CN103048701B - Atmospheric optical parameter measurer for astronomical site survey - Google Patents
Atmospheric optical parameter measurer for astronomical site survey Download PDFInfo
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- CN103048701B CN103048701B CN201210566259.3A CN201210566259A CN103048701B CN 103048701 B CN103048701 B CN 103048701B CN 201210566259 A CN201210566259 A CN 201210566259A CN 103048701 B CN103048701 B CN 103048701B
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Abstract
The invention discloses an atmospheric optical parameter measurer for astronomical site survey. The measurer consists of a small telescope, a charge-coupled device (CCD) image sensor and a computer, and is characterized in that a collimator (with a grid division board) and an entrance pupil splitting mirror are sequentially arranged in front of an entrance pupil of the small telescope; and an openable/closable beam splitter, a four-channel photon counting part, an optical imaging relay lens and a CCD image sensor are sequentially arranged on an optical axis behind the entrance pupil of the small telescope, wherein the four-channel photon counting part is positioned on the focal plane of the small telescope; the grid division board and a wide-field eyepiece are positioned above the beam splitter; and the output of the four-channel photon counting part and the CCD image sensor is connected with the computer. The atmospheric optical parameter measurer for the astronomical site survey can be used for simultaneously measuring atmospheric seeing, free atmosphere seeing, an isoplanatic angle and an approximate turbulence intensity profile, and is convenient to assemble and adjust and high in reliability.
Description
Technical field
The present invention relates to atmospheric optics field, be specifically related to a kind of atmospheric optical parameter measurer for astronomical site survey, is a kind of measuring equipment carrying out atmosphere optical parameter measurement.
Background technology
Using the occasion of ADAPTIVE OPTICS SYSTEMS, needing to understand the parameters such as local, atmospheric seeing at that time, the addressing of Ye Shi astronomical observatory and the indispensable important parameter of astronomical sight.The parameter of quantitative description atmospheric seeing is exactly atmospheric coherence length, and it characterizes the air coherence in a certain specific light path on certain horizontal spacing, and is used widely in the omnidistance atmospheric turbulence intensity of sign and adaptive optics phase correction techniques.
Be the major parameter determining ADAPTIVE OPTICS SYSTEMS correction visual field etc. dizzy angle, it characterizes the angle-dependence of the light wave wavefront being arrived observation station by atmospheric turbulence.If the angle between the two-beam of the different directions of the system of arrival such as to exceed at the dizzy angle, the correlativity between them will reduce rapidly.
When light wave transmits in turbulent atmosphere, light wave parameter (intensity, phase place and the direction of propagation etc.) rises and falls because of turbulent perturbation, this fluctuating is caused by refractive index random variation, therefore to Refractive-index-structure parameter be measured as the research drift of light beam and expansion, the transmission etc. of image provides foundation.Simultaneously by the distribution of turbulence intensity with path, the parameter of some other sign turbulent flow conditions can be calculated, as coherent length, etc. dizzy angle etc.
Current existing atmospheric seeing monitor, such as difference image moving monitor, by adding up the relative motion Real-Time Monitoring atmospheric seeing of single astrology two small-bore imagings in pupil plane.This apparatus structure is simple, and the station seeing be widely used in is measured, and China is in Yunnan Observatory and the prosperous research station of Nation Astronomical Observatory, and the places such as western Astronomical Site Testing had this Seeing Monitor to run.
Its concrete structure and principle of work are: on small-bore (about 350mm) telescopical entrance pupil, usually place the entrance pupil segmentation mirror that a piece has two sub-aperture (50-100mm), and in sub-aperture, place little angle of wedge wedge mirror, the wavefront of this sub-aperture of arrival is made to produce, thus same target satellite produces nonoverlapping double image after two sub-aperture, finally record a series of double image with ccd image sensor, and count the variance of double image relative position, can seeing be calculated.
Need by converting to the measurement of atmospheric turbulence intensity etc. the measurement at dizzy angle, the method for most convenient uses stellar scintillation method, namely according to the fluctuating variance of the light intensity of fixed star, and the dizzy angles such as measurement.
Based on atmospheric seeing and etc. the measuring method at dizzy angle, the while of existing or completed the instrument of these two parameter measurements by replacing pupil template.And the multiple aperture sensor that glitters is glittered by the star image measured on different size aperture, utilize glitter and turbulent flow relation gain freedom atmospheric seeing and etc. dizzy angle.
At present, the measurement means of turbulence profile mainly contains the methods such as sounding balloon, the radar inverting of Wind outline ripple and acoustic radar measurement, but they have respective deficiency, as data are, non-light-wave band is directly measured, measuring accuracy is not high, measuring distance is limited, need the supporting measurement of other parameters, limits target zone and the precision of measurement.And the multiple aperture adopting light-wave band to measure glitters, sensor is directly measured measured, there is real-time superiority, can measure simultaneously free atmosphere seeing, etc. multiple atmospheric optical parameters such as dizzy angle and approximate turbulence profile, be successfully configured Cerro Tololo, Mauna Kea, Cerro Paranal, 30 meters of telescope addressing points, South Pole Dome C etc. carry out the measurement of platform location.In addition, combination multiple aperture glitters sensor and difference image moving monitor, makes full use of both advantages, and is successfully applied to 30 meters of telescope addressings.China there is no the successful Application multiple aperture sensor that glitters and measures, and also lacks the research to its gordian technique.But multiple aperture glitters sensor construction complexity, and difficulty of processing is high, and difficulty is debug at scene.
Therefore, at present need a kind of new atmospheric optical parameter measurer for astronomical site survey, this measuring instrument need make full use of multiple aperture and to glitter the advantage of sensor and difference image moving monitor, meets scene simultaneously and debugs conveniently, reliably and with long-term.And not yet there is this measuring instrument in prior art.
summary of the invention
The object of this invention is to provide a kind of can measure simultaneously atmospheric seeing, free atmosphere seeing, etc. the atmospheric optical parameter measurer for astronomical site survey of dizzy angle and approximate turbulence profile, this atmospheric optical parameter measurer for astronomical site survey is debug conveniently, good reliability.
The technical scheme of patent of the present invention is as follows: a kind of atmospheric optical parameter measurer for astronomical site survey, is made up of, it is characterized in that race glass, CCD image sensor and computing machine:
In the front at described race glass entrance pupil place, be provided with successively: parallel light tube U1, entrance pupil segmentation mirror U2(with grid graticule are, entrance pupil segmentation mirror U2 is positioned at race glass entrance pupil place, and parallel light tube U1 is arranged on entrance pupil segmentation mirror U2 front, and its light source is grid graticule);
On the optical axis at the rear at described race glass entrance pupil place, be provided with successively: can the spectroscope (abbreviation spectroscope) of folding, four-way photon counting parts U3, optical imagery relay lens and ccd image sensor; Wherein, four-way photon counting parts U3 is positioned on race glass focal plane;
Grid graticule and wide visual field eyepiece be positioned at described can spectroscopical top of folding;
The output of described four-way photon counting parts, ccd image sensor, connects described computing machine.
In other words, atmospheric optical parameter measurer for astronomical site survey of the present invention primarily of parallel light tube, entrance pupil segmentation mirror, race glass, can the spectroscope of folding, grid graticule, eyepiece, four-way photon counting parts, optical imagery relay lens, CCD image sensor and computing machine composition.Entrance pupil segmentation mirror front is provided with parallel light tube, and its light source is grid graticule; Entrance pupil segmentation mirror is positioned at the entrance pupil place of race glass, and it is made up of 1 through hole, 2 identical angle of wedge wedge mirrors and 1 cover wedge mirror group; Wedge mirror group is made up of with 3 ring wedge mirrors of the angle of wedge and 1 wedge mirror the concyclic heart; Front, race glass focal plane is provided with can the spectroscope of folding, is provided with grid graticule and eyepiece above spectroscope; Race glass focal plane is provided with four-way photon counting parts, four-way photon counting parts axis is through hole, and 4 photomultipliers are arranged on around this through hole end; Central area, focal plane is imaged onto on ccd image sensor by optical imagery relay lens.
In above scheme, the structure of described four-way photon counting parts is: be provided with the bearing that axis is through hole; This bearing is provided with four photomultipliers be evenly distributed on same circle.
The structure of described entrance pupil segmentation mirror is: be provided with the bearing with through hole; This bearing is provided with the wedge mirror of two the identical angles of wedge be evenly distributed on same circle, a through hole and a wedge mirror group; Wherein the angle of wedge of two wedge mirrors is 25 ".
To above-mentioned each component content and be used as following explanation:
After spectroscope bullet closes, from the parallel light wave of parallel light tube by the entrance pupil segmentation through hole of mirror and race glass, through spectroscope light splitting, a road light wave images on grid graticule, another road light wave is optically imaged relay lens and images on CCD image sensor, debugs for system.After spectroscope flicks, from the parallel light wave of parallel light tube by the entrance pupil segmentation through hole of mirror and race glass system, be directly optically imaged relay lens and image on CCD image sensor, backup system automatic focusing.
After spectroscope flicks, from single starlight ripple through entrance pupil segmentation mirror is divided into two-beam ripple after 2 identical angle of wedge wedge mirror deviations, be incident on race glass, and image in CCD image sensor through optical imagery relay lens simultaneously, measure for atmospheric seeing; From single starlight ripple through entrance pupil segmentation mirror is divided into four bundle light waves after wedge mirror group deviation, be incident on race glass, and converge on 4 photomultipliers of four-way photon counting parts respectively, for measurement of glittering.Computing machine utilize glitter and the relation of turbulent flow directly measure free atmosphere seeing and etc. dizzy angle, use inverse problem computational algorithm to recover approximate turbulence profile simultaneously.
The object of this invention is to provide a kind of can measure simultaneously atmospheric seeing, free atmosphere seeing, etc. the atmospheric optical parameter measurer for astronomical site survey of dizzy angle and approximate turbulence profile, this atmospheric optical parameter measurer for astronomical site survey is debug conveniently, good reliability.Relative to prior art, the invention has the beneficial effects as follows: (1) structure adopts parallel light tube, grid graticule and wide visual field eyepiece facilitate system for field to debug.(2) structure adopts parallel light tube and CCD image sensor, backup system automatic focusing.(3) entrance pupil segmentation mirror optical spectroscopy there is not yet open report so far.Entrance pupil pupil segmentation mirror is composed individual components by this technology, and extraneous vibration does not affect entrance pupil segmentation mirror performance.This technical side atmospheric optical parameter measurer for astronomical site survey scene debug, greatly improve reliability.
accompanying drawing explanation
Fig. 1 is light channel structure figure of the present invention.
Fig. 2 is the structural representation of entrance pupil of the present invention segmentation mirror and four-way photon counting parts.
embodiment
Embodiment 1, atmospheric optical parameter measurer for astronomical site survey.See Fig. 1 and Fig. 2: the bore of race glass 1 is Φ 355.6mm, and focal length is 3910mm, 400 ~ 700 nanometer apochromatism broadband imagings, centre wavelength is 550 nanometers.Parallel light tube U1 is arranged on entrance pupil segmentation mirror U2 front, and it is with grid graticule.Entrance pupil segmentation mirror U2 is positioned at race glass entrance pupil place, and it is formed by with the bearing 7 of Φ 100mm through hole, Φ 100mm wedge mirror 8, Φ 100mm wedge mirror 10, wedge mirror group 9; The angle of wedge of wedge mirror 8 and 10 is 25 "; Wedge mirror group 9 by overall diameter Φ 85.25mm interior diameter Φ 58.5mm ring wedge mirror, overall diameter Φ 58.5mm interior diameter Φ 33mm ring wedge mirror, overall diameter Φ 33mm interior diameter Φ 19.5mm ring wedge mirror, the mutual half-twist of diameter of phi 19.5mm wedge mirror is gluing forms, in wedge mirror group 9, the wedge mirror angle of wedge is 24 ', and the concyclic heart.The spectroscope 2 of folding can be positioned at front, race glass focal plane.Overall diameter Φ 42.5mm grid graticule 3 and 70 ° of wide visual field Ultima LX 32mm eyepieces 4 are positioned at above spectroscope 2.Four-way photon counting parts U3 is positioned on race glass focal plane, and it comprises bearing 11 that axis is through hole, model is R1635P shore pine photomultiplier 12,13,14 and 15.Optical imagery relay lens 5 is positioned at four-way photon counting parts U3 rear, and central area, focal plane is imaged onto on ccd image sensor 6 by it.The model of ccd image sensor 6 is JAI-BM141GE.
The combination backup system automatic focusing of parallel light tube U1 and ccd image sensor 6.The spectroscope 2 of folding, grid graticule 3 and wide visual field eyepiece 4 can be convenient to system for field and debug.The combination of wedge mirror 8, wedge mirror 10, race glass 1, optical imagery relay lens 5 and ccd image sensor 6 realizes atmospheric seeing monitoring.The combination of wedge mirror group 9, race glass 1 and four-way photon counting parts U3 realizes single star and to glitter monitoring.Through air comprehensive parameter measuring analysis software calculate after can obtain atmospheric envelope seeing, free atmosphere seeing, etc. the various atmospheric optical parameters such as dizzy angle and approximate turbulence profile.
Claims (2)
1. an atmospheric optical parameter measurer for astronomical site survey, is made up of race glass, CCD image sensor and computing machine, it is characterized in that:
In the front at described race glass entrance pupil place, be provided with successively: with parallel light tube (U1), entrance pupil segmentation mirror (U2) of grid graticule;
On the optical axis at the rear at described race glass entrance pupil place, be provided with successively: can the spectroscope of folding, four-way photon counting parts (U3), optical imagery relay lens and ccd image sensor; Wherein, four-way photon counting parts (U3) are positioned on race glass focal plane;
Another grid graticule (3) and wide visual field eyepiece be positioned at described can spectroscopical top of folding;
The output of described four-way photon counting parts, ccd image sensor, connects described computing machine;
The structure of described four-way photon counting parts is: be provided with the bearing that axis is through hole; This bearing is provided with four photomultipliers be evenly distributed on same circle;
The structure of described entrance pupil segmentation mirror is: be provided with the bearing with through hole; This bearing is provided with the wedge mirror of two the identical angles of wedge be evenly distributed on same circle, a through hole and a wedge mirror group;
The wedge mirror of two identical angles of wedge in described entrance pupil segmentation mirror, its angle of wedge is 25 ".
2. atmospheric optical parameter measurer for astronomical site survey according to claim 1, is characterized in that: the bore of described race glass is Φ 355.6mm, and focal length is 3910mm, and 400 ~ 700 nanometer apochromatism broadband imagings, centre wavelength is 550 nanometers.
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| CN103335816B (en) * | 2013-06-28 | 2015-05-20 | 中国科学院国家天文台南京天文光学技术研究所 | Optical turbulence sensor and method for combining multi-aperture glitter and differential image motion |
| CN103487010B (en) * | 2013-07-03 | 2016-01-06 | 中国人民解放军63655部队 | A kind of dizzy angle measuring system such as grade based on three ring apodization mirrors and method |
| CN104537180B (en) * | 2015-01-04 | 2017-05-17 | 中国科学院国家天文台南京天文光学技术研究所 | Numerical simulation method of astronomical site selection atmospheric optical parameter measurement instrument |
| RU2591263C1 (en) * | 2015-05-15 | 2016-07-20 | Федеральное государственное бюджетное учреждение науки Главная (Пулковская) астрономическая обсерватория Российской академии наук (ГАО РАН) | Method of analysing changes in climate of earth and system therefor |
| CN108458856A (en) * | 2018-01-04 | 2018-08-28 | 中国科学院国家天文台南京天文光学技术研究所 | The detection device and its method of segmentation detection dome seeing based on laser light source |
| CN110954506B (en) * | 2019-11-08 | 2020-10-23 | 南昌大学 | Three-parameter comprehensive measurement method for whole-layer atmospheric optical turbulence |
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| DE3776080D1 (en) * | 1986-04-24 | 1992-02-27 | Roland Sommer | DEVICE AND METHOD FOR MEASURING THE FLOW RATE OF A FREE FLOW IN THE SPACE. |
| US6279393B1 (en) * | 1999-08-24 | 2001-08-28 | Mountain High E&S | System for isotropically measuring fluid movement in three-dimensions |
| CN100590457C (en) * | 2006-11-15 | 2010-02-17 | 中国科学院安徽光学精密机械研究所 | Four-hole difference image moving atmosphere optical parameter measurement instrument |
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