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[7736-12] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First Light Adaptive Optics (FLAO) system Acceptance Test results.

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Presentation on theme: "[7736-12] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First Light Adaptive Optics (FLAO) system Acceptance Test results."— Presentation transcript:

1 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First Light Adaptive Optics (FLAO) system Acceptance Test results (and beyond!) The main results of the European acceptance test and first 12 nights of commissioning runs at the LBT telescope of the natural guide star based, single conjugate AO system of LBT. Presented by: S. Esposito

2 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Authors Osservatorio Astrofisico di Arcetri ( Italy ) : S. Esposito, A. Riccardi, G. Agapito, C. Arcidiacono, R. Briguglio, L. Busoni, L. Fini, A. Gherardi, J. C. Guerra, F. Quirós-Pacheco, F. Pieralli, E. Pinna, A. Puglisi, P. Ranfagni, P. Salinari, P. Stefanini, A. Tozzi,, M. Xompero Large Binocular Telescope Observatory : G. Brusa-Zappellini, R. Demers, J. Brynnel Acknowledgements: LBTO telescope crew, TO, J. Hill Support Astronomer: F. Mannucci ESO: R. Arsenault

3 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Talk overview  Main results of the FLAO acceptance test in Europe: 14 th – 18 th December 2009  Summary of system installation at the telescope: 10 th February – 15 th March 2010  Results from the first two on sky runs: 1.24 th May -3 rd June, 2010, [8nights/2days] 2.18 th – 25 th June, 2010, [4nights/1day]

4 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system key components LBT672a unit 911mm diameter 1.6mm thick, (Mirror lab) 672 actuators Settling time < 1ms 30nm WFE LBT WFS unit Pyramid sensor 30x30 to 5x5 subap. Tilt mod.  2-6  D 1Kfps max [30x30] J. Hill, (June 27 th ) F. Quiros, (June 28 th ) J. Brynnel, (July 2 nd ) A. Riccardi, (July 2 nd )

5 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 IRTC. The LBT InfraRed Test Camera to record images. It has J and H filters and 3 sampling of 10; 20 ; 100 mas/pix. A dichroic reflect VIS to WFS and trasnmit NIR to IRTC Acceptance test: Test Tower optical set-up REFERENCE SOURCE generating a point-like source in the focal plane with an f/15 beam as the LBT F/. The light source is an incandescence lamp. RETROREFLECTOR is composed by a f/1 parabola and a flat mirror. Reflects back incoming lights & reimages the pupil on the Adaptive Secondary   

6 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: IM measurements Bin#1Bin#2Bin#3Bin#4 KL modePyramid Signals (S x, S y ) Num.Shape Bin Mode Sampling [#subaps] Num. of valid subaps. Max num of modes Pyr. Modulation [± /D] 130x (3) 215x x x IM acquired using fast push pull technique & closed loop.

7 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: SR in H band BIN1 495modes BIN2 153modes BIN3 66 modes BIN4 36modes FLAO lab meas. FLAO goal FLAO baseline Measurements conditions were intermediate between baseline and goal assumptions for RON; # of modes, thin shell flat. Closed loop test in solar tower with artificial turbulence: SR values in H band vs. star magnitude. K band SR values achieved by scaling the SR measured in H band with Marechal formula FLAO lab meas. FLAO goal FLAO baseline K band SR values

8 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: corrected PSFs M R =8.5, SR H =83% arcsec M R =10.5, SR H =58% arcsec M R =12.3, SR H =45% arcsec Seeing-limited, SR H =0.5%M R =14.6, SR H =23% arcsec M R =16.4, SR H =5% arcsec Emulated turbulence: seeing of 0.8”, V=15 m/s bin1bin2 bin3 bin2 bin4

9 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: corrected wavefront modal decomposition FQ MRMR Bin modeF s (Hz)Phot. /subap. / framen mod mod. (  wfs /D) gSR (H band) The modal decomposition of the wavefront residuals for the 4 different binning modes.

10 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: SR vs. seeing condition (0.6”) (0.8”) (1.5”) SR values of the seeing limited cases Measured value of the SR in H band for seeing values of 0.6, 0.8 and 1.5 arcsec

11 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

12 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

13 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

14 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

15 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

16 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

17 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 FLAO system LBT February 9 th --March 17 th.

18 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First on sky results: May 25 th Intensities between open and closed loop rescaled for displaying purposes. LBT InfraRed Test Camera images: H band, 10mas/pixel scale The object: HD , K0, R=7.5, I=6.9, H=5.8, Triple Star The atmosphere: seeing 0.6arcsec V band Elevation FLAO parameters: 1 KHz, 30x30 subaps, 400 corrected modes Results: SR H 65%..73% 3.2 arcsec Some of the first closed loop images acquired the 25 th of May

19 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 The HD images and SR The reference: HD [14:13: :37:34.2 ] R =7.1, H=4.4, J=5.1, K5III The atmosphere: seeing 0.9arcsec V band FLAO parameters: 1KHz, 30x30 subaps, 400 corrected modes 0.72” H Band 75% SR in 12sec J Band 46.6% SR in 20 sec Best SRs achieved! 85% H (1s) 47% J (1s)

20 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 High H band SR images The reference: HD175658, R =6.5, H=2.5 The atmosphere: seeing 0.9 arcsec V band FLAO parameters: 1KHz, 30x30 subaps, 400 corrected modes

21 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Sensor: E2V CCD47 Filter 850nm; BW 40nm First on sky results: corrected image at 850nm Star mag => R=9.3 J=7.5 H=6.7 Drizzling of 5 images SR~20% FWHM=40mas (DL=20mas) IRTC H Band, scale=10mas/pix, SR~65% Texp=6s, scale= 20mas/pix Horizontal cut The 850nm SR is consistent with Marechal scaling of 65% SR in H band

22 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First on sky results: a 40mas separation binary Image data H band 4s exposure time SR > 60% (no correction for 2 nd star flux) FLAO parameters 30x30 subaps 400 corrected modes 1Khz frame rate Star companion

23 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Average value of closed loop time is 4h/night over 12 nights. Each point correspond to a different target and reports an average value of the achieved SR. H band SR vs star mag & seeing Seeing values measured by LBT DIMM K band SR values scaled from previous plot 2MASS J R+I mag 17.0 SR 6.2% H band FWHM 0.1 arcsec DIMM 0.9” 7x7 subaps 36 modes, 200 Hz 16 ph/subap/frame 2MASS J R+I mag 17.8 FWHM gain 1.4 DIMM 0.9” 7x7 subaps 5 modes, 100Hz 18 ph/subap/frame Two on sky runs performed: May 25 th -June 3 rd, June 18 th – June 25 th

24 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 HST WFPC3 H Band 20min Imaging globular cluster NGC6341-M92 Dati sulla configurazione del sistema adattivo durante la osservazione LBT test camera Limiting Magnitude H = 21, in 10minutes (with AO on) The reference: R 11.5 The atmosphere: seeing 0.7arcsec V band Elevation FLAO parameters: 0.5KHz, 15x15 subaps, 153 corrected modes FLAO H Band 8min ~10 arcsec Composite image J+H

25 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Conclusion  FLAO acceptance test in December 2009 was successful. The system meets specifications. H band SR of 80% and 5% at 8 and 16.5 magnitude star with 0.8 arcsec and v=15m/s.  System was installed at LBT in period February/March  On sky first operation is successful: SRs H(K) of 85(92) with mag 8 and SRs H(K) of 6.2 (22) with mag 17.0 (0.8” seeing).  FLAO system commissioning is scheduled to finish by the end of the year  FLAO average closed loop time of about 4 hours/night over 12 nights.

26 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First on sky results: a 40mas separation binary AR 4s exp. time H band images: raw image (left) and with shift&add (right). The improvement in peak intensity is a factor Data reduction shows vibration lines at 13Hz and 23 Hz (res. tilt jitter 5-10 mas). Composite image J+H SR > 60% FLAO parameters 30x30 subaps 400 corrected modes 1Khz frame rate

27 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Acceptance test: IM lab measurements Measurement in fast push-pull requires tipically 5 minutes for 600 modes. Mode #0 Mode #1 Mode #2 Exposure Settling time wait 1.Acquire IM in open loop. 2.Generate a REC with 10 modes. 3.Measure a new IM in closed loop with 10 modes & low gain (0.05). Basic steps of IM acquisition

28 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Titoli di coda

29 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 The FLAO solar tower test F2 F1 F/15.0 F/ mm mm 911mm LBT IRTC LUCIFER dichroic window LBT672 WFS unit Test of the complete AO system in Europe: 1. Test of system performance: SR vs. star mag, r0, v_wind 2. Test of system observing modes: a) Seeing limited mode b) Field stabilization mode c) AO mode Light from WFS ref. source FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

30 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Seeing generation WFS computation unit (BCU) AO RECONSTRUCTOR Turbulence history act=1,672 A disturbance simulating the OPD variation of a given phase screen is added to each one of the actuator commands computed by the FLAO reconstructor. WFS slopes ACT disturbance ACT commands ACT final commands Optical coupling FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

31 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 W unit and InfraRed test Camera (IRTC) FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

32 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 The FLAO control software The FLAO system is controlled by a complex architecture control SW made up of various parts showed in the picture below. The control SW has three main levels of commands listed below from top to bottom: IIF Master instrument LBT TCS 1) The command issued by the master instruments like IRTC or LUCIFER to TCS (IIF calls to TCS module called IIF). 2) The commands issued by the AOS to the AO supervisor SW. 3) The command issued by the AO supervisor and AO arbitrators. These commands includes low level commands to control AO system HW. AOS control AOS GUI FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

33 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Controlling the FLAO system Load a particular flat on the secondary mirror. Used mainly in SLM. Set ref. source nominal co-ordinates, magnitude and color. Use of system look-up table. Command to acquire the reference star moving the WFS stages. Command to start closed

34 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 System automatic configuration Columns: # mag bin freq phot modes base rec filtering pupils slopenull tt gain fw1_acq fw2_acq fw1_obs fw2_obs TVbin TVfreq TVavg TVflux 6.0 maximum magnitude KL _ pureIntegrator zero KL _ pureIntegrator zero KL _ pureIntegrator zero KL _ pureIntegrator zero KL _ pureIntegrator zero KL _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero #Columns: # mag bin freq phot modes base rec filtering pupils slopenull tt gain fw1_acq fw2_acq fw1_obs fw2_obs TVbin TVfreq TVavg TVflux 6.0 maximum magnitude KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero KL_v _ pureIntegrator zero AO mode conf. table Field Stabilization mode conf. table R0=0.13 Vband, v_wind = 15 m/s FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

35 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 H band measured Strehl ratios Baseline assumptions Goal assumptions Measurement conditions CCD RON14,8.0, ,7.0, ,6.7,4.0 #modes ( mag)351595, Thin shell rms [nm] (Sr =95% H band) FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

36 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Corrected PSFs in H band (0.8”,v_wind15m/s) M R =16.4, SR H =5% M R =8.5, SR H =83%M R =12.3, SR H =45% M R =14.6, SR H =23% Uncorrected SR = 0.5% FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

37 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Modal decomposition of correction MRMR Binning mode f s (Hz) photons / subap. / frame n mod mod. (  wfs /D) gSR (H band) FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

38 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 SR vs. seeing conditions 0.6” 0.8” 1.5” FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

39 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Interpolated K band SRs This is done by computing, in simulation, the corresponding K_band SR achieved when a given H_band SR is found. To obtain the K band Srs values we scaled the measured H band results to K band by using an interpolation function identified by numerical simulations. FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

40 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Sky coverage estimate full, long and short dash lines refer to the Galactic plane, middle latitude and Galactic pole Assume 30 arcsec of isoplanatic patch radius [A. Tokovinin] [F. Roddier] FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

41 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Commissioning main tasks Task nameDuration (days) DescriptionMilestoneSuccess criteria LBT672a & W#2 re- integration 10Reintegration of LBT672 and W unit. Alignment check. Units & FLAO system functional checks FLAO sub- system re- integrated. Functional check passed FLAO System compliance to requirements (compliance matrix) FLAO functional test Telescope installation of FLAO system 12a) Telescope Installation of LBT672a, W#2, retro- reflecting optics. IRTC. b) FLAO aligned with retro- reflector. FLAO system aligned. IRTC aligned. FLAO system alignment in specifications. (FLAO_09,FLAO_06) FLAO initial test and 1 st light on sky 15 days 5 nights a) Control SW test. b) 1 st light on sky in closed loop 1 st corrected images Closed loop done with 200 modes for high flux. FLAO closed loop test. 20 days 17 nights Closed loop test with FLAO with different fluxes: a) Engineering mode b) Observing modes FLAO closed loop achieved in engineering and observing modes. SR values >= baseline values defined in FLAO_01. Final system test 14 nightsSystem performance testFLAO system commissioned with IRTC FLAO performance >= baseline performance defined in FLAO_01 Commissioning campaign duration: -total time 93 days -days 57 - (good) nights 36 eq. to 54 nigths FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

42 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 AO Commissioning activity 1.System unpacking, re- integration &check 10DD 2. Telescope installation of subsystems 12DD 3. System initial day-time calibration Activity start date 10Feb10 6. First light on sky 5NN 5. Daytime test with retro- reflector 4. Telescope operation in seeing limited mode with adaptive secondary FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

43 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Manpower for FLAO #1 commissioning The required manpower is found compatible with the available resources of the group. The group relevant personnel is composed by 17 persons. About 5- 7 personnel units will be available in Arcetri to progress with FLAO#2 test in solar tower (13/01/10-06/07/10). FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)

44 [ ] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 Conclusions  FLAO #1 has been in operation for 5 months in Arcetri. Test phase has been concluded with the FLAO acceptance test.  FLAO acceptance was OK. 1. measured SRs equal or close to goal values. a) SR 85(80)% in K (H) band bright stars (8.5,9.5 mag) b) SR 16(5) % in K (H) band faint stars (16.5 mag) 2. FLAO control SW able to go from power on to closed loop in 5/6 click successfully (including ref. source acquisition).  FLAO #1 is now being shipped to LBT, arrival scheduled for February 10.  FLAO #1 telescope first light is scheduled in May FP7-JRA1 progress meeting 2, January 2010, Florence (ITALY)


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