Polarimetry and spectral imaging of mature Jupiter and super Earth SEE COAST

Transcription

1 Polarimetry and spectral imaging of mature Jupiter and super Earth SEE COAST Jean Schneider, A. Boccaletti, P. Baudoz, G. Tinetti, D. Stam, R. Gratton,...

2 Eth Zurich Univ. of Leiden Univ. Amsterdam CSL IAP Univ. of Torun Obs. Tauntenburg LUAN Univ. Nantes Obs. Geneva LAOG UCL London ULg LUTH LESIA Instituto de astrofisica de Canaria 2

3 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 3

4 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 4

5 How are you doing mate? not yet 5

6 Complementarity of techniques 6

7 Complementarity of techniques Gaia Astrometry Sim 7

8 Complementarity of techniques Geometrical probability Light curve quality 8

9 Complementarity of techniques Larger telescopes Dedicated instruments 9

10 Complementarity of techniques 2/3 ~Time m/s cm/s 10

11 Complementarity of techniques 11

12 Complementarity of techniques Direct imaging Transit SPECTRA & POLARIZATION 12

13 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 13

14 Ground/space complementarity We are here Space-based 2011 Ground-based >

15 Ground/space complementarity We are here HST m + OA Silla, CFH Space-based > m + OA VLT, Keck, Gemini Ground-based 15

16 Ground/space complementarity HST m + OA Silla, CFH Space-based We are here m + OA VLT, Keck, Gemini > m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based 16

17 Ground/space complementarity HST m + OA Silla, CFH Space-based We are here m + OA VLT, Keck, Gemini m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based > /42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 17

18 Ground/space complementarity Space-based We are here HST SPICA MIR: Old EGPs JWST NIR + MIR: Old EGPs m + OA Silla, CFH m + OA VLT, Keck, Gemini m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based > /42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 18

19 Ground/space complementarity Space-based We are here HST SPICA MIR: Old EGPs? Darwin/TPF-I MIR: Earth TPF-C Vis: Earth JWST NIR + MIR: Old EGPs m + OA Silla, CFH m + OA VLT, Keck, Gemini m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based? > /42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 19

20 Ground/space complementarity Space-based We are here HST? SPICA MIR: Old EGPs Opportunity for space projects JWST NIR + MIR: Old EGPs m + OA Silla, CFH m + OA VLT, Keck, Gemini m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based Darwin/TPF-I MIR: Earth TPF-C Vis: Earth Visible light? Old giants & super-earths > /42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 20

21 Ground/space complementarity Space-based We are here HST JWST NIR + MIR: Old EGPs m + OA Silla, CFH m + OA VLT, Keck, Gemini m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based? SPICA MIR: Old EGPs Darwin/TPF-I MIR: Earth TPF-C Vis: Earth SEE COAST Vis/NIR Old Jupiter + Super Earth ? > /42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 21

22 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 22

23 See Coast will characterize : What's expected : Mature Jupiter (~5Gyr) Super Earth Brighter Atmosphere, climate Variations, habitable Around nearby star Exo-zodiacal disk And unexpected objects! Stay open-minded (cf. hot Jupiter in 1995) 23

24 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 24

25 Spectroscopy : chemical composition Solid planets Giant planets 25

26 Polarimetry : physical informations Clouds / albedo Polarization Spectrum Jupiter-like planet - Stam et al

27 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 27

28 How many detections? Nearby stars (<20pc) 1e-6 1e-7 =600nm 1e-5 IWA Planet-star contrast (V band) 1e-4 Gratton et al. 1e-8 1e-9 1e-10 1e Planet-star (arcsec) Raphaëlseparation Galicher 10 28

29 How many detections? Nearby stars (<20pc) 1e-7 =1.2 m Gratton et al. IWA 1e-6 =600nm 1e-5 IWA Planet-star contrast (V band) 1e-4 1e-8 1e-9 1e-10 1e Planet-star (arcsec) Raphaëlseparation Galicher 10 29

30 How many detections? Nearby stars (<20pc) 1e-7 =1.2 m 1e-6 Gratton et al. IWA 1e-5 =600nm IWA =400nm IWA Planet-star contrast (V band) 1e-4 1e-8 1e-9 1e-10 1e Planet-star (arcsec) Raphaëlseparation Galicher 10 30

31 How many detections? Nearby stars (<20pc) 1e-7 =1.2 m 1e-6 Gratton et al. IWA 1e-5 =600nm IWA =400nm IWA Planet-star contrast (V band) 1e-4 1e-8 1e-9 1e-9 1e-10 1e-10 1e Planet-star (arcsec) Raphaëlseparation Galicher 10 31

32 How many detections? Nearby stars (<20pc) 1e-6 1e-7 1e-8 =1.2 m 1e-5 =600nm IWA =400nm Planet-star contrast (V band) 1e-4 Gratton et al. 1) 1e-10 contrast 2) Small inner working angle 1e-9 1e-9 1e-10 1e-10 1e Planet-star (arcsec) Raphaëlseparation Galicher 10 32

33 Outline Why direct imaging? Why from space (SEE COAST)? Which kinds of objects? Spectroscopy and polarimetry interest? What's detected by 1.5meter telescope? Which technology? 33

34 SEE Coast : proposed to Cosmic Vision Parameter Value Hyperbolic secondary mirror 4,85m long Entrance pupil diameter D > 1.5m Spectral Range 0.4 to 1.2 µ m Spectral Resolution R>40 Contrast (after speckle 2 λ /D < 10-9 Contrast (after speckle 4 λ /D < Orbit for 6 months visibility, high thermal stability L2 Lagrangian Two folding mirrors Focal plane Parabolic primary mirror Submitted in 2007 to ESA Cosmic Vision 34

35 SEE Coast : proposed to Cosmic Vision Parameter Value 1) Coronagraph Entrance pupil diameter D > 1.5m Range 0.4 to 1.2 µ m 2) Wavefront control (aspectral few nm rms from science image) R>40 3) Differential imagingspectral Resolution Contrast (after speckle < 10 2 λ /D 4) Integral field spectrometer/polarimeter -9 Hyperbolic secondary mirror 4,85m long Contrast (after speckle 4 λ /D < Orbit for 6 months visibility, high thermal stability L2 Lagrangian Two folding mirrors Focal plane Parabolic primary mirror Submitted in 2007 to ESA Cosmic Vision 35

36 Achromatic coronagraph Laboratory planet Multi-stage four quadrant phase mask coronagraph Contrast : at 4.5 /D = 20% Visible light Baudoz et al. 2007, 08 36

37 Wavefront sensor in the science image Speckle nulling in a limited FOV with a DM (JPL) 37

38 Wavefront sensor in the science image Speckle nulling in a limited FOV with a DM (JPL) SCC measure Actuator position SH measure Self-coherent camera (SCC) Galicher et al. 2008, 2009 Remember Marion Mas' talk 38

39 Integral Field Spectrometer + Self coherent camera Aberrations = function of (Fresnel propagation) Wavelength Classical IFS strongly limited Wavelength One solution : SCC IFS Field of view position 39

40 Summary Direct imaging : unexplored domain of parameter space Space telescope : visible light See coast requires : 1e 10 contrast and small IWA (2 /D) Spectrometry low resolution spectra of young/old Jupiter (<20pc, 8 10 AU) colors of super Earths (<10pc, 4 5 AU) low resolution spectra of self luminous planets (NIR) Polarimetry : more physical informations See coast next steps : refine optical design and derive science cases technology with coronagraphy, wavefront control, differential imaging Cosmic vision proposal in late

41 Tha nk you fo r your atte ntio n If you want to participate in this project, please contact :, raphael.galicher 'at' obspm.fr Jean Schneider, jean.schneider 'at' obspm.fr 41