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

- 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

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

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

HARMONI Overview HARMONI = High Angular Resolution - Monolithic - Optical and Nearinfrared - Integral field spectrograph First light ELT instrument Workhorse instrument - visible and near-infrared spectroscopy (0.5 2.4 µm) Integral Field Spectrograph providing ~ 30 000 spectra per exposure 3D data cube

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) 0.45-0.8, 0.8-1.35, 1.45-2.45 0.8-1.0, 1.1-1.35, 1.45-1.85, 1.95-2.45 Z or J_high or H_high or K_high 0.9, 1.2, 1.65, 2.2 (TBD) R ~3000 ~7500 ~20000 3D data cube

1.52 x 2.14 HARMONI Overview HARMONI = 4 spatial scales 60 x 30 mas 0.61 x 0.86 214 x152 spaxels 20 mas 10 mas 4 mas 3.04 x 4.28 3D data cube 6.42 x 9.12

1.52 x 2.14 HARMONI Overview HARMONI = 4 spatial scales 60 x 30 mas 0.61 x 0.86 214 x152 spaxels 20 mas 10 mas 4 mas Assisted 3.04 x 4.28 with 6.42 x 9.12 Adaptive Optics

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

HARMONI HARMONI, SCAO & LTAO implementation

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

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

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

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

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

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

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

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

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

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

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

HARMONI SCAO High Contrast : Spectral characterization of young Jupiters around nearby stars in H & K bands at R=3000-20000, with a 10-6 contrast at 200mas. From A. Carlotti, A. Vigan, D. Mouillet, M. Bonnefois

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

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

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

HARMONI LTAO Laser constellation R0 scaled 0.6 90km ZA=0 Optimal LGS constellation between R=[15-40] SR (K Band) 0.4 0.2 180km ZA=60 130km ZA=45 Small constellation greatly helps for tomographic error See Thierry Fusco talk on Thursday 20 40 60 80 LGS Radius (arcsec)

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

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

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

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

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

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 10-10 Atmosphere = 15 mas Windshake = 263 mas 10-2 10-1 10 0 10 1 10 2 Temporal frequency [Hz] But windshake is isoplanatic: we can use the telescope WFS to reduce it

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. 0.6 0.4 0.2 50% Sky Cov. for 5mas 10% Sky Cov. for 2mas 0.0 0 5 10 jitter (mas)

HARMONI LTAO Sensing on NGS See Carlos Correia poster on Thursday

See Carlos Correia poster on Thursday HARMONI LTAO Sensing on NGS 16 11 15 Cosmos Field 14 13 10 9 0.3 LTAO 1NGS 12 8 9 7 6 0.1 5 4 jitter [mas] 10 DEC + 2.17 [deg] DEC + 27.94 [deg] 11 7 0.2 6 4 3 0.1 3 GoodS Field 0.0 2 1 LTAO 1NGS Old ESO profile 0.0 2 1 0 0.1 RA + 53.00 [deg] 0.2 0.1 0 0.0 0.1 RA + 150.05 [deg] 0.2 The NGS strategy fulfills the science requirements for all observations jitter [mas] 0.2

Conclusion: HARMONI schedule 12/2017 PDR 2019 2023 FDR MAIT

Conclusion: HARMONI schedule Dr. Frans Snik 12/2017 PDR 2019 FDR MAIT 2023 2024: integration at the telescope 2024: 1 st light!

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

https://www.ict.inaf.it/indico/event/521/ Register now, for the 2 to 4 October 2017 in Padova, Italy

https://www.ict.inaf.it/indico/event/521/ Marseille 2016 Register now, for the 2 to 4 October 2017 in Padova, Italy

HARMONI SCAO SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity 7 9 13 15 17