[7736-12] Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010 First...

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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

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AuthorsOsservatorio 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. HillSupport Astronomer: F. MannucciESO: R. Arsenault

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Talk overview

Main results of the FLAO acceptance test in Europe: 14th – 18th December 2009

Summary of system installation at the telescope: 10th February – 15th March 2010

Results from the first two on sky runs: 1. 24th May -3rd June, 2010,

[8nights/2days]2. 18th – 25th June, 2010, [4nights/1day]

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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 /l D• 1Kfps max [30x30]

J. Hill, 7733-8 (June 27th )F. Quiros, 7736-128 (June 28th )J. Brynnel, 7733-89 (July 2nd )A. Riccardi, 7736-82 (July 2nd )

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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.

RETROREFLECTORis composed by a f/1 parabola and a flat mirror. Reflects back incoming lights & reimages the pupil on the Adaptive Secondary

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Acceptance test: IM measurements

100

20

4

Bin#1 Bin#2 Bin#3 Bin#4

KL mode Pyramid Signals (Sx, Sy)

Num. Shape

BinMode

Sampling[#subaps]

Num. ofvalid subaps.

Max num ofmodes

Pyr. Modulation[±/D]

1 30x30 678 496 2 (3)

2 15x15 177 153 3

3 10x10 72 66 6

4 7x7 48 36 6

IM acquired using fast push pull technique & closed loop.

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Acceptance test: SR in H band

BIN1495modes

BIN2153modes

BIN366modes BIN4

36modes

FLAO lab meas.FLAO goalFLAO 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 goalFLAO baseline

K band SR values

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Acceptance test: corrected PSFsMR=8.5, SRH=83%

arcsec

MR=10.5, SRH=58%

arcsec

MR=12.3, SRH=45%

arcsec

Seeing-limited, SRH=0.5%MR=14.6, SRH=23%

arcsec

MR=16.4, SRH=5%

arcsec

Emulated turbulence: seeing of 0.8”, V=15 m/s

bin1 bin2

bin3

bin2

bin4

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Acceptance test: corrected wavefront modal decomposition

FQ

MR Bin mode Fs (Hz) Phot. /subap. / frame nmod mod. (wfs/D) g SR (H band)

8.5 1 1000 231 496 2.0 0.4 83

12.3 2 625 42 153 3.0 1.0 45

14.6 3 200 41 66 6.0 0.9 23

16.4 4 100 24 36 6.0 0.6 5

The modal decomposition of the wavefront residuals for the 4 different binning modes.

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Acceptance test: SR vs. seeing condition

0.010 (0.6”)0.005 (0.8”)

0.001 (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

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FLAO system installation @ LBTFebruary 9th --March 17th .

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First on sky results: May 25th

Intensities between open and closed loop rescaled for displaying purposes.

LBT InfraRed Test Camera images: H band, 10mas/pixel scale

The object:HD 124085, K0, R=7.5 , I=6.9, H=5.8, Triple StarThe atmosphere:seeing 0.6arcsec V band Elevation 58..64FLAO parameters:1 KHz, 30x30 subaps, 400 corrected modesResults: SR H 65%..73%

3.2 arcsec

Some of the first closed loop images acquired the 25th of May

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The HD 124624 images and SRThe reference:HD 124624 [14:13:54.67 +37:37:34.2 ]R =7.1, H=4.4, J=5.1, K5III The atmosphere:seeing 0.9arcsec V bandFLAO 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)

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High H band SR images

The reference: HD175658, R =6.5, H=2.5 The atmosphere: seeing 0.9 arcsec V bandFLAO parameters: 1KHz, 30x30 subaps, 400 corrected modes

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Sensor: E2V CCD47 Filter 850nm; BW 40nm

First on sky results: corrected image at 850nmStar 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

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First on sky results: a 40mas separation binary

Image dataH band 4s exposure time SR > 60% (no correction for 2nd star flux)

FLAO parameters30x30 subaps400 corrected modes1Khz frame rate

Star companion

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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 plot2MASS J19460752+2231122

R+I mag 17.0SR 6.2% H bandFWHM 0.1 arcsecDIMM 0.9”7x7 subaps36 modes, 200 Hz16 ph/subap/frame

2MASS J19334425+1947482R+I mag 17.8FWHM gain 1.4DIMM 0.9”7x7 subaps5 modes, 100Hz18 ph/subap/frame

Two on sky runs performed: May 25th-June 3rd, June 18th – June 25th

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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 11.5The atmosphere:seeing 0.7arcsec V bandElevation 58..69FLAO parameters:0.5KHz, 15x15 subaps, 153 corrected modes

FLAO H Band 8min

~10 arcsec

Composite image J+HComposite image J+H

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Conclusion

FLAO acceptance test in 14-18 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 2010.

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 2010.

FLAO average closed loop time of about 4 hours/night over 12 nights.

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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 1.20. Data reduction shows vibration lines at 13Hz and 23 Hz (res. tilt jitter 5-10 mas).

Composite image J+H

SR > 60%

FLAO parameters30x30 subaps400 corrected modes1Khz frame rate

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Acceptance test: IM lab measurements

Measurement in fast push-pull requires tipically 5 minutes for 600 modes.

Mode #0 Mode #1Mode #2

ExposureSettling 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

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Titoli di coda

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The FLAO solar tower test

F2

F1F/15.0

F/1.22

13

71

3m

m1

06

4.7

mm

911mm

LBT IRTC

LUCIFER dichroicwindow

LBT672

WFS unit

Test of the complete AO system in Europe:1. Test of system performance: SR vs. star mag, r0, v_wind2. 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, 14-15 January 2010, Florence (ITALY)

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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 disturbanceACT commands

ACT final commands

Optical coupling


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W unit and InfraRed test Camera (IRTC)FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)

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The FLAO control softwareThe 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:

IIFMaster

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


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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010Controlling 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

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System automatic configuration

Columns:# 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19mag bin freq phot modes base rec filtering pupils slopenull tt gain fw1_acq fw2_acq fw1_obs fw2_obs TVbin TVfreq TVavg TVflux6.0 maximum magnitude8.5 1 1000 213 496 KL 20091207_165435 pureIntegrator 20090925-113454 zero 2 0.3 0 0 0 0 4 4.3 20 5000 9.5 1 1000 85 496 KL 20091207_165435 pureIntegrator 20090925-113454 zero 2 0.3 0 0 0 0 4 4.3 20 2000 10.5 2 800 166 153 KL 20091105_175922 pureIntegrator 20090928-221919 zero 3 0.9 0 0 0 0 16 12.6 100 5000 11.5 2 625 84 153 KL 20091105_175922 pureIntegrator 20090928-221919 zero 3 0.9 0 0 0 0 16 12.6 100 180012.5 2 625 34 153 KL 20091105_175922 pureIntegrator 20090928-221919 zero 3 0.9 3 0 0 0 16 12.6 100 700013.5 2 400 21 153 KL 20091105_175922 pureIntegrator 20090928-221919 zero 3 0.9 3 0 0 0 16 12.6 100 250014.5 3 200 35 66 KL_v2 20091208_180600 pureIntegrator 20090928-222825 zero 6 0.8 4 0 0 0 16 12.6 100 170015.5 4 200 28 36 KL_v2 20091209_195122 pureIntegrator 20091110-152038 zero 6 0.6 4 0 0 0 16 12.6 100 60016.5 4 100 22 36 KL_v2 20091209_195122 pureIntegrator 20091110-152038 zero 6 0.6 4 0 0 0 16 12.6 100 250

#Columns:# 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19mag bin freq phot modes base rec filtering pupils slopenull tt gain fw1_acq fw2_acq fw1_obs fw2_obs TVbin TVfreq TVavg TVflux6.0 maximum magnitude8.5 4 500 7066 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 0 0 0 0 4 4.3 20 5000 9.5 4 500 2812 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 0 0 0 0 4 4.3 20 2000 10.5 4 500 1120 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 0 0 0 0 16 12.6 100 5000 11.5 4 500 444 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 0 0 0 0 16 12.6 100 180012.5 4 500 176 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 3 0 0 0 16 12.6 100 700013.5 4 500 70 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 3 0 0 0 16 12.6 100 250014.5 4 500 28 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 4 0 0 0 16 12.6 100 170015.5 4 400 14 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 4 0 0 0 16 12.6 100 60016.5 4 100 22 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 4 0 0 0 16 12.6 100 25017.5 4 100 8 5 KL_v2 20091210_181737 pureIntegrator 20091110-152038 zero 6 0.8 4 0 0 0 16 12.6 100 125

AO mode conf. table

Field Stabilization mode conf. table

R0=0.13 Vband, v_wind = 15 m/s


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H band measured Strehl ratios

Baseline assumptions

Goal assumptions

Measurement conditions

CCD RON 14,8.0,5.0 11.5,7.0,4.0 11.0,6.7,4.0

#modes (8.5-9.5 mag) 351 595,495 495

Thin shell rms [nm] 60 30 30 (Sr =95% H band)


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Corrected PSFs in H band (0.8”,v_wind15m/s)

MR=16.4, SRH=5%

MR=8.5, SRH=83% MR=12.3, SRH=45%

MR=14.6, SRH=23%

Uncorrected SR = 0.5%


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Modal decomposition of correction

MR Binning mode

fs(Hz)

photons / subap. / frame

nmod mod. (wfs/D)

g SR (H band)

8.5 1 1000 231 496 2.0 0.4 .83

12.3 2 625 42 153 3.0 1.0 .45

14.6 3 200 41 66 6.0 0.9 .23

16.4 4 100 24 36 6.0 0.6 .05


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SR vs. seeing conditions

0.6”

0.8”

1.5”


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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.


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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]


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Commissioning main tasksTask name Duration

(days)Description Milestone Success criteria

LBT672a & W#2 re-integration

10 Reintegration 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

12 a) 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 1st light on sky

15 days5 nights

a) Control SW test.b) 1st light on sky in closed loop

1st corrected images

Closed loop done with 200 modes for high flux.

FLAO closed loop test.

20 days17 nights

Closed loop test with FLAO with different fluxes:a) Engineering modeb) Observing modes

FLAO closed loop achieved in engineering and observing modes.

SR values >= baseline values defined in FLAO_01.

Final system test

14 nights System performance test FLAO 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


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AO Commissioning activity1. 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


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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).


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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 2010.


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