SHARK-NIR overview and optomechanical design: an update
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1 SHARK-NIR overview and optomechanical design: an update Davide Greggio The SHARK-NIR Team: J.Farinato 1, F.Pedichini 2, E.Pinna 3, C.Baffa 3, A.Baruffolo 1, M.Bergomi 1, A.Bianco 8, L.Carbonaro 3, E.Carolo 1, A.Carlotti 4, M.Centrone 2, L.Close 5, J.Codona 5, M.De Pascale 1, M.Dima 1, S.Esposito 3, D.Fantinel 1, G.Farisato 1, W.Gaessler 6, E.Giallongo 2, D.Greggio 1, J.C.Guerra 5, O.Guyon 5, P.Hinz 5, C.Knapic 9, F.Lisi 3, D.Magrin 1, L.Marafatto 1,7, A.Puglisi 3, R.Ragazzoni 1, B.Salasnich 1, M.Stangalini 2, R.Smareglia 9, D.Vassallo 1,7, C.Verinaud 4, V.Viotto 1, A.Zanutta 8
2 WHY SHARK Considering: The excellent AO performance The current and next generation LBT instruments scenario The Northern Emisphere scenario The strong science case The wish to make a fast track project We proposed to build: a simple camera (compact, light, close to the WFS) designed for high contrast imaging working in VIS and NIR bands capable to do: Coronagraphy Direct Imaging LR Spectroscopy
3 WHAT IS SHARK? SHARK-NIR Coronagraphic camera with spectroscopic capabilities Extreme adaptive optics correction of FLAO Synergy with other LBT instruments: SHARK-VIS, LMIRCam Pyramid WFS Pyramid WFS SHARK-NIR SHARK NIR J; H LSS R~100 R~1000 LMIRCam K; L; M SHARK VIS R; I SHARK-VIS
4 SHARK POSITION AT LBT Photo credit: LBTO - Enrico Sacchetti LINC-NIRVANA SHARK-VIS SHARK-NIR LBTI LUCI
5 SHARK SCIENCE TARGETS Main science target: direct imaging of exo-planets (detection and characterization) Other science: Brown dwarfs Protoplanetary disks Stellar jets AGN
6 INSTRUMENT SPECIFICATIONS SHARK NIR main characteristics Observing Modes Imaging/Coronagraphy/Spectroscopy/DBI Detector format [px] 2048x2048 ( 1220x1220 used area) Waveband [μm] FoV x ["] 18 FoV y ["] 18 FoV along the diagonal ["] 25.5 Plate scale [mas/px] 14.5 Airy 0.96 micron [px] 2 # of mirrors in the camera 8 (3 flat, 1DM and 4 OA s) ADC Yes Nominal Strehl at <18 FoV diameter (in all Bands) >98%
7 OPTO-MECHANICAL LAYOUT Optical bench + Cryostat SHARK Holding structure
8 OPTO-MECHANICAL LAYOUT
9 CORONAGRAPHY IN SHARK 1 st pupil plane Intermediate focal plane 2 nd pupil plane Science focal plane Apodizer, shaped pupil Star occulter Lyot stop Scientific image I(x) occulter I(x) I(x) Lyot stop I(x) x Weak companion x x Weak companion x
10 CORONAGRAPHIC TECHNIQUES Gaussian Lyot Shaped pupil (both symmetric and asymmetric discovery space) APLC/4 Quadrant (?) Field stabilized mode (de-rotator ON) requires circular symmetric masks (Classical Lyot and Gaussian Lyot). Shaped Pupil and APLC are used in Pupil stabilized mode (de-rotator OFF)
11 CORONAGRAPHIC PERFORMANCE 5-σ detection limit in H band for Rmag=8 with SOUL Seeing 0.4 Seeing 0.6
12 ~300 mm SHARK OPTICAL LAYOUT apodizer beam splitter to the tip-tilt WFS Tip-tilt mirror ADC incoming light Pupil lens (deployable) cryostat window detector fold mirror fold mirror occulters and slit Lyot stop, GRISM Science filter wheels fold mirror Narcissus mirror cold baffle
13 ~300 mm SHARK OPTICAL LAYOUT apodizer beam splitter to the tip-tilt WFS incoming light Tip-tilt mirror ADC Pupil lens (deployable) Coronagraphic planes cryostat window detector fold mirror fold mirror occulters and slit Lyot stop, GRISM Science filter wheels fold mirror Narcissus mirror cold baffle
14 ~300 mm SHARK OPTICAL LAYOUT tip-tilt sensor apodizer beam splitter to the tip-tilt WFS Closed loop Tip-tilt mirror ADC incoming light Pupil lens (deployable) cryostat window Beam splitter detector fold mirror fold mirror occulters and slit Lyot stop, GRISM Science filter wheels fold mirror Narcissus mirror cold baffle
15 SPECTROSCOPIC MODE Dispersing element DISPERSIVE ELEMENTS Low Res Prism Medium Res Grism R CORO SLITS WITH OCCULTER Slit width Occulter size Coro slit mas 100 mas Coro slit mas 200 mas GRISM/PRISM Focal plane CORO SLIT
16 DUAL BAND IMAGING MODE DUAL BAND FILTERS Name λ 1 [nm] Δλ 1 [nm] λ 2 [nm] Δλ 2 [nm] HOLE(no DBI) Radial FoV 1 H2-H ContJ-Pa β ContH-Fe II Phase diversity
17 RECENT UPDATES FAST TT SENSOR Tip-tilt WFS upgrade New InGaAs camera (C- RED2) Sensitive in the full SHARK- NIR waveband ( μm) Frame-rate up to 14KHz (with 32X32 px window) Same FoV as before (11 x13 ) Low RON (<25e - ) 3 mas precision up to 1KHz BEFORE NOW
18 RECENT UPDATES INTERNAL NCPA CORRECTION Tip-tilt mirror upgrade Tip-tilt mirror replaced by ALPAO DM actuators, 13.5 mm pupil NCPA can be corrected internally without affecting pyramid s performance Smaller volume NCPA measured with phase diversity on science image
19 THE SHARK-NIR TEAM INAF-Padova (Project Responsible, Opto-Mechanics and INS Software) INAF-Arcetri (AO Interaction and NIR camera testing support) Steward Observatory (LBTI interfaces, NIR camera sub-system) INAF-Brera (Dispersive elements design) MPIA (for motors electronics and SW design support) IPAG (CORO mask design) INAF-Roma (Coordination with VIS Channel) INAF-Trieste (Data archiving) Science team (astronomers from 12 institutes)
20 CURRENT STATUS LBT board approval: end of April 2017 Procurement phase: June 2017 September 2018 AIV phase: September 2017 January 2019 Preliminary Acceptance Europe: January 2019 Commissioning start: June 2019 SHARK-NIR operation: October 2019
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