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The V-SHARK Team: F.Pedichini 2, J.Farinato 1, E.Pinna 3, L.Carbonaro 3, M.Centrone 2, S.Esposito 3, F.Fiore 2, A.Fontana 2, E.Giallongo 2, J.C.Guerra.

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Presentation on theme: "The V-SHARK Team: F.Pedichini 2, J.Farinato 1, E.Pinna 3, L.Carbonaro 3, M.Centrone 2, S.Esposito 3, F.Fiore 2, A.Fontana 2, E.Giallongo 2, J.C.Guerra."— Presentation transcript:

1 The V-SHARK Team: F.Pedichini 2, J.Farinato 1, E.Pinna 3, L.Carbonaro 3, M.Centrone 2, S.Esposito 3, F.Fiore 2, A.Fontana 2, E.Giallongo 2, J.C.Guerra 6, P. Hinz 6, R.Ragazzoni 1, L. Sabatini 2, M.Stangalini 2, V. Testa 2 1) INAF PADOVA2) INAF ROMA 3) INAF-ARCETRI6) STEWARD OBSERVATORY – ARIZONA (USA) The V-SHARK Team: F.Pedichini 2, J.Farinato 1, E.Pinna 3, L.Carbonaro 3, M.Centrone 2, S.Esposito 3, F.Fiore 2, A.Fontana 2, E.Giallongo 2, J.C.Guerra 6, P. Hinz 6, R.Ragazzoni 1, L. Sabatini 2, M.Stangalini 2, V. Testa 2 1) INAF PADOVA2) INAF ROMA 3) INAF-ARCETRI6) STEWARD OBSERVATORY – ARIZONA (USA) THE VISUAL CHANNEL OF SHARK @ LBT Fernando Pedichini on behalf the V-SHARK Team V-SHARK@LBT -- INAF exoplanet Rome meeting November 7, 2014

2 F. Pedichini instrument design, (PI) F. Ambrosinocontrols M. Centronecontrol and camera software L. Sabatinithesis student M. StangaliniA.O. optical simulation code V. Testadata reduction F. Fiorescience E. Giallongo science In good synergy with the NIR-SHARK team! F. Pedichini instrument design, (PI) F. Ambrosinocontrols M. Centronecontrol and camera software L. Sabatinithesis student M. StangaliniA.O. optical simulation code V. Testadata reduction F. Fiorescience E. Giallongo science In good synergy with the NIR-SHARK team! WHO IS V-SHARK @ INAF ROME V-SHARK@LBT -- INAF exoplanet Rome meeting November 7, 2014

3 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. 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. THIS IS FLAO @ LBT ! V-SHARK@LBT -- INAF exoplanet Rome meeting November 7, 2014

4 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 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 V-SHARK IN A NUTSHELL V-SHARK@LBT -- INAF exoplanet Rome meeting November 7, 2014 THERE WILL BE V-SHARK

5 V-SHARK@LBT -- INAF exoplanet Rome meeting November 7, 2014 F #15 from M3 Pick-Up arm LBTI AGW unit Dicroich Optical breadboard

6 The first design of VIS Channel [1.0] 6 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 sSPECIFICATION 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 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting

7 Zemax data for optical quality 7 OPTICS Strehl >99% Scale 1.63 mas /µm AO Residual 80÷100 nm Strehl 50% @ 650 nm OPTICS Strehl >99% Scale 1.63 mas /µm AO Residual 80÷100 nm Strehl 50% @ 650 nm November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting Minimalistic off-axis parabolas collimator-camera optical relay

8 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting 8 The current design of VIS Channel [2.0] Pick-up dichroic ADC direct imager Filter wheel 1 Occulter wheel To LBTI WFS f#15 beam COLLIMATOR Pupil wheel CAMERA Dichroic 600÷750 nm imager 750÷900 nm imager movable fix Filter wheel 2 active disabled

9 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting 9 The current design of VIS Channel [2.0] Pick-up dichroic ADC direct imager Filter wheel 1 Occulter wheel To LBTI WFS f#15 beam COLLIMATOR Pupil wheel CAMERA Dichroic 600÷750 nm imager 750÷900 nm imager movable fix Filter wheel 2 active disabled

10 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting 10 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 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

11 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting 11 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. Simulated limit Contrast Performance 10 pc 1 J 4 J 10 J 50 J 5 pc PSF reconstruction issues related to NCPA

12 Minimization of the NCP Aberrations November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting 12 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 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 Pupil plane Input Output

13 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 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 13

14 V-SHARK the ForeRunner experiment 24/2/2014 INAF-OAR funded 14 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 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

15 15 November 7, 2014 V-SHARK@LBT -- INAF exoplanet Rome meeting Adaptive Optics can work at visible; running fast, saving the errors and then you may get this…! Courtesy of S. Jefferies (Maui Air Force Lab) GRAZIE..!

16 BET on V_SHARK….! November 7, 2014 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. 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. V-SHARK@LBT -- INAF exoplanet Rome meeting 16 Laird Close’ famous sentence: “with the SHARK VIS arm, wherever you point it’s a paper!”


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