K2 - 19 , THE FIRST K2 MULTI-PLANETARY SYSTEM SHOWING TTVS Susana - - PowerPoint PPT Presentation

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K2 - 19 , THE FIRST K2 MULTI-PLANETARY SYSTEM SHOWING TTVS Susana C.C. Barros Instituto de Astrofsica e Cincias do Espao, Porto , Portugal Formerly @ Laboratoire dAstrophysique de Marseille, France Collaborators: Almenara, J.M.;

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SLIDE 1

K2 - 19 , THE FIRST K2 MULTI-PLANETARY SYSTEM SHOWING TTVS

Susana C.C. Barros Instituto de Astrofísica e Ciências do Espaço, Porto , Portugal

Formerly @ Laboratoire d’Astrophysique de Marseille, France

Collaborators: Almenara, J.M.; Demangeon, O.; Tsantaki, M.; Santerne, A.; Armstrong, D.; Barrado, D.; Brown, D.; Deleuil, M.; Lillo, J.; Osborn, H.; Pollacco, D.; Abe, L.; Andre, P.; Bendjoya, P.; Boisse, I.; Bonomo, A.; Bouchy, F.; Bruno, G.; Rey Cerda, J.; Courcoul, B.; Díaz, R.; Hebrard, G; Kirk, J.; Lachurie, J.; Lam, K.; Martinez, P.; McCormac, J.; Moutou, C.; Rajpurohit, A.; Rivet, J.-P.; Spake, J.; Suárez, O.; Toublanc, D.; Walker, S.

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SLIDE 2

Outline

  • K2-19 discovery summary
  • Describe photodynamic model
  • Despite the short duration of K2 we can detect TTVs and

constrain the masses of the both planets

  • Astro-ph: 1510.0147

6 October 2015 Susana Barros

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TTV analysis didn’t die with Kepler

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SLIDE 3

K2-19b & c (EPIC 201505350)

  • Discovered in K2 - Campaign 1 with duration ~ 75 days
  • Close to 3:2 mean motion resonance
  • Validated with PASTISà 99.2% probability for the planetary system

Armstrong et al. 2015

Susana Barros 6 October 2015

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Pb ~ 8 days, Rb= 7.23+/-0.6 Rearth Pc ~ 12 days Rc= 4.21+/-0.31 Rearth

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SLIDE 4

C1 duration ~75 days

Near mean motion resonance

Closeness to resonance à TTVs expected Follow-up transit larger inner planet b ~200 days after K2

6 October 2015 Susana Barros

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Armstrong et al. 2015/arXiv:1503.00692

Constrain the masses: Mb < 245 MEarth, Mc < 280 MEarth

Planet b

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SLIDE 5

Near resonant systems

6 October 2015 Susana Barros

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  • Amplitude of the TTV curve is

proportional to the dynamic masses and eccentricity (Holman et al 2005, Agol 2005, Lithwick et al. 2012)

  • The libration period is inversely

proportional to the distance to the resonance.

  • K2-19 is one of the closest

systems to 3:2 MMR à long libration period > 1.5 years not detectable in the duration

  • ur observations

Adapted from Lithwick et al. 2012

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SLIDE 6

Chopping short period TTVs

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KOI-142 (Kepler-88) Nesvorny et al 2013 later confirmed Barros et al 2014

  • TTVs short-timescale component “chopping” at synodic timescale

(Nesvorný & Beaugé 2010; Nesvorný & Vokrouhlický 2014; Deck & Agol 2015).

  • Proportional to mass ratios, lifts degeneracy à uniquely estimate

the planetary masses.

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SLIDE 7

Photodynamical model

Mercury N-body Transit/RV model Likehood

6 October 2015 Susana Barros

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MCMC

masses and radius of all bodies + planetary orbital parameters at reference time

Almenara, J. M. et al. 2015, MNRAS, 453, 2644

Standard TTV: fit transit times àTTVs à system dynamics

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SLIDE 8

Advantages

  • Fully consistent analysis
  • Exploit all photometric measurements (e.g. TTVs, TDVs)
  • Doppler detection + light curve à Absolute masses
  • Dynamics helps constrain the TTVs and TDVs à Higher

precision in system parameters (Almenara et al. 2015)

  • Less sensitive to systematics
  • Long computation time

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Derived from the model gravitationally assisted

Disadvantage

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SLIDE 9

LAM K2 pipeline

  • Based on CoRoT imagette pipeline (Barros et al. 2014)
  • Optimised aperture to maximise S/N (e.g. Adda et al. 2000)
  • Self-flat field correction method (Vanderburg & Jonhson 2014)

Susana Barros 6 October 2015

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Barros et al in prep

20 40 60 80 0.990 0.995 1.000 1.005 20 40 60 80 Time−2456810. 0.990 0.995 1.000 1.005 Normalised flux

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SLIDE 10

K2 detrending – Campaign 1

6 October 2015 Susana Barros

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For more information about the K2 pipeline please see the poster 4

8 10 12 14 16 18 mag 101 102 103 104 105 106 rms (ppm) white noise level corrected raw

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SLIDE 11

Transit fitting K2

6 October 2015 Susana Barros

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0.992 0.994 0.996 0.998 1.000 1.002

  • Rel. flux

13.2 13.35 13.5 −500 −250 250 500

O-C [ppm]

17.1 17.25 17.4

1

21.15 21.3 21.45

1 2

29.1 29.25 29.4

3

37.05 37.2 37.35

2

40.95 41.1 41.25

4

44.85 45.0 45.15 45.3 0.992 0.994 0.996 0.998 1.000 1.002

  • Rel. flux

3 5

52.8 52.95 53.1 −500 −250 250 500

O-C [ppm] 6

60.75 60.9 61.05

4

64.8 64.95 65.1

7

68.7 68.85 69.0

BJD - 2,456,800 5 8

76.65 76.8 76.95

9

84.6 84.75 84.9

6

88.65 88.8 88.95

Planet b Planet c

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SLIDE 12

Follow–up transit observations

  • Epoch 34 - 40 cm NITES telescope La Palma
  • Epoch 35 - 1m C2PU/Omicron at Calerm, France
  • Epoch 36 - Belesta 82-cm, France

Susana Barros 6 October 2015

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0.99 1.0 1.01

  • Rel. flux

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7082.55 7082.70 7082.85 −0.01 0.00 0.01

O-C 35

7090.50 7090.65 7090.80

BJD - 2,450,000 36

7098.45 7098.6 7098.75

Planet b

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SLIDE 13

Spectroscopic observations

  • 10 observations with SOPHIE at 1.93m OHP (France)

Susana Barros 6 October 2015

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7.16 7.18 7.20 7.22 7.24 7.26 7.28 7.30 7.32 Radial Velocity [km s−1] 7040 7050 7060 7070 7080 7090 7100 7110 7120 7130 7140 BJD - 2,450,000 −50 50 O-C [m s−1]

  • Doppler signature not

detected

  • Require stellar priors

from stellar models

  • Spectral analysis, late G dwarf: Teff = 5390 +/- 180K,

logg=4.42 +/- 0.34dex, Fe/H=0.19 +/- 0.12dex M* = 0.92 +/- 0.08 MSun, R* = 0.93 +/- 0.20 RSun

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SLIDE 14

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Results

Dynamically constrained – independent from stellar parameters

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Planetary composition

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Mb = 44 +/- 12 Mc = 15.9 +/- 7.0

M-R models for solid planets (Zeng et al 2013) M-R models for planets with H/He envelopes for different metal enrichment Z (Barraffe et al 2008)

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SLIDE 16

6 October 2015 Susana Barros

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−60 −40 −20 20 40 60 TTV [min] 6800 6900 7000 7100 7200 7300 7400 BJD - 2,450,000 −200 −150 −100 −50 50 100 150 200 TTV [min]

Planet b Planet c

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SLIDE 17

Compare with traditional TTV

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Values agree Double uncertainties

−15 −10 −5 5 10 15 TTV [min] 6800 6850 6900 6950 7000 7050 7100 BJD - 2,450,000 −15 −10 −5 5 10 15 TTV [min]

Planet b Planet c

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SLIDE 18

K2 data only: chopping is detected!

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−2 −1 1 2 TTV [min] 6810 6820 6830 6840 6850 6860 6870 6880 6890 BJD - 2,450,000 −6 −5 −4 −3 −2 −1 1 2 3 4 5 6 TTV [min]

Planet b Planet c

= 0.474 +/-0.16 = 0.000142+/-0.000038

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SLIDE 19

Take home messages

  • The planets have significant gaseous envelopes and

K2-19c has higher metal enrichment than K2-19b.

  • A photodynamical model leads to a better constrain on the

system parameters.

  • Detecting short period TTVs (chopping) in K2-19 allows to

constrain the system without long time coverage. Powerful tool for K2, CHEOPS, TESS…

6 October 2015 Susana Barros

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Thanks

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SLIDE 20

Narita et al.

  • AO imaging à no contaminant
  • High resolution spectroscopy Teff = 5345 +/- 17K,

logg=4.39 +/- 0.05dex, Fe/H=0.07 +/- 0.03dex M* = 0.902 +/- 0.01 MSun, R* = 0.914 +/- 0.03 Rsun

  • Fit light curve to derive TTVs
  • Use synodic chopping formula Deck and Agol 2015

applied to planet b TTVs à Mc = 21.4 +/- 1.9 assuming circular and coplanar orbits

6 October 2015 Susana Barros

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SLIDE 21

Dynamic parameters

6 October 2015 Susana Barros

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K2 K2 + RV + transits K2 + RV + STAR K2 + RV + transits + STAR

0.0 0.5 1.0 1.5 2.0 2.5 PlanetHost1 qp 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 PDF

run10 run12 run13 run14

0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 PlanetHost1 q+ 2000 4000 6000 8000 10000 12000 14000 PDF

run10 run12 run13 run14

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SLIDE 22

6 October 2015 Susana Barros

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0.95 1.05 1.15 KeplerLC jitter 0.074 0.076 0.078 Planet b Rp/R? 87.5 175.0 262.5 Planet b ! 87.4 88.2 89.1 Planet b i 100.0 200.0 300.0 Planet b M 0.12 0.2 0.27 Planet b Mp 0.073 0.077 0.082 Planet b a 0.09 0.18 0.26 Planet b e 0.0445 0.046 0.0475 Planet c Rp/R? 100.0 200.0 300.0 Planet c ! 88.5 90.0 91.5 Planet c i 100.0 200.0 300.0 Planet c M 0.04 0.07 0.11 Planet c Mp 0.096 0.103 0.109 Planet c a 0.09 0.18 0.26 Planet c e 168.8 177.5 186.2 Planet c n 1.1 1.8 2.4 SOPHIE jitter 7.21 7.23 7.25 Star 0.85 1.0 1.15 Star M? 0.85 1.0 1.15 Star R? 0.4 0.45 0.5 Star ua 0.999993 1.000015 1.000038 KeplerLC foot 0.15 0.19 0.24 Star ub 0.95 1.05 1.15 KeplerLC jitter 0.074 0.076 0.078 Planet b Rp/R? 87.5 175.0 262.5 Planet b ! 87.4 88.2 89.1 Planet b i 100.0 200.0 300.0 Planet b M 0.12 0.2 0.27 Planet b Mp 0.073 0.077 0.082 Planet b a 0.09 0.18 0.26 Planet b e 0.0445 0.046 0.0475 Planet c Rp/R? 100.0 200.0 300.0 Planet c ! 88.5 90.0 91.5 Planet c i 100.0 200.0 300.0 Planet c M 0.04 0.07 0.11 Planet c Mp 0.096 0.103 0.109 Planet c a 0.09 0.18 0.26 Planet c e 168.8 177.5 186.2 Planet c n 1.1 1.8 2.4 SOPHIE jitter 7.21 7.23 7.25 Star 0.85 1.0 1.15 Star M? 0.85 1.0 1.15 Star R? 0.4 0.45 0.5 Star ua