as to vary the focal length of the telescope according to a plurality of focal lengths fi (i index from 1 to n) between a minimum focal length fmin and a maximum focal length fmax.
    The three mirrors M1, M2 and M3 are arranged so that the first mirror and the second mirror form an object at infinity of an intermediate image located between the second mirror and the third mirror, the third mirror forming this intermediate image a final image in the first focal plane of the telescope in which the first detector D. is placed
    The first, second and third mirrors are of fixed shape characterized by at least one conical and a radius of curvature.
    Furthermore, the telescope at minimum focal length has a first exit pupil PS1 at a first position P1, and the telescope at maximum focal length has a second exit pupil PS2 at a second position P2.
    The plurality of aspherical components CAi is associated respectively with the plurality of focal lengths fi, each aspheric component being arranged on an optical path of a beam corresponding to said associated focal length when the telescope operates at said associated focal point, and outside the associated optical path to another focal length when the telescope is operating at said other focal length.
    The aspherical components are disposed at respectively a plurality of PCAi positions located between the first and second positions.
    The method 60 comprises a first step 100 which determines values of conics and radii of curvature, called initial values, of the first, second and third mirrors of the telescope:
    M1 (c1, R1); M2 (c2, R2), M3 (c3, R3).
    These initial values are compatible with both the minimum focal length fmin and the maximum focal length fmax, without the presence of the aspherical components, and are determined from the Korsh equations, by a first optimization of the image quality in the foreground. focal length of the telescope according to a predetermined criterion.
    According to a second step 200, a taper value of the third mirror c'3inf is determined, from the initial taper c3 of the third mirror, from which the telescope presents, without the presence of the aspherical components and for the minimum and maximum focal lengths. , aberrations compensated by the aspherical components CA1 and CAn respectively associated with the focal lengths fmin and fmax.
    Then in a step 300 a new conicity value of the third mirror c'3 is determined, the position PCAi and the shape of the surface Si of each aspheric component CAi by a second optimization, so as to correct the compensable aberrations and to optimize the image quality in the first focal plane of the telescope according to the predetermined criterion. The shape of each Si surface includes at least first order spherical aberration and focus.
    Preferably, the method 60 also comprises a step 400 consisting in determining a new conicity of the first mirror c’1 and a new conicity c’2 of the second mirror M2, so as to further improve the image quality according to the predetermined criterion.
    Preferably, the method 60 according to also comprises a step 500 consisting in refining the surface Si of each aspheric component by further integrating a spherical aberration of the second order so as to further improve the image quality according to the predetermined criterion.
    Typically the predetermined criterion is to minimize a WFE waveform error.
    FIG. 24 illustrates the evolution of the WFE RMS averaged over the different focal lengths at the end of each step of the process, that is to say as a function of the different modifications introduced into the optical system, for the example of the telescope given above.
    The WFE obtained after the first optimization based on the Korsch equations is of the order of 560 nm, incompatible with the WFE RMS constraint <50 nm. By modifying the taper value of M3 to modify the sign of astigmatism, the WFE is degraded (no aspheric compensation component yet). On the other hand, by introducing for each focal length an aspherical component whose surface includes first order spherical aberration and focus, the WFE is greatly improved at around one hundred nm. The modification of the conicities of M1 and M2 makes it possible to decrease the WFE below fifty nm, and the final optimization, introducing dei spherical aberration of the second order, makes it possible to further decrease it to ten nm.
    权利要求:
    Claims (20)
    [1" id="c-fr-0001]
    1. Anastigmat telescope (30) with three aspherical mirrors comprising at least a first concave mirror (M1), a second convex mirror (M2), a third concave mirror (M3) and a first detector (D), and having an optical axis ( O),
    -the three mirrors being arranged so that the first mirror (M1) and the second mirror (M2) form from an object to infinity an intermediate image located between the second mirror and the third mirror, the third mirror (M3) forming of this intermediate image a final image in a first focal plane of the telescope (P F ) in which the first detector is placed, the first, second and third mirrors being of fixed shape characterized by at least one radius of curvature and a taper, the telescope further comprising:
    - means (5) for linear displacement of the third mirror (M3) on the optical axis of the telescope (O) so as to vary the focal length of the telescope according to a plurality of focal lengths (fi) between at least one minimum focal length (fmin ) and a maximum focal length (fmax), the telescope at the minimum focal length having a first exit pupil (PS1) at a first position (P1), and the telescope at the maximum focal length having a second exit pupil (PS2) at a second position (P2),
    a plurality of aspherical optical components (CAi) associated respectively with the plurality of focal lengths (fi), disposed respectively at a plurality of positions (PCAi) located between the first and the second position, each aspherical component being disposed on an optical path d a beam corresponding to said associated focal length when the telescope is operating at said associated focal length, and outside the optical path associated with another focal length when the telescope is operating at said other focal length,
    means of variation of the optical path arranged between the aspherical components and the first detector (D), and configured so that said first detector remains positioned in the first focal plane of the telescope,
    -the third mirror having a new conicity (c'3) determined from an initial conicity (c3), the initial conicity (c3) being determined from the Korsch equations, the new conicity (c'3) being determined so that the telescope presents, without the presence of said aspherical components and for the minimum and maximum focal lengths, aberrations compensable by said aspherical components,
    - the position (PCAi) and the shape of the surface (Si) of each aspherical component being determined so as to correct said compensable aberrations of said telescope for the associated focal (fi) and to optimize the image quality in the first focal plane of the telescope according to a predetermined criterion.
    [2" id="c-fr-0002]
    2. Telescope according to claim 1 wherein said shape of the surface (Si) of each aspherical component comprises first order spherical aberration (Z9ca) and focus (Z4ca)
    [3" id="c-fr-0003]
    3. Telescope according to claim 2 wherein said shape of the surface of each aspheric component further comprises a second order spherical aberration (Z16ca) to further improve the image quality according to said criterion.
    [4" id="c-fr-0004]
    4. Telescope according to one of the preceding claims, in which the new conicity (c’3) deviates from the initial conicity by more than 5% and by less than 30%
    [5" id="c-fr-0005]
    5. Telescope according to one of the preceding claims, in which a new conicity of the first mirror (c'1) and a new conicity of the second mirror (c'2) are determined respectively from an initial conicity of the first mirror (c1 ) and an initial conicity of the second mirror (c2), the initial conicities being determined from the Korsch equations, the new conicities being determined so as to further improve the image quality of said telescope according to said criterion.
    [6" id="c-fr-0006]
    6. Anastigmat telescope according to one of the preceding claims, characterized in that each surface of an aspherical component (Si) is defined from the coefficients of the Fringe Zernike polynomials Z4, Z9 and if necessary Z16.
    [7" id="c-fr-0007]
    7. Telescope according to one of the preceding claims, in which:
    -a positive astigmatism (A +) such as an astigmatism for which a tangential focus is located before a sagittal focus,
    -a negative astigmatism (A-) as an astigmatism for which a sagittal focus is located before a tangential focus,
    -a positive coma like a coma for which a shape of the spot image of a source point is a "comet" whose tail moves away from the optical axis and,
    -a negative coma like a coma for which a form of the image spot of a source point is a "comet" whose tail is directed towards the optical axis, the compensable aberrations being of positive astigmatism (A +) and of positive coma (C +) for maximum focal length, positive astigmatism (A +) and negative coma (C-) for minimum focal length.
    [8" id="c-fr-0008]
    8. Telescope according to one of the preceding claims, in which:
    -a positive astigmatism (A +) such as an astigmatism for which a tangential focus is located before a sagittal focus,
    -a negative astigmatism (A-) as an astigmatism for which a sagittal focus is located before a tangential focus, and in which the new conicity of the third mirror (c'3) is determined so as to modify the sign of the astigmatism of the telescope for minimum focal length, without the presence of an aspherical component.
    [9" id="c-fr-0009]
    9. Telescope according to one of the preceding claims for which the predetermined criterion consists in minimizing a waveform error (WFE).
    [10" id="c-fr-0010]
    10. Telescope according to one of the preceding claims for which said positions of the aspherical components are separated from each other by a maximum of 50 mm.
    [11" id="c-fr-0011]
    11. Telescope according to one of the preceding claims, in which at least one aspheric optical component is retractable so as to be disposed on the optical path of the beam corresponding to the associated focal length when the telescope operates at said associated focal length, and outside the paths. optics associated with the other focal lengths when the telescope operates at one of these other focal lengths.
    [12" id="c-fr-0012]
    12. The telescope according to claim 11, in which the aspherical optical components are retractable mirrors (MAi).
    [13" id="c-fr-0013]
    13. The telescope according to claim 12, in which the retractable mirrors are mounted on a single support (80), the positions of the retractable mirrors then being substantially identical.
    [14" id="c-fr-0014]
    14. Telescope according to one of claims 1 to 10 wherein said aspherical components are retractable mirrors (MAi) mounted on a single support (80), said support further comprising a position for which no retractable mirror is on the way optical beam incident on said support, the beam then passing through the support along a secondary optical path (86), the telescope further comprising:
    an optical device (85) disposed on the secondary optical path, configured to generate a second focal plane (P ' F ) of the telescope corresponding to a chosen focal length (f), said optical device (85) being further configured to correct said compensable aberrations of said telescope and to optimize the image quality in the second focal plane of the telescope (P "according to said predetermined criterion and,
    a second detector (D ') disposed in the second focal plane of the telescope (P' F ), and sensitive in a second spectral band (SB2) different from a first spectral band of sensitivity (SB1) of the first detector.
    [15" id="c-fr-0015]
    15. The telescope according to claim 14 in which the optical device (85) is adapted to operate in transmission in the second spectral band (SB2), in which the first spectral band is included in the visible and the second spectral band is included in the infrared, and in which the chosen focal length (f) has a value less than the minimum focal length.
    [16" id="c-fr-0016]
    16. Telescope according to one of claims 1 to 11 wherein at least one aspherical component is a blade operating in transmission.
    [17" id="c-fr-0017]
    17. Telescope according to one of the preceding claims comprising only two focal lengths, the minimum focal length and the maximum focal length.
    [18" id="c-fr-0018]
    18. Method (60) for determining parameters of an anastigmat telescope comprising three aspherical mirrors, a first concave mirror (M1), a second convex mirror (M2), a third concave mirror (M3), a first detector (D) , a plurality of aspherical components (Can) and means (5) for linear displacement of the third mirror on an optical axis (O) of the telescope so as to vary the focal length of the telescope according to a plurality of focal lengths (fi) between at least a minimum focal length (fmin) and a maximum focal length (fmax), the three mirrors being arranged so that the first mirror and the second mirror form from an object to infinity an intermediate image situated between the second mirror and the third mirror , the third mirror forming this intermediate image of a final image in the first focal plane of the telescope in which the first detector is placed, the first, second and third mirrors being of fixed shape characterized by at least one conical and a radius d curvature, the telescope at minimum focal length having a first exit pupil (PS1) at a first position (P1), and the telescope at maximum focal length having a second exit pupil (PS2) at a second position (P2), the plurality of aspherical components (CAi) being associated respectively with the plurality of focal lengths (fi), each aspheric component being arranged on an optical path of a beam corresponding to said associated focal length when the telescope is operating with said associated focal length, and outside of the optical path associated with another focal length when the telescope operates at said other focal length, said aspherical components being disposed respectively at a plurality of positions (PCAi) located between the first and second positions, the method comprising the steps consisting in:
    -determine (100) values of conics and radii of curvature called initial values of the first (c1, R1), second (c2, R2), and third (c3, R3) mirrors of said compatible telescope of minimum focal length (fmin) and the maximum focal length (fmax), without the presence of said aspherical components, from the Korsh equations, by a first optimization of the image quality in the first focal plane of the telescope according to a predetermined criterion,
    -determine (200) a taper value of the third mirror (c'3inf), from the initial taper of the third mirror (c3), from which the telescope presents, without the presence of said aspherical components and for the minimum focal lengths and maximum, aberrations compensated by the aspherical components respectively associated with said minimum and maximum focal lengths,
    - determining (300) a new taper value of the third mirror (c'3), the position (PCAi) and the shape of the surface (Si) of each aspherical component by a second optimization, so as to correct said compensable aberrations and optimizing the image quality in the first focal plane of the telescope according to the predetermined criterion, the shape of said surfaces of the aspherical components comprising at least first order spherical aberration (Z9ca) and focus (Z4 C a) ·
    [19" id="c-fr-0019]
    19 The method of claim 18 further comprising a step of determining (400) a new conicity of the first (c’1) and second (c’2) mirrors so as to further improve the image quality according to the predetermined criterion.
    [20" id="c-fr-0020]
    20. The method of claim 19 further comprising a step (500) of refining the determination of the shape of the surface (Si) of each aspheric component by further integrating a second order spherical aberration (Z16ca) so as to improve still the image quality according to the predetermined criterion.
    1/24
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    同族专利:
    公开号 | 公开日
    ES2877682T3|2021-11-17|
    US10866403B2|2020-12-15|
    FR3060135A1|2018-06-15|
    FR3060136B1|2019-05-17|
    US20180164573A1|2018-06-14|
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    US8534851B2|2010-07-20|2013-09-17|Raytheon Company|Multiple path substantially symmetric three-mirror anastigmat|FR3072784B1|2017-10-19|2019-11-15|Thales|TELESCOPE TYPE KORSH AMELIORE|
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    CN111487754B|2019-01-25|2021-04-23|清华大学|Free-form surface off-axis three-mirror imaging system|
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    法律状态:
    2018-02-27| PLFP| Fee payment|Year of fee payment: 2 |
    2018-06-15| PLSC| Publication of the preliminary search report|Effective date: 20180615 |
    2020-02-27| PLFP| Fee payment|Year of fee payment: 4 |
    2021-02-25| PLFP| Fee payment|Year of fee payment: 5 |
    2022-02-21| PLFP| Fee payment|Year of fee payment: 6 |
    优先权:
    申请号 | 申请日 | 专利标题
    FR1601770A|FR3060135A1|2016-12-13|2016-12-13|COMPACT TELESCOPE HAVING A PLURALITY OF FOCUS COMPENSATED BY ASPHERIC OPTICAL COMPONENTS|
    FR1601770|2016-12-13|ES17205097T| ES2877682T3|2016-12-13|2017-12-04|Compact telescope with multiple focal lengths compensated by aspherical optics|
    EP17205097.3A| EP3336594B1|2016-12-13|2017-12-04|Compact telescope having a plurality of focal distances compensated by non-spherical optical components|
    US15/840,555| US10866403B2|2016-12-13|2017-12-13|Compact telescope having a plurality of focal lengths and compensated by aspherical optical components|
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