The Subaru Coronagraphic Extreme-AO system (SCExAO)

Transcription

1 The Subaru Coronagraphic Extreme-AO system (SCExAO) O. Guyon, N. Jovanovic, F. Martinache, G. Singh, J. Lozi, C. Clergeon, T. Kudo, D. Doughty, S. Goebel, P. Phatak, J. Morino and J. Males Subaru Telescope, National Astronomical Observatory of Japan VAMPIRES FIRST COCORO VECTOR VORTEX AO188 P. Tuthill B. Norris G. Schworer P. Stewart FPM DESIGN K. Newman E. Huby G. Perrin L. Gauchet S. Lacour F. Marchis S. Vievard O. Lai G. Duchene T. Kotani J. Woillez N. Murakami O. Fumika N. Baba T. Matsuo J. Nishikawa M. Tamura J. Kuhn E. Serabyn CHARIS J. Kasdin M. A. Peters T. Groff M. Galvin M. Carr Y. Minowa Y. Hayano MKIDS B. Mazin S. Meeker M. Strader J. Van Eyken

2 The roadmap... TMT MKIDS CHARIS SAPHIRA+spec kle control VAMPIRES/FIRST SCExAO

3 AO188 General-purpose SCAO system NGS and sodium LGS modes 188 curvature system Visible lucky imaging RAVEN MOAO/GLAO University of Victoria IRCS Imaging+spectroscopy Kyoto-3D Visible light IfU Univ. of Tokyo + Kyoto Univ. SCExAO is a central part of Exoplanet instrumentation at Subaru Telescope Together with its modules and IRD, it provides Subaru Telescope with unique and broad exoplanet discovery and characterization capabilites YOU CAN APPLY TO USE SCExAO VAMPIRES Aperture masking + polarimetry Univ of Sydney FIRST Spectro- Interferometry Observatoire de Paris SAPHIRA near-ir photon counting camera Univ of Hawaii IfA [until 2016] SCExAO Extreme-AO + coronagraphy CHARIS Near-IR IFS, optimized for high contrast imaging NAOJ + Princeton Univ. optical mode fiber [2016] IRD Near-IR Doppler radial velocity [>2016?] HiCIAO Near-IR high contrast imaging with coronagraph [until ~2016] MKIDs exoplanet camera Near-IR/Vis photon counting camera with wavelength resolution NAOJ + UCSB [2016] We are preparing SCExAO to be visitor instrument on TMT OPTIMIZED FOR SMALL IWA (<0.1 mas) reflected light giant planets on Subaru Earths around M-type stars on TMT

4 SCExAO Telescope Properties: Single object AO Narrow field-of-view (<10 ) Natural guide star AO188 - Facility AO 30% Strehl in H-band SCExAO VIS IR HiCIAO High contrast imaging instrument optimized for very small inner working angle (1-3 λ/d) Uses advanced technologies, continuously evolves to take advantage of new concepts, detectors etc... Prime high contrast imaging system in the world until ELTs Prototype for ELT habitable planets spectroscopic characterizer

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6 Key Features: Reflective relay optics addressing chromaticity Wavefront sensing: - Non-modulated pyramid WFS (VIS), 3.6 khz - Coronagraphic low order wavefront sensor (IR) for non-common tip/tilt errors Wavefront control 2k DM and gas supply system Fast frame rate internal science camera (IR) Active speckle nulling/control High perf. coronagraphs PIAA, Vector Vortex, 4QPM, 8OPM, shaped pupil (IR) Visible Aperture Masking Polarimetric Interferometer for Resolving Exoplanetory Signatures (VAMPIRES) (VIS) Fibered Imager for a Single Telescope (FIRST) (VIS) Fourier Lucky imaging (VIS) Broadband diffraction limited internal cal. Source + phase turbulence simulator

7 Latest speckle nulling results on-sky Single frames: 50 us Meta data: Date: June 2 nd 2014 Target: RX Boo (also repeated on Vega) Seeing: <0.6 AO correction: 0.06 post-ao corrected in H-band (0.04 is diffraction-limit) Coronagraph: None (used Vortex on Vega) Region of interest Martinache, F. et. al. On-sky speckle nulling demonstration at small angular separation with (SCExAO) instrument, ArXiv: Sum of 5000 frames: shift and add Martinache, F. et. al. On-sky speckle nulling with the Subaru coronagraphic extreme AO (SCExAO) instrument, paper no: , Thursday, 4 pm, AO session

8 High-order wavefront correction Extreme AO High order correction provided by highly sensitive non-modulated pyramid wavefront sensor, with deep depletion EMCCD Corrects 1500 modes at 3.6 khz Operates behind AO188, i.e. second stage AO correction (offers 30-40% Strehl in H-band) Offers 90% Strehl in H-band Tested with turbulence simulator in the lab: 300 nm RMS wavefront error, windspeed 5 m/s 1.5 khz loop speed ( 3.6 khz in Apr 2015) 830 modes ( 1500 modes in Apr 2015) Achieved extreme-ao performance on realistic turbulence simulation

9 High-order wavefront correction Extreme AO (Nov 2014, internal source + 300nm WFE)

10 SCExAO visible images FWHM 17mas Resolves some stars

11 VAMPIRES sub-diffraction limited imager/polarimeter Aperture masking interferometer enables subdiffraction limited imaging Polarimeter extremely precise with 4 layers of calibration Operates from nm very high angular resolution The VAMPIRES instrument: Imaging the innermost regions of protoplanetary disks with polarimetric interferometry, Norris et. al, 2015, MNRAS

12 VAMPIRES On-sky results from engineering Chi Cyg Measurement of W Hydra dust shell June 2014 Engineering Chi Cyg Power spectrum (log scale) Note fall-off in power at longer BLs, since object is resolved. No polarized structure detected around Chi Cyg. However (unpolarized) diameter still measured: VAMPIRES-measured diameter: 32.2 ± 0.13 mas (750 nm) Literature Values: 32.8± 4.10 mas (V band) (CHARM catalog, Richichi et al. 2005)

13 FIRST sub-diffraction limited spectro-imager Splits Subaru pupil into discrete coherent beams, filtered and transported by single mode fibers Beams are recombined into a linear fringe pattern which is dispersed on a photon-counting detector Well calibrated high angular resolution imaging + spectroscopy in nm

14 FIRST : on-sky results (Eta Peg) Raw data

15 SCExAO high contrast imaging capabilities: expected schedule NearIR planet detection at moderate contrast NearIR planet imaging at high contrast Visible light interferometry, polarimetry (disks, stellar physics) Near-IR spectroscopic characterization Ultra-High contrast reflected light strong visible light capabilities VAMPIRES PyWFS FIRST CHARIS SAPHIRA MKIDs Phase 1 LOWFS + slow speckle control Moderate contrast improvement over HiCIAO Small IWA (~2 l/d) coronagraphy Phase 2 Significant contrast improvement over HiCIAO thanks to ExAO High SR (~0.9) more robust performance for coronagraph and LOWFS systems Smaller IWA (~1 l/d) Full system (CHARIS+MKIDS) MKIDs camera faster speckle control and better calibration significantly higher contrast at small separation (~1e-8) Spectroscopy: CHARIS + MKIDS provide spectroscopy from ~0.8 um to 2.7um

16 CHARIS Integral Field Spectrograph (2016) Major Science Objective: Spectral characterization of Exoplanets, Disks, Brown dwarfs 2.07 x2.07 FOV LOW RESOLUTION MODE: R~19, J+H+K Band 65-70% instrument throughput, 15% (10% K) from atmosphere to detector HIGH RESOLUTION MODE: R~70-90: J,H, and K Bands 55-60% instrument throughput, ~15% from atmosphere to detector New technology contributions: Crosstalk Mitigation and New Dispersion Modes

17 CHARIS Integral Field Spectrograph (2016) ZeroDur Telescope Foreoptics

18 MKIDs camera (2016) Enables photon-counting performance in near-ir, with energy resolution MKIDs + MEMS for a smart focal plane high contrast camera (NAOJ / UCSB) Pixels are microwave resonators at ~100mK photon hits resonator frequency changes MKIDs detector MKIDs Palomar

19 <800nm Wavefront control for ultra-high contrast Extreme-AO LOOP High speed pyramid wavefront sensor Measures aberrations 3.7 khz Hz Hz CORONAGRAPHIC LOW ORDER LOOP Near-IR camera Measures loworder aberrations nm (rejected by coronagraph) MKIDs camera Facility Adaptive Optics system Sharpens image 2000 actuator Deformable mirror >800nm coronagraph system removes starlight nm Measures residual starlight SPECKLE CONTROL LOOP nm CHARIS spectrograph Exoplanet spectra

20 SCExAO uniquely expands exoplanetary system characterization capabilities Central star: Diameter, shape, pulsations, limb darkening (FIRST, IRD) Binarity masses, constrain RV measurements (FIRST/VAMPIRES/IRD) Chemical composition (IRD) Planet mass and orbit from RV (IRD) + imaging Reflected visible light spectra from postcoronagraph fiber-fed spectroscopy (SCExAO + IRD) Near-IR spectroscopy (CHARIS + MKIDs) Hot inner dust (thermal emission): visible spectroimaging (FIRST) nearir spectroimaging (CHARIS+MKIDs) Reflected light dust: visible spectroimaging (FIRST) polarimetric imaging (VAMPIRES) near-ir imaging+spectroscopy (CHARIS+MKIDs)

21 Opportunities and challenges SCExAO will be the prime high contrast imaging system until ELTs will image and characterize known RV planets will map disks and disk/planets interactions first reflected light images of giant planets push to lower mass planets and shorter wavelength unique visible light diffraction limited imaging capabilities Huge benefits from complementary measurements between modules SCExAO will benefit from ULTIMATE-Subaru feed SCExAO directly from telescope (no AO188): higher throughput, better performance SCExAO and modules should feed an active, world-leading exoplanetary systems international research group (following and expanding on SEEDS). Coherent scientific planning between SCExAO modules (including IRD) is essential to take full advantage of new capabilities SCExAO is testing and maturing technologies that will be used on future space coronagraph missions (WFIRST for example) Active and innovative research group (observations + instrumentation) will position NAOJ+partners to take the first spectra of habitable planets with TMT First spectroscopic observations to look for life outside solar system

22 SCExAO and TMT We intend to ready SCExAO for TMT, as a visitor instrument soon after first light Prime science case (focused survey): spectroscopy of habitable planets around nearby M-type stars SCExAO is ideally suited for this (high contrast + small IWA) SCExAO on TMT Note: It is assumed here that each star has a habitable planet Only ~15% of these circles are real still plenty of opportunities

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