The β Pictoris Heritage 1- IPAG - Institut de Planétologie et Astrophysique de Grenoble 2- LESIA - Observatoire de Paris 3- STSI – Space Telesope Sciente Institute 4- ESO – European Southern Observatory ESO 30’ Talk, Friday 10, 2010 – ESO/Santiago Gaël Chauvin Anne-Marie Lagrange 1, Mickael Bonnefoy 1, Anthony Boccaletti 2, David Mouillet 1, David Ehrenreich 1, Daniel Apai 3, Daniel Rouan 2, Damien Gratadour 2, Markus Kasper 4 & Julien Girard 4

Outline The β Pictoris Heritage I- Introduction to β Pictoris Young nearby association, star & debris-disk II- Technics & NaCo Imaging Challenge, evolution, limitations & observations III- The β Pic b Giant Planet Detection, recovery, characterization & origin IV- Perspectives

I- Introduction The young, nearby association Member of the young, nearby β Pictoris association Co-moving group, (U,V,W) = (0.3, -11.5, -2.5) km.s-1 Age diagnostics (12 Myr), Isochrones, Li, Hα and X-ray Now, up to 30 members Prime targets for giant planet Imaging, as young EGPs are hotter and brighter at young ages. Zuckerman et al. (2001); Torres et al. (2006)

I- Introduction Formation scenario Galactic space position and motion closely related to Sco-Cen & its 2 sub-groups: LCC and UCL Common dynamical evolution Sequence of successive episodes of triggered star formation: BPMG, TWA, and η & ε Cha Joint action of expanding shells and SN events Dynamical age = Myr Ortega et al. (2002, 2009)

I- Introduction Bright Southern Source V = 3.86; K = 3.5, L’ = 3.5 Spectral type A5V Mass = 1.75 Msun d = 19.3 pc Age (Myrs) = 12 Myrs Fe/H : IR excess detected by IRAS 1984: First use of a stellar Coronograph (after Lyot). > Detection of a circumstellar disk β Pictoris: The star Smith &Terrile (1984)

I- Introduction The debris-disk around β Pictoris Re-processed dust (small grains) Large variety of structures: - Main disk (PA = 31.4 o ) - Inner warp (PA = 35.6 o ) - Global “Butterfly” asymmetries - 4 Belts (6, 16, 32 and 52 AU) ESO3.6m - ADONIS/SHARP (H, FoV 12.5”) Mouillet al. 97 Mouillet et al. 97; Heap et al. 00 Augereau et al. 01; Okamoto et al. 04 Golimowki et al. 06; Freistetter et al. 07

I- Introduction The debris-disk around β Pictoris HST/STIS, Heap et al. 00 HST/ACS, Golimowski et al. 06 Re-processed dust (small grains) Large variety of structures: - Main disk (PA = 31.4 o ) - Inner warp (PA = 35.6 o ) - Global “Butterfly” asymmetries - 4 Belts (6, 16, 32 and 52 AU)

I- Introduction The debris-disk around β Pictoris Re-processed dust (small grains) Large variety of structures: - Main disk (PA = 31.4 o ) - Inner warp (PA = 35.6 o ) - Global “Butterfly” asymmetries - 4 Belts (6, 16, 32 and 52 AU) Falling evaporating bodies, Observed in spectroscopic lines Explained by the presence of one or several planets of 2, 0.5 and 0.1 Mjup at 12, 25 and 44 AU, resp. Beust & Morbidelli 00

I- Introduction The debris-disk around β Pictoris Re-processed dust (small grains) Large variety of structures: - Main disk (PA = 31.4 o ) - Inner warp (PA = 35.6 o ) - Global “Butterfly” asymmetries - 4 Belts (6, 16, 32 and 52 AU) Falling evaporating bodies, Observed in spectroscopic lines Explained by the presence of one or several planets of 2, 0.5 and 0.1 Mjup at 12, 25 and 44 AU, resp. Freistetter et al. (2007)

Outline The β Pictoris Heritage I- Introduction to β Pictoris Young nearby association, star & debris-disk II- Technics & NaCo Imaging Challenge, evolution, limitations & observations III- The β Pic b Giant Planet Detection, recovery, characterization & origin IV- Perspectives

Why Imaging? II- Techniques

Detect/characterize something faint, angularly close to something bright Imaging: an observing challenge! II- Techniques  High image quality - High angular resolution, PSF Stability - Calibration of static aberrations  Stellar Halo Brightness ‏ - Halo attenuation/PSF subtraction - Speckle noise  Intrinsic companion faintness - Long overall observations HIP95270 (Tuc-Hor) VLT/NaCo H, 10” by 10” (?)

ESO3.6m/Come-On+ SH WFS; 62 actuators; Sr = 40-50% Neuhäuser et al 05 Sr < 10% Janson et al. 07‏  GQ lup star (K7V; V=11.4; K=7.1) VLT/NACO Impressive evolution High Angular Resolution II- Techniques VLT/NACO SH WFS; 185 actuators Sr > 90% 2012 – SPHERE SH WFS; 1700 actuators

The art of PSF subtraction II- Techniques β Pictoris, ADI-L’, T obs = 60min FoV = 2.5” by 2.5”, Field Rot. ~ 60deg High Contrast at inner angles  Main limitation (< ’’): Atmospheric & instrumental speckles  Coronagraphy - Occulting and Lyot-pupil mask - 4QP Mask, Boccaletti et al new concepts: PIAAC, ALC, APC, Vortex.  Differential Imaging - PSF-reference (RDI) - Spectral (SDI), Close et al Polarimetric (PDI) - Angular (ADI), Marois et al. 06  Post-processing tools - LOCI, Lafrenière et al ANDROMEDA, Mugnier et al. 10

NaCo high-contrast upgrades II- Techniques 2001, Nov: NaCo First-lights! 2004: Aladdin Detector upgrade 2005: Simultaneous differential Imaging mode 2006: 4QPM coronagraph 2008: Pupil-tracking upgrade 2010: APP, apodized pupil plane 2011: APP-Spec, Vortex, DAM… NaCo/Yepun-Nasmyth B

ADI: Photometry & astrometry II- Techniques Need for adapted tools,  Local insertion of fake-negative planets to recover astrometry & photometry

Outline The β Pictoris Heritage I- Introduction to β Pictoris Young nearby association, star & debris-disk II- Technics & NaCo Imaging Challenge, evolution, limitations & observations III- The β Pic b Giant Planet Detection, recovery, characterization & origin IV- Perspectives

NaCo observing campaigns UT DateESO-programFT/PTmodebandRemark 2002 Nov C-0565FTCORH,Kdisk detection 2003 Nov C-0624FTIMSATL’planet detection 2008 Nov C-713FTIMSATL’no detection 2009 Feb 11, C-5037FTIMSATL’no detection 2009 Oct C-0207FTIMSATL’recovery 2009 Nov 25, C-0396FTIMSATL’ Dec 26, C-0739PTIMSATL’ Mar C-5057PTIMSATKs Apr C-5057PTIMSATKs Apr C-5057PTAPPNB Sep C-0277PTIMSATL’ Nov 14, C-0341PTIMSATL’, Ks- III- Results

Planetary Candidate Detection III- Results GTO-2003 observations Nov 10, 11 and 13, 2003 Field-Tracking observation Reference at same parall. angle 2008, A.-M. Lagrange re-analysis 1 st analysis: Sky-subtraction problem Planet candidate detection! ΔL’ = 7.7 mag Sep = mas Fake-planet simulations Redetection in all 3 nights If planet: 8-9 Mjup at proj. dist. of 8 AU Related to the 1981 Bpic transit? Lecavelier Des Etangs et al. 09 Nov 2003 (NaCo-L’) 500 mas

Early-2009 Non-detection III- Results Follow-up early-2009 campaign Jan and Feb 2009 Field-Tracking observation Reference at same parall. angle No re-detection down to 6.5 AU Constrain on the orbital properties: a, e, ω… most probable solution: - e < 0.1; a= 8-9 AU, - Larger a still possible (> 17 AU), - after quadrature, - Assuming prograde rotation Lagrange et al. 09b; Fitzgerald et al. 09; Olofsson 01

III- Results Transit 81 Detection 03 Non-Detection 09 quadrature 17.1 AU 52.8 yrs 8.1 AU 17.2 yrs Early-2009 Non-detection Follow-up early-2009 campaign Jan and Feb 2009 Field-Tracking observation Reference at same parall. angle No re-detection down to 6.5 AU Constrain on the orbital properties: a, e, ω… most probable solution: - e < 0.1; a= 8-9 AU, - Larger a still possible (> 17 AU), - after quadrature, - Assuming prograde rotation Lagrange et al. 09b; Fitzgerald et al. 09; Olofsson 01

III- Results Nov 2003Oct mas Follow-up late-2009 campaign Oct Field-Tracking observation Reference at same parall. angle Re-detection on the SW part ΔL’ = mag Sep = mas Candidate Confirmed as a bound companion P = yrs a = AU e < 0.05; i ~ 90 deg PA = deg > Main Disks/Warp? β Pictoris b Recovery

III- Results Additional confirmation & characterization NaCo APP NB4.05-imaging Observation: 10 Apr, 2010 ΔNB4.05 = mag Sep = mas Quanz et al. 10 NaCo Ks-imaging Observation: 20 March, 2010 ΔKs = mag Sep = mas Bonnefoy et al. 10, submitted Mar 2010 (NaCo-Ks)

III- Results Additional confirmation & characterization NaCo APP NB4.05-imaging Observation: 10 Apr, 2010 ΔNB4.05 = mag Sep = mas Quanz et al. 10 NaCo Ks-imaging Observation: 20 March, 2010 ΔKs = mag Sep = mas Bonnefoy et al. 10, submitted (K- L’) = Red and dusty atmosphere Field dwarfs: SpT = [L2 – T0]

III- Results Additional confirmation & characterization NaCo APP NB4.05-imaging Observation: 10 Apr, 2010 ΔNB4.05 = mag Sep = mas Quanz et al. 10 NaCo Ks-imaging Observation: 20 March, 2010 ΔKs = mag Sep = mas Bonnefoy et al. 10, submitted (K- L’) = Red and dusty atmosphere Teff = K; logg = [ ]

Mass determination? Cold start Hot start. RV + Disk dynamics: M < 20 Mjup. Evolutionary model predictions: - Companion KL’ photometry - β Pictoris: 19.3pc and 12 Myr > “Hot-start”: 8-9 Mjup (Baraffe et al. 03) > “Cold start”: BD-stellar masses (Marley et al. 07) “Cold start”’ models failed to reproduce β Pic b luminosity, i.e the energy release during the Gas accretion shock. β Pic b Predicted Mass & Origin III- Results

Core Accretion does not work at > AU > Core or Disk fragmentation ? (Dodson –Robinson et al. 09; Boley et al. 09) Inner limit to the Core or Disk fragmentation? β Pictoris b: serious candidate for a formation mechanism via CA Origin III- Results

Outline The β Pictoris Heritage I- Introduction to β Pictoris Young nearby association, star & debris-disk II- Technics & NaCo campaigns Challenge, evolution, limitations & observations III- The β Pic b Giant Planet Detection, recovery, characterization & origin IV- Perspectives

- PerspectivesIV- Perspectives candidate confirmed, characterized (different modes, teams & bands) > waiting for confirmation from other facilities (Gemini, Keck). Follow-up and refinement of the Orbital properties. Inside the main disk or in the warp? Dynamical Implication?. Spectral Characterization: - add. Photometry, spectroscopy, - Atmosphere properties, impact of low-gravity atmosphere. Use of Complementary techniques: - RV-HARPS, ok but active-star - VLTI/PIONIER, CP precision? - Astrometry (GAIA) and Transit, > dynamical mass for evolutionary model calibration!. Search for Giant planets c and d!. VLT/SPHERE (early-2012): Prime target for the Science Verification!