Jean- Luc Beuzit and David Mouillet

Transcription

1 ONERA Scien,fic Days / Journées Scien,fiques Onera High Contrast Imaging / Imagerie à Haute Dynamique Perspec8ves for exoplanet imaging Jean- Luc Beuzit and David Mouillet

2 Perspec8ve: back in 8me A rela8vely recent technique: on general use instruments 90 s: first ahempts Coronagraph: Lyot Planetary coronagraph AO: ADONIS on ESO- 3.6m No AO Reference differen8al imaging 10 1 Bpic: Smith & Terrile, 1984 Mouillet et al., 1997

3 Perspec8ve: back in 8me A rela8vely recent technique: on general use instruments 90 s: first tries 2000 s: larger investment, strong learning curve: More powerful AO system on 8- m telescopes. AO and coronagraphy associated but not yet op8mized Huge efforts on observing procedures (reference, ADI, SDI), and data processing Large observing programs

4 Perspec8ve: back in 8me A rela8vely recent technique: on general use instruments 90 s: first tries 2000 s: larger investment, strong learning curve Coronagraph: Lyot Planetary coronagraph AO: ADONIS on ESO- 3.6m No AO Reference differen8al imaging 10 1 Coronagraph: Lyot AO: NAOS on ESO- 8m Reference differen8al imaging (matching parallac8c angles) Bpic: Smith & Terrile, 1984 Mouillet et al., 1997 Lagrange et al., 2008

5 Perspec8ve: back in 8me A rela8vely recent technique: on general use instruments 90 s: first tries 2000 s: larger investment, strong learning curve Now: first dedicated instruments for High contrast (XAO, coronagraphy, high stability, various differen8al imaging modes) Large surveys: survey observa8on tools, keep «good» sensi8vity High resolu8on PSF Saturated PSF Coronagraphic image ~ 3-20 λ/d

6 Performance Key numbers Marois et al 08 Thalmann et al 09 Lagrange et al., 08, 10

7 High Contrast Imaging instruments today Instrumen t FLAO MagAO P3K SCExAO DM WFS Features Speed Res. WFE Speckle Calib DSM, 672 Act DSM, 585 Act Piezo, Act Bimorph MEMS 1k GPI Piezo ~100 + ~1500 MEMS SPHERE Piezo 1377 Act PYRWFS 3 / 6 l/d mod PYRWFS SF-SHS, quad-cell PYRWFS no mod SF-SHS, quad-cell SF-SHS, 6px subap - ~30 Hz, 0 db, 900 Hz framrate Vibr. Ctrl, Vis Cam Woofer/ Tweeter. CALSYS, VVC CLOWFS PIAA, Vis Cam Woofer/ Tweeter. CALSYS Vibr. Ctrl, Vis Cam 1 khz framerate ~70 Hz, 0 db, 2 khz framerate ~120 nm rms (sky) ~ nm rms (lab) ~150 nm rms (sky) ADI SDI, ADI SD, SDI 1 khz Tbd SDI, ADI 1 khz framerate ~ 100 Hz, 0 db, < 1.38 khz frame 24 nm inband ~100 nm rms (lab) SDI, ADI SD, SDI, PDI, ADI Status In operation In operation In operation Partly in operation, upgr. path 1 st light about now 1 st light May 14

8 Where to go next?

9 Where to go next?

10 Where to go next?

11 (1) Fine characteriza8on of known EGPs Goals and typical numbers: SNR 100 to 1000 Photometric monitoring (1% to 0.1%) à towards exoplanet meteorology! Orbital mo8on follow- up (dynamical masses, orbit perturba8ons..) Molecular absorp8on in NIR: Exact shape and depth of absorp8on (composi8on, dust content) Absorp8on at high resolu8on (several thousands) Polarisa8on Needs: Similar sensi8vity and contrast with much higher SNR, stability. Higher spectral resolu8on. No need for survey capability, rather pointed observa8ons.

12 Where to go next?

13 (2) Detec8ng fainter planets Goals: Either same planet mass around older stars (possibly closer): Complete the general planet content sta8s8cs (star mass, age, separa8on) Monitor the complementari8es with astrometry (e.g. GAIA) Sub- Jupiter masses around young ( yr) stars: Can be cri8cal for planets (expectedly lighter) around low- mass stars Revisit on- going surveys for more complete exoplanet census Natural learning curve from exis8ng capabili8es and path finder for future instruments Needs: Can be started NOW on exis8ng 8- m telescopes From contrast 10-6 to 10-8 poten8al use in survey mode: dis8nguish poten8al restric8on on selected targets (brightest or specific targets for planet mul8plicity )

14 Where to go next?

15 (3) Similar EGPs closer to stars Goals: Complete the mass- separa8on diagram Depending on stellar type, may complete or overlap with RV techniques Complementary with interferometric techniques, pupil masking Pathfinder for future very ambi8ous project (towards HZ, and/or space purposes: on smaller telescopes, same separa8on = smaller # λ/d) Needs: Separa8on range below 100 mas: typically mas, with contrast > 10 5 Can be started without survey approach: long exposures on targets that could be selected from other techniques Benefit from larger telescope diameter (early moderate contrast on ELT?) Towards specific high contrast for short separa8ons (RDI, coherence, dedicated coronos, specific ahen8on to low order aberra8ons) where usual approaches like ADI and SDI loose efficiency. à specific R&D «à la ScexAO»?

16 Where to go next?

17 (4) Planets around (very) young stars Goals: Stars in star- forming regions: a few 10 6 yr (instead of ) Probe EGP content, dynamics and interac8on with disks shortly aver/during forma8on Moderate contrast allows to probe sub- Jupiter masses Needs: Star forming regions are not close (few 100 pc) à need access to short separa8ons, and high AO sensi8vity (strong interest for NIR: very red objects) Similar needs to (3), while keeping sensi8vity! Benefit from larger telescope diameter (early moderate contrast on E- ELT?)

18 Where to go next?

19 (5) Towards imaging planets in HZ Goals: Characteriza8on for both emission and reflected light Need both very short separa8on (<~30 mas) and very high contrast (in in range) No need for survey approach Possible space- based / ground based approaches (with slightly different separa8on/contrast trade- offs) Probe EGP content, dynamics and interac8on with disks shortly aver/during forma8on Moderate contrast allows to probe sub- Jupiter masses Needs: Long term approach, ELT, dedicated techniques for shortest separa8ons Specific interest from the ground on M stars (interest for sensi8ve NIR sensors)

20 The E- ELT Project: Instrument Roadmap Instruments - First Light AO Mode λ (µm) Resolu,on FoV / Sampling Add. Mode E- CAM 2024 SCAO, MCAO - IMG - MRS BB, NB / 3 mas Astrometry 40µas Coronagraphy E- IFU 2024 SCAO, LTAO - IFU / 4mas / 40mas Coronagraphy E- MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Coronagraphy Polarimetry E- HIRES /2028 SCAO - HRS Polarimetry E- MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Mul8plex ~ 400 Mul8plex ~100 Mul8plex ~10 Imaging? E- PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Coronagraphy Polarimetry

21 Expected detec8on capability of PCS on E- ELT Smaller IWA Higher contrast 2000s, 8- m 2014, 8-m 2025+, 37- m Bonavita et al., 2012

22 Some remarks on corresponding R&D and concept studies Phased approach needed including laboratory developments, full understanding of upcoming instruments, upgrades of 8- m instruments, Dis8nc8on survey versus target selected observa8ons has impact on designs AO residuals versus quasi- sta8c measurements: both are important and coupled (spa8al/temporal structure of residuals, measurement/ compensa8on overlap?) AO speed and sensi8vity remains an issue on bright targets; NIR sensing important in some cases Current approaches need to be improved: PSF structure and stability, RDI, signal processing including various sources of PSF a priori knowledge, diversity Amplitude, chroma8city issues: only star8ng. Unfriendly aperture very likely! Specific «new» needs for very short separa8ons

23 Conclusions Very exci8ng 8me! Significant progress in 20+ years A lot to learn with current systems Facing the challenge of ELTs and space projects