Anne-Marie Lagrange 1 et al 1 Laboratoire d’Astrophysique de Grenoble, France IAU276 – October, 11, 2010 The candidate companion around Pictoris.

Anne-Marie Lagrange 1 et al

1Laboratoire d’Astrophysique de Grenoble, France

IAU276 – October, 11, 2010

The candidate companion around b Pictoris

HR8799 bcd (~7-10MJup; 24,38,64AU)Marois et al. (2008)

Formation process ??

Fomalhautb (<3MJup; 115AU)Kalas et al. (2008)

2M1207B (~5-8MJup; 50AU)Chauvin et al. (2004;2005)

ABPic b (~13MJup; 250AU)Chauvin et al. (2005a)

Planet candidate around beta Pictoris

Lagrange et al (2009a, 2009b)

400mas

N

E

Planet candidate . ΔL’ = 7.7 ± 0.3 => M~9MJup if bound. Sep = 411 ± 8 mas (~8 AU) proj. P.A. = 31.8 ± 1.3 deg (disk P.A. ~ 33 deg)Teff ~1500KAge ~12 Myr

VLT/NaCo2003

February 2009

Lagrange et al (2009); see also Fitzgerald and Kalas (2009)

6s limit( L_abs=9.8)

After quad.

Before quad.

Planet around beta Pictoris

Lagrange et al (2010)

N

E400mas

300mas

VLT/NaCo2003

VLT/NaCoFall 2009

Semi-major axis: ~8-14 AU

Augereau et al. (2001b)

Planet on an inclined orbit, 10 AU

~ 80 UA

Augereau et al. (2001b)Augereau et al. (2001b)

Mouillet et al. (1997)

Constraints from the warp modeling

90’s: Falling Evaporating Bodies onb Pictoris=> indirect evidence for planet ?

Vidal-Madjar, Lagrange, Beust, Morbidelli…

A massive Giant Planet at ~10AU explains: The inner warp and other disk asymetries

The FEBs

Implications on planet formation scenari : Giant Planets form rapidly (< a few Myr) Formation process: could be core accretion (see Keenedy & Kenyon 08) Test of evolutionary model: unique test given its short period

NB4.05 mic Dusty model

Quanz et al (2010)

Ks s13 Ks s27

Bonnefoy et al (2010)

• a=8AU => maximum mass~30 Mjup• a=14AU => maximum mass~10Mjup

Future of exo-planets imaging