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

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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

May 16, 2023 331 likes •485 views

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 V E F R A N O I S B

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SLIDE 1

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

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SLIDE 2

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

C O N T E X T

RV
 Imaging
 Transit
 Microlensing

2

41 systems with a>4AU
 detected using radial velocities

3 m/s 1 m/s 30 cm/s V E J S U N Info from exoplanet.eu, exoplanets.org and I. Boisse 2014

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SLIDE 3

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

C O N T E X T

RV
 Imaging
 Transit
 Microlensing

3

41 systems with a>4AU
 detected using radial velocities

3 m/s 1 m/s 30 cm/s V E J S U N Info from exoplanet.eu, exoplanets.org and I. Boisse 2014

R V + I M A G I N G + A S T R O M E T RY

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SLIDE 4

C O N T E X T

4

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

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SLIDE 5

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

P R O G R A M S

5

  • Long-period exoplanets and brown

dwarfs

  • Historical ELODIE catalog
  • ~60 targets, G and K stars
  • +20 years of data
  • Allows us to look for giant planets at

a>5 AU

  • Orbital evolution of hot Jupiters:

Possible interaction with another companion

  • Few cases of transiting hot Jupiters

in multi- planetary systems with long- period giant planets

  • ~35 targets (CoRoT, Kepler, HAT,

WASP) 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

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SLIDE 6

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

P R O G R A M S

6

  • Long-period exoplanets and brown

dwarfs

  • Historical ELODIE catalog
  • ~60 targets, G and K stars
  • +20 years of data
  • Allows us to look for giant planets at

a>5 AU

  • Orbital evolution of hot Jupiters:

Possible interaction with another companion

  • Few cases of transiting hot Jupiters

in multi- planetary systems with long- period giant planets

  • ~35 targets (CoRoT, Kepler, HAT,

WASP) 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

C O M P L E M E N TA RY T O S I M I L A R P R O G R A M S I N T H E S O U T H

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SLIDE 7

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 :

P R O G R A M S

7

  • Instrumental drifts & offsets
  • Offset between ELODIE, SOPHIE

and SOPHIE+ data

  • Long-term variations in RVs due to

instrumental effects

  • Magnetic cycles
  • Correlations with activity index (log

R’HK) and CCF parameters (bisector, FWHM, contrast)

  • Evolution of activity indices (Ca II and

Hα 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 )

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SLIDE 8

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 :

P R O G R A M S

8

  • Magnetic cycles

Radial velocities 𝐼𝛽 index 𝐼𝛽: As Gomes da Silva et al. 2013, 𝜀𝜇𝐼𝛽 =0,678 nm

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SLIDE 9

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 :

P R O G R A M S

9

  • Magnetic cycles

Radial velocities H alpha index 𝐼𝛽: As Gomes da Silva et al. 2013, 𝜀𝜇𝐼𝛽 =0,678 nm

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SLIDE 10

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

R E S U LT S

B O I S S E E T A L . 2 0 1 2

P [days] = 5894 e = 0.38 a [AU] = 6.7 Mp sin i [MJup] = 2.71 P [days] = 3999 e = 0.16 a [AU] = 5.1 Mp sin i [MJup] = 1.90

+5584

  • 1498

+0.28

  • 0.32

+4.0

  • 1.4

+1.14

  • 0.66

+469

  • 541

+0.27

  • 0.22

+0.6

  • 0.7

+0.67

  • 0.53

U P D AT E D O R B I T S

P [days] =3841 ± 54 e = 0.25 ± 0.06 a [AU] = 4.8 Mp sin i [MJup] = 2.25 P [days] = 5655 ± 904 e = 0.6 ± 0.1 a [AU] = 6.2 Mp sin i [MJup] = 2.16

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SLIDE 11

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

R E S U LT 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] = 4743.6 ± 5.6 e = 0.455 ± 0.004 a [AU] = 5.9 Mc sin i [MJup] = 47.8 P [days] = 5405 ± 81 e = 0.344 ± 0.007 a [AU] = 6.1 Mc sin i [MJup] = 31.8

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

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SLIDE 12

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

R E S U LT S

−500 500 1000 5600 5800 6000 6200 6400 6600 6800 7000 −200 200

. . RV [m/s] BJD − 2450000.0 [days] O−C [m/s] . . corot20

P R E L I M I N A RY R E S U LT S

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SLIDE 13

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

R E S U LT 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 +

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SLIDE 14

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