CN202885806U - Multifunctional astronomical theodolite - Google Patents
Multifunctional astronomical theodolite Download PDFInfo
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- CN202885806U CN202885806U CN 201220499608 CN201220499608U CN202885806U CN 202885806 U CN202885806 U CN 202885806U CN 201220499608 CN201220499608 CN 201220499608 CN 201220499608 U CN201220499608 U CN 201220499608U CN 202885806 U CN202885806 U CN 202885806U
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Abstract
The utility model provides a multifunctional astronomical theodolite, belongs to the technical field of an astrometric instrument and solves the problems of an axis collimation system in a low-latitude meridian circle that the structure is complicated and a data processing period is long. The multifunctional astronomical theodolite comprises a longitude and latitude base and a reflection telescope; a left horizontal axis and a right horizontal axis are respectively mounted on a left fork arm and a right fork arm; an upper disc is sleeved on an azimuth axis of a middle disc; an axis end of the azimuth axis is provided with an azimuth coded disc; the back end of the reflection telescope is provided with a micrometer dial with a CCD (Charge Coupled Device) camera; the left horizontal axis is provided with a coded disc No.1 and the right horizontal axis is provided with a coded disc No.2; the coded discs No.1and the No.2 are annular grating angle encoders; and the outer sides of the coded discs No.1 and the No.2 are respectively provided with two pairs of reading heads which are in diameter orthogonal distribution. According to the multifunctional astronomical theodolite disclosed by the utility model, a jerk value of each axis end can be solved by eccentric errors of each coded disc, the measurement efficiency of oscillating quantity of a height axis is improved and the detection structure is simple.
Description
Technical field
The utility model belongs to the astrometric instrument technical field, and is particularly a kind of for astrometric transit.
Background technology
In optical object's surveying instrument, meridian circle is used for measuring the fixed star coordinate, sets up reference frame at celestial sphere.Meridian instrument, prismatic astrolabe, photoelectric astrolabe, photographic zenith tube and zenith instrument etc. be used for to be measured universal time or Ghandler motion, for scientific research and national defense construction provide earth rotation parameter (ERP).They all take pedal line or mercury face as benchmark, by the mensuration of position of heavenly body, obtain desired measurement result.
External meridian circle is to be exclusively used in the astronomical instrument of measuring star place, setting up Celestial Reference System, and this instrument is helped to improve its theoretical precision of measuring star place by German astronomer Mei Ye and reached 2 rads by Denmark astronomer Luo Moyu invention in 1689.The astronomer Si Teluwei of Russia in 1839 have set up the principle of absolute determination position of heavenly body in newly-built pul Ke Wo astronomical observatory, and through after instrument manufacturing is progressively proposed strict requirement and progressively introduces utility appliance and technology, measuring accuracy progressively is improved, and has reached 0.4 rad to 20 middle of century.
Meridian circle originally is the refracting telescope of 15～20 centimetres of bores, 2.0～2.5 meters of focal lengths, by the pivot of lens barrel stage casing left and right horizontal axle axle head, is bearing in the V-type groove on the foundation pier of both sides, is close to the lens barrel place on the transverse axis vertical circle is housed.This instrument volume is larger, uses optical circle as the angle measurement benchmark, and requirement on machining accuracy is very high, carries out visual observation.And former observation procedure can only be implemented observation at high latitude area.In 20 end of the centurys, Yunnan Observatory has successfully been developed lower latitude meridian circle, adopts Observation principle and the method for original creation, has realized in the absolute determination of low latitudes to the position of heavenly body.Lower latitude meridian circle adopts autocollimator, uses optical circle as the main benchmark of measurement of angle, utilizes line array CCD as the photoelectric measurement element, has still used pivot, adopts gear drive.
Because lower latitude meridian circle uses optical circle to take measurement of an angle, the swing of its transverse axis axis has adopted the axle colimated light system to measure, axle colimated light system complex structure, and data processing cycle is long.
Summary of the invention
For solving axle colimated light system complex structure, the long problem of data processing cycle that is used for measuring height axle axis oscillating in the existing lower latitude meridian circle, the utility model provides a kind of Multifunction astronomical transit, and its technical scheme is as follows:
The Multifunction astronomical transit comprises longitude and latitude seat and the reflecting telescope that is installed on the longitude and latitude seat;
Described reflecting telescope is installed on the left transverse axis and the intermediate mass between the right transverse axis of longitude and latitude seat, the spindle nose of left transverse axis and right transverse axis is installed in respectively on the left yoke and right yoke that coils, upper dish is sleeved on the azimuth axis in the mid-game, the orientation code-disc is installed on the axle head of azimuth axis, between upper dish and the mid-game surface bearing is installed, mid-game is installed on the supporting base on the chassis, and the chassis is installed on the foundation pier;
Near the intermediate mass place vertical worm gear is installed on described left transverse axis or the right transverse axis, vertical worm gear and worm mesh, worm screw is connected with servomotor through kinematic train;
The rear end of described reflecting telescope is equipped with the dial gauge with the CCD camera;
The spindle nose of described left transverse axis and right transverse axis is cylindrical, is installed in respectively on the deep groove ball bearing that arranges on left yoke and the right yoke;
Be provided with a figure disc on the described left transverse axis, be provided with two figure discs on the right transverse axis, a described figure disc and two figure discs are the circular grating angular encoder;
At the left yoke that is positioned at the figure disc outside two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
1, B
1, C
1, D
1, read head A wherein
1Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
1, C
1Be the diameter setting, read head B
1, D
1Be the diameter setting, read head A
1, C
1Line and read head B
1, D
1Line orthogonal thereto;
At the right yoke that is positioned at the two figure discs outside two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
2, B
2, C
2, D
2, read head A wherein
2Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
2, C
2Be the diameter setting, read head B
2, D
2Be the diameter setting, read head A
2, C
2Line and read head B
2, D
2Line orthogonal thereto.
Detect the method for altitude axis axle head beat with above-mentioned Multifunction astronomical transit, comprise following sequential steps:
One figure disc, two figure discs and corresponding read head are installed;
Step 2.1: the orientation code-disc of transit is rotated to 0 °, make altitude axis along the east-west direction setting, make a figure disc be positioned at the west end of altitude axis, two figure discs are positioned at the east of altitude axis;
Step 2.2: by identical corner step pitch rotation altitude axis, make telescope point to respectively the identical default zenith distance of several spacings along meridian direction, when gathering each default zenith distance i of pointing of the telescope, read head A
1, C
1Poor (the A of reading
1-C
1)
i, read head B
1, D
1Poor (the B of reading
1-D
1)
i, read head A
2, C
2Poor (the A of reading
2-C
2)
i, read head B
2, D
2Poor (the B of reading
2-D
2)
i
Step 2.3: with all default zenith distance i and (A
1-C
1)
iIn the following formula 1 of substitution:
Formula 1:(A
1-C
1)
i=Δ A
01+ 2r
C11Sin (a
C11+ i)+v
i
V in the following formula
iBe stochastic error, from following formula, calculate parameter Δ A with least square method
01, r
C11And a
C11, wherein, Δ A
01Represent diameter read head A
1, C
1The zero deviation of difference of reading;
Step 2.4: with all default zenith distance i and (B
1-D
1)
iIn the following formula 2 of substitution:
Formula 2:(B
1-D
1)
i=Δ B
01+ 2r
C12Sin (a
C12+ i+90 °)+v
i
V in the following formula
iBe stochastic error, from following formula, calculate parameter Δ B with least square method
01, r
C12And a
C12, wherein, Δ B
01Represent diameter read head B
1, D
1The zero deviation of difference of reading;
Get r
C1=(r
C11+ r
C12)/2, the r in the formula
C1Represent the sinusoidal amplitude of periodicity eccentric error of a figure disc;
Get a
C1=(a
C11+ a
C12)/2, a in the formula
C1Represent the sinusoidal initial phase of periodicity eccentric error of a figure disc;
Step 2.5: with all default zenith distance i and (A
2-C
2)
iIn the following formula 3 of substitution:
Formula 3:(A
2-C
2)
i=Δ A
02+ 2r
C21Sin (a
C21+ i)+v
i
V in the following formula
iBe stochastic error, from following formula, calculate parameter Δ A with least square method
02, r
C21And a
C21, wherein, Δ A
02Represent diameter read head A
2, C
2The zero deviation of difference of reading;
Step 2.6: with all default zenith distance i and (B
2-D
2)
iIn the following formula 4 of substitution:
Formula 4:(B
2-D
2)
i=Δ B
02+ 2r
C22Sin (a
C22+ i+90 °)+v
i
V in the following formula
iBe stochastic error, from following formula, calculate parameter Δ B with least square method
02, r
C22And a
C22, wherein, Δ B
02Represent diameter read head B
2, C
2The zero deviation of difference of reading;
Get r
C2=(r
C21+ r
C22)/2, the r in the formula
C2Represent the sinusoidal amplitude of periodicity eccentric error of two figure discs;
Get a
C2=(a
C21+ a
C22)/2, a in the formula
C2Represent the sinusoidal initial phase of periodicity eccentric error of two figure discs;
Step 3.1: the orientation code-disc of transit is rotated to 0 °, make altitude axis along the east-west direction setting, make a figure disc be positioned at the west end of altitude axis, two figure discs are positioned at the east of altitude axis;
Step 3.2: along meridian direction rotation altitude axis, make telescope point to respectively the celestial body to be measured that zenith distance is z, gather read head A
1, C
1Poor (the A of reading
1-C
1)
z, read head B
1, D
1Poor (the B of reading
1-D
1)
z, read head A
2, C
2Poor (the A of reading
2-C
2)
i, read head B
2, D
2Poor (the B of reading
2-D
2)
i, among the following formula 5-8 of difference substitution, and will find the solution the Δ A that obtains in the step 2
01, Δ B
01, r
C1And a
C1, and Δ A
02, Δ B
02, r
C2And a
C2Among the following formula 5-8 of substitution:
Formula 5:
Formula 6:
Formula 7:
Formula 8:
Calculated respectively by above-mentioned formula
With
Wherein,
With
The side-play amount that the altitude axis west is held northwards and made progress when being respectively observation celestial body to be measured,
With
The altitude axis the east side-play amount with making progress to the south when being respectively observation celestial body to be measured;
Get
The altitude axis the east is with respect to the beat amount of west end on North and South direction when observing celestial body to be measured;
Get
The beat amount that the altitude axis the east makes progress with respect to the west end when observing celestial body to be measured.
In the said method, the default zenith distance i in the described step 2 can be that the step pitch between-75 ° and 75 ° is 1 ° round values angle.
In the said method, the described side-play amount that makes progress all refers to the side-play amount on the direction opposite with gravity direction, such as:
Altitude axis west end side-play amount upwards when observing celestial body to be measured, its implication is
The side-play amount of altitude axis west end on the direction opposite with gravity direction when observing celestial body to be measured.
The utility model adopts the two ends at altitude axis, a height steel band code-disc respectively is set, it is the digital angle scrambler, and two pairs of read heads that the quadrature diameter distributes, variation by each code-disc eccentric error, it is the variation of the difference of diameter two read head readings, calculate respectively beat direction and value that each axle head is caused by axial system error, and then calculate direction and the value of the real-time beat of altitude axis in observation process, thereby substitute the axle collimating apparatus, because the measurement result of grating encoder is digital quantity, therefore greatly improved the efficient of altitude axis string pendulum momentum survey, and detection architecture is simpler.Originally adopt the axle colimated light system to measure axis oscillating, obtain analog image, carry out again digital processing and obtain digital signal.Observe every night the image that obtains, needed process in 4 hours consuming time.And after adopting the dicode dish to detect, can immediately obtain to swing parameter, even realize the real time measure.
For there is scoring errors in the orientation code-disc that solves existing astronomical theodolite, affect the problem of accuracy of observation, the utility model provides the code-disc delineation of a kind of Multifunction astronomical transit orientation to correct device, and its technical scheme is as follows:
Along coiling on the orientation code-disc periphery two pairs of read heads that are the diameter omnidirectional distribution are installed, the angle between adjacent two read heads is 90 °.
Come the delineation correcting method of the other side's bit code dish to comprise following sequential steps with above-mentioned Multifunction astronomical transit:
Step 1: erecting equipment:
Coiling of orientation code-disc periphery read head is installed;
Choose some fixed star i to be measured, every fixed star i to be measured 2 is observed and calculates to step 6 according to the following steps;
Step 2: the star overwriting moment initial value t that obtains fixed star i to be measured
0:
Select one of them fixed star i to be measured, orientation code-disc with transit rotates to position angle A first, 12 seconds constantly before fixed star i star picture to be measured passes through the range of telescope perpendicular bisector of transit, use first the CCD camera to fixed star i star to be measured as 6 seconds of exposure, then with 12 seconds rotating around azimuth axis the longitude and latitude seat of transit, make orientation code-disc rotation to position angle A+180 °, and with telescope around horizontal rotational shaft, the angle of rotation is the twice angle of the zenith distance of fixed star i to be measured, make telescope again point to this fixed star i to be measured and 6 seconds of exposure, calculate the star overwriting initial value t of fixed star i to be measured by following formula
0:
t
0＝(t
(A)+t
(A+180°))/2+Δx·k/cosδ；
In the following formula, t
(A)When representing code-disc rotation in orientation to position angle A fixed star i to be measured star as exposure constantly, t
(A, A+180 °)When representing code-disc rotation in orientation to position angle A+180 ° fixed star i to be measured star as exposure constantly, the star image position of fixed star i to be measured on CCD camera target surface was poor when Δ x represented the orientation code-disc and rotates respectively to position angle A and A+180 °, k represents the picture dot engineer's scale of the CCD camera of main optical path system, and δ represents the apparent declination of fixed star i to be measured;
Step 3: cross constantly t by following formula theory of computation star
1:
In the following formula,
In the following formula,
In the above-mentioned formula, α represents the apparent right ascension of fixed star i to be measured, t
2Represent the angle between declination circle and the meridian circle, i.e. hour angle, q represent the parallactic angle that consists of between the vertical circle of the declination circle of fixed star i to be measured and position angle A,
Represent local adopted lattide, δ represents the apparent declination of fixed star i to be measured;
Step 4: by the deviation delta A of following formula calculating observation true bearing constantly with respect to the nominal orientation:
ΔA＝-cosδ?cosq?cscz?Δt；
In the following formula, δ represents the apparent declination of fixed star i to be measured, and q represents the parallactic angle that consists of between the vertical circle of the declination circle of fixed star i to be measured and position angle A, and z represents the zenith distance of fixed star i to be measured;
In the following formula, Δ t=t
0-t
1
Step 5: the mean value θ of the orientation code wheel reading when calculating the observation of rotating shaft front and back by following formula:
θ＝(θ
(A)+θ
(A+180°)-180°)/2；
In the following formula, θ
(A)When representing orientation code-disc rotation to position angle A, the mean value of four read head readings of orientation code-disc periphery, θ
(A+180 °)When representing orientation code-disc rotation to position angle A+180 °, the mean value of four read head readings of orientation code-disc periphery;
Step 6: with the Δ A in the step 4 and the following formula of θ substitution in the step 5, when the computer azimuth code-disc rotates to position angle A, the correction reading A of orientation code-disc
i:
A
i＝ΔA+θ；
Step 7: the A that gets all fixed star i to be measured
iThe arithmetic mean of value namely obtains described transit when the orientation code-disc rotates to position angle A, the correction reading A of orientation code-disc
(A)
Above-mentioned position angle A can be 45 °, 90 ° or 135 °.
Utilize the utility model to correct device, can detect and correct astronomical theodolite orientation code-disc scoring errors easily, realize the raising of Instrument observation precision, mainly be that the scoring errors of code-disc is done correction, take the circular grating scrambler of Reinshaw as example, the dividing precision of the product of its 200mm diameter approximately 0.9 ", adopt this method should bring up to approximately 0.1 ", so that the reading of orientation code-disc is more reliable.
As preferred version of the present utility model:
The axle body of the left transverse axis between left yoke and intermediate mass is truncated cone-shaped, and the axle body of the right transverse axis between right yoke and intermediate mass is truncated cone-shaped.This structure is in order to make the performance of the rigidity such as it has, and purpose is to use less material to obtain larger rigidity.
As preferred version of the present utility model:
Described reflecting telescope is Cassegrain telescope, comprise primary mirror and secondary mirror, lens barrel between primary mirror and secondary mirror is provided with an autocollimation level crossing, the normal of autocollimation level crossing is parallel with the optical axis of primary mirror, the secondary mirror focus place that is positioned at the medium pore rear end of primary mirror is provided with the CCD camera, be provided with half-reflecting half mirror between primary mirror and the CCD camera, be provided with slit plate at the catoptrical optical axis of half-reflecting half mirror, be provided with a unthreaded hole on the slit plate.
The course of work of above-mentioned autocollimation level crossing is as follows: bulb is set behind slit plate, the light that bulb sends is by behind the slit plate, form 1 pointolite, after half-reflecting half mirror, secondary mirror and primary mirror reflection, form directional light, directional light is returned by the autocollimation flat mirror reflects perpendicular to optical axis, by behind the half-reflecting half mirror, is imaging on the CCD photoelectric device light-sensitive surface in the focal plane of primary mirror again.Because the impact of gravity, when the different height of pointing of the telescope, the optical axis that telescope primary mirror and secondary mirror can relative intermediate mass produce small deflection and then make main optical path is with respect to intermediate mass, also namely deflect with respect to the autocollimation level crossing, at this moment the some the position of image on the CCD light-sensitive surface will be moved.
As preferred version of the present utility model:
The front and back ends of described right yoke respectively is equipped with an electric level, and described electric level comprises collimator and quicksilver horizon, and collimator is straight down, be installed on the right yoke, quicksilver horizon be arranged on be positioned at collimator below on coil;
In the described collimator along being disposed with from the top down CCD camera, half-reflecting half mirror and collimating mirror on the optical axis, catoptrical optical axis at half-reflecting half mirror is provided with the light source slit plate, be provided with three row unthreaded holes on the light source slit plate, be provided with three unthreaded holes on every row.
The course of work of above-mentioned electric level is as follows: the light that sends at the light source slit plate forms 3 * 3 pointolites, through half-reflecting half mirror, behind the collimating mirror, form directional light, directional light is reflected by the mercury reflecting surface perpendicular to the quicksilver horizon of optical axis, again by behind the half-reflecting half mirror, imaging on the light-sensitive surface of the CCD camera on the focal plane of collimating mirror, when the above part integral body run-off the straight of dish on the moving instrument of the upper dribbling of instrument, the optical axis of collimator has represented gravity direction with respect to the mercury reflecting surface, can think the constant small deflection that has, thereby the position of the some picture battle array that becomes on the CCD light-sensitive surface is changed.The electricity level is in fact to adopt the mercury face to replace the autocollimation level crossing, and the characteristics of bringing thus are: when the common mercury face of the relative mercury face of telescope is the constant small inclination that has, can detect tilt quantity by self-collimation measurement.
The utility model Multifunction astronomical transit is a kind of small-sized, light, full automatic astrometric instrument with several functions, it is the small-sized reflecting telescope with multiple error measuring means, it can intersect in any a plurality of uniform orientation observation, and can the real time measure and the various error instantaneous values of elimination instrument.
The Multifunction astronomical transit can be used for carrying out the mensuration of astronomical warp, latitude, extracts the information of clean, reliable pedal line direction ANOMALOUS VARIATIONS, and by pedal line ANOMALOUS VARIATIONS triangle monitoring net, the extraction information of earthquake; Be used to simultaneously and rebuild China's earth rotation parameter (ERP) terrestrial optical measuring system, high-precision universal time and latitude determination value are provided routinely; It can also be at the instantaneous astronomical atmospheric refraction of a plurality of uniform direction-findings, set up local multi-faceted astronomical atmospheric refraction Model Measured and the Model Measured of atmospheric refraction delay correction, except get rid of pedal line change in the various systematic errors that cause of atmospheric factor and being conducive to the GPS measurement matches, also as future relevant department set up the needs of local atmospheric refraction model and the surveying instrument produced; In addition, according to the feasibility of studying in advance at present, it can also tilt on ground on every side, long term monitoring fixed observer station, and by its astronomical sight of self and cooperating of non-astronomical sight, obtains round-the-clock pedal line change picture.
Aspect apparatus structure, compare with lower latitude meridian circle, done many-sided improvement, mainly contain: adopt circular grating scrambler (being called for short the ring grating) to substitute optical circle, be used for the control of instrument corner and the high-acruracy survey of corner, realize the digitizing of measurement of angle, improved measuring accuracy; Electricity level system adopts area array CCD to substitute line array CCD as detector, and adopts the porous star tester to replace slit plate; Adopt two height code-discs to detect the beat of altitude axis, realized the robotization of measuring, improved measuring accuracy, reduced the accuracy requirement to machining.
Description of drawings
Fig. 1 is the front view of the utility model Multifunction astronomical transit;
Fig. 2 is read head A among Fig. 1
1, B
1, C
1, D
1Along the perspective view of W direction on a figure disc;
Fig. 3 is read head A among Fig. 1
2, B
2, C
2, D
2Along the perspective view of E direction on two figure discs;
Fig. 4 is four distribution schematic diagrams that are the read head of diameter omnidirectional distribution installing along orientation code-disc periphery among Fig. 1;
Fig. 5 is the telescopical index path among Fig. 1;
Fig. 6 is the index path of the electric level among Fig. 1.
Embodiment
Multifunction astronomical transit as shown in Figure 1 comprises longitude and latitude seat and the reflecting telescope 8 that is installed on the longitude and latitude seat;
Described reflecting telescope 8 is installed on the left transverse axis 5 and the intermediate mass 9 between the right transverse axis 6 of longitude and latitude seat, the spindle nose of left transverse axis 5 and right transverse axis 6 is installed in respectively on the left yoke 3 and right yoke 4 on the dish 20, upper dish 20 is sleeved on the azimuth axis 15 in the mid-game 19, orientation code-disc 16 is installed on the axle head of azimuth axis 15, between upper dish 20 and the mid-game 19 surface bearing 13 is installed, mid-game 19 is installed on the supporting base 14 on the chassis 18, and chassis 18 is installed on the foundation pier 17;
Near intermediate mass 9 places vertical worm gear 11 is installed on described left transverse axis 5 or the right transverse axis 6, vertical worm gear 11 and worm mesh, worm screw is connected with servomotor through kinematic train;
The rear end of described reflecting telescope 8 is equipped with the dial gauge with the CCD camera;
The spindle nose of described left transverse axis 5 and right transverse axis 6 is cylindrical, is installed in respectively on the deep groove ball bearing 7 that arranges on left yoke 3 and the right yoke 4;
Be provided with a figure disc 1 on the described left transverse axis 5, be provided with two figure discs 2 on the right transverse axis 6, a described figure disc 1 and two figure discs 2 are the circular grating angular encoder;
As shown in Figure 2, at the left yoke 3 that is positioned at a figure disc 1 outside two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
1, B
1, C
1, D
1, read head A wherein
1Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
1, C
1Be the diameter setting, read head B
1, D
1Be the diameter setting, read head A
1, C
1Line and read head B
1, D
1Line orthogonal thereto;
As shown in Figure 3, at the right yoke 4 that is positioned at two figure discs, 2 outsides two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
2, B
2, C
2, D
2, read head A wherein
2Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
2, C
2Be the diameter setting, read head B
2, D
2Be the diameter setting, read head A
2, C
2Line and read head B
2, D
2Line orthogonal thereto.
As shown in Figure 4, along two pairs of read heads 12 that are the diameter omnidirectional distribution are installed on the upper dish 20 of orientation code-disc 16 peripheries, the angle between adjacent two read heads 12 is 90 °.
As shown in Figure 1, the axle body of the left transverse axis 5 between left yoke 3 and intermediate mass 9 is truncated cone-shaped, and the axle body of the right transverse axis 6 between right yoke 4 and intermediate mass 9 is truncated cone-shaped.
As shown in Figure 5, described reflecting telescope 8 is Cassegrain telescope, comprise primary mirror 23 and secondary mirror 24, lens barrel between primary mirror 23 and secondary mirror 24 is provided with an autocollimation level crossing 25, the normal of autocollimation level crossing 25 is parallel with the optical axis of primary mirror 23, the secondary mirror focus place that is positioned at the medium pore rear end of primary mirror 23 is provided with CCD camera 28, be provided with half-reflecting half mirror 26 between primary mirror 23 and the CCD camera 28, catoptrical optical axis at half-reflecting half mirror 26 is provided with slit plate 27, is provided with a unthreaded hole on the slit plate 27.
As shown in Figure 1, the front and back ends of described right yoke 4 respectively is equipped with an electric level, and described electric level comprises collimator 22 and quicksilver horizon 21, and collimator 22 is straight down, be installed on the right yoke 4, quicksilver horizon 21 is arranged on the upper dish 20 that is positioned at collimator 22 belows;
As shown in Figure 6, in the described collimator 22 along being disposed with from the top down CD camera 29, half-reflecting half mirror 30 and collimating mirror 31 on the optical axis, catoptrical optical axis at half-reflecting half mirror 30 is provided with light source slit plate 32, be provided with three row unthreaded holes on the light source slit plate 32, be provided with three unthreaded holes on every row.
Claims (5)
1. the Multifunction astronomical transit comprises longitude and latitude seat and the reflecting telescope (8) that is installed on the longitude and latitude seat;
Described reflecting telescope (8) is installed on the left transverse axis (5) and the intermediate mass (9) between the right transverse axis (6) of longitude and latitude seat, the spindle nose of left transverse axis (5) and right transverse axis (6) is installed in respectively on the left yoke (3) and right yoke (4) on the dish (20), upper dish (20) is sleeved on the azimuth axis (15) in the mid-game (19), orientation code-disc (16) is installed on the axle head of azimuth axis (15), between upper dish (20) and the mid-game (19) surface bearing (13) is installed, mid-game (19) is installed on the supporting base (14) on the chassis (18), and chassis (18) are installed on the foundation pier (17);
Described left transverse axis (5) or right transverse axis (6) are upper locates to be equipped with vertical worm gear (11) near intermediate mass (9), vertical worm gear (11) and worm mesh, and worm screw is connected with servomotor through kinematic train;
It is characterized in that:
The rear end of described reflecting telescope (8) is equipped with the dial gauge with the CCD camera;
The spindle nose of described left transverse axis (5) and right transverse axis (6) is cylindrical, is installed in respectively on the upper deep groove ball bearing (7) that arranges of left yoke (3) and right yoke (4);
Be provided with a figure disc (1) on the described left transverse axis (5), be provided with two figure discs (2) on the right transverse axis (6), a described figure disc (1) and two figure discs (2) are the circular grating angular encoder;
At the left yoke (3) that is positioned at a figure disc (1) outside two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
1, B
1, C
1, D
1, read head A wherein
1Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
1, C
1Be the diameter setting, read head B
1, D
1Be the diameter setting, read head A
1, C
1Line and read head B
1, D
1Line orthogonal thereto;
At the right yoke (4) that is positioned at two figure discs (2) outside two pairs of read heads that are the diameter omnidirectional distribution are set, are respectively read head A by arranged clockwise
2, B
2, C
2, D
2, read head A wherein
2Be positioned at the top of vertical direction, the angle between adjacent two read heads is 90 °, read head A
2, C
2Be the diameter setting, read head B
2, D
2Be the diameter setting, read head A
2, C
2Line and read head B
2, D
2Line orthogonal thereto.
2. Multifunction astronomical transit according to claim 1 is characterized in that:
Along two pairs of read heads (12) that are the diameter omnidirectional distribution are installed on the upper dish (20) of orientation code-disc (16) periphery, the angle between adjacent two read heads (12) is 90 °.
3. Multifunction astronomical transit according to claim 1 and 2 is characterized in that:
The axle body that is positioned at the left transverse axis (5) between left yoke (3) and the intermediate mass (9) is truncated cone-shaped, and the axle body that is positioned at the right transverse axis (6) between right yoke (4) and the intermediate mass (9) is truncated cone-shaped.
4. Multifunction astronomical transit according to claim 3 is characterized in that:
Described reflecting telescope (8) is Cassegrain telescope, comprise primary mirror (23) and secondary mirror (24), be positioned on the lens barrel between primary mirror (23) and the secondary mirror (24) and be provided with an autocollimation level crossing (25), the normal of autocollimation level crossing (25) is parallel with the optical axis of primary mirror (23), the secondary mirror focus place that is positioned at the medium pore rear end of primary mirror (23) is provided with CCD camera (28), be provided with half-reflecting half mirror (26) between primary mirror (23) and the CCD camera (28), catoptrical optical axis at half-reflecting half mirror (26) is provided with slit plate (27), is provided with a unthreaded hole on the slit plate (27).
5. Multifunction astronomical transit according to claim 4 is characterized in that:
The front and back ends of described right yoke (4) respectively is equipped with an electric level, described electric level comprises collimator (22) and quicksilver horizon (21), collimator (22) is straight down, be installed on the right yoke (4), quicksilver horizon (21) is arranged on the upper dish (20) that is positioned at collimator (22) below;
In the described collimator (22) along being disposed with from the top down CCD camera (29), half-reflecting half mirror (30) and collimating mirror (31) on the optical axis, catoptrical optical axis at half-reflecting half mirror (30) is provided with light source slit plate (32), and the light source slit plate is provided with several unthreaded holes on (32).
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| CN 201220499608 CN202885806U (en) | 2012-09-27 | 2012-09-27 | Multifunctional astronomical theodolite |
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| CN 201220499608 CN202885806U (en) | 2012-09-27 | 2012-09-27 | Multifunctional astronomical theodolite |
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Cited By (6)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN102878977A (en) * | 2012-09-27 | 2013-01-16 | 中国科学院云南天文台 | Multifunctional astronomical theodolite |
| CN103499331A (en) * | 2013-09-28 | 2014-01-08 | 中国科学院云南天文台 | Novel astrolabe |
| CN103837159A (en) * | 2014-03-04 | 2014-06-04 | 中国科学院光电技术研究所 | Orthogonal decoupling correction method for theodolite orientation correction model |
| CN108508842A (en) * | 2018-04-04 | 2018-09-07 | 中国工程物理研究院激光聚变研究中心 | The straightness error detection method of numerically-controlled machine tool the linear guide |
| CN112212825A (en) * | 2020-09-27 | 2021-01-12 | 中国科学院西安光学精密机械研究所 | Coaxial auto-collimation adjusting device and method for pitch axis of theodolite for astronomical observation |
| CN113251995A (en) * | 2021-05-18 | 2021-08-13 | 中国科学院云南天文台 | Method for obtaining all-weather astronomical longitude and latitude indirect measurement value |
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2012
- 2012-09-27 CN CN 201220499608 patent/CN202885806U/en not_active Withdrawn - After Issue
Cited By (10)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN102878977A (en) * | 2012-09-27 | 2013-01-16 | 中国科学院云南天文台 | Multifunctional astronomical theodolite |
| CN102878977B (en) * | 2012-09-27 | 2014-10-08 | 中国科学院云南天文台 | Multifunctional astronomical theodolite |
| CN103499331A (en) * | 2013-09-28 | 2014-01-08 | 中国科学院云南天文台 | Novel astrolabe |
| CN103837159A (en) * | 2014-03-04 | 2014-06-04 | 中国科学院光电技术研究所 | Orthogonal decoupling correction method for theodolite orientation correction model |
| CN103837159B (en) * | 2014-03-04 | 2016-08-31 | 中国科学院光电技术研究所 | A kind of theodolite points to correction model orthogonalization decoupling modification method |
| CN108508842A (en) * | 2018-04-04 | 2018-09-07 | 中国工程物理研究院激光聚变研究中心 | The straightness error detection method of numerically-controlled machine tool the linear guide |
| CN112212825A (en) * | 2020-09-27 | 2021-01-12 | 中国科学院西安光学精密机械研究所 | Coaxial auto-collimation adjusting device and method for pitch axis of theodolite for astronomical observation |
| CN112212825B (en) * | 2020-09-27 | 2021-10-15 | 中国科学院西安光学精密机械研究所 | Coaxial auto-collimation adjusting device and method for pitch axis of theodolite for astronomical observation |
| CN113251995A (en) * | 2021-05-18 | 2021-08-13 | 中国科学院云南天文台 | Method for obtaining all-weather astronomical longitude and latitude indirect measurement value |
| CN113251995B (en) * | 2021-05-18 | 2023-03-21 | 中国科学院云南天文台 | Method for obtaining all-weather astronomical longitude and latitude indirect measurement value |
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