- The AO modes for HARMONI - From Classical to Laser-assisted tomographic AO systems

Transcription

1 - The AO modes for HARMONI - From Classical to Laser-assisted tomographic AO systems Benoît Neichel, Thierry Fusco, Carlos M. Correia, Kjetil Dohlen, Leonardo Blanco, Kacem El Hadi, Jean-François Sauvage, Noah Schwartz, Yoshito Ono, Fraser Clarke, Emmanuel Hugot, Miska Le Louarn, Niranjan A. Thatte, Matthias Tecza, Hermine Schnetler, Ian Bryson, Angus M. Gallie, David M. Henry, Tim J. Morris, Richard M. Myers, Joël Vernet, Jérôme Paufique, Peter Hammersley, Jean-Luc Gach, Alexis Carlotti, Ariadna Calcines, Pascal Vola, Sandrine Pascal, Marc Llored, Dave Melotte, Olivier Martin, Arlette Pecontal, Andrew Reeves, James Osbron, Matthew Townson

2 HARMONI Overview HARMONI Consortium Partner Associate Partner Responsibilities University of Oxford STFC RAL Space Spectrographs & Obs. Prep STFC UK ATC Edinburgh Univ. of Durham Cryostat, AIV, Rotator, LTAO IAC, Tenerife CSIC CAB (INTA), Madrid CRAL, Lyon LAM, Marseille IPAG, Grenoble IRAP, Toulouse ONERA, Paris IPAG, Grenoble Pre-optics & Electronics Calibration & Sec. guiding IFU & Software SCAO, LTAO, High Contrast

3 HARMONI Overview HARMONI Consortium Partner Associate Partner Responsibilities University of Oxford STFC RAL Space Spectrographs & Obs. Prep STFC UK ATC Edinburgh Univ. of Durham Cryostat, AIV, Rotator, LTAO IAC, Tenerife CSIC CAB (INTA), Madrid CRAL, Lyon LAM, Marseille IPAG, Grenoble IRAP, Toulouse ONERA, Paris IPAG, Grenoble Pre-optics & Electronics Calibration & Sec. guiding IFU & Software SCAO, LTAO, High Contrast Thanks for hosting us this week!!

4 HARMONI Overview HARMONI = High Angular Resolution - Monolithic - Optical and Nearinfrared - Integral field spectrograph First light ELT instrument

5 HARMONI Overview HARMONI = High Angular Resolution - Monolithic - Optical and Nearinfrared - Integral field spectrograph First light ELT instrument Workhorse instrument - visible and near-infrared spectroscopy ( µm) Integral Field Spectrograph providing ~ spectra per exposure 3D data cube

6 HARMONI Overview Bands V+R or I+z+J or H+K I+z or J or H or K HARMONI = 3 resolving powers Wavelengths (μm) , , , , , Z or J_high or H_high or K_high 0.9, 1.2, 1.65, 2.2 (TBD) R ~3000 ~7500 ~ D data cube

7 1.52 x 2.14 HARMONI Overview HARMONI = 4 spatial scales 60 x 30 mas 0.61 x x152 spaxels 20 mas 10 mas 4 mas 3.04 x D data cube 6.42 x 9.12

8 1.52 x 2.14 HARMONI Overview HARMONI = 4 spatial scales 60 x 30 mas 0.61 x x152 spaxels 20 mas 10 mas 4 mas Assisted 3.04 x 4.28 with 6.42 x 9.12 Adaptive Optics

9 HARMONI: Two AO modes Single Conjugated AO Laser Tomography AO x6 High-Performance Low sky coverage High-Performance & sky coverage

10 HARMONI HARMONI, SCAO & LTAO implementation

11 HARMONI HARMONI, SCAO & LTAO implementation Telescope Pre-Focal Station Focal plane Relay Seeing limited Light from telescope Re-imaged focal plane HARMONI Cryostat Nasmyth Platform

12 HARMONI HARMONI, SCAO & LTAO implementation Telescope Pre-Focal Station Focal plane Relay Seeing limited Light from telescope SCAO WFS SCAO dichroic SCAO HARMONI Cryostat Nasmyth Platform

13 HARMONI HARMONI, SCAO & LTAO implementation Telescope Pre-Focal Station Dichroic Relay Seeing limited Light from telescope LGS (<0.6um) NGS Pick-off Truth Pick-off SCAO LTAO LGSWFS Module HARMONI Cryostat Nasmyth Platform

14 HARMONI HARMONI, SCAO & LTAO implementation LGSWFS From Telescope SCAO & NGS WFS IFS

15 HARMONI HARMONI, SCAO & LTAO implementation LGSWFS From Telescope SCAO & NGS WFS IFS

16 HARMONI SCAO SCAO system baseline is to use a pyramid WFS:

17 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity +2 mag.

18 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity

19 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the Island effect

20 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the Island effect See Noah Schwartz talk on Friday 50cm Spiders

21 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the Island effect See Noah Schwartz talk on Friday

22 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the Island effect Small modulation provides information on what s behind the spider + Secret ingredient See Noah Schwartz talk on Friday

23 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the Island effect Small modulation provides information on what s behind the spider + Secret ingredient See Noah Schwartz talk on Friday Before After SCAO will provide a SR of >70% in K-band Residuals less than 50nm

24 HARMONI SCAO High Contrast : Spectral characterization of young Jupiters around nearby stars in H & K bands at R= , with a 10-6 contrast at 200mas. From A. Carlotti, A. Vigan, D. Mouillet, M. Bonnefois

25 HARMONI SCAO High Contrast : Simulated data of 4 planets w/ 10-6 planets contrast & 51 Eri b-like synthetic spectrum (2h exp. with H=6 star). From A. Carlotti, A. Vigan, D. Mouillet, M. Bonnefois

26 HARMONI HARMONI, SCAO & LTAO implementation LGSWFS High-Order Loop SCAO & NGS WFS Low-Order Loop

27 HARMONI LTAO LTAO Top-Level Specifications: 4 mas 10 mas 20 mas 60 x 30 mas Strehl K > 60% Jitter < 2mas Sky Coverage >10% at the Pole EE (20mas) > 40% Jitter < 5mas Sky Coverage of >50% at the Pole EE (40mas) > 50% Jitter < 10mas Sky Coverage of >90% at the Pole

28 HARMONI LTAO LTAO Top-Level Specifications: 4 mas 10 mas 20 mas 60 x 30 mas Strehl K > 60% Jitter < 2mas Sky Coverage >10% at the Pole EE (20mas) > 40% Jitter < 5mas Sky Coverage of >50% at the Pole EE (40mas) > 50% Jitter < 10mas Sky Coverage of >90% at the Pole Set requirements on the LGS High-Order Loop

29 HARMONI LTAO LTAO Top-Level Specifications: 4 mas 10 mas 20 mas 60 x 30 mas Strehl K > 60% Jitter < 2mas Sky Coverage >10% at the Pole EE (20mas) > 40% Jitter < 5mas Sky Coverage of >50% at the Pole EE (40mas) > 50% Jitter < 10mas Sky Coverage of >90% at the Pole Set requirements on the LGS High-Order Loop Set requirements on the NGS Low-Order Loop

30 HARMONI LTAO Laser constellation R0 scaled km ZA=0 Optimal LGS constellation between R=[15-40] SR (K Band) km ZA=60 130km ZA=45 Small constellation greatly helps for tomographic error See Thierry Fusco talk on Thursday LGS Radius (arcsec)

31 HARMONI LTAO Sensing on LGS Sodium layer T ~ 20km H ~ 80km Predicted spot elongation pattern LLT Pupil plane LLT Detector plane Distance from launch site

32 HARMONI LTAO Dealing with spot elongation 1 25 LLT Pupil plane Ideally, we need subapertures with 25x25 pixels of ~1 Detector plane Distance from launch site For 80x80 subapertures, we need 2000 x 2000 pixels

33 HARMONI LTAO Dealing with spot truncation LLT Pupil plane Most likely, we will have no more than 10x10 pixels Detector plane Distance from launch site Strong truncation

34 HARMONI LTAO Dealing with spot truncation Truncation induces biases that are projected on-axis by the Tomography Up to 300nm x6 See Leo Blanco talk on Thursday

35 HARMONI LTAO Dealing with spot truncation One way to reduce this impact is to reject the truncated measurements Down to 80nm x6 See Leo Blanco talk on Thursday

36 HARMONI LTAO Sensing on NGS Main offender is the telescope Windshake Single-Sided Amplitude Spectrum of y(t) PSD ATM PSD WS 10-5 Y(f) 2 /Hz Atmosphere = 15 mas Windshake = 263 mas Temporal frequency [Hz] But windshake is isoplanatic: we can use the telescope WFS to reduce it

37 HARMONI LTAO Sensing on NGS Jitter control strategy: Use bright but far stars to compensate windshake with telescope WFS Use faint but close star to compensate atmospheric jitter 1.2 to 2.2 microns 2x2 Shack-Hartmann 8 mas / pixel 125 pixel / subap. 500 Hz

38 HARMONI LTAO Sensing on NGS Jitter control strategy: Use bright but far stars to compensate windshake with telescope WFS Use faint but close star to compensate atmospheric jitter 1.2 to 2.2 microns 0.8 South galactic Pole 90% Sky Cov. for 10mas 2x2 Shack-Hartmann 8 mas / pixel 125 pixel / subap. 500 Hz Sky Cov % Sky Cov. for 5mas 10% Sky Cov. for 2mas jitter (mas)

39 HARMONI LTAO Sensing on NGS See Carlos Correia poster on Thursday

40 See Carlos Correia poster on Thursday HARMONI LTAO Sensing on NGS Cosmos Field LTAO 1NGS jitter [mas] 10 DEC [deg] DEC [deg] GoodS Field LTAO 1NGS Old ESO profile RA [deg] RA [deg] 0.2 The NGS strategy fulfills the science requirements for all observations jitter [mas] 0.2

41 Conclusion: HARMONI schedule 12/2017 PDR FDR MAIT

42 Conclusion: HARMONI schedule Dr. Frans Snik 12/2017 PDR 2019 FDR MAIT : integration at the telescope 2024: 1 st light!

43 - The AO modes for HARMONI - 1 more slide before Coffee Break!

44 Register now, for the 2 to 4 October 2017 in Padova, Italy

45 Marseille 2016 Register now, for the 2 to 4 October 2017 in Padova, Italy

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47 HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity