[7736- 12] 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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[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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[7736-12]
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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,
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.
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
Two on sky runs performed: May 25th-June 3rd, June 18th – June 25th
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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 11.5The 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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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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 1.20. Data reduction shows vibration lines at 13Hz and 23 Hz (res. tilt jitter 5-10 mas).
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 #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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
Titoli di coda
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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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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 disturbanceACT commands
ACT final commands
Optical coupling
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
W unit and InfraRed test Camera (IRTC)FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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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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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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)
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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%
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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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, 14-15 January 2010, Florence (ITALY)
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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, 14-15 January 2010, Florence (ITALY)
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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, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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 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
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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Astronomical Telescopes and Instrumentation 2010, June 27-July2, San Diego, 2010
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
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)
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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, 14-15 January 2010, Florence (ITALY)
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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 2010.
FP7-JRA1 progress meeting 2, 14-15 January 2010, Florence (ITALY)