Star Waves Pro II User manual
Contents
1. Innovations Foresight Reference and User Manual POWER BY SYSTEM May 2015 revision 3 nnova tions Foresight 2015 O Powered by Alcor System For any improvement and suggestions please contact customerservice innovationsforesight com Some screen copies may not reflect the latest release of the product hardware software Innovations Foresight 2015 O Powered by Alcor System 1 Prerequisites Please first install the software and refers to the Shack Hartmann software documentation before starting so that to get familiarized with the simulation mode of the software This is very important and will allow you to perform measurements in a more efficient way 2 System description 2 1 What s in the box This picture shows what s in the box regarding this system Innovations Foresight 2015 O Powered by Alcor System 3 4 Illuminated pinhole IO Reticule eyepiece illuminator red 6 USB cable Software and documentation 2 2 Main module The Star Waves pro ll system is made of several sub assemblies Please do not remove the shack Hartmann module from the rest of the assembly this can add dusts to the sensor and micro lens and discard usable spot to be used for the wavefront analysis The 2 inches telescope input contains the collimator of the system 12 mm wheel to rotate to kte e OO ii illuminate the reticle eyepiece Du Shack Hartmann module Innovations Foresigh2. be m I 1 1 1 1 I 1 l L 1 1 1 l 1 I l I I I 1 I 1 1 L I 1 1 1 1 1 I I oo je j e m EE coossococohkosocoosccoos 1 I I 1 1 1 L 1 1 1 1 1 1 I 1 I r EIL Spatial frequency cycirmm This software also features zonal wavefront reconstruction This is like a 3D model of the wavefront 48 Innovations Foresight 2015 O Powered by Alcor System TiKX Y removed Defocus removed Astig 45 removed Astig 45 removed Coma X removed Coma Y removed The display tab allows playing with spot elongation from reference that can by scaled by a user input factor for better clarity Capture Analysis properties Display Spot display Display Elongations E scaled by w Remove tilt w Remove defocus w Remove comas The blue line indicates the spot deviation from the reference scaled by 50x Tilt defocus and comas contributions have been eliminated to show the spot deviation from the reference that is the center of the green box Innovations Foresight 2015 O Powered by Alcor System 49 ji i 7 E A LL AN 8 8 eS fF EN NE wx n EN m ES EE MD N 4 SSR PEP a amp 5 4 wA AR P4 AN LI LEM Lu WE NES WE E es M EI da 7 pr E au m NX ES MI NS ET BE ENN ANN ai WE CES H y Lo dd A A AO pou LET J LEONE i
3. I Saturated pevels 0 Pupdl statistics Close saburation 0 X2274 129849 V 239 Spot 82090 X 274 95 1 849 95 82153 R 2091 L 2089 T 2027 150 124 st 32 25 20 107 112 96 69 43 26 19 e 5 6 K 3 23 18 46 se 4 38 29 2 n Min 15 Max 150 06 08 2014 15 57 06 831 2140 Read process start 06 08 2014 15 57 08 908 2140 Image read types6 06 08 2014 15 57 08 974 2140 Image display cuts 14 108 06 08 2014 15 57 09 391 2140 Meve14 0 Max 15 0 Means 14 0 Noise 1 06 08 2014 15 57 09 392 2140 All wavefront Analyses disabled 06 08 2014 15 57 09 985 Main Image grabed high cut 14 00 Low cut 108 00 Max 252 at lt 2169 12614 Minz9 at X 2592 Y 356 Z w rde em T PAP RA Note incoming image from the camera can be saved as a FITS file or CPA file for offline reprocessing allowing to compute wavefront without been connected to the system to measure When the spots level are within expectations 255096 dynamic go to the menu Measurements perform spot reference calibration Innovations Foresight 2015 O Powered by Alcor System 13 Analy Perform spot reference calibration Load reference grid position Text file SHEI Load reference grid position Binary file enter PST TT ep Set the detection level to 150 ADU this is a 256 ADU level camera then for the spot distance click Auto button and leave 8 as maximum acceptable spot roundness deviation First pass spot summit det
4. LEM MS mi 6 L s w u am CTUM UN Um m be o FK c DNE Eos ow NE ms La a T wow w wow yox ow ETE KON ww o Eg 6 4 549 we a Kg ee we 7 ww w O CE NOD mS NO m ED gs BO SD MO a m 1s le ae d U El T pu ciue EE d a LJ LI A atopy ae W NM OR A ON a Ae LN ME 7 A E Na MIN Fal fo 2 o 3 an 7w Fd E F Mm w w mmu wm KOW eee we ee aa LED NE E _ BEN 2L 52 Hu ES MO NO ED EO wo sU ms WD us c EN E E m El R A NR N NR tw ma Mu Tomm Boh 4o mou wow y w E E NS NU E NY AR E ND zi LES B Eo E LES NE NE NU Sidhe eee Et ET e A _ Mu fme Su NO EX MO ES MI ED MG EDS ET l S BM n NBN RI NIE E M EJ ET E E m WA an B 4 Ww LI Li CO Eo CE A NO DEL Z lt Li Fi Liu ma A mi EI wu Eu Br Bo BD M ME SS x LIE m S NI EE E A NM X E Ii LI ci LEN A A AA BT BD ES E El E T ki a ww d Dom mon ann Na e md x4 d da m fj a N A L EY RO D B BE T Ac Some spots can be eliminated from the wavefront reconstruction by left clicking the mouse Confirmation is asked to the user o Remove this spot 477 i al The removed spot has a red cross over it and will not be longer used for further analysis Innovations Foresight 2015 O Powered by Alcor System 50 To restore the spot left click on it
5. or for restoring all the spots press Reset removed spots Reset removed spots The Spot position tab shows the raw spot deviation in Y and X position versus spot number This can be used to track spot that have a deviation above or below the main spot distribution Innovations Foresight 2015 Powered by Alcor System 51 den U D a t de t 1 t f ep dr Fh desounen MO adla A e oda C te ae ee ka il a e cessekbsesseoun T 1 4 41 t a 5 d yo gt C P OL 1 177 U 4 nn ves PERO NEUSS d BAN d d 7 wy S a js Pr R t U AAA A T TTTITTT U L len RR ec e r 2 o a E om LI 1 oda 1 T nS 1 S A LT ru PELLE A E Le ware cab U 1 1 Sora monn n don U K corras rr rr rro porro eem mj ee rr rro pro of Lo ee ee er eene a da simone E 6 3 gt za an 4 4 wo d2 O64 1 1 AA r TS E shel a e Mon T Ld 52 EE Ld AI anan o ST yv amp tL L 1 U gt e Ss pono o o A LIT pe r a ee s 4 wt e 1 lt a Ke e AU D E a od E S 2 o e a
6. Mis ip gt Ms AS Sia iia A AE a t ol lai RAE E FA c Ts Eta Sun see Dv cac Tr rare A sat Mis R as 1 1 1 1 1 1 1 1 1 i 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 i P mm AER eH mem 1 1 1 1 EN 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 Astigmatism leads to wavefront error or 120 nm rms If astigmatism is removed only other wavefront errors will remain Basic aberrations removal Remove a and Y tip tilt Remove Defocus Remove Cama X Remove Coma Y Remove Astig U Remove Astig 45 Remove Z8 3rd spherical Remove 29 Remove 210 Pa Pa Pa Pa fa fa E E l The resulting wavefront shows 31 nm rms error and various non dominant Zernike except some trefoid Innovations Foresight 2015 O Powered by Alcor System 45 emike nm 21 Tilt x 15315 3 set to zero 22 Ti 147 438 set to zero 3 Defocus 33 5 set to zero 4 Astigmatizm 45 157 4 set to zen zh Astigmatizm 457 235 1 set to zero 6 Lama x 219 7 set to zero Zr Lama 1 43 2 set to zero Z 3rd spherical 5 5 29 Trefoil x 61 7 10 Trefoil y 36 5 11 Sth astigmatism 45 13 2 12 5th astigmatism 0 90 12 6 13 Tetrafoil 1 32 1 14 Tetrafoil 2 15 6 15 5th Trefoil s axis FB 16 5th Trefoil y axis Fl 17 Sth Coma x axiz 2 7 18 5th Coma p asis 5 9 219 Sth spherical 18 3 25 th spherical 5 5 36 Sth spherical 8 1 Z26 Quadrafoil 1
7. NW no wavefront computation checkbox set the exposure time to something like 0 007 sec and camera gain to 10 Be sure the calibration pinhole be turned on and at the right position inside the 2 tube Then press gt gt Acquire image lt lt The image from the camera appears Very important now and you have not so much to take care about it during simulation but now with real light you will have to take care of this is the image level The image shall never show saturated spots because of too much light or too long exposure time The bar graph at the end of the yellow arrow indicates the saturation level and amount of saturated pixels for the whole image and inside the analysis pupil Adjust camera gain and exposure time so that to be close to saturation but never with saturated pixels more than say 100 pixels If the signal is too low this is not good either In that case increase exposure time and gain accordingly All saturated pixels will be displayed as green in the image This very important because performing measurement with saturated spots or spots that have too low level can jeopardize critically the measurements Innovations Foresight 2015 O Powered by Alcor System 11 Capture Analysis properties Display Image acquisition Pupil parameters Center X pixels 1900 zd Center Y pixels 600 Radius pixels 600 Z R Radius Obec BackGround Box definition X left pixels 163 A
8. Right pixels 55 Y Bottom pixels IE Y Top pixels 276 i Background box statistics Max ADU 15 0 Mean ADU 14 0 Noise ADU 0 1 Camera control Loop e Nw gt gt cquire image lt lt Settings Exp s 0 007 Gain 110 Stack Images Substract dark w Save image as CPA file All image statistics l Saturated pixels 0 Pupill statistics G Close saturation 0 Shack Hartmann Spots have a sparse distribution inside the image and are quite smalls this is normal because of the micro lens focal length Innovations Foresight 2015 O Powered by Alcor System 12 Shack Hartmann alyser gt Version 15 7 build 51 compiled on 04 08 20 lt 10070 sec 1 exposurets File Display Measurements Setup Camera Liveview About Capture Analysis properties Display Image acquisibon Pupd parameters Center poets leno 2 Ral gen Center Y poets 1600 2 Radus poets 600 El Radius Obsc 10 j BackGround Box definition X left pixels 69 a X Right pixels 55 a Y Bottom peels 1 7 RE Y Top pexels 276 3 d Background box statistics Max ADU 15 0 Mean ADU 14 0 Noise ADU 0 1 Camera control A p tf Loop gt gt Acquire image lt lt G NW Settings E xD 5 U 007 Gain 1 0 Stack images Substract dark w Save mage as CPA Ne AN mage statistics
9. X X 6 e aG G u a G Ha 6G 6G G G G 1s e KR lt E 8 e es s MM Xii s lI 1 Mx XM X oo oo e a 6 G G XXX XM G X X X sss 5 Nx a ao G MM XXE 8 n co t aG G s a 8 a a a 9 c ogG es 6 G es a G 6G a a a s The next case shows a bad sampled pupil F ratio is too low pupil radius is 500 pixels which is really too low and collimator focal length is too short Collimator shall be exchanged Innovations Foresight 2015 O Powered by Alcor System 24 Reference grid active not displayed E un E IE NECI O TO AOS OO O O O X LL a e ki LI ka ki LA ki gt EI LJ L a Ld L3 LJ LI LJ E a LJ a gt a L ki ki E a L a LI LI gt D E S a LJ LI a L E a a LJ ki LJ Li e LJ Ld L a LI 9 a LU LJ de e gt Li a L EI LJ a a U a a LJ E e LI LA ki Li L e LI LJ gt gt LA LJ a LJ Li kai ES Li LI ES ki Ld LJ a a b L LI LJ LJ 9 a T a LJ a e a El a LJ bi ki LI a gt a LJ LJ L LU LJ LI a LJ La a e EJ L a LI Li a LI LJ LJ a LJ LI a LJ LI LI a gt LJ N LJ a LJ E LJ a Ld a a e ki ka Li LA gt L Li Li L4 EJ gt a a Li a U lt ES LI LI gt LI a a a LJ ki gt LI LJ a 5 L4 LI LJ gt LI LI a e Ld ki a e a LI a LJ LJ a LJ LJ Li LJ s ki E Li LI E LI EI gt 6 The next image displays a pupil that is too large with respect to the image frame top and bottom It will lead to missing surfaces to be measured The F
10. added this way Then the following message appears Innovations Foresight 2015 O Powered by Alcor System 19 O Spot number 1436 has been added to the list of reference spots save it to the disk 2014 07 25 04h35m01s_Test_5H5mall2 bxt The software prompts the user that a new reference spot can be added to the list to be saved to the hard disk otherwise spot will be used but not saved to disk In this way a cluster of spots can be added to the reference list If the Shack Hartmann camera module is dismounted from the rest of the assembly the calibration shall be performed again when remounted as well when exchanging collimators Innovations Foresight 2015 O Powered by Alcor System 20 2 5 Exchanging collimators This system can accommodate with different focal length of a collimators in order to Optimize the spot sampling rate with respect to the size of the analyzed telescope system pupil the idea is to get as much spot as possible without cropping the pupil by the detector s edge Benefit from parallel or afocal beam to reach the micro lens array and not working with a lot of defocus within the pupil The principle is achieved by a simple achromatic lens as follows Telescope refractor or system focal s plane h l A Innovations Foresight 2015 O Powered by Alcor System 21 The Star Wave Pro II Shack Hartmann analyzer comes with one collimator a calibration pin hole and t
11. ratio is too small and thus collimator focal length is too large Also in this case collimator shall be exchanged to get the whole pupil to be sampled Innovations Foresight 2015 O Powered by Alcor System 25 Reference grid active not displayed Each collimator has a label indicating the F ratio range to be used in the next picture this is from F 7 to F 9 4 Innovations Foresight 2015 O Powered by Alcor System 26 f A U w apew ueuJJ8c ul S6SOLTL 1 To exchange collimator simply unscrew it from the main module this is M42x0 75 thread and remove the collimator module The red arrow is showing the motion needed to screw the collimator to the main module the green screw to remove the collimator Innovations Foresight 2015 O Powered by Alcor System 27 Then screw the module you plan to use for the given F ratio from the system to measure Innovations Foresight 2015 O Powered by Alcor System 28 tif to fioa When such a change is performed do not forget this extremely important A Either to use a previous grid reference file that is attached to this collimator Or perform collimator calibration see above for accurate process description The collimator are tuned to be parafocal which means that the focus is the same whatever the collimator and eyepiece focus position shall not be changed The next image shows where the grid reference file can be set Innovations Foresight 2015 O Powe
12. the image of the pinhole shall be found in the eyepiece s center 200um If not there are two ways to get it at the center Rotate the pinhole inside the 2 tube Innovations Foresight 2015 O Powered by Alcor System 30 Change the tilt of the eyepiece this can be achieved by using the three push pull screws located at the edges of the eyepiece support Screw 1 is pushing 1 5 mm Allen wrench screw 2 is pulling 2 5 mm Allen wrench To be able to move them at least unscrew one of those counter clockwise rotation By playing with the screws the tilt of the eyepiece can be changed and better centering can be achieved This is not a mandatory step and most of the case the centering is achieved by rotating the pinhole body 3 Measurement procedure Now with a calibrated system the Star Waves Pro II can be installed to a telescope or other equivalent system to perform measurements The system can be inserted into telescope eyepiece holder or focuser that has 2 input diameter Manual or electric focuser is a mandatory feature focusing by sliding the tube manually is not recommended Innovations Foresight 2015 O Powered by Alcor System 31 Um uas R 10 20 e N Innovations Foresight 2015 O Powered by Alcor System 32 The system focal plane shall be put where the horizontal yellow line is depicted in the next image The focal plane position can be adjusted with the focuser knob rotation and by l
13. 18 6 22 Duadrafoil 2 4 3 Al units in nm Min 96 9 Rms 31 3 Mas 180 3 b PeakP 277 2 FIT error as pixel per spot 3 837 All units in Lambda X Peak to Peak 2 0 Ams 17 86 zernike Coets absolute value The PSF strehl ratio is 88 80 EE radius gives the radius where 80 of the energy sits expressed in microns and arcsec Diffraction limited figures are recalled here for comparison Innovations Foresight 2015 Powered by Alcor System 46 Strehl ratio 88 40 in 1 32E D10 Mas 8 84E 001 l Y 101 20 000334 Strehl ratio 8B AU 80 EE radius 3 45 pm diffract 2 05 pm 2 37 arcsec diffract 1 41 arcsec MTF X and Y axis is also reported here with as blue diffraction limited MTF Innovations Foresight 2015 O Powered by Alcor System 47 MTF X profile je aaa b K ele de aa K b aje akanj naje deh e K ke de A PII III III HHHH m m m mmm b m m m m de aj m m m m m E oosseococoldoecsocoseosor I I I I I I I I J U I I I I I I I I I I I I I I I I I I E I H I 1 I 1 1 i 1 I 1 1 1 1 I T 1 I 1 1 P oocosococoldlocooooos Spatial frequency cycirmm MTF profile aje makonn pala de aaa kaj aje dako aj ele a aaa A m m m m mmm mb m m m de
14. 2 gt a emm T D Y spot positions pixels Bees L take ki A i LETETTE U U T 7 U to s desen U U L E o qe 41 9 v T A des rr 1 1 MM T B AA LIC ons nm Mie ura eim diu im E Fail tr b diet NE w Z o di T0 i Lies ec amp esf oOo E a 4 2 eet i kone ee yi E N PE APA L 1 i c HIT N ds y RT ka v Em un ree T bene ooo Nr Stee ee A RAN d dec rm 2d Y Ae U AAA buco 1 aH DA o wm m o 4 Ke A e 1 iae deer a Pat p A P aL B I ee III III B III TI B pese Powered by Alcor System ight 2015 O Fores e a pa a ya o 1 e IONS Innovat
15. 44 pm diffract 2 05 pm 5 80 arcsec diffract 1 41 arcsec PSF display type Linear Basic aberratians removal Remove a and r tip tilt Remove Defocus Remove Coma X Remove Coma Y Remove Astig U Remove Astig 45 Remove 26 3rd spherical Remove lt 9 Remove 10 dA E P P ISS S S Coma is due to optical misalignment and can be discarded to see other relevant defects Then press Re analyze button In the next image the coma is nulled Innovations Foresight 2015 O Powered by Alcor System 44 Zemike nm 21 Tilt 15315 3 set to zero ee Tilt 147438 set to zero 4 Defacus 337 5 set to zero 4 Ashgmatism 45 157 4 zh Astigmatizm 45 236 1 Zb Coma A 219 7 set to zero ZT Lama t 43 2 set to zero zB 3rd spherical 5 5 29 Trefol 3 61 7 10 Trefol 36 5 11 Sth astigmatism 45 13 2 212 5th astigmatism 0 90 12 6 13 Tetrafoil 1 32 1 14 Tetrafoil 2 16 6 15 5th Trefol s asis 7 9 216 5th Trefoil p asis 7 1 17 5th Coma sz axis 21 7 18 5th Coma y axis 5 9 19 5th spherical 18 3 25 rth spherical 55 36 3th spherical 8 1 26 Duadrafoil 1 18 6 22 Duadrafoil 2 3 3 All units in nm kin 300 4 Ams 120 0 Max 358 5 Peak P 558 9 FIT error as pixel per spot 3 837 All units in Lambda 7 Peak to Peak 0 8 Am 4 6 Zernike Coets absolute value 1 1 1 1 1 1 1 1 1 1 1 1 1 Li 1 1 1 1 xd ep Ter oc desir rn
16. ace and the modal based on zernikes mode is presented in the next image Wavefront reconstruction occurs also automatically after image acquisition completion when the NW checkbox is left un checked Innovations Foresight 2015 O Powered by Alcor System 42 Zend el Tilt 15315 3 set to zero z Til 14743 8 set to zero 3 Defocus 337 5 set to zero 24 Ashgmatism 45 157 4 zh Astigmatizm 457 236 1 zb Coma x 219 7 zr Coma t 43 2 8 3rd spherical 5 5 29 Trefoil x 61 7 10 Trefol 36 5 11 Sth astigmatism 45 19 2 12 Sth astigmatism 0 307 126 13 Tetrafoil 1 32 1 14 Tetrafoil 2 16 6 15 5th Trefol x axis FB 16 5th T refoil y axis Fl 1 Sth Coma s axis 21 7 18 5th Coma y axis 5 9 19 Sth spherical 18 3 225 rth spherical 55 236 Sth spherical 8 1 26 Buadrafall 1 18 6 Zaf Quadratoil 2 9 3 AN units in nm Min 333 8 Ams 143 7 Mas 395 9 Peak P 729 7 FIT error as pixel per spot 3 837 All units in Lambda Peak to Peak 0 8 Rms 3 8 Zernike Coets absolute value 4 Se cic ce cem so olaa com E eke T cc eee compe Tis eat LI ote qe pce L lt eke lt R E This analysis shows that this system is quite affected by astigmatism and coma Innovations Foresight 2015 O Powered by Alcor System Min 8 38E O11 Max 1 10E 001 X 22 Y 123 0 000035 Strehl ratio 10 97 80 EE radius 8
17. date S hack Hartmann Reference grid Pixel size square um 22 iE e Uk fle will be loaded on first Microlens focal length mm B3 User scavadoresD a grid simulatian dat Microlenses pitch pum 110 k Change file Wavelength nm 532 Centraid setup Measurement system For barycentric centraiding used mostly in the software just consider a given percentage of highest value peels value inside the plens bos Correct measurment from 28 Br 4 6 1 l l 35 spherical aberration beam splitter cube y Percentage of highest pixel value a Value lwaye number 0 035 Comp This value is updated by the spot calibration Come reference process and shall be correct Will be substracted to lt otherwise all barycentric centroiding might be Multiply bu 1 all resulting wavetront 1 incorrect Flat mirror double pass system System to be measured Save mage tiles az System s name W FITS file E imulatian SH CPA file 1500 Mao need to be HES SHR ne MM accurate thisis Uthers Diameter mm 300 used for MTF Remove central obscuration for MODAL analysis computations only Confirm spot restere removal OR Cancel Other group boxes are not important at that stage just ignore for the time being Innovations Foresight 2015 O Powered by Alcor System Then set the background box definition like this is set in the next image outside any place where a spot can go Enable the
18. distribution and 8 is the figure entered into the previous input form This spot 768 can be re inserted into the list click the bottom list 1 then the top list comes with the spot 768 click 2 to re enable the spot the spot 768 is displayed inside the image within a green square 3 or white circle Innovations Foresight 2015 Powered by Alcor System 15 769 770 771 772 773 774 775 776 777 778 775 780 781 782 783 784 785 786 mma K XK KKR KK KIS K IK K K KIK K IK K Ka B T X 59204 20 X 1014 22 2 1064 08 1113 95 X 1163 87 X 1213 81 X 1263 807 X 1313 85 X 1363 593 X 1413 48 A 1463 32 X 1513 25 2 1563 20 2 1613 07 X 1062 99 X 1712 835 X 17862 74 X 1812 6805 TP m 4 rm Y 1049 38 Y 1050 139 Y 1050 67 Y 1051 27 Y 1051 73 Y 1052 13 Y 1052 72 Y 1053 25 Y 1053 73 Y 1054 25 Y 1054 739 Y 1055 28 Y 1055 76 Y 1056 26 Y 1058 80 Y 1057 33 Y 1057 84 Y 1058 33 Y 1058 839 A a mma IE pa HHHH L b Amount of spots found 1435 List of removed spots at first pass due to FWHM beeing out 314 88 1043 38 5 14 Minz4 51 max 5 14 Save in psHts amp t E Ev 2 Mame ET te hiy Recent Places Desktop Date modified Type No items match your search Y Network File name Feference_grid 5ave as type tet files hd Cancel Innovations Foresight 2015 O Powered by Alcor System This messag
19. e appears from more information see the software manual This is the amount of brightest pixels used per micro lens square that will be used to perform the barycenter centroiding of the spots Once calibration achieved all validated reference spots have their green dashed square of excursion Innovations Foresight 2015 O Powered by Alcor System 17 Some spots do not have a square around them this means that they have been discarded or not validated Those spots will not be used for further analysis This is because they do not match one or many of the following criteria Spot that has a too low signal to noise ratio Spot has not the proper aspect roundness ratio not consistent shape This can be due by defective micro lens manufacturing dust on micro lens array or micro lens to close to the holding mechanics The next picture shows different defective micro lens that leads to discarded spots This is not critical and the software can cope with some defective spots at any places over the image Defective or discarded spots are not an issue at all for modal wavefront reconstruction but can be an issue sometime for zonal wavefront reconstruction Innovations Foresight 2015 O Powered by Alcor System 18 Nevertheless a new reference spot can be forced to be written into the list by right mouse click and holding shift key at the same time the mouse being over a spot that has no green square A new reference spot can be
20. ection threshold ADU al Auto Approximate spot distance Pixels 50 Auto M aximum accepted spot roundness ratio aspect E Cancel Expert gt gt Then this form appears after spot reference detection Innovations Foresight 2015 Powered by Alcor System 14 La w kai La La La La La La w La La La La La La La La La m H 775 40 5824 54 A B874 80 A 524 TI 4272 63 X 1024 55 X 1074 44 H 1124 34 X 1174 23 1224 14 1274 03 1323 92 A4 1373 87 A 1423_72 H 1473 65 X 1523 54 1573 43 A 1623 35 A l673 29 EF PA R 41 50 56 Y 50 45 Y 50 95 Y 51 51 Y 51 99 Y 52 495 Y 53 02 Y 53 45 Y 54 03 Y 54 52 Y 55 03 Y 55 565 Y 56 05 Y 56 58 Y 57 06 Y 57 60 Y 58 16 Y 58 63 Y 53 13 PILE C A On Ex i EE Il Rod MPs MPs A MPs af Ps as PS as EO abs af af aO ES i 10 1 ss 00 J 1 oO EEEEEEEEEHHEH ET Histogram FWHM o 4 r T 4 rF 1 rp yon ap ar n paspor ee pocuecopoeoo Amount of spots found 1435 List of removed spots at first pass due to FWHM beeing out 314 88 1043 38 5 14 4 5 43 3 1 Min 4 51 max 5 14 mean 4 72 median 4 72 stdeyv 0 05 dmean 49 9 Cancel Spot 768 has been discarded because its size is 5 14 pixels that this higher than 4 72 8 0 05 5 12 where 4 72 is the mean spot size or FWHM 0 05 pixel is the standard deviation of spot size
21. he necessary software for acquisition and analysis Nine collimators are available to cover telescopes with F numbers stretching from F 3 to F 20 F 4 F 8 At the minimum F Number the collimator images the star across 100 of the sensor chip area at the maximum F number the image occupies 50 of the sensor area We recommend to aim for a 80 of coverage The next image shows a good sampling the pupil diameter is well inside the image frame not too large and not too small This is a good match A good amount of spots can be used the pupil is very well sampled The Pupil radius is 913 pixels in this case Capture Analysis properties Display Pupil parameters Centers pisels 1 190 Center Y pels 939 Radius pels 983 m 3 Fist N i Radius Obzc t Innovations Foresight 2015 O Powered by Alcor System 22 Reference grid active not displayed The next image shows another sampling case this is a bit small but can be used for measurement The amount of usable spots is decreased by 5096 compared to the case discussed above This could be considered as the lower limit The F ration is too large for this collimator Innovations Foresight 2015 O Powered by Alcor System 23 Reference grid acbve not displayed Nm un un o a o e 5 o L Li gt gt as 6 e Ga e a a ss 5 Ss G G G G ss a OO M MN Iz xXx G 8 6 G MX XE MM G a a e M 1 8 es e XM XM XM XM X NM X MX e
22. n be dangerous to use such a pattern for measurements Innovations Foresight 2015 O Powered by Alcor System 39 BackGround Box definition X left pixels 32 x Right pixels 142 e Y Bottom pixels 3 Y Top pixels 402 3 Background box statistics Max ADU 1 4 Mean ADU 0 3 Noise ADU 0 2 Camera control non Loop Acquire image j NW Settings Exp s 0 02 Gain 500 Stack 5 images Substract dark G Obs Temp AYT Pike421 V Save image as CPA file All image statistics Dynamic OK 0 Pupill statistics ka t Dynamic OK 0 A273 Y 67 V 1 A LIE MEZ M LL E E 1L l LIE LE NE ML M LZ Ln d DIS E E x gt L For minimizing the effect of the atmospheric turbulence it is strongly advised to Stack incoming images so that the effect of the turbulence can be nulled or decreased Stacking 10 images is a good figure Camera control Loop NW gt gt Acquire image lt lt Settings Exp s 0 02 Gan 500 Images Analysis will be achieved only when all the required images have been recorded The yellow circle shape defines the pupil to be analyzed The pupil center must be adjusted to the image center using mouse the pupil diameter Radius pixels If central obscuration is present its radius Radius Obsc can be increased File Display Measurements et Capture Analysis pr
23. on of the pinhole image at the center of the reticle is factory made If not well focused you can adjust the focus by sliding the eyepiece into the tube Once focused with the eyepiece do not remove the eyepiece when measuring at the telescope leave it as it If not perfectly centered the calibration pinhole can be rotated inside the 2 tube to get into the center of the reticle 200um Calibration can start connect the camera USB link to a PC then launch the software men setup Pu rcm Disconnect camera teie gt resl 1064 Center Y pixels s Radius pixels 682 Radius bsc 143 Backlaround Box definition left pixels es Innovations Foresight 2015 Powered by Alcor System 8 and click Disconnect camera Again click Camera Setup and connect System setup Pupil parameters Camera Setup and connect Center X pels 1064 Rat Center Y pels 381 m Radius pixels 682 We L Alliance Vision Technology camera Camera setup Click here to setup camera Set the form as follows Video format frame rate FPS and so on then click OK twice Innovations Foresight 2015 O Powered by Alcor System 9 Device Settings Video Capture Device Device Name DMK 72AUCO2 BR Serial Number 0x28410103 Properties Device Settings Video Norm Video Format Frame Rate FP5 Input Channel Flip Video Horizontal Flip Video Vertical Up
24. ontrol Loop gt gt Acquire image lt lt F Nw Settings Exp 3 0 3 Stack E Images Substract dark e w Save image as CPA file All image statistics TT TTT YY Dynamic UK 0 Pupill statistics w Dinamic DK 0 Or instance a 0 3 sec exposure produce The image of the star looks as following a large donut this is the image of the entrance telescope pupil including central obscuration Innovations Foresight 2015 O Powered by Alcor System 37 Li B LJ LI LI LJ Li E Li ES ki The next image shows that the exposure time or the gain or both are too high 27346 pixels are saturated and the saturated pixels are displayed as green Innovations Foresight 2015 O Powered by Alcor System 38 Camera control UE Loop gt gt cquire image lt lt Nw Settings Exp s 11 Gain 11000 Stack E images Substract dark G 10bs Temp sAVT Pike421 lv Save image as CPA file All image statistics L SARS RO H SA A O O l Saturated pixels 27346 Pupill statistics UBER T bl AA ES E LE E d B e l Saturation 18033 l O o o o o o o o o o 0000000000 000000Q0000 00000000060 0000000000 06000000000 0000000000 0000000000 0000000000 0000000000 0000000000 A 4 Y 305 Y 5 Exposure or gain time shall be reduced In the next image the exposure time is too low the blue bar graph is too close to the left ie too low level and this ca
25. ooking at the star at the eyepiece The position or focus of the reticle shall not be moved after calibration has been achieved Of course the system can accommodate from slight defocus but shall be kept as low as possible This is easy by looking into the eyepiece the star as you would observe usually Innovations Foresight 2015 O Powered by Alcor System 33 Telescope refractor or any system to measure focal plane position Incoming light from telescope The telescope shall now be aimed at a bright star having magnitude less than 1 For instance testing a simple Dobson telescope that has no sidereal tracking is even possible if the telescope is aimed at Polaris star Other telescope shall have sidereal tracking when using other stars because the Star Waves Pro II has a limited field of view and the star does not stay very long in the field of view Innovations Foresight 2015 O Powered by Alcor System 34 The star shall be centered with the eyepiece the same way it was with the calibration pinhole As well as the focus shall be adjusted the same way Innovations Foresight 2015 O Powered by Alcor System 35 200um Now perform image acquisition with exposure time and gain that is suitable for your star Avoid exposure time above 1s stay below 3s The dynamic of the spot shall be between 50 and 90 like the blue bar graphs show hereafter Innovations Foresight 2015 O Powered by Alcor System 36 Camera c
26. operties Display Pupil parameters Center X pels 1 466 E Center pixels E bul E m Radius pixels 667 Fist Radius Uber 138 E Innovations Foresight 2015 O Powered by Alcor System 40 The inner and outer diameter shall be adjusted so that to border bright spots In the Analysis properties tab the image can be analyzed i e spot position extracted and wavefront computed Use enhanced centroiding enable modal and zonal wavefront computation and enable PSF computing Basic and non pertinent aberration such as tilts X Y and defocus shall be disabled Innovations Foresight 2015 O Powered by Alcor System 41 Capture He Analyze Image Spot detection setup Signal to noise 110 Use fixed threshold Threshold 40111 UU Lentroids t Barycentric 1X brightest pixels Enhanced slower lt j Computations No wavefront computations Wavetront camp Zonal Wavefront comp Modal y f Wavetront comp Madalezanal onal reconstructor algorithm f Jacobi slowest C 2 Bauss Siedel f 3 Succ Over Relaxation SUR 4 Jacobi SOR fastest PSF Modal computation t Do not compute PSF Do compute PSF Basic aberrations removal Remove a and r tip tilt Remove Defocus Remove Loma X Remove Loma T Remove Astig Remove Astig 45 Remove 8 drd spherical Remove 4 Remove 210 M0 l et The wavefront reconstruction can take pl
27. red by Alcor System 29 Shack Hartmann Pixel size square pm I2 Micralens focal length mm 188 Microlenses pitch pum TD ooo Wavelength nm EN Measurement system Flat mirror double pass system L Correct measurment from 28 br 4 6F 1 spherical aberration beam splitter cube Value wave number 10 176 Comp Will be substracted to 28 Multiply by 1 all resulting wavefront Others Remove central obscuration for MODAL analysis IF checked Annular emikes will be used instead Confirm spot restere remoeval w Reference grid Reference grid position file will be loaded on first Image acquisition CwcavadorekProjets nces cole Sram ret 1 Change file Centraid setup For barycentric centroiding used mostly in the software just consider a given percentage of highest value pixels value inside the plens bos Percentage af highest pixel value 10 9 Es This value is updated by the spot calibration reference process and shall be correct otherwise all barycentric centroiding might be incorrect Save image files az C FITS file f CFA tile UK Cancel System to be measured System s name SN 41 410535 Test azel oth be 1500 No need to be accurate this Is Diameter mm 300 used hor MTF Operator s name only computations Cavadare Serial number Company Logo BMP file CAcavadore Curl Fe ogokLogo LIefl I SB bmp Change file During calibration
28. t 2015 O Powered by Alcor System 2 inches 50 8mm telescope input The eyepiece is attached by small screws please do not dismount it because this is tuned in a specific way Also do not split the camera module from the beam splitter module euas z o a 3 Q 3 b 3 lt S6SOL7L 1 Camera module Beam splitter module Innovations Foresight 2015 Powered by Alcor System 2 3 Calibration module To run the calibration module attach the jack wire to it and connect the other side of the cable to either USB or main AC depending on the cable type Then the 5um pinhole illuminates The calibration module is a fragile part do not touch press pinch pin where the pinhole illuminates Damaging it can jeopardize its performance Pinhole DO NOT TOUCH or PRESS 2 4 Calibration procedure Calibration is a mandatory step and without it your device cannot produce any valid measurements Calibration shall be achieved for each set of collimator if any Introduce the calibration module inside the Star Waves pro ll push it till it cannot slide anymore Innovations Foresight 2015 O Powered by Alcor System 6 DI ill i i Innovations Foresight 2015 Powered by Alcor System By looking into the reticle eyepiece the image of the pinhole can be seen and this should appear as a bright image in the center of the reticle The adjustment of the positi
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