• 专利附录
  • 专利说明
  • 权利要求
  • 类似技术
  • 同族专利
  • 引用文献
  • 法律状态
  • 优先权
    • 专利摘要:
    The general field of the invention is that of three-mirror anastigmatic telescopes comprising at least a first concave mirror (M1), a second convex mirror (M2) and a concave third mirror (M3), the three mirrors being arranged in such a way that the first mirror and the second mirror form an object at infinity, an intermediate image located between the second mirror and the third mirror an intermediate image, the third mirror forming this intermediate image a final image in the focal plane of the telescope . In the architecture of the telescope according to the invention, at least the surface of the third concave mirror (M3) is a φ-polynomial surface.
    公开号:FR3036503A1
    申请号:FR1501064
    申请日:2015-05-22
    公开日:2016-11-25
    发明作者:Nicolas Tetaz；Thierry Viard
    申请人:Thales SA；
    IPC主号:
    专利说明:

    [0001] BACKGROUND OF THE INVENTION The field of the invention is that of telescopes and more particularly telescopes of observations embedded in satellites. More specifically, the field of the invention relates to catoptric systems with large focal lengths.
    [0002] There are two forms of angular field depending on the type of receiver associated with the telescope. For linear receivers, the angular field is worth a few degrees in a first direction of space and a few tenths of degrees in the perpendicular direction. For matrix receivers, the angular field is worth a few degrees in both directions of space. The optical architecture of this type of telescope includes only classically off-axis mirrors. This type of architecture makes it possible to make compact telescopes, having a very good transmission and completely devoid of chromatic aberrations. The image quality must also be excellent throughout the field. Therefore, the optical architecture must be perfectly corrected for geometric aberrations such as spherical aberration, coma, field curvature and astigmatism. Several optical solutions have been proposed to achieve such architectures. A first type of anastigmatic telescope optical architecture comprises three mirrors. These telescopes are also called "telescopes TMA" according to the Anglo-Saxon terminology meaning "Three Mirrors Anastigmat". Conventionally, the mirrors of a TMA telescope are not inclined or "tilted". If the mirrors are all on a common optical axis, there is a significant central obscuration. To suppress the central occultation, one realizes either an "off-axis" of field and / or "an off-axis" of pupil. Indeed, we can tilt the mirrors to remove the central obscuration, but this solution brings geometric aberrations 3036503 2 of astigmatism and coma eccentricity that are generally not acceptable. There are TMA telescopes whose mirrors are slightly tilted and / or eccentric. Generally, the inclination of the mirror does not exceed 1 5 or 2 degrees. This optical solution makes it possible to reduce to the margin the off-axis of field and / or pupil necessary, but not to completely eliminate them. An example of this type of telescope with three mirrors is shown in Figure 1. In this figure and following, we adopted the following conventions. The figures are views in a sectional plane. The mirrors are represented by bold circular arcs. The photosensitive detector D of the telescope is represented by a rectangle. Two representative light rays of the pupil edge rays for the central field have also been shown. These light rays are represented by fine lines. In FIGS. 2 and 7, the intermediate planes are represented by dashed lines. In the case of Figure 1, the three mirrors are aspherical. The first mirror M1 is concave, the second mirror M2 is convex and the third mirror M3 is concave. TMA telescopes offer important linear fields.
    [0003] Thus, the linear field can exceed 15 degrees. However, given focal length, their size is consistent and becomes prohibitive for certain applications, especially when the pupil of the telescope has a large diameter or when the focal length is important. There is also a second type of optical architecture more compact than the previous architecture. These telescopes are called "Korsch". Their architecture shown in Figure 2 is a variant of the previous architecture. The Korsch telescopes are also a combination of three concave-convex-concave type M1, M2 and M3 aspherical mirrors, but the optical combination has an intermediate focal plane PH between the second mirror M2 and the third mirror M3. The mirror MR of FIG. 2 is a simple plane mirror and does not intervene in the optical combination. Unfortunately, their field is limited. Thus, the linear field can not easily exceed 3 degrees. By way of example, a Korsch telescope with a focal length of 10 meters open to F / 4 may have a linear field of 3 ° x 0.5 °. In this case, the error 3036503 3 RMS on the wave surface or WFE RMS, the acronym for "WaveFront Error Root Mean Square" does not exceed 1/20 in the entire field of the telescope. As has been said, the mirrors used in the optical combinations of the TMA or Korsch telescopes are aspherical mirrors. More precisely, their surface is defined by a conic and aspherical terms of revolution. However, these surfaces are not perfectly adapted to correct the aberrations of optical systems that no longer have an axis of symmetry such as telescopes TMA or Korsch. Conventional TMAs have a symmetry of revolution. However, they are not used on their optical axis, but in the field. The TMAs are perfectly corrected from the aberrations in the center of the field, on the optical axis, but the occultation makes this point of the field inaccessible. The field of the telescope is thus eccentric.
    [0004] The further away from the optical center, the lower the image quality because the system is no longer perfectly corrected for aberrations. Thus, the WFS RMS of the previous Korsch telescope goes to X / 4 when the linear field changes from 3 ° x0.5 ° to 6 ° x0.5 °. This error is no longer compatible with the required performance. This is a first limitation.
    [0005] On the other hand, in a conventional Korsch, a hole must be made in the first mirror in order to allow the light to pass as shown in FIG. 2. The first drawback related to the presence of this opening is a decrease in the useful surface area. primary mirror of the order of 15 to 20%. The second drawback is of a mechanical nature. For a field smaller than 3 °, the size of the hole is acceptable, but if the field of view is increased, the size of the hole becomes large and makes it necessary to make the mirror Ml in two distinct parts, which poses important mechanical problems. . This point is illustrated in Figure 3. To the left of this figure, there is shown a mirror M1 with a TM1 opening sufficient to pass a field of 3 degrees 30 by 0.5 degrees. On the right of Figure 3, there is shown a mirror in two parts M1 'and M1 "separated by the opening Tmi, the two parts being necessary to let a field of 6 degrees by 0.5 degrees. mirror necessarily degrades the modulation transfer function or FTM of the telescope as seen in Figure 4 where are 3036503 4 represented on the one hand the actual FTM of the telescope with its opening and theoretical FTM without opening. A new type of optical surface has been developed.These surfaces are known as "freeform" or "freeform." In general, a freeform optic is a surface that has no symmetry of revolution. Generally, each definition responds to a particular need, is adapted to a specific calculation and optimization mode and, of course, to a specific embodiment thereof. For examples, the mathematical definitions of a freeform surface can be the following: - Surface freeform defined by XY polynomials. Clearly, this area being defined in a space (x, y, z), if z (x, y) represents the coordinate z of a point on this surface, we have the relation: z (x, y) = 4 1+ 11- (1 + k) c 2 + y + 1A, xl yk C being the curvature of the surface, where k is the taper constant, A being constants, i, j and k being indices varying between 0 and three integers, respectively. This surface corresponds to an extension of the classical definition of aspherical surfaces by generalizing it to a surface without symmetry of revolution; Freeform surface defined by phi-polynomials, for example Zernike or Q-Forbes polynomials. Zernike surfaces are the most commonly used. A surface of Zernike is defined in polar coordinates in a space (p, cp, z), if z (p, (p) represents the coordinate z of a point of this surface, we have the relation: c (f2), + Zi is a Zernike polynomial of order j and ci is the constant associated with this polynomial, j being an index varying respectively between 0 and an integer. 2 x2 + y2) z (P, C0) = 3036503 5 The GW Forbes publication entitled "Characterizing the shape of freeform optics" 30.01.2012No1.20, No. 3 / Optics Express 2483 describes surfaces defined by phi-polynomials from Q-Forbes. - Freeform surface defined by local equations of freeform subfields of different definition. - Freeform surface defined by hybrid descriptions such as, for example, surfaces mixing phi-polynomial surfaces and so-called "NURBS" surfaces, which stands for "Non-Uniform Rational Basis Splines" or "Non-uniform Rational B-Spline" surfaces.
    [0006] These freeform surfaces have been used for the realization of telescopes with three mirrors. A first architecture of this type is shown in FIG. 5. The architecture is a triangular combination with three convex-concave-concave mirrors in which at least two of the three mirrors are freeform surface mirrors. It is found in several publications including US Patent No. 8,616,712 entitled "Nonsymmetric optical system and design method for nonsymmetric optical system". This optical solution makes it possible to reach important fields but does not have the required compactness.
    [0007] A second architecture of this type is shown in FIG. 6. The architecture is also a concave-concave convex three-mirror combination of which at least one of the three mirrors is a freeform mirror. It is found in several publications including US patent application 2014/0124649 entitled "Off-axial three-mirror system". This optical solution makes it possible to reach important fields but, again, does not have the compactness required when the focal length is large. The telescope according to the invention also comprises one or more free-form mirrors so as to better correct the optical aberrations than the aspherical mirrors. This gain in quality is used to increase the field of Korsch telescopes while maintaining a small footprint. More precisely, the subject of the invention is a three-mirror anastigmat telescope comprising at least a first concave mirror, a second convex mirror and a third concave mirror, the three mirrors being arranged so that the first mirror and the second mirror 3036503 6 form of an object at infinity, an intermediate image situated between the second mirror and the third mirror, the third mirror forming a final image of this intermediate image in the focal plane of the telescope, characterized in that the surface of the third mirror concave is a surface (p-polynomial.
    [0008] Advantageously, the surface of the first concave mirror is a p-polynomial surface Advantageously, the surface of the second convex mirror is a p-polynomial surface Advantageously, the pupil of the telescope is located at the level of the first concave mirror. the angular linear field is greater than 6 degrees in a direction of space Advantageously, the angular field is greater than 2.5 degrees in two perpendicular directions of space.
    [0009] Advantageously, the normal in the center of the surface of the first concave mirror is inclined by a few degrees on the optical axis of the telescope defined by the ray passing through the center of the entrance pupil and perpendicular to this pupil, the normal in the center the surface of the second convex mirror is inclined by a few degrees on the optical axis of the telescope and the normal in the center of the surface of the third concave mirror is inclined by a few degrees on the optical axis of the telescope. Advantageously, the opening of the telescope is between 7 and 25. The invention also relates to a method of setting up a three-mirror anastigmat telescope comprising a first concave mirror, a second convex mirror and a third concave mirror, the three mirrors being arranged so that the first mirror and the second mirror form an object at infinity, an intermediate image located between the second mirror and the third mirror, the third mirror forming a final image of this intermediate image in the focal plane of the telescope, the method being implemented by a software for calculating optical combinations, characterized in that the method comprises at least the following steps: in a first step, determination of the paraxial parameters of the telescope; 3036503 7 - In a second step, implementation of the optical combination of the telescope in a Korsch type configuration comprising the three aspherical mirrors, determination of the main aberrations in the field by the theory of nodal aberrations and determination of the corresponding WFE 5 RMS ; In a third step, adding to the definition of the aspherical surface of one of the mirrors of the optical combination of the Zernike polynomial coefficients corresponding to the calculated aberrations, said surface thus being a freeform surface (p-polynomial; fourth step, suppressing the closure of the primary mirror by rotating at least one of the mirrors and modifying the shape of the freeform surface mirror, so as to correct the aberrations created by the rotation of the mirror and modification of Zernike polynomials to reduce the WFE RMS below a predetermined threshold.
    [0010] Advantageously, the surface definition modifications made in the third step or in the fourth step also concern the surface of one of the other two mirrors of the telescope. The invention will be better understood and other advantages will become apparent on reading the description which will follow given by way of nonlimiting example and with reference to the appended figures, in which: FIG. 1 represents a first optical architecture of anastigmatic telescopes with three so-called mirrors "TMA telescopes" according to the prior art; FIG. 2 represents a second optical architecture of three-mirror anastigmatic telescopes known as "Korsch telescopes" according to the prior art; Figure 3 shows a front view of a Korsch telescope primary mirror with its central aperture in two different field configurations; Figure 4 shows the modulation transfer function of the centrally aperture Korsch telescope; Fig. 5 shows a third optical architecture of three-mirror anastigmatic telescopes having a freeform mirror according to the prior art; FIG. 6 represents a fourth optical architecture of three-mirror anastigmatic telescopes comprising a freeform mirror according to the prior art; FIG. 7 represents an optical architecture of three-mirror anastigmatic telescopes according to the invention. By way of example, FIG. 7 represents an optical architecture of three-mirror anastigmatic telescopes according to the invention. This architecture comprises a first concave mirror M1, a second convex mirror M2 and a third mirror M3 concave. In this figure, the optical axis X passing through the center of the pupil P is represented by dotted lines and the normal NM1, NM2 and NM3 on the surface of the mirrors M1, M2 and M3 by arrows arranged in the center of the mirrors. . This architecture is derived from Korsch architectures 15 as previously described. But, it is demonstrated that the use of freeform surface mirrors makes it possible to significantly increase the accessible anastigmat field. According to the architectures employed, the gain is substantially a factor of 2. The three mirrors are arranged so that the first mirror and the second mirror form an object at infinity, an intermediate image located in a focusing plane. PH located between the second mirror and the third mirror. The third mirror forms a final image of this intermediate image in the focal plane of the telescope where the detector D is located, At least the surface of the third concave mirror is a surface 25 (p-polynomial) The surfaces of the first and second mirrors The pupil P of the telescope is located at the first concave mirror M. As can be seen in FIG. 7, the normal NM1 at the center of the surface of the first concave mirror M1 is inclined by a few degrees. degrees on the optical axis X of the telescope defined by the ray passing through the center of the entrance pupil and perpendicular to this pupil, the normal NM2 in the center of the surface of the second convex mirror M2 is inclined by a few degrees on the X optical axis of the telescope and the normal Nm3 in the center of the surface of the 3036503 9 third mirror M3 concave is inclined a few degrees on the optical axis X of the telescope.This configuration with three mirrors comprising an intermediate focal plane, a pupil located at the level of the first mirror and surface mirrors (p-polynomial with a slight inclination on the axis) make it possible to obtain at the same time a large optical field, an open system and a smaller space requirement than the solutions of the prior art. The method of calculating the optical combination of the telescope 10 is based on the analysis of aberrations expressed in the form of Zernike polynomials in the field. This analysis makes it possible to determine the values of the Zernike coefficients to be applied to the different mirrors M1, M2 and M3. The method used is based on nodal aberration theory, known as "Nodal Aberration Theory" generalized to freeform surfaces. This method is described in K. Fuerschbach's "Theory of aberration fields for general optical systems with freeform surfaces". It is set up using a software for calculating optical combinations.
    [0011] In a first step, the telaxial parameters of the telescope, that is, its focal length, aperture, and field, are determined. In a second step, the optical combination of the telescope is set up in a Korsch type configuration with three simply aspheric mirrors. In this second step, no occultations due to the different mirrors are taken into account. The main aberrations in the field are then determined by nodal aberration theory, that is, aberrations of astigmatism, coma and spherical aberration, and the WFE RMS in the Korsch field with three aspherical mirrors. .
    [0012] In a third step, at least the surface of one of the mirrors of the optical combination is supplemented with Zernike coefficients corresponding to the calculated aberrations so as to decrease and / or eliminate them in the entire field of the telescope. The optical solution found remains theoretical because the light is partially blocked by the mirrors.
    [0013] Finally, in a fourth and last step, this shutter is removed by a rotation of the mirrors. These rotations allow the optics to continue working on the optical axis. However, this tilt brings astigmatism and coma. To correct the aberrations made, the shape of the freeform mirror (s) is modified. Based on the theory of nodal aberrations, it is possible to correct the aberrations created by the rotations of the mirrors by directly modifying the Zernike polynomials applied to each of the three mirrors. The influence of the Zernike polynomials on the mirrors is different depending on the position of the mirror with respect to the pupil. Thus the Zernike polynomials applied to a mirror disposed in the pupil in the neighborhood of the pupil such as the mirror M1 of FIG. 5 have an influence on all the points of the field, which is not the case for the mirror M3. which is far from a pupil. Of course, the third and fourth steps can be performed simultaneously. In a telescope according to the invention, the angular linear field may be greater than 6 degrees in a space direction where the angular field may be greater than 2.5 degrees in two mutually perpendicular directions of space. The pupillary aperture is between 7 and 25. On the other hand, the absence of opening in the primary mirror makes it possible to increase the useful area by 15 to 20%, to increase the modulation transfer function at the level of the pupil. medium frequencies and to simplify the technical realization. For example, a Korsch telescope with a 10 meter focal distance open at f / 4 can have a linear field of 6 ° x0.5 °. In this case, the root mean square error on the wave surface or WFE RMS, which stands for "WaveFront Error Root Mean Square", does not exceed X / 24 throughout the telescope field.
    权利要求:
    Claims (10)
    [0001]
    REVENDICATIONS1. A three-mirror anastigmat telescope comprising at least a first concave mirror (M1), a second convex mirror (M2) and a concave third mirror (M3), the three mirrors being arranged so that the first mirror and the second mirror form a mirror an object at infinity, an intermediate image located between the second mirror and the third mirror, the third mirror forming a final image of this intermediate image in the focal plane of the telescope, characterized in that the surface of the third mirror (M3) concave is a surface (p-polynomial.
    [0002]
    2. Anastigmat telescope according to claim 1, characterized in that the surface of the first concave mirror (M1) is a (p-polynomial) surface.
    [0003]
    Anastigmat telescope according to claim 1, characterized in that the surface of the convex second mirror (M2) is a polynomial surface.
    [0004]
    4. Anastigmat telescope according to one of the preceding claims, characterized in that the pupil (P) of the telescope is located at the level of the first concave mirror.
    [0005]
    5. Anastigmat telescope according to one of the preceding claims, characterized in that the angular linear field is greater than 6 degrees in a direction of space. 25
    [0006]
    6. Anastigmat telescope according to one of the preceding claims, characterized in that the angular field is greater than 2.5 degrees in two perpendicular directions of the space. 30
    [0007]
    7. Anastigmat telescope according to one of the preceding claims, characterized in that the normal (NM1) in the center of the surface of the first concave mirror is inclined by a few degrees on the optical axis (X) of the telescope defined by the passing ray. by the center of the entrance pupil 3036503 12 and perpendicular to this pupil, the normal (NM2) in the center of the surface of the second convex mirror is inclined by a few degrees on the optical axis of the telescope and the normal (NM3) in the center of the surface of the third concave mirror is inclined a few degrees on the optical axis of the telescope.
    [0008]
    Anastigmat telescope according to one of the preceding claims, characterized in that the opening of the telescope is between 7 and 25. 10
    [0009]
    9. A method of setting up a three-mirror anastigmat telescope comprising a first concave mirror (M1), a second convex mirror (M2) and a concave third mirror (M3), the three mirrors being arranged in such a way that the first mirror mirror and the second mirror forms an object at infinity, an intermediate image located between the second mirror and the third mirror, the third mirror forming of this intermediate image a final image in the focal plane of the telescope, the method being implemented by a software for calculating optical combinations, characterized in that the method comprises at least the following steps: in a first step, determination of the paraxial parameters of the telescope; - In a second step, implementation of the optical combination of the telescope in a Korsch type configuration comprising the three aspherical mirrors, determination of the main aberrations in the field by the theory of nodal aberrations and determination of the corresponding WFE RMS; In a third step, adding to the definition of the aspherical surface of one of the mirrors of the optical combination of the Zernike polynomial coefficients corresponding to the calculated aberrations, said surface thus being a freeform (p-polynomial) surface. fourth step, suppressing the closure of the primary mirror by rotating at least one of the mirrors and modifying the shape of the freeform surface mirror, so as to correct the aberrations created by the rotation of the mirror and modification of Zernike polynomials to reduce the WFE RMS below a predetermined threshold.
    [0010]
    10. A method of setting up an anastigmat telescope according to claim 9, characterized in that the surface definition modifications made in the third step or in the fourth step also concern the surface of one of the other two mirrors of the telescope. . 5
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    同族专利:
    公开号 | 公开日
    EP3096169A1|2016-11-23|
    FR3036503B1|2017-05-26|
    US20160341948A1|2016-11-24|
    US10386625B2|2019-08-20|
    EP3096169B1|2021-10-06|
    引用文献:
    公开号 | 申请日 | 公开日 | 申请人 | 专利标题
    US3674334A|1971-01-04|1972-07-04|Perkin Elmer Corp|Catoptric anastigmatic afocal optical system|
    US20050013021A1|2003-06-10|2005-01-20|Olympus Corporation|Decentered optical system, light transmitting device, light receiving device, and optical system|
    US20140124657A1|2012-11-06|2014-05-08|Jun Zhu|Off-axial three-mirror system|
    US8616712B2|2011-03-24|2013-12-31|University Of Rochester|Nonsymmetric optical system and design method for nonsymmetric optical system|
    CN103809278B|2012-11-06|2016-09-14|清华大学|Off-axis three anti-mirrors|CN108345094B|2017-01-24|2020-02-07|清华大学|Mixed surface off-axis three-mirror optical system|
    US10191275B1|2017-07-06|2019-01-29|Bae Systems Information And Electronic Systems Integration Inc.|Three-mirror anastigmat having rectangular aperture stop|
    CN109188665B|2018-08-14|2020-08-11|北京理工大学|Off-axis three-mirror imaging system based on flat-plate phase element|
    CN109188666B|2018-11-01|2020-08-18|长春理工大学|0.4-5 mu m waveband off-axis three-mirror optical system with 350mm caliber and 1778.9mm focal length|
    FR3089640B1|2018-12-11|2021-03-12|Thales Sa|BISPECTRAL ANASTIGMATE TELESCOPE|
    CN109669260A|2018-12-29|2019-04-23|润坤光学科技有限公司|Fast coke ratio based on secondary imaging minimizes off-axis three anti-freeform optics system|
    CN110927943A|2019-12-26|2020-03-27|中国科学院长春光学精密机械与物理研究所|Off-axis three-reflection diffuse reflection plate lighting system|
    法律状态:
    2016-04-26| PLFP| Fee payment|Year of fee payment: 2 |
    2016-11-25| PLSC| Search report ready|Effective date: 20161125 |
    2017-04-27| PLFP| Fee payment|Year of fee payment: 3 |
    2018-05-01| PLFP| Fee payment|Year of fee payment: 4 |
    2019-04-29| PLFP| Fee payment|Year of fee payment: 5 |
    2020-05-05| PLFP| Fee payment|Year of fee payment: 6 |
    2021-04-26| PLFP| Fee payment|Year of fee payment: 7 |
    优先权:
    申请号 | 申请日 | 专利标题
    FR1501064A|FR3036503B1|2015-05-22|2015-05-22|TELESCOPE COMPACT ANASTIGMAT WITH THREE MIRRORS OF KORSCH TYPE|FR1501064A| FR3036503B1|2015-05-22|2015-05-22|TELESCOPE COMPACT ANASTIGMAT WITH THREE MIRRORS OF KORSCH TYPE|
    EP16169292.6A| EP3096169B1|2015-05-22|2016-05-12|Compact korsch-type three-mirror anastigmat telescope|
    US15/154,722| US10386625B2|2015-05-22|2016-05-13|Korsch-type compact three-mirror anastigmat telescope|
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