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November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
THE VISUAL CHANNEL
OF SHARK @ LBT
The V-SHARK Team: F.Pedichini2, J.Farinato1, E.Pinna3, L.Carbonaro3,
M.Centrone2, S.Esposito3, F.Fiore2, A.Fontana2, E.Giallongo2,
J.C.Guerra6, P. Hinz6 , R.Ragazzoni1, L. Sabatini2 , M.Stangalini2, V. Testa2
1) INAF PADOVA 2) INAF ROMA
3) INAF-ARCETRI 6) STEWARD OBSERVATORY – ARIZONA (USA)
Fernando Pedichini on behalf the V-SHARK Team
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
WHO IS V-SHARK @ INAF ROME
F. Pedichini
F. Ambrosino
M. Centrone
L. Sabatini
M. Stangalini
V. Testa
instrument design, (PI)
controls
control and camera software
thesis student
A.O. optical simulation code
data reduction
F. Fiore
E. Giallongo
science
science
In good synergy with the NIR-SHARK team!
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
THIS IS FLAO @ LBT !
HIP76041 at CCD47 (guider) using 750nm-10nm
seeing 1” 600 modes F#35 -> scale = 7.2mas/pix
Courtesy of S. Esposito and E. Pinna on behalf of the FLAO team.
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
V-SHARK IN A NUTSHELL
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High resolution fast imager with FLAO@LBT
Bynocular AO from 600 ÷ 900 and 900 ÷2200 nm
Experimental focal plane for coronagraph and…
Synchronous recording of wave-front residual
THERE WILL BE V-SHARK
V-SHARK@LBT -- INAF exoplanet Rome meeting
November 7, 2014
Optical breadboard
Dicroich
Pick-Up arm
LBTI AGW unit
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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The first design of VIS Channel [1.0]
SPECIFICATION
Direct Imager
 Field of view = (20x25)" or (8x10)"
 Sampling 4÷10 mas /pixel
 ADC bandwidth 600 ÷ 900 nm
Coronagraph
 Field of view = (5x5)"
 Sampling 4÷10 mas /pixel
 Focal plane 6 x occulter
 Pupil plane 6 x stops/apodizers
Detector
 Fast sCMOS imager 1 e- r.o.n.
 Exposure 10e-4 ÷ 30 s
V-SHARK@LBT -- INAF exoplanet Rome meeting
November 7, 2014
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Zemax data for optical quality
Minimalistic off-axis parabolas collimator-camera optical relay
Diff. Limit
0.0000, 0.0000 (deg)
0.0003, 0.0000 (deg)
0.0000, 0.0003 (deg)
-0.0014, 0.0000 (deg)
0.0000, -0.0014 (deg)
OPTICS
 Strehl >99%
 Scale 1.63 mas /µm
Fraction of Enclosed Energy
1.0
0.9
0.8
0.7
AO
 Residual 80÷100 nm
 Strehl 50% @ 650 nm
0.6
0.5
0.4
0.3
0.2
0.1
0.0
0
10
20
30
40
50
60
70
80
90
100
Half Width From Centroid in µm
FFT Diffraction Ensquared Energy
LBT BC off-axis ellipse
15/08/2013
Wavelength: 0.600000 µm
Surface: Image
LBTI_V_SHARK.zmx
Configuration 1 of 1
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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The current design of VIS Channel [2.0]
To LBTI
WFS
f#15
beam
Pick-up
dichroic
ADC
Filter
wheel 1
direct
imager
Occulter
wheel
CAMERA
Filter
wheel 2
Dichroic
600÷750 nm
imager
750÷900 nm
imager
Pupil
wheel
COLLIMATOR
active
movable
disabled
fix
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
9
The current design of VIS Channel [2.0]
To LBTI
WFS
Filter
wheel 1
f#15
beam
Pick-up
dichroic
Filter
wheel 2
Dichroic
600÷750 nm
imager
750÷900 nm
imager
Occulter
wheel
ADC
CAMERA
direct
imager
Pupil
wheel
COLLIMATOR
active
movable
disabled
fix
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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The Zyla fast sCMOS detector
The imagers proposed for the focal planes of V-SHARK are based on the
Zyla sCMOS technology of ANDOR :
 sCmos detector with 2k x 2k squared pixels of 6.5micron side
 Average Q.E. > 60% between 500 and 800 nm
 Read Out Noise ~ 1e- at 280 Mpix/s
 Dark current < 0.1e-/s
 1000 frame per seconds on 200 x 200 pixel sub array
 Global and rolling shutter with ext. sync. (read out time 10µs/line couple)
 Data and control interface USB 3.0 or Camera Link
 Binning up to 8x and subfield selectable with 1 pixel granularity
 Less than 15 k€ delivery in one month
V-SHARK@LBT -- INAF exoplanet Rome meeting
November 7, 2014
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Simulated limit Contrast Performance
10 J
Expected contrast using
coronagraphs with 90 mas IWA
(~5λ/D). Simulation performed at
675nm, 50nm bandwidth using
FLAO residual turbulence at 0.4
arcsec seeing.
50 J
4J
1J
10 pc
5 pc
PSF reconstruction issues related to NCPA
V-SHARK@LBT -- INAF exoplanet Rome meeting
November 7, 2014
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Minimization of the NCP Aberrations
Compact minimalistic reflective design and close to the WFS
Daytime characterization of NCPA by means of the LBTI
Calibration Source and retroreflector.
Continuos monitoring of tracking due to sCMOS technology
Two relayed focal planes at different wavelenghts for SDI
In progress study about a single surface Lyot coronagraph
Input
Pupil plane
Output
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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Critical issues on the V-Shark design
ADC is in convergent beam: we do have a baseline design for
the ADC based on the double triplet of Magellan AO
Flexures producing 1µm offset at M2 are equivalent to
about 1λ/D at focal plane: Pick-Up arm and all the frame
must be very stiff and with short paths
Optical quality of surfaces to avoid wavefront degradation:
better than a total of 40 nm: optical polishing < λ/20 at
550nm, minimalistic optical design with a coronagraph made
up by only two optical surfaces in reflection
Field or Camera rotator? Baseline is ADI and SDI optimized!
Thermal stress on mechanics: by design compact and
insulated
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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V-SHARK the ForeRunner experiment 24/2/2014
INAF-OAR funded
Unfortunately bad weather
Still, very useful for PSF characterization with
simulated seeing (0.8”)
NCPA of about 100nm due to dichroic mount
limited the Strehl to only 32%
It would be very valuable to make an on-sky
test, to have a real VIS PSF
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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Adaptive Optics can work at visible; running fast, saving
the errors and then you may get this…!
GRAZIE..!
Courtesy of S. Jefferies (Maui Air Force Lab)
November 7, 2014
V-SHARK@LBT -- INAF exoplanet Rome meeting
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BET on V_SHARK….!
Cheap and fast but not dirty!
 System Engineering and LabView
 Almost COTS subcomponents
 Raw Cash Flow is 620 k€ in 24 months (300 HW, 120 Tv, 200
Grants)
Small and compact with minimal optics
Forerunner is at LBT and soon may have filters and ADC
(VisAO…)
Modular expansion and binocular with NIR-SHARK
Unique opportunity to do AO imaging in the 600÷900 nm.
Laird Close’ famous sentence: “with the SHARK VIS arm,
wherever you point it’s a paper!”