AU2021102434A4 - The Wide Field of View Telescope Optical System for Sitian Project - Google Patents
The Wide Field of View Telescope Optical System for Sitian Project Download PDFInfo
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- AU2021102434A4 AU2021102434A4 AU2021102434A AU2021102434A AU2021102434A4 AU 2021102434 A4 AU2021102434 A4 AU 2021102434A4 AU 2021102434 A AU2021102434 A AU 2021102434A AU 2021102434 A AU2021102434 A AU 2021102434A AU 2021102434 A4 AU2021102434 A4 AU 2021102434A4
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- 230000003287 optical effect Effects 0.000 title claims abstract description 95
- 230000004075 alteration Effects 0.000 claims abstract description 27
- 238000005375 photometry Methods 0.000 claims description 4
- 238000010586 diagram Methods 0.000 abstract description 17
- 238000012544 monitoring process Methods 0.000 abstract description 3
- 230000009466 transformation Effects 0.000 abstract description 2
- 238000001514 detection method Methods 0.000 abstract 2
- VYPSYNLAJGMNEJ-UHFFFAOYSA-N Silicium dioxide Chemical compound O=[Si]=O VYPSYNLAJGMNEJ-UHFFFAOYSA-N 0.000 description 6
- 239000005350 fused silica glass Substances 0.000 description 6
- 201000009310 astigmatism Diseases 0.000 description 5
- 206010010071 Coma Diseases 0.000 description 4
- 238000011161 development Methods 0.000 description 3
- 238000013461 design Methods 0.000 description 2
- 239000000463 material Substances 0.000 description 2
- 238000013441 quality evaluation Methods 0.000 description 2
- 230000001052 transient effect Effects 0.000 description 2
- 102100038784 Carbohydrate sulfotransferase 4 Human genes 0.000 description 1
- 101710158423 Carbohydrate sulfotransferase 4 Proteins 0.000 description 1
- 239000000919 ceramic Substances 0.000 description 1
- 238000012937 correction Methods 0.000 description 1
- 239000006185 dispersion Substances 0.000 description 1
- 230000000694 effects Effects 0.000 description 1
- 238000003384 imaging method Methods 0.000 description 1
- 230000006872 improvement Effects 0.000 description 1
- 238000000034 method Methods 0.000 description 1
- 239000013081 microcrystal Substances 0.000 description 1
- 230000008569 process Effects 0.000 description 1
- 238000012545 processing Methods 0.000 description 1
- 210000001747 pupil Anatomy 0.000 description 1
- 230000035945 sensitivity Effects 0.000 description 1
- 238000000844 transformation Methods 0.000 description 1
- 238000002834 transmittance Methods 0.000 description 1
Classifications
-
- G—PHYSICS
- G02—OPTICS
- G02B—OPTICAL ELEMENTS, SYSTEMS OR APPARATUS
- G02B17/00—Systems with reflecting surfaces, with or without refracting elements
- G02B17/08—Catadioptric systems
- G02B17/0884—Catadioptric systems having a pupil corrector
- G02B17/0888—Catadioptric systems having a pupil corrector the corrector having at least one aspheric surface, e.g. Schmidt plates
-
- G—PHYSICS
- G02—OPTICS
- G02B—OPTICAL ELEMENTS, SYSTEMS OR APPARATUS
- G02B17/00—Systems with reflecting surfaces, with or without refracting elements
- G02B17/08—Catadioptric systems
- G02B17/0804—Catadioptric systems using two curved mirrors
- G02B17/0808—Catadioptric systems using two curved mirrors on-axis systems with at least one of the mirrors having a central aperture
-
- G—PHYSICS
- G02—OPTICS
- G02B—OPTICAL ELEMENTS, SYSTEMS OR APPARATUS
- G02B23/00—Telescopes, e.g. binoculars; Periscopes; Instruments for viewing the inside of hollow bodies; Viewfinders; Optical aiming or sighting devices
- G02B23/02—Telescopes, e.g. binoculars; Periscopes; Instruments for viewing the inside of hollow bodies; Viewfinders; Optical aiming or sighting devices involving prisms or mirrors
- G02B23/06—Telescopes, e.g. binoculars; Periscopes; Instruments for viewing the inside of hollow bodies; Viewfinders; Optical aiming or sighting devices involving prisms or mirrors having a focussing action, e.g. parabolic mirror
-
- G—PHYSICS
- G02—OPTICS
- G02B—OPTICAL ELEMENTS, SYSTEMS OR APPARATUS
- G02B27/00—Optical systems or apparatus not provided for by any of the groups G02B1/00 - G02B26/00, G02B30/00
- G02B27/0025—Optical systems or apparatus not provided for by any of the groups G02B1/00 - G02B26/00, G02B30/00 for optical correction, e.g. distorsion, aberration
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- General Physics & Mathematics (AREA)
- Optics & Photonics (AREA)
- Astronomy & Astrophysics (AREA)
- Telescopes (AREA)
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Abstract
SiTian is an ambitious ground-based all-sky optical monitoring project, developed by the
Chinese Academy of Sciences. The concept is an integrated network of dozens of 1-m-class
telescopes deployed partly in China and partly at various other sites around the world. The
main science goals are the detection, identification and monitoring of optical transients (such
as gravitational wave events, fast radio bursts, supernovae) on the largely unknown timescales
of less than 1 day; SiTian will also provide a treasure trove of data for studies of AGN, quasars,
variable stars, planets, asteroids, and microlensing events. To achieve those goals, SiTian will
scan at least 10,000 square deg of sky every 30 min, down to a detection limit of V~21 mag.
The wide field of view optical system for SiTian Project, known as SiTian optical system, is
characterized in that the catadioptric telescope optical system includes an aspheric corrector
plate A with a central hole, a spherical or aspheric reflective primary mirror B, a spherical lens
C, a spherical lens D, a spherical lens E, an optical filter F, a camera window G and a focal
plane H, which are arranged in sequence along the incident direction of light from front to back.
Specifically, the aspheric plate A with a central hole is annular, and the diameter of the central
hole is approximately the maximum lens diameter of the corrector lens group. Located at the
position of the optical system aperture stop, it is used to correct the spherical aberration of the
spherical or aspherical reflection primary mirror. An optical system with a large field of view
and excellent image quality is disclosed in the invention, which belongs to the transformation
of Schmidt telescopes. In addition, its primary mirror diameter is smaller than the traditional
Schmidt telescopes, while meeting the same optical parameters. In the present invention, the
camera is outside the lens tube, and there is no heat source in the lens tube, so the optical image
quality will not be affected; the length of the lens tube is reduced by half; and the flat image
surface has excellent image quality and uniform throughout the whole field of view.
1/3
FIGURES
Figure 1A schematic diagram of the optical structure of the invention.
B
---
r-----
Figure 2The structural diagram of the optical system of Embodiment 1.
e a ySpot Diagram
60c modi-.chmidt 7dqege21nzm
Figure 3A full field image spot diagram (450-550nm band range) of Embodiment 1.
Description
1/3 FIGURES
r----- ---
Figure 1A schematic diagram of the optical structure of the invention. B
Figure 2The structural diagram of the optical system of Embodiment 1.
e a ySpot Diagram
60c modi-.chmidt 7dqege21nzm
Figure 3A full field image spot diagram (450-550nm band range) of Embodiment 1.
The Wide Field of View Telescope Optical System for Sitian Project
The invention belongs to the field of photoelectric imaging technology, and specifically
relates to optical systems for survey telescopes, which is a catadioptric large-field of view
telescope optical system. This invention was funded by the National Natural Science
Foundation of China (11503062) and the 973 Project (2013CB834900).
Astronomy is a subject driven by observation. In terms of development trends,
astronomical observations are pursuing large-aperture, large field of view, high image
quality, high sensitivity, and full-band coverage. The development of time-domain
astronomy especially needs advanced telescopes. On the other hand, with the
development of human aerospace activities, the number of large-scale space debris has
exceeded 20,000, and it continues to grow at a rate of more than 5% every year, which
poses a serious threat to spacecraft. Therefore, space debris monitoring telescopes have
increasing demands on optical telescopes.
The optical systems of large-aperture and large-field of view telescopes can be divided
into four categories of Cassegrain plus corrector type, three-mirror anastigmatism type,
prime focus type, and Schmidt type.
Cassegrain system plus corrector type, such as SLOAN sky survey telescope, Pan
STARRS and Spain's JST telescope, has a dual-reflection focus system composed of
primary mirror, secondary mirror and corrector. Further, the system has a focal ratio
between F3-F5, and is equipped with a larger secondary mirror as well as a large center obscuration. Moreover, the maximum field of view can be about 3.5° under reasonable circumstances. The three-mirror anastigmatism type, such as the LSST (Large Synoptic
Survey Telescope) being designed and constructed in the United States, is composed of
three aspherical reflectors and a corrector group, which can achieve excellent image
quality and is suitable for systems with fast focal ratios. But with large obscuration, it is
difficult to process that three aspherical reflectors. Under reasonable circumstances, the
maximum field of view can be about 3.5°. The prime focus plus corrector type, such as
the DESI (Dark Energy Spectroscopic Instrument) in the United States, is to add 4
correctors and 2 atmospheric dispersion correctors to the prime focus of a 4-meter
telescope. Under reasonable circumstances, the prime focus system can achieve a field of
view of 2~5°. The Schmidt type, such as the Zwicky Transient Facility telescope, has a
transmission-model aspheric corrector plate with a diameter of about 1.3 meters, which is
located at the center of the primary mirror, and taken as the entrance pupil of the optical
system. The system has excellent image quality, but the lens tube is long. The camera is
in the middle of the lens tube, and a curved focal plane is formed by mosaic chips to
achieve a 7x7° super large field of view. The SiTian optical system can realize a flat
focal plane with a short lens tube and a large field of view by addingfield-of-view
correctors.
At present, most telescope optical systems with a field of view greater than 5° for
photometry often adopt the types of prime focus and Schmidt. Under the same
requirements, compared with the prime focus type, the Schmidt type optical system has a
uniform image quality throughout the whole field of view, a better image quality, and a
higher transmittance.
The working principle of the Schmidt telescope optical system is as follows. Known
telescope monochromatic aberrations include spherical aberration, coma aberration,
astigmatism, curvature of field, and distortion. And chromatic aberrations include
magnification chromatic aberration and lateral chromatic aberration. For a telescope
optical system with a single spherical primary mirror, the aperture stop is placed at the
center of sphere of the primary mirror, and the system has no coma aberration,
astigmatism, or chromatic aberration. Its distortion does not degrade the resolution of the
image. The field of view is small limited by spherical aberration and field curvature. In
1931, Bernhard Schmidt proposed to use an aspherical corrector plate to correct the
spherical aberration of the primary mirror. The aspherical plate was placed at the center
of sphere of the primary mirror and set as aperture stop. The kind of optical system can
completely correct spherical aberration, coma aberration, and astigmatism. Besides, using
a curved image surface, the image quality of the large field of view is excellent. Based on
the traditional Schmidt telescope optical system, (1) in 1935, Yrj6 Vdis£15 and Franklin
Wright suggested to put the aspheric corrector plate at the focal plane of the aspheric
primary mirror to obtain a short-tube Schmidt optical system with a flat image surface;
(2) in 1962, Su Dingqiang and others proposed to place the aspheric corrector plate near
the focal plane position of the aspheric primary mirror to correct spherical aberration and
coma aberration, residual astigmatism and field area, so as to obtain a Schmidt optical
system with a curved image plane; (3) in 1980, Wang Lanjuan and Su Dingqiang
proposed to place the aspheric corrector plate at different positions from the center of the
aspheric primary mirror to the focal plane, and add an aspheric corrector plate in front of
the focal plane to correct the residual astigmatism and obtain a short-tube Schmidt optical system with a flat image surface and excellent image quality; (4) in 2008, in order to develop the China Antarctic Survey Telescope, Yuan Xiangyan and Su Dingqiang proposed a new type of Schmidt telescope optical system, which used an aspheric corrector plate to correct the spherical aberration of the oblate spherical aspheric primary mirror, and corrected the field of view aberration and chromatic aberration with the corrector mirror group. As a result, a short-tube Schmidt telescope optical system with a flat image surface and excellent image quality was obtained.
The Schmidt telescope optical system has been widely used in astronomical observations.
Representative Schmidt optical telescopes include the United States' 0.95-meter Kepler
Mission Telescope, 1.2-meter UK Schmidt Telescope, 1.22-meter Zwicky Transient
Facility, 1. 2m China Xuyi Near-Earth Object Search Telescope and 0.5m China
Antarctic Survey Telescope.
The Schmidt telescope optical system has advantages in large field of view optical
systems. However, the existing Schmidt telescope has a long lens tube, and the image
plane of the traditional Schmidt telescope is curved and inside the optical tube, making it
difficult to mount the cameras.
In order to overcome the shortcomings of the traditional Schmidt telescope optical
system, the SiTian wide field of view optical system is proposed in the invention.
The purpose of the present invention is to provide an optical system with a large field of
view and excellent image quality, which belongs to the transformations of Schmidt
telescope optical system, and overcomes the shortcomings of the traditional Schmidt
telescope optical system. The SiTian optical system proposed in the present invention has a smaller primary mirror diameter while meeting the same optical parameters as the traditional Schmidt. With the camera outside the lens tube and without heat source in the lens tube, the optical image quality will not be degraded. Meanwhile, the length of the lens tube is reduced by half; and flat image quality is excellent.
The technical solution for accomplishing the invention task of this application is
described below.
A SiTian optical system (optical system of catadioptric telescope with large field of view)
is characterized in that the catadioptric telescope optical system includes an aspheric
corrector plate A with a central hole, a spherical or aspheric reflective primary mirror B, a
spherical lens C, a spherical lens D, a spherical lens E, an optical filter F, a camera
window G and a focal plane H, which are arranged in sequence along the incident
direction of light from front to back.
One surface of the aspherical corrector plate A is flat, and the other surface is aspherical
without focal power. The surface type is determined by the following formula,
Z CrZ -+ a 4 r4 + a 6 r6+ a~rs
Wherein, k is the aspherical conic coefficient, a4, a6, and as are the coefficients of the
aspherical surface, r is the height of the aspherical surface in the vertical direction from
the optical axis, and z is the horizontal distance from the aspherical surface to the center
of the lens.
The present invention is a large-aperture telescope optical system with a large field of
view (with field diameter of 7). Assuming that the optical parameters are 60cm aperture,
field of view, focal ratio 2, wave band 450-900nm, image quality with 80% energy
concentration and diameter less than 18tm, the systems that can achieve this assumption include prime focus system (1 aspherical reflection primary mirror plus 5 spherical correctors) and Schmidt optical system (traditional type and SiTian type).
Optical System Schmidt Telescope Prime Focus Present Invention Aperture (mm) 600 600 600 Primary Mirror (mm) 800<D<915 600 700 Image Quality (80% Energy Concentration 15 18 15 and Diameter (mm)) Lens Size (mm) 250 >300 250 Number of Spherical 2 > 5 2 Lenses Obscuration 18 25 18 Camera Position Inside the Closed Outside the Tube Outside the Closed Tube Tube Tube Length About 3m 1.5m 1.5m Processing Difficulty Aspheric Plate AsphericrPrimary Aspheric Plate ____________________Mirror
Through comparison, it can be concluded that the present invention is a telescope optical
system with significant advantages. Based on the improvement of the Schmidt telescope
optical system, the invention can achieve a field of view greater than 7°. While meeting
the same optical parameters, the primary mirror diameter is smaller than the
traditional Schmidt configurations. The camera is outside the lens tube, and there is no
heat source in the lens tube, so the optical image quality will not be affected. In addition, the
length of the lens tube is reduced by half; and the flat image surface has excellent image
quality.
Figure 1 is a schematic diagram of the optical structure of the invention.
Figure 2 is the structural diagram of the optical system of Embodiment 1.
Figure 3 is a full field image spot diagram (450-550nm band range) of Embodiment 1.
Figure 4 is a full field image spot diagram (550-700nm band range) of Embodiment 1.
Figure 5 is a full field image spot diagram (700-900nm band range) of Embodiment 1.
Figure 6 is the structural diagram of the optical system of Embodiment 2.
Figure 7 is a full field image spot diagram (450-550nm band range) of Embodiment 2.
Figure 8 is a full field image spot diagram (550-700nm band range) of Embodiment 2.
Figure 9 is a full field image spot diagram (700-900nm band range) of Embodiment 2.
Note: figures 2-9 are generated by optical design software Zemax OpticStudio, with
software serial number of L101809.
The invention is further described in combination with following figures and
Embodiments.
Embodiment 1
The design indexes of optical system were as follows.
Aperture: 600mm;
Optical field of view: 7.070 diameter for circular field of view (5x5° for square field of
view);
Image plane: 154mm diameter;
Pixel scale: 1.67 arc-seconds/10 im;
Telescope system surface occlusion: 18%;
Image quality: 80% energy concentration, diameter less than 15im;
Field of view vignetting: less than 5%;
Observation wavelength: 450nm-900nm.
The SiTian optical system with aperture of 600mm and focal ratio of 2.06 included an
aspheric corrector plate A with a central hole, a spherical or aspheric reflective primary
mirror B, a spherical lens C, a spherical lens D, a spherical lens E, an optical filter F, a camera window G and a focal plane H, which were arranged in sequence along the incident direction of light from front to back. Specifically, the aspheric corrector plate A was annular, and the diameter of the central hole was the maximum lens diameter of the corrector lens group. Located at the position of the optical system aperture stop, it was used to correct the spherical aberration of the spherical reflection primary mirror. The spherical corrector lens group was in front of the focal plane to correct aberrations and chromatic aberrations in the field of view. Further, the telescope was equipped with an optical filter to realize sub-band photometry observation and excellent image quality could be achieved through the thickness of the filter and sub-band focus compensation.
This optical system could obtain such a flat image plane with 80% of the energy of the
full field of view image quality concentrated in a 15m diameter circular area.
Image quality evaluation
When the observation wavelength was 450nm550nm, 80% of the full field of view
image quality energy was concentrated in a diameter range of 14.6um; when the
observation wavelength was 550nm-700nm, 80% of the full field of view image quality
energy was concentrated in a diameter range of 11.4m; when the observation
wavelength was 700nm-900nm, 80% of the full field of view image quality energy was
concentrated in a diameter range of 14.9m.
Optical System Parameters
Component Component Radius of Spacing Clear Aspheric label name curvature and Material aperture coefficient (mm) thickness (mm) A Aspheric Plane 24 Fused silica 600 corrector plate 30000 1300 a4=2.8E-11 B Primary mirror -2910 1228 Glass- 700 Ceramics C Corrector lens 1 -460 30 D-LAF82L 250 -180 6 D Corrector lens 2 -180 48 H-ZPK5 230 6800 77 E Optical filter Plane 10 Fused silica 180 Plane 15 F Camera window Plane 6 Fused silica 160 Plane 9 G Focal plane Plane 154 Embodiment 2 Optical system of catadioptric large field telescope (SiTian optical system), referring to Fig. 6
The design indexes of optical system were as follows.
Aperture: 1000mm;
Optical field of view: 7.070 diameter for circular field of view (5x5° for square field of
view);
Image plane: 255mm diameter;
Pixel scale: 1 arc-second/10[tm;
Telescope system surface occlusion: 21%;
Image quality: 80% energy concentration, diameter less than 20[m;
Field of view vignetting: less than 2%;
Observation wavelength: 400nm-900nm.
The SiTian optical system with aperture of 1000mm and focal ratio of 2.06 included an
aspheric corrector plate A with a central hole, a spherical or aspheric reflective primary
mirror B, a spherical lens C, a spherical lens D, a spherical lens E, an optical filter F, a
camera window G and a focal plane H, which were arranged in sequence along the
incident direction of light from front to back. Specifically, the aspheric corrector plate A was annular, and the diameter of the central hole was the maximum lens diameter of the corrector lens group. Located at the position of the optical system aperture stop, it was used to correct the spherical aberration of the spherical reflection primary mirror. The spherical corrector lens group was in front of the focal plane to correct aberrations and chromatic aberrations in the field of view. Further, the telescope was equipped with an optical filter to realize sub-band photometry observation and excellent image quality could be achieved through the thickness of the filter and sub-band focus compensation.
The optical system could obtain such a flat image plane with 80% of the energy of the
full field of view image quality concentrated in a 15m diameter circular area.
Image quality evaluation
When the observation wavelength was 400nm-550nm, 80% of the full field-of-view
image quality energy was concentrated in the diameter range of 20[m; when the
observation wavelength was 550nm-700nm, 80% of the full field-of-view image quality
energy was concentrated in the diameter range of 14.8tm; when the observation
wavelength was 700nm-900nm, 80% of the full field-of-view image quality energy was
concentrated in the diameter range of 19m.
Different from Embodiment 1, in Embodiment 2, a correction lens was added and the
primary mirror was aspheric, which further increased the aperture of the optical system
and the coverage of the wavelength band. Therefore, the resulting image quality was
excellent.
Optical System Parameters
Component Component Radius of Spacing Clear Aspheric label name curvature and Material aperture coefficient (mm) thickness (mm) A Aspheric plane 40 Fused silica 1000 corrector plate
54100 2200 a4=6.2E-12 Aspheric B pri Microcrystal 1258 k=-1 primarymirror -5060 2092 a4=6.2E-12 C Corrector lens 1 -784 65 H-APK5 452 935 2 D Corrector lens 2 915 40 H-BAK5 448 -412 0.2 E Corrector lens 3 -406 65 FPL53 392 11000 130 F Optical filter Plane 20 Fused silica 300 Plane 30 G Camera window Plane 20 Fused silica 270 Plane 9 H Focal plane Plane 255
Claims (5)
1. The SiTian optical system, characterized in that the catadioptric telescope optical
system is composed of an aspheric corrector plate A with a central hole, a spherical
or aspheric reflective primary mirror B, three spherical lenses of C, D and E, an
optical filter F, a camera window G and a focal plane H, which are arranged in
sequence along the incident direction of light from front to back.
2. The SiTian optical system as stated in Claim 1, characterized in that the aspheric
corrector plate A with a central hole is annular, wherein the diameter of the central
hole is about the maximum lens diameter of the corrector lens group. Located at the
position of the optical system aperture stop, the aspheric corrector plate A is used to
correct the spherical aberration of the spherical or aspherical reflection primary
mirror.
3. The SiTian optical system as stated in Claim 1, characterized in that the spherical
corrector lens group B is in front of the focal plane and used to correct aberrations
and chromatic aberrations in the field of view.
4. The SiTian optical system as stated in Claim 1, characterized in that the telescope is
equipped with an optical filter to realize sub-band photometry observation and further the
excellent image quality can be achieved by adjusting the thickness of the filter and sub-band
focusing compensation.
5. The SiTian optical system as stated in any one of Claims 1-4, characterized in that
the aspheric plate A with a central hole has a flat surface on one side, and an aspherical
surface with no optical power on the other side. The surface type is determined by the
following formula of
Z = 1+1 2r2 + a4 r 4 +a 6 r6 + ar 1+yi-l(1+k)c r2
Wherein, k is the aspherical conic coefficient, a4, a6, and as are the coefficients of the
aspherical surface, r is the height of the aspherical surface in the vertical direction from
the optical axis, and z is the horizontal distance from the aspherical surface to the center
of the lens.
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Cited By (1)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN115243017A (en) * | 2022-08-03 | 2022-10-25 | 上海研鼎信息技术有限公司 | Method and equipment for improving image quality |
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Cited By (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN115243017A (en) * | 2022-08-03 | 2022-10-25 | 上海研鼎信息技术有限公司 | Method and equipment for improving image quality |
| CN115243017B (en) * | 2022-08-03 | 2024-06-07 | 上海研鼎信息技术有限公司 | Method and equipment for improving image quality |
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