Direct Imaging of Exoplanets

Transcription

1 Habilitation à Diriger des Recherches, UGA-IPAG, 31 Mai 2016 Direct Imaging of Exoplanets - Gaël Chauvin Institute of Planetology & Astrophysics of Grenoble, France

2 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & technics 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives

3 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & technics 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives Mickael Bonnefoy s PhD Julien Rameau s PhD

4 I- Twenty years of exoplanetary science Observational success Two decades of exoplanet studies Hot-Jupiters Discoveries First glimpse of Exoplanetary atmospheres More than 1000 known EPs (>2000 Kepler EPs?) Diversity of planetary architectures Images/spectra of Super-Jupiters Super-Earths in Habitable Zone Discovery of Earth-mass planets Mayor & Queloz 95 Mayor et al. 11; Triaud et al. 10; Swain et al. 08; Desert et al. 12; Bonfils et al. 09; Udry & Santos 07 Batalha et al. 13; Howard 12

5 I- Twenty years of exoplanetary science Impressive evolution

6 I- Twenty years of exoplanetary science Impressive evolution

7 I- Twenty years of exoplanetary science Impressive evolution

8 I- Twenty years of exoplanetary science Why Imaging? Direct detection of planetary photons I/ Orbital & Physical properties > Giant planets at wide orbits (>10 AU) > Luminosity, a, e, i, ω, T0 (?) Lagrange, Bonnefoy, Chauvin et al. 10 Chauvin et al. 12; Bonnefoy et al. 13, 14

9 I- Twenty years of exoplanetary science Why Imaging? Direct detection of planetary photons I/ Orbital & Physical properties > Giant planets at wide orbits (>10 AU) > Luminosity, a, e, i, ω, T0 II/ Atmosphere > Non-strongly irradiated EGPs > Low-gravity, clouds, non-lte... Janson et al. 10; Skemer et al. 12 Konopacky et al. 13; Bonnefoy et al. 13, 14

10 I- Twenty years of exoplanetary science Why Imaging? SAO Fomalhaut Direct detection of planetary photons I/ Orbital & Physical properties > Giant planets at wide orbits (>10 AU) > Luminosity, a, e, i, ω, T0 HD Bpic The Moth II/ Atmosphere > Non-strongly irradiated EGPs > Low-gravity, clouds, non-lte... Janson et al. 10; Skemer et al. 12 Konopacky et al. 13; Bonnefoy et al. 13, 14 III/ Architecture > Dynmical Stability & Evolution > Planet disk connection Mouillet et al. 97; Kalas et al. 04, 08; Buenzli et al. 10; Rameau et al. 12; Grady et al. 12; Lagrange et al. 12;

11 I- Twenty years of exoplanetary science Why Imaging? Fundamental unanwered questions How do Giant Planets form? o 1, 2 or 3 formation processes? At different timescales/locations? o Influence of initial conditions (stellar mass, metallicity, multiplicity, environment)? What are the physical properties of Young Jupiters, Saturns (L, R, T eff, composition )? o Today, 1-2 orders of magnitude uncertainty on Young Jupiter Luminosities o Orbital distribution at all orbits from massive Jupiters to Neptunes Giants Formation, evolution and physical properties of telluric planets, o Fraction inside the Habitable Zone capable to host Life? o Atmosphere & Physical properties? Best diagnostics for bio-signatures? Which future instrumentation to characterize bio-signatures/exo-life? o Space/ground? Interferometry/coronography/spectroscopy? Visible/infrared?

12 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & techniques 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives

13 II- Challenge & Technics Dedicated Instrumentation 1. High angular resolution Space telescope 10m-telescopes + AO HST (NICMOS, ACS) LBT Gemini S/N (NICI, GPI) VLT(NaCo, SPHERE) Subaru (HiCIAO, SCExAO) Keck

14 End-April 2014

15 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution SAXO Extreme-Adaptive Optics 90% Strehl in H-band; (Coherent energy In PSF core) - Deformable Mirror: High orders; 41 x 41 actuators SPHERE/Comm-1 May 2014 SPHERE@IPAG Seeing-limited median seeing Sr H-band = 90% 0.8 H-band - Wave Front Sensing: Shack-Hartmann, 40x40 lenslets, Red-sensitive sub-e CCD Frequency = 1.2kHz Anti-aliasing spatial filtering - Sparta Real-Time Computer Command; non-common path aberration corrections Beuzit et al. 08 Contrast =

16 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution SAXO Extreme-Adaptive Optics 90% Strehl in H-band; (Coherent energy In PSF core) - Deformable Mirror: High orders; 41 x 41 actuators SPHERE/Comm-1 May 2014 SPHERE median seeing Sr = 90% 0.8 H-band - Wave Front Sensing: Shack-Hartmann, 40x40 lenslets, Red-sensitive sub-e CCD Frequency = 1.2kHz Anti-aliasing spatial filtering - Sparta Real-Time Computer Command; non-common path aberration corrections Beuzit et al. 08 Contrast =

17 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution Impressive evolution in AO correction over 20yrs! GQ lup star (K7V; V=11.4; K=7.1; BD ) ESO3.6m/Come-On+ SH WFS; 62 actuators; Sr < 10% Janson et al VLT/NACO SH WFS; 185 actuators Sr = 40-50% Neuhäuser et al 05 VLT/NACO SPHERE/IRDIS SH WFS; 1200 actuators Sr Sr > = 90% 80% Delorme et al., in prep

18 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution Impressive evolution in AO correction ober 20yrs! GQ lup star (K7V; V=11.4; K=7.1; BD ) ESO3.6m/Come-On+ SH WFS; 62 actuators; Sr < 10% Janson et al VLT/NACO SH WFS; 185 actuators Sr = 40-50% Neuhäuser et al 05 VLT/NACO SPHERE/IRDIS SH WFS; 1200 actuators Sr Sr > = 90% 80% Delorme et al., in prep

19 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution 2. Stellar-light attenuation Coronagraphy (B. Lyot) - Pupil and Image Control. PTTM, ITTM/HODM. Low-aberrations/Centering control (DTTS) SPHERE/Comm-1 May 2014 SPHERE@IPAG median seeing Sr = 90% 0.8 H-band Apo+Stop - Pupil Masks:. Apodizer or/and Lyot Stop - Focal plane masks:. Classical Lyot Coronograph. Apodized Classical-Lyot. Apodized 4QP Mask, Boccaletti et al. 08 Beuzit et al. 08 Contrast =

20 II- Challenge & Technics Path for Exoplanet Imaging 1. High angular resolution 2. Stellar-light attenuation 3. Speckles subtraction Main limitation (<1.0 ): Residual Turbulent/quasi-statics speckles - Differential Imaging techniques. Polarimetric (PDI). Spectral (SDI), Racine et al. 99. Angular (ADI), Marois et al. 06 SPHERE/Comm-1 May 2014 SPHERE@IPAG median seeing Sr = 90% 0.8 DBI: H2-H3 Apo+Stop - Minimizing WFE (Coffee, ZELDA ) - Post-processing tools. LOCI, Lafrenière et al. 07. ANDROMEDA, Mugnier et al. 10. KLIP/PCA, Soummer et al. 12 Contrast =

21 II- Challenge & Technics Detection performances High Contrast at inner angles Contrast Detection Limits: Various Telescopes/Instruments H-band; T obs = min Young star (H = 5-6 mag), 30 pc, 10 Myr SPHERE/GPI

22 II- Challenge & Technics Detection performances High Contrast at inner angles Detection Limits: Various Telescopes/Instruments H-band; T obs = min Young star (H = 5-6 mag), 30 pc, 10 Myr Luminosity Mass conversion COND03 Evol. Models (Hot-start), Baraffe et al. 03 Accessing planetary-forming regions down to 6 10 AU SPHERE/GPI

23 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & techniques 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & pespectives

24 III- Targets, surveys & discoveries Targets for Planet Imaging Age,. Young Giant Planets are hotter & brighter Distance, : 5 50 AU (@50 pc) Mass,. GKM dwarfs, fainter, more favorable in terms of contrast. AF stars, could form massive EGPs? Kenyon & Hartman 08 (< Gyr) (< pc) (BAFGKM) IR Excess, RV trends, very nearby

25 III- Targets, surveys & discoveries Targets for Planet Imaging Young stars near the Sun, TW Hya, isolated T Tauri star (Rucinski & Krautter 1983) additional members of TWA (Kastner et al. 1997) Shkolnik et al. 12

26 III- Targets, surveys & discoveries Targets for Planet Imaging Young stars near the Sun, TW Hya, isolated T Tauri star (Rucinski & Krautter 1983) additional members of TWA (Kastner et al. 1997) About 10 new associations, (TWA, β Pic, AB Dor, Tuc/Hor, η Cha, e Cha, Carina, Columba...) Unveiling low-mass members (< 1.0 Gyr), nearby Moving Groups, Today, 500+ known Young (<100 Myr) & Nearby (<100 pc) stars Extension to Intermediate-old (< 1.0 Gyr), nearby Moving Groups, (Castor, Herculis-Lyra, Argus, Octantis. and in the Field) Age & membership diagnostics: isochrone, (Li, H α ), X-ray, kinematics... Zuckerman, Song et al.; Torres, de la Reza et al.; Mamajek et al.; Montes et al. Shkolnik et al. 12; Gagné et al. 14, 15

27 III- Targets, surveys & discoveries Direct Imaging Surveys See Chauvin et al. 2015

28 III- Targets, surveys & discoveries Direct Imaging Surveys IPAG See Chauvin et al. 2015

29 III- Targets, surveys & discoveries Discoveries Timeline (not exhaustive: between 7 50 imaged exoplanets; Gl229 B (Nakajima et al. 94) TWA5 B (Lowrance et al. 99) HR7329 B (Lowrance et al. 00) GSC8047B (Chauvin et al. 03) 2m1207 b (Chauvin et al. 04, 05) First Imaged substellar companion (Nakajima et al. 94) IR detectors/coronography DH Tau b (Itoh et al. 05) CHXR73 b (Luhman et al. 05) AB Pic b (Chauvin et al. 05) GQ Lup b (Neuhauser et al. 05) RXJ1609 b (Lafrenière et al. 08) HR8799bcd (Marois et al. 08) Fomalhaut b (Kalas et al. 08) Beta Pic b (Lagrange et al. 08, 10) CT Cha b (Schmidt et al. 10) HR8799 e (Marois et al. 10) Kappa And b (Carson et al. 13) HD95086 b (Rameau et al. 13, 14) GJ504 b (Kuzuhara et al. 13) 2M0103 b (Delorme et al. 13) 51 Eri b (Macintosh et al. 15)

30 III- Targets, surveys & discoveries Discoveries Timeline (not exhaustive: between 7 50 imaged exoplanets; Gl229 B (Nakajima et al. 94) TWA5 B (Lowrance et al. 99) HR7329 B (Lowrance et al. 00) GSC8047B (Chauvin et al. 03) 2m1207 b (Chauvin et al. 04, 05) First Planetary mass companion (Chauvin et al. 04, 05) IR detectors/coronography + 10m Telescope + AO DH Tau b (Itoh et al. 05) CHXR73 b (Luhman et al. 05) AB Pic b (Chauvin et al. 05) GQ Lup b (Neuhauser et al. 05) RXJ1609 b (Lafrenière et al. 08) HR8799bcd (Marois et al. 08) Fomalhaut b (Kalas et al. 08) Beta Pic b (Lagrange et al. 08, 10) CT Cha b (Schmidt et al. 10) HR8799 e (Marois et al. 10) Kappa And b (Carson et al. 13) HD95086 b (Rameau et al. 13, 14) GJ504 b (Kuzuhara et al. 13) 2M0103 b (Delorme et al. 13) 51 Eri b (Macintosh et al. 15)

31 III- Targets, surveys & discoveries Discoveries Timeline (not exhaustive: between 7 50 imaged exoplanets; Gl229 B (Nakajima et al. 94) TWA5 B (Lowrance et al. 99) HR7329 B (Lowrance et al. 00) GSC8047B (Chauvin et al. 03) low-mass ratio planets at less than 100 AU around A stars Marois+08; Kalas+08; Lagrange+08 2m1207 b (Chauvin et al. 04, 05) DH Tau b (Itoh et al. 05) CHXR73 b (Luhman et al. 05) AB Pic b (Chauvin et al. 05) GQ Lup b (Neuhauser et al. 05) RXJ1609 b (Lafrenière et al. 08) HR8799bcd (Marois et al. 08) Fomalhaut b (Kalas et al. 08) Beta Pic b (Lagrange et al. 08, 10) CT Cha b (Schmidt et al. 10) HR8799 e (Marois et al. 10) Kappa And b (Carson et al. 13) HD95086 b (Rameau et al. 13, 14) GJ504 b (Kuzuhara et al. 13) 2M0103 b (Delorme et al. 13) 51 Eri b (Macintosh et al. 15) IR detectors/coronography + 10m Telescope + AO + Differential techniques

32 III- Targets, surveys & discoveries Discoveries Timeline (not exhaustive: between 7 50 imaged exoplanets; Gl229 B (Nakajima et al. 94) TWA5 B (Lowrance et al. 99) HR7329 B (Lowrance et al. 00) GSC8047B (Chauvin et al. 03) 2m1207 b (Chauvin et al. 04, 05) DH Tau b (Itoh et al. 05) First GPI planet, 2 14 AU Macintosh+15 CHXR73 b (Luhman et al. 05) AB Pic b (Chauvin et al. 05) GQ Lup b (Neuhauser et al. 05) RXJ1609 b (Lafrenière et al. 08) HR8799bcd (Marois et al. 08) Fomalhaut b (Kalas et al. 08) Beta Pic b (Lagrange et al. 08, 10) CT Cha b (Schmidt et al. 10) HR8799 e (Marois et al. 10) Kappa And b (Carson et al. 13) HD95086 b (Rameau et al. 13, 14) GJ504 b (Kuzuhara et al. 13) 2M0103 b (Delorme et al. 13) 51 Eri b (Macintosh et al. 15) IR detectors/coronography + 10m Telescope + AO + Differential techniques +XAO imagers (GPI/SPHERE)

33 III- Targets, surveys & discoveries SPHERE/GPI surveys Entering the Era of Systematic searches, GPIES, GPI Exoplanet Survey Sample of 600 A-M stars, Young (<100 Myr, <75 pc) and adolescent (<300 Myr, < 35pc) 890 hours over 3 years, service mode SHINE, Sphere High-ImagiNg of Exoplanets Sample of A-M stars, Moving groups members and young field stars (<150 pc and < 1 Gyr), 2000 hours (200 nights) over 5 years, started in Feb 2015, visitor mode (+ 200 hrs for DISK science hrs for REFLECTED LIGHT planets) Chauvin, Desidera+SHINE-team 2016, in prep; Vigan+15; Zurlo+16; Bonnefoy+16; Maire+16; Lagrange+16 Garufi+16; Olofsson+16; Perrot+16; Milli+16, subm.; Mesa+16, subm.; deboer+16, subm.. SCExAO, building on the SEEDS Legacy

34 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & techniques 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives Mickael Bonnefoy s PhD

35 IV- Physics of exoplanets Unexpected properties Colors & spectra Field brown dwarf color-magnitude sequence Leggett et al. 01; Dahn et al. 02; Knapp et al. 2004

36 IV- Physics of exoplanets Unexpected properties Colors & spectra Field brown dwarf color-magnitude sequence Leggett et al. 01; Dahn et al. 02; Knapp et al m1207 b: very-red & underluminous compared to the field L-T-type sequence 3-4 M jup, T eff = 1600 ± 300K, mid/late L-type Chauvin et al. 04, 05

37 IV- Physics of exoplanets Unexpected properties Colors & spectra Field brown dwarf color-magnitude sequence Leggett et al. 01; Dahn et al. 02; Knapp et al m1207 b: very-red & underluminous compared to the field L-T-type sequence 3-4 M jup, T eff = 1600 ± 300K, mid/late L-type Chauvin et al. 04, 05 Today: Mostly young, late-m to late L-type Giants. Redder (underluminous) at M/L & L/T transition,. CH4 absorption inhibited (2m1207b; HR8799b). enhanced photometric variability Impact of low-gravity conditions? Presence of thick clouds? metal-enhancement & non-lte processes? Barman et al. 11ab; Madhusudhan et al. 11; Metchev et al. 14 New! 3 young T-exoplanets: GU Psc b, GJ504 b & 51 Eri b Naud et al. 12, Kuzahara et al. 13; Macintosh et al. 15

38 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) SINFONI-Lib

39 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Uniform physical characterization. Atomic/molecular systematic identification. Empirical analysis (young versus field dwarfs). Indices and equivalent widths (T eff /log-g sensitive). Spectral synthesis using atmosphere models Bonnefoy, Chauvin et al. 10, 14; Manjavacas et al. 14;

40 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Uniform physical characterization. Atomic/molecular systematic identification. Empirical analysis (young versus field dwarfs). Indices and equivalent widths (T eff /log-g sensitive). Spectral synthesis using atmosphere models Bonnefoy, Chauvin et al. 10, 14; Manjavacas et al. 14;

41 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Uniform physical characterization. Atomic/molecular systematic identification. Empirical analysis (young versus field dwarfs). Indices and equivalent widths (T eff /log-g sensitive). Spectral synthesis using atmosphere models Bonnefoy, Chauvin et al. 10, 14; Manjavacas et al. 14;

42 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs BTSETTL-2010 (Allard et al.) Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Uniform physical characterization. Atomic/molecular systematic identification. Empirical analysis (young versus field dwarfs). Indices and equivalent widths (T eff /log-g sensitive). Spectral synthesis using atmosphere models Bonnefoy, Chauvin et al. 10, 14; Manjavacas et al. 14;

43 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Main results/conclusions:. Uniform charac. of spectral/physical properties,. Systematic feedback on latest generation of atmosphere models (BT-SETTL, DRIFT-PHOENIX),. Young intermediate-gravity early-l dwarfs can be up to K cooler than their older counterpart,. Reference for today s planet characterization: AB Pic b, Bonnefoy et al. 10, 14, 16; Vigan et al. 15; Maire et al. 16; Mesa et al. 16; Samland et al. 16 Pic b, GJ758 B, HR8799 bcde, 51 Eri b, GJ504 b Bonnefoy, Chauvin, Lagrange et al. 14

44 IV- Physics of exoplanets Young BD as exoplanet analogs NIR Library of young mid-m to mid-l dwarfs Uniform/systematic spectroscopic characterization 21 young dwarfs close to the De-burning limit, i.e with Mass = [4 30] M jup & T eff = [ ] K. VLT/SINFONI, J and H+K, R = ( ). VLT/ISAAC, J, H, K, R = ( ) Main results/conclusions:. Uniform charac. of spectral/physical properties,. Systematic feedback on latest generation of atmosphere models (BT-SETTL, DRIFT-PHOENIX),. Young intermediate-gravity early-l dwarfs can be up to K cooler than their older counterpart,. Reference for today s planet characterization: AB Pic b, Bonnefoy et al. 10, 14, 16; Vigan et al. 15; Maire et al. 16; Mesa et al. 16; Samland et al. 16 Pic b, GJ758 B, HR8799 bcde, 51 Eri b, GJ504 b Independent confirmation by combined parallax + SED analysis Filippazzo et al. 15

45 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & techniques 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives Julien Rameau s PhD

46 V- Architecture, occurrence & formation Mechanism(s) of formation Three main proposed processes for planets/planemos: Core Accretion Pollack et al. 94 Gravitational Instability Cameron 78 Gravo-turbulent fragmentation Hennebelel & Chabrier 11

47 V- Architecture, occurrence & formation Mechanism(s) of formation Three main proposed processes for planets/planemos: Core Accretion Pollack et al. 94 Gravitational Instability Cameron 78 Gravo-turbulent fragmentation Hennebelel & Chabrier 11 No universal picture to explain all observed planets!

48 V- Architecture, occurrence & formation Giants around young AF stars DUSTIES survey to search/count for Pic-analogs Sample selection. Homgeneous sample of 60 young (20-50 Myr), nearby (~50pc) and AF stars. Dusty: IR excess from IRAS,ISO and SPITZER/MIPS. Members of moving groups (AB Dor, TWA, β Pic, η Cha, Tuc-Hor ) VLT/NaCo campaigns. Angular differential imaging at L (3.8 m). Visitor/Service observing btw 2009 and Advanced post-processing algorithms Goals:. Discovery of new Pic-analogs. Planet occurrence for this young AF sample. Testing predictions of planet formation theories HR7329 B pic AB Pic HR8799 Rameau, Chauvin, Lagrange et al. 13a

49 V- Architecture, occurrence & formation Giants around young AF stars Hd95086b: a 4 Jupiter mass planet in a two-belts system HD A8-type star. LCC member, 17 Myr-old, located at 90.4 pc. Large dust-to-star ratio: L dust /L star = 1e-3 HD95086b. Sep = 624 ± 8 mas, PA = ± 0.8deg. ΔL = 9.6 ± 0.2 mag. Predicted properties: 4-5 M 56AU NaCo-Lp ADI (Jan 2012) Neptune s orbit HD95086b Rameau, Chauvin, Lagrange et al. 13b,c

50 V- Architecture, occurrence & formation Giants around young AF stars Hd95086b: a 4 Jupiter mass planet in a two-belts system HD A8-type star. LCC member, 17 Myr-old, located at 90.4 pc. Large dust-to-star ratio: L dust /L star = 1e-3 HD95086b. Sep = 624 ± 8 mas, PA = ± 0.8deg. ΔL = 9.6 ± 0.2 mag. Predicted properties: 4-5 M 56AU. Follow-up: NiCi and GPI (H-band). Empirical analysis: L6-L8 -type giant,. BTSETTL: T eff = K, log(g)~3.5 Galicher, Rameau, Bonnefoy et al. 14

51 V- Architecture, occurrence & formation Giants around young AF stars Hd95086b: a 4 Jupiter mass planet in a two-belts system HD A8-type star. LCC member, 17 Myr-old, located at 90.4 pc. Large dust-to-star ratio: L dust /L star = 1e-3 HD95086b. Sep = 624 ± 8 mas, PA = ± 0.8deg. ΔL = 9.6 ± 0.2 mag. Predicted properties: 4-5 M 56AU. Follow-up: NiCi and GPI (H-band). Empirical analysis: L6-L8 -type giant,. BTSETTL: T eff = K, log(g)~3.5 Two-belts system. Outer belt resolved by Herschel PACS. SED analysis reveals warm and cold components. Influence of HD95086b on the disk structure? Moor et al. 13; Su et al AU

52 V- Architecture, occurrence & formation Giants around young AF stars Occurrence of system with wide orbits (>10 AU) Giant(s)? DUSTIES Survey Detection probabilities. Survey completeness based on all detection limits. Monte-Carlo simulation with MESS code. Orbital parameter distribution (uniform): (M p, sma, Ω,, cos(i), T p, ecc. < 0.6) Bonavita, Chauvin et al. 12; Chauvin et al Mostly-sensitive btw AU for massive (> 3 Mjup) planets Rameau, Chauvin, Lagrange et al. 13a

53 V- Architecture, occurrence & formation Giants around young AF stars Occurrence of system with wide orbits (>10 AU) Giant(s)? DUSTIES Survey Detection probabilities. Survey completeness based on all detection limits. Monte-Carlo simulation with MESS code. Orbital parameter distribution (uniform): (M p, sma, Ω,, cos(i), T p, ecc. < 0.6) Bonavita, Chauvin et al. 12. Mostly-sensitive btw AU for massive (> 3 Mjup) planets Planetary system occurrence:. sma:[ AU] & M p :[1 13 M Jup ]. 2 positive detections in DUSTIES. f EGP = 16.1%, [ ]% for CL = 68% For comparison:. Higher than for M dwarfs (Lannier et al. 2016). RV: f EGP ~ 9.7% for [ M Jup ] planets at < 5 AU, Rameau, Chauvin, Lagrange et al. 13a

54 V- Architecture, occurrence & formation Giants around young AF stars Link to formation models? GI, not a dominant mechanism based on current predictions/observations Or need a second stage of fragmentation in sub-fragments Janson et al. 10

55 V- Architecture, occurrence & formation Giants around young AF stars Link to formation models? GI, not a dominant mechanism based on current predictions/observations Or need a second stage of fragmentation in sub-fragments Bulk of the predicted CA population marginally accessible with 1st generation of planet imagers Rameau, Chauvin, Lagrange et al. 13a Alternatives?. Gravo-turbulent fragmentation cannot explain non-hierarchical multiple systems. Pebble accretion at large orbits. Dynamical evolution (Disk-planet outward migration/scattering) Mordasini et al. simulations for 2M sun stars

56 V- Architecture, occurrence & formation Giants around young AF stars Link to formation models? Perspectives SPHERE_SHINE (102 targets) NACO_LP (80 targets)

57 Outline Direct Imaging of Exoplanets 1. Twenty years of exoplanetary science 2. Challenges & technics 3. Targets, surveys & main discoveries 4. Physics of exoplanets 5. Architecture, occurrence & formation 6. Conclusions & perspectives

58 VI- Conclusions & perspectives Conclusions Direct imaging, a powerful technique, Very complementary to RV, Transit, Astrometry and -Lensing Unique for giant planets at wide orbits (> 5-10 AU) To characterize physical properties, architectures & occurrence Relies on a well defined set of technological/innovant steps XAO, coronography and Differential techniques Heavily involved into building/exploiting Direct Imaging Instruments at IPAG Key surveys & results achieved since 2003 SPHERE: Systematics surveys of well selected young, nearby stars Fully dedicated instruments to Exoplanets search and characterization (Orbits, Atmospheres, Disks, Architecture ) Physics of giant planets (Mickael s Bonnefoy PhD; Maxime s Cudel PhD) Young brown dwarfs as exoplanets analogs (SINFONI Library of late-m/mid-l dwarfs) Reference study for current exoplanet characterization (empirical/model analysis) Architecture, occurrence & formation (Julien Rameau s PhD) Discovery of HD95086b, a young massive Jupiters in a two-belts planetary system Occurrence of Giants around young, AF stars. Reject GI (probably GTF) as dominant mechanisms SPHERE/SHINE will significantly fill the statistical gap down to 5-10 AU.

59 VI- Conclusions & perspectives Perspectives A rich forthcoming decade

60 VI- Conclusions & perspectives The E-ELT project The Telescope 40-m class telescope: largest opticalinfrared telescope in the world. (GMT = 25m; TMT = 30m) Segmented primary mirror. Adaptive optics assisted telescope. Diffraction limited performance: 12mas@K-band Wide field of view: 7arcmin. Mid-latitude site (Amazones/Chile). Fast instrument changes. VLT level of operations efficiency.

61 VI- Conclusions & perspectives The E-ELT project Instrumentation roadmap (exoplanetary science cases) instruments - First Light E-CAM 2025 E-IFU 2025 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40mas Coronography / 4mas / 40mas Coronography E-MIDIR 2026 SCAO, LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Coronography Polarimetry E-HIRES SCAO - HRS Polarimetry E-MOS MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Coronography Polarimetry Low Medium High-priority

62 VI- Conclusions & perspectives Synergies

63 VI- Conclusions & perspectives Synergies GAIA SPHERE E-CAM/IFU/MIDIR JWST TESS, CHEOPS PLATO ESPRESSO E-PCS?

64 VI- Conclusions & perspectives Synergies GAIA SPHERE E-CAM/IFU/MIDIR TESS, CHEOPS PLATO ESPRESSO E-PCS? JWST Occurence/Architecture Periods Charact. of Giant as cool as Jupiter Physical properties of young Jupiters Imaging of super-earths with PCS? First detection of bio-signatures

65 Merci!

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67 VLT/SPHERE Description & Status Design CPI De-rotator HWP2 Focus 1 ITTM HWP1 PTTM Polar Cal Focus 2 DM Focus 4 DTTS NIR ADC VIS ADC Focus 3 VIS corono ZIMPOL WFS IRDIS NIR corono DTTP IFS

68 VLT/SPHERE Description & Status Overwiew FoV ZIMPOL IRDIS IFS Sq 3.5 (instantaneous) Up to 4 radius (mosaic) Sq 11 Sq 1.77 Spectral Range μm μm /1.65 μm Spectral information Linear Polarisation BB, NB Simultaneous on same detector, x 2 arms, exchangeable BB, NB Slit spectro: 50/400 Simultaneous dual beam, exchangeable 50 / 30 x Coronography: no /4Q / Lyot Rotation at Nasmyth: Pupil-stab. (instrument fixed wrt tel.) Field-stab (slit spectro, long DIT ) No rotation: minimize crosstalk ) AO sensitivity for high contrast: R=9.5 for NIR; R=9 for R; R=7.8 for whole VIS Separation range where improved contrast: 2-20 λ/d, ie mas in R, or mas in H Mode switching: not VIS and NIR in same night