R A D I A L V E L O C I T Y S E A R C H F O R L O N G - P E R I - PowerPoint PPT Presentation

R A D I A L V E L O C I T Y S E A R C H F O R L O N G - P E R I O D E X O P L A N E T S A N D B R O W N D WA R F S W I T H E L O D I E A N D S O P H I E J AV I E R A R E Y O B S E R VAT O I R E D E G E N È V E F R A N Ç O I S B O U C H Y, S T É P H A N E U D RY, I S A B E L L E B O I S S E G . H E B R A R D , X . D E L F O S S E , C . M O U T O U , D . E H R E N R E I C H , T. F O R V E I L L E , F. P E P E , N . S A N T O S , D . S É G R A N S A N , L . A R N O L D , M . D E L E U I L , A . S A N T E R N E , V. B O U R R I E R , R . D I A Z , X . B O N F I L S , B . C O U R C O L , P. W I L S O N , N . A S T U D I L L O , O . D E M A N G E O N O H P 2 0 1 5 : T W E N T Y Y E A R S O F G I A N T E X O P L A N E T S

C O N T E X T A C U R R E N T V I E W O F L O N G - P E R I O D E X O P L A N E T S RV 
 Imaging 
 3 m/s Transit 
 J 1 m/s S 30 cm/s Microlensing U N 41 systems with V E a>4AU 
 detected using radial velocities Info from exoplanet.eu, exoplanets.org and I. Boisse 2014 2

C O N T E X T A C U R R E N T V I E W O F L O N G - P E R I O D E X O P L A N E T S RV 
 Imaging 
 R V + I M A G I N G + A S T R O M E T RY 3 m/s Transit 
 J 1 m/s S 30 cm/s Microlensing U N 41 systems with V E a>4AU 
 detected using radial velocities Info from exoplanet.eu, exoplanets.org and I. Boisse 2014 3

C O N T E X T A C U R R E N T V I E W O F B R O W N D WA R F S • No clear dividing line between very massive planets and brown dwarfs 
 • Only a few BD companions with orbital period larger than 10 years: 4 CORALIE (Sahlmann et al. 2011), 1 HARPS (Lo Curto et al. 2010; Feroz et al. 2011), 5 ELODIE- • SOPHIE (Bouchy et al. 2015, accepted) • Number of BDs rises with the orbital period (Ma & Ge, 2014) M A & G E , 2 0 1 4 4

P R O G R A M S F O L L O W- U P O F E L O D I E L O N G - T E R M F O L L O W- U P L O N G P E R I O D S O F K N O W N T R A N S I T I N G H O T J U P I T E R S • Long-period exoplanets and brown • Orbital evolution of hot Jupiters: dwarfs Possible interaction with another companion • Historical ELODIE catalog • Few cases of transiting hot Jupiters • ~60 targets, G and K stars in multi- planetary systems with long- period giant planets • +20 years of data • ~35 targets (CoRoT, Kepler, HAT, • Allows us to look for giant planets at WASP) a>5 AU 5

P R O G R A M S F O L L O W- U P O F E L O D I E L O N G - T E R M F O L L O W- U P L O N G P E R I O D S O F K N O W N T R A N S I T I N G H O T J U P I T E R S • Long-period exoplanets and brown • Orbital evolution of hot Jupiters: C O M P L E M E N TA RY dwarfs Possible interaction with another T O S I M I L A R companion P R O G R A M S I N T H E • Historical ELODIE catalog S O U T H • Few cases of transiting hot Jupiters • ~60 targets, G and K stars in multi- planetary systems with long- period giant planets • +20 years of data • ~35 targets (CoRoT, Kepler, HAT, • Allows us to look for giant planets at WASP) a>5 AU 6

P R O G R A M S W H E N D E A L I N G W I T H L O N G - P E R I O D E X O P L A N E T S , W E M U S T C O N S I D E R : • Instrumental drifts & offsets • Magnetic cycles • Correlations with activity index (log • Offset between ELODIE, SOPHIE R’ HK ) and CCF parameters (bisector, and SOPHIE+ data FWHM, contrast) • Long-term variations in RVs due to • Evolution of activity indices (Ca II and instrumental effects H α lines) F O L L O W - U P O F C O N S TA N T S TA R S ( B . C O U R C O L ) A C T I V I T Y I N D I C E S ( I . B O I S S E & O . G I R A U LT ) 7

P R O G R A M S W H E N D E A L I N G W I T H L O N G - P E R I O D E X O P L A N E T S , W E M U S T C O N S I D E R : • Magnetic cycles 𝐼𝛽 index Radial velocities 𝐼𝛽 : As Gomes da Silva et al. 2013, 𝜀𝜇 𝐼𝛽 =0,678 nm 8

P R O G R A M S W H E N D E A L I N G W I T H L O N G - P E R I O D E X O P L A N E T S , W E M U S T C O N S I D E R : • Magnetic cycles H alpha index Radial velocities 𝐼𝛽 : As Gomes da Silva et al. 2013, 𝜀𝜇 𝐼𝛽 =0,678 nm 9

R E S U LT S F O L L O W- U P O F E L O D I E L O N G P E R I O D S B O I S S E E T A L . 2 0 1 2 +5584 +469 P [days] = 5894 P [days] = 3999 -1498 -541 +0.28 e = 0.38 e = 0.16 +0.27 -0.32 -0.22 +4.0 +0.6 a [AU] = 6.7 a [AU] = 5.1 -1.4 -0.7 +1.14 +0.67 Mp sin i [MJup] = 2.71 Mp sin i [MJup] = 1.90 -0.66 -0.53 U P D AT E D O R B I T S P [days] = 5655 ± 904 P [days] =3841 ± 54 e = 0.6 ± 0.1 e = 0.25 ± 0.06 a [AU] = 6.2 a [AU] = 4.8 Mp sin i [MJup] = 2.16 Mp sin i [MJup] = 2.25

R E S U LT S F O L L O W- U P O F E L O D I E L O N G P E R I O D S B O U C H Y E T A L . 2 0 1 5 , A C C E P T E D P [days] = 5405 ± 81 P [days] = 4743.6 ± 5.6 e = 0.344 ± 0.007 e = 0.455 ± 0.004 a [AU] = 6.1 a [AU] = 5.9 Mc sin i [MJup] = 31.8 Mc sin i [MJup] = 47.8 I N T E R E S T I N G C A S E S I N T H I S P R O G R A M

R E S U LT S L O N G - T E R M F O L L O W- U P O F K N O W N T R A N S I T I N G H O T J U P I T E R S P R E L I M I N A RY R E S U LT S . . corot20 1000 500 RV [m/s] 0 − 500 200 O − C [m/s] 0 − 200 5600 5800 6000 6200 6400 6600 6800 7000 BJD − 2450000.0 [days] . .

R E S U LT S F O L L O W- U P O F E L O D I E L O N G P E R I O D S • Synergy with Direct Imaging • Collaboration with J. Hagelberg (University of Hawai’i) • Subaru / SCExAO H - B A N D I M A G E – S E PA R AT I O N 0 . 4 ” R A D I A L V E L O C I T I E S : E L O D I E , S O P H I E , S O P H I E +

D I S C U S S I O N & C O N C L U S I O N S • The search for long-period planets and BDs is biased by the relatively small number of long term surveys • Our recent results double the number of known BD companions with orbital period longer than 10 years • This helps to set up a better observational base with which to compare models and theories of formation and evolution of BDs • RV measurements do not constrain the orbital inclination, so we have only the minimum mass . We need complementary observational constraints to determine the true mass or to exclude the stellar nature of the companion. These companions are excellent candidates for astrometry and direct imaging • The separation between planets and BDs may be related not only to the mass, but also the formation scenario . Statistical properties of BD companions should permit to distinguish between different formation and evolution models