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K2-19, The first K2 muti-planetary system showing TTVs

Published online by Cambridge University Press:  27 October 2016

S. C. C. Barros ,
J. M. Almenara ,
O. Demangeon ,
M. Tsantaki ,
A. Santerne ,
D. J. Armstrong ,
D. Barrado ,
D. Brown ,
M. Deleuil  and
J. Lillo-Box
...Show all authors
S. C. C. Barros
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal
J. M. Almenara
Affiliation:
Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France CNRS, IPAG, F-38000 Grenoble, France
O. Demangeon
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
M. Tsantaki
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal
A. Santerne
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal
D. J. Armstrong
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
D. Barrado
Affiliation:
Departamento de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESAC campus 28691 Villanueva de la Cañada (Madrid), Spain
D. Brown
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
M. Deleuil
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
J. Lillo-Box
Affiliation:
Departamento de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESAC campus 28691 Villanueva de la Cañada (Madrid), Spain
H. Osborn
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
D. Pollacco
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
L. Abe
Affiliation:
Laboratoire Lagrange, UMR7239, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d'Azur, F-06300 Nice, France
P. Andre
Affiliation:
Observatoire de Belesta en Lauragais - Assoc. Astronomie Adagio 30 Route de Revel 31450 Varennes, France
P. Bendjoya
Affiliation:
Laboratoire Lagrange, UMR7239, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d'Azur, F-06300 Nice, France
I. Boisse
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
A. S. Bonomo
Affiliation:
INAF - Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025, Pino Torinese, Italy
F. Bouchy
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
G. Bruno
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
J. Rey Cerda
Affiliation:
Observatoire Astronomique de l'Universite de Genève, 51 chemin des Maillettes, 1290 Versoix, Switzerland
B. Courcol
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
R. F. Díaz
Affiliation:
Observatoire Astronomique de l'Universite de Genève, 51 chemin des Maillettes, 1290 Versoix, Switzerland
G. Hébrard
Affiliation:
Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France Observatoire de Haute-Provence, Université d'Aix-Marseille & CNRS, 04870 Saint Michel l'Observatoire, France
J. Kirk
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
J. C. Lachurié
Affiliation:
Observatoire de Belesta en Lauragais - Assoc. Astronomie Adagio 30 Route de Revel 31450 Varennes, France
K. W. F. Lam
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
P. Martinez
Affiliation:
Observatoire de Belesta en Lauragais - Assoc. Astronomie Adagio 30 Route de Revel 31450 Varennes, France
J. McCormac
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
C. Moutou
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt CNRS, Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy., Kamuela, HI 96743, USA
A. Rajpurohit
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France email: susana.barros@astro.up.pt
J.-P. Rivet
Affiliation:
Laboratoire Lagrange, UMR7239, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d'Azur, F-06300 Nice, France
J. Spake
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
O. Suarez
Affiliation:
Laboratoire Lagrange, UMR7239, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d'Azur, F-06300 Nice, France
D. Toublanc
Affiliation:
Observatoire de Belesta en Lauragais - Assoc. Astronomie Adagio 30 Route de Revel 31450 Varennes, France Universite de Toulouse, UPS-CNRS, IRAP, 9 Av. colonel Roche, 31028 Toulouse, France
S. R. Walker
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
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Abstract

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In traditional transit timing variations (TTVs) analysis of multi-planetary systems, the individual TTVs are first derived from transit fitting and later modelled using n-body dynamic simulations to constrain planetary masses. We show that fitting simultaneously the transit light curves with the system dynamics (photo-dynamical model) increases the precision of the TTV measurements and helps constrain the system architecture. We exemplify the advantages of applying this photo-dynamical model to a multi-planetary system found in K2 data very close to 3:2 mean motion resonance, K2-19. In this case the period of the larger TTV variations (libration period) is much longer (>1.5 years) than the duration of the K2 observations (80 days). However, our method allows to detect the short period TTVs produced by the orbital conjunctions between the planets that in turn permits to uniquely characterise the system. Therefore, our method can be used to constrain the masses of near-resonant systems even when the full libration curve is not observed.

Keywords

Planet detectiondynamical evolution and stabilityK2-19radial velocity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29A: Astronomy in Focus , August 2015 , pp. 51 - 56
Copyright
Copyright © International Astronomical Union 2016 

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