High-contrast imaging with E-ELT/HARMONI A. Carlotti, C. Vérinaud, J.-L. Beuzit, D. Mouillet - IPAG D. Gratadour - LESIA Spectroscopy with HARMONI - 07/2015 - Oxford University 1
Imaging young giant planets Planetary population model for young stars 0.1 UA 1 UA 10 UA (at 10 parsecs) Planet/star relative contrast (at 1.65 μm) V T J S SPHERE Angular separation (arcsec) Gratton, 2014 (from Bonavita et al. 2012) 2
What contrast for HARMONI? HARMONI is not specifically optimized for high-contrast Single component vs. dedicated high-contrast arm Spec: 10-6 at 200mas ; Goal: 10-5 -10-6 at 40mas Follow-up of SPHERE, GPI, and other targets ; Medium spectral resolution makes possible observation of K & CO lines. Characterization of planets around M dwarves. Observation of the inner edge of debris disks & associated planetary or substellar companions. 3
Imaging young giant planets Planetary population model for young stars 0.1 UA 1 UA 10 UA (at 10 parsecs) Planet/star relative contrast (at 1.65 μm) V T J S SPHERE Angular separation (arcsec) Gratton, 2014 (from Bonavita et al. 2012) 4
Limitations on contrast Telescope AO (M4 has ~74 actuators across pupil) Telescope aperture (segments discontinuities, obscuration) Instrument stability: temporal & chromatic NCPA thermal drift, chromatic pupil shift, Instrument limitations: non-corrected atmospheric dispersion limited access to pupil & image planes cross-talk & diffusion in the IFS 5
AO: semi-analytical approach 1 - Analytic 2D power spectrum of atmospheric residuals (after SCAO ; ~180nm RMS) 2 - Best fit of M1 by M4: Aberrations on each segment create ~60nm RMS global wavefront error. conservative case ideal case 3 - Non common path estimation/calibration error - 5nm RMS in this example. - Exhaustive system analysis required. 6
AO: semi-analytical approach Infinitely long exposure (no photon noise) 10-0 PSF cross-section (5-sigma detection limits) 10-2 atmospheric residuals 10-4 quasi-statics ideal coronagraph conservative case 10-6 differential imaging 10-0 10-2 10-4 50mas 100mas atmospheric residuals quasi-statics 10-5 - 10-6 ideal coronagraph ideal case 10-6 differential imaging 7
AO: end-to-end model GPU-based COMPASS platform (Gratadour et al. 2014, Carlotti et al., 2014) Open-source, freely distributed code ; Uses Nvidia s CUDA software & hardware. Segments introduce phase & amplitude discontinuities: 1% reflectivity ; 50nm piston ; 50nm TT ; 50nm defocus w/ 10nm mean 8
AO: end-to-end model PSF Strehl ratio ~70% w/ E-ELT aperture w/ apodizer Diffraction dominated PSF Apodized PSF w/ halo Development of a COMPASS extension for high-contrast imaging. 9
Compatible coronagraphs Baseline constraints: - atmospheric dispersion not corrected => No focal plane mask. - Pupil plane masks are the only option here. Pupil Image (log scale) 1.4-2.45 μm band 10
Apodizing the aperture see Aime & Soummer 2001, Vanderbei et al. 2003, Carlotti et al. 2011 Apodized Lyot coronagraph (as used in VLT/SPHERE & Gemini/GPI): Apodized aperture Apodized PSF Shaped pupil coronagraph (as used in WFIRST-AFTA and in SUBARU/SCExAO): 11
Compatible coronagraphs Solution to satisfy constraints: - direct apodization, i.e., Shaped Pupils, APP, still compatible. - pupil tracking mode enables angular differential imaging. Pupil Image (log scale) IFU Slice 12
Aperture constraints Missing segments Central obscuration constrains the coronagraph Nominal E-ELT E-ELT -5 rings TMT Not a decisive problem for 1 st light instruments Δmag=12.5 detection, i.e., 10-5 contrast & same # of photons in the PSF core: Nominal E-ELT: E-ELT -5 rings: TMT: 30% obsc.: 36 mas 63% obsc.: 54 mas 14% obsc.: 37 mas 13
Advantages of a dedicated arm Simplest option: 1 apodizer & 1 focal plane mask reduces diffusion, dynamical range on camera w/ a (simple) ADC to allow APLC-like configuration: smaller angular separation ~30mas w/ same contrast weaker chromatic variations of NCPA => better stability 14
IFS: cross-talk & diffusion Local contamination from spectral & spatial cross-talks Global contamination due to 0.5% diffusion 1.4μm 2.4μm 1.4-2.4μm band 15
PSF spreads during exposure Conservative example with a star 5h from meridian, 63 from zenith 1min exposure leads to 6.4mas dispersion. Relative positions for two epochs: PSF blur is minimized by targeting blue star: T0, Z0 T0+Δt, Z1 > Z0 worst blur if blue star is targeted: (2.45μm observation) worst blur if red star is targeted: (0.8μm observation) rescaled 16
Quasi-static aberrations 0.4 0.3 0.2 0.1 0 0.1 0.2 0.3 0.4 PSF w/ cross-talk & diffusion 0.4 0.3 0.2 0.1 0 0.1 0.2 0.3 0.4 Angular distance (arcsec) 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 5.5 100nm RMS residual aberrations. - temporal evolution? Only one surface rotates wrt. instrument. - chromatic evolution? Fresnel effects to be modeled. Diffusion produces 10-5 plumes artefacts. PSF is blurred vertically due to cross-talk, dispersion 17
Summary HARMONI has great potential for planet characterization: 10-100 times the spectral resolution of SPHERE down to 40 mas angular sep. (5 times smaller than at VLT) Robust coronagraphic solutions exist. Next steps for the preliminary design phase: Detailed system analysis required for NCPA. What to expect from post-processing algorithms? Development of a GPU-based coronagraphic module 18