Photodynamical mass determination of the multiplanetary system K2-19
Date Issued
2015
Author(s)
Barros, S. C. C.
•
Almenara, J. M.
•
Demangeon, O.
•
•
Santerne, A.
•
Armstrong, D. J.
•
Barrado, D.
•
Brown, D.
•
Deleuil, M.
•
Lillo-Box, J.
•
Osborn, H.
•
Pollacco, D.
•
Abe, L.
•
Andre, P.
•
Bendjoya, P.
•
Boisse, I.
•
•
Bouchy, F.
•
•
Cerda, J. Rey
•
Courcol, B.
•
Díaz, R. F.
•
Hébrard, G.
•
Kirk, J.
•
Lachurié, J. C.
•
Lam, K. W. F.
•
Martinez, P.
•
McCormac, J.
•
Moutou, C.
•
Rajpurohit, A.
•
Rivet, J. -P.
•
Spake, J.
•
Suarez, O.
•
Toublanc, D.
•
Walker, S. R.
Description
Based on observations collected with the NASA Kepler satellite and with the SOPHIE spectrograph on the 1.93-m telescope at Observatoire de Haute-Provence (CNRS), France. We thank the staff at Haute-Provence Observatory. SCCB acknowledges support by grants 98761 by CNES and the Fundação para a Ciência e a Tecnologia (FCT) through the Investigador FCT Contract No. IF/01312/2014. This work was also supported by FCT through the research grant UID/FIS/04434/2013. JMA acknowledges funding from the European Research Council under the ERC Grant Agreement no. 337591-ExTrA. OD acknowledges support by the CNES grant 124378. AS is supported by the European Union under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. We thank the referee for his suggestions that improved the manuscript.
Abstract
K2-19 is the second multiplanetary system discovered with K2 observations. The system is composed of two Neptune size planets close to the 3:2 mean-motion resonance. To better characterize the system we obtained two additional transit observations of K2-19b and five additional radial velocity observations. These were combined with K2 data and fitted simultaneously with the system dynamics (photodynamical model) which increases the precision of the transit time measurements. The higher transit time precision allows us to detect the chopping signal of the dynamic interaction of the planets that in turn permits to uniquely characterize the system. Although the reflex motion of the star was not detected, dynamic modelling of the system allowed us to derive planetary masses of Mb = 44 ± 12 M⊕ and Mc = 15.9 ± 7.0 M⊕ for the inner and the outer planets, respectively, leading to densities close to Uranus. We also show that our method allows the derivation of mass ratios using only the 80 d of observations during the first campaign of K2.
Volume
454
Issue
4
Start page
4267
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.454.4267B
Rights
open.access
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