Polarimetry and spectral imaging of mature Jupiter and super Earth SEE COAST Jean Schneider, A. Boccaletti, P. Baudoz, G. Tinetti, D. Stam, R. Gratton,...
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
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
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
How are you doing mate? not yet 5
Complementarity of techniques http://exoplanet.eu 6
Complementarity of techniques Gaia Astrometry Sim http://exoplanet.eu 7
Complementarity of techniques Geometrical probability Light curve quality http://exoplanet.eu 8
Complementarity of techniques Larger telescopes Dedicated instruments http://exoplanet.eu 9
Complementarity of techniques 2/3 ~Time m/s cm/s http://exoplanet.eu 10
Complementarity of techniques http://exoplanet.eu 11
Complementarity of techniques Direct imaging Transit SPECTRA & POLARIZATION 12
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
Ground/space complementarity We are here 1995 2000 2010 Space-based 2011 Ground-based 2017-2020 >2025-30 14
Ground/space complementarity We are here HST 1995 4m + OA Silla, CFH 2000 2010 Space-based 2011 2017-2020 >2025-30 8m + OA VLT, Keck, Gemini Ground-based 15
Ground/space complementarity HST 1995 4m + OA Silla, CFH Space-based We are here 2000 8m + OA VLT, Keck, Gemini 2010 2011 2017-2020 >2025-30 8m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based 16
Ground/space complementarity HST 1995 4m + OA Silla, CFH Space-based We are here 2000 8m + OA VLT, Keck, Gemini 2010 2011 8m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based 2017-2020 >2025-30 30/42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 17
Ground/space complementarity Space-based We are here HST SPICA MIR: Old EGPs JWST NIR + MIR: Old EGPs 1995 4m + OA Silla, CFH 2000 8m + OA VLT, Keck, Gemini 2010 2011 8m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based 2017-2020 >2025-30 30/42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 18
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 1995 4m + OA Silla, CFH 2000 8m + OA VLT, Keck, Gemini 2010 2011 8m + XAO SPHERE / GPI / HICIAO NIR : EGPs young/massive/nearby Ground-based? 2017-2020 >2025-30 30/42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 19
Ground/space complementarity Space-based We are here HST? SPICA MIR: Old EGPs Opportunity for space projects JWST NIR + MIR: Old EGPs 1995 4m + OA Silla, CFH 2000 8m + OA VLT, Keck, Gemini 2010 2011 8m + 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 2017-2020 >2025-30 30/42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 20
Ground/space complementarity Space-based We are here HST JWST NIR + MIR: Old EGPs 1995 4m + OA Silla, CFH 2000 8m + OA VLT, Keck, Gemini 2010 2011 8m + 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 2017-2020? >2025-30 30/42m + XAO EPICS, PFI, etc with ELTs NIR : EGPs intermediate Old + Super-Earth? 21
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
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
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
Spectroscopy : chemical composition Solid planets Giant planets 25
Polarimetry : physical informations Clouds / albedo Polarization Spectrum Jupiter-like planet - Stam et al. 2005 26
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
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-11 0.01 0.1 1 Planet-star (arcsec) Raphaëlseparation Galicher 10 28
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-11 0.01 0.1 1 Planet-star (arcsec) Raphaëlseparation Galicher 10 29
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-11 0.01 0.1 1 Planet-star (arcsec) Raphaëlseparation Galicher 10 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-9 1e-10 1e-10 1e-11 0.01 0.1 1 Planet-star (arcsec) Raphaëlseparation Galicher 10 31
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-11 0.01 0.1 1 Planet-star (arcsec) Raphaëlseparation Galicher 10 32
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
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 subtraction) @ 2 λ /D < 10-9 Contrast (after speckle subtraction) @ 4 λ /D < 10-10 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
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 subtraction) @ 2 λ /D 4) Integral field spectrometer/polarimeter -9 Hyperbolic secondary mirror 4,85m long Contrast (after speckle subtraction) @ 4 λ /D < 10-10 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
Achromatic coronagraph Laboratory planet Multi-stage four quadrant phase mask coronagraph Contrast : 6.7 10-9 at 4.5 /D = 20% Visible light Baudoz et al. 2007, 08 36
Wavefront sensor in the science image Speckle nulling in a limited FOV with a DM (JPL) 37
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
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
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 2010 40
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