The orbit and mass of the third planet in the Kepler-56 system

Oderah Justin Otor; Benjamin T. Montet; John Asher Johnson; David Charbonneau; Andrew Collier Cameron; Andrew W. Howard; Howard Isaacson; David W. Latham; Mercedes Lopez-Morales; Christophe Lovis; Michel Mayor; Giusi Micela; Emilio Molinari; Francesco Pepe; Giampaolo Piotto; David F. Phillips; Didier Queloz; Ken Rice; Dimitar Sasselov; Damien Ségransan; Alessandro Sozzetti; Stéphane Udry; Chris Watson

doi:10.3847/0004-6256/152/6/165

The orbit and mass of the third planet in the Kepler-56 system

Oderah Justin Otor
, Benjamin T. Montet
, John Asher Johnson
, David Charbonneau
, Andrew Collier Cameron
, Andrew W. Howard
, Howard Isaacson
, David W. Latham
, Mercedes Lopez-Morales
, Christophe Lovis
, Michel Mayor
, Giusi Micela
, Emilio Molinari
, Francesco Pepe
, Giampaolo Piotto
, David F. Phillips
, Didier Queloz
, Ken Rice
, Dimitar Sasselov
, Damien Ségransan

Alessandro Sozzetti, Stéphane Udry, Chris Watson

Research output: Contribution to journal › Article › peer-review

Abstract

While the vast majority of multiple-planet systems have orbital angular momentum axes that align with the spin axis of their host star, Kepler-56 is an exception: its two transiting planets are coplanar yet misaligned by at least 40° with respect to the rotation axis of their host star. Additional follow-up observations of Kepler-56 suggest the presence of a massive, non-transiting companion that may help explain this misalignment. We model the transit data along with Keck/HIRES and HARPS-N radial velocity data to update the masses of the two transiting planets and infer the physical properties of the third, non-transiting planet. We employ a Markov Chain Monte Carlo sampler to calculate the best-fitting orbital parameters and their uncertainties for each planet. We find the outer planet has a period of 1002 ± 5 days and minimum mass of 5.61 ± 0.38 M_Jup . We also place a 95% upper limit of 0.80 m s^-1 yr^-1 on long-term trends caused by additional, more distant companions.

Original language	English
Article number	165
Number of pages	7
Journal	Astronomical Journal
Volume	152
Issue number	6
DOIs	https://doi.org/10.3847/0004-6256/152/6/165
Publication status	Published - 1 Dec 2016

Keywords

Planets and satellites: fundamental parameters
Planets and satellites: individual (Kepler-56)
Techniques: radial velocities

Access to Document

10.3847/0004-6256/152/6/165

CollierCameron_2016_AJ_ThirdPlanet_FinalPubVersion
© 2016. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.3847/0004-6256/152/6/165
Final published version, 1.33 MB

https://arxiv.org/abs/1608.03627

Handle.net

Persistent link

Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018
Jardine, M. (PI), Cameron, A. (CoI), Cyganowski, C. (CoI), Horne, K. (CoI) & Wood, K. (CoI)
Science & Technology Facilities Council
1/04/15 → 31/03/18
Project: Standard
EU FP7 Space ETAEARTH: ETAEARTH
Cameron, A. (PI)
Joint Research Centre European Commission
1/01/13 → 31/12/17
Project: Standard

Cite this

Otor, O. J., Montet, B. T., Johnson, J. A., Charbonneau, D., Collier Cameron, A., Howard, A. W., Isaacson, H., Latham, D. W., Lopez-Morales, M., Lovis, C., Mayor, M., Micela, G., Molinari, E., Pepe, F., Piotto, G., Phillips, D. F., Queloz, D., Rice, K., Sasselov, D., ... Watson, C. (2016). The orbit and mass of the third planet in the Kepler-56 system. Astronomical Journal, 152(6), Article 165. https://doi.org/10.3847/0004-6256/152/6/165

@article{aaf4eb928ac94a8fa6aef08c92e4c61d,

title = "The orbit and mass of the third planet in the Kepler-56 system",

abstract = "While the vast majority of multiple-planet systems have orbital angular momentum axes that align with the spin axis of their host star, Kepler-56 is an exception: its two transiting planets are coplanar yet misaligned by at least 40° with respect to the rotation axis of their host star. Additional follow-up observations of Kepler-56 suggest the presence of a massive, non-transiting companion that may help explain this misalignment. We model the transit data along with Keck/HIRES and HARPS-N radial velocity data to update the masses of the two transiting planets and infer the physical properties of the third, non-transiting planet. We employ a Markov Chain Monte Carlo sampler to calculate the best-fitting orbital parameters and their uncertainties for each planet. We find the outer planet has a period of 1002 ± 5 days and minimum mass of 5.61 ± 0.38 MJup . We also place a 95\% upper limit of 0.80 m s-1 yr-1 on long-term trends caused by additional, more distant companions.",

keywords = "Planets and satellites: fundamental parameters, Planets and satellites: individual (Kepler-56), Techniques: radial velocities",

author = "Otor, \{Oderah Justin\} and Montet, \{Benjamin T.\} and Johnson, \{John Asher\} and David Charbonneau and \{Collier Cameron\}, Andrew and Howard, \{Andrew W.\} and Howard Isaacson and Latham, \{David W.\} and Mercedes Lopez-Morales and Christophe Lovis and Michel Mayor and Giusi Micela and Emilio Molinari and Francesco Pepe and Giampaolo Piotto and Phillips, \{David F.\} and Didier Queloz and Ken Rice and Dimitar Sasselov and Damien S{\'e}gransan and Alessandro Sozzetti and St{\'e}phane Udry and Chris Watson",

year = "2016",

month = dec,

day = "1",

doi = "10.3847/0004-6256/152/6/165",

language = "English",

volume = "152",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "6",

}

Otor, OJ, Montet, BT, Johnson, JA, Charbonneau, D, Collier Cameron, A, Howard, AW, Isaacson, H, Latham, DW, Lopez-Morales, M, Lovis, C, Mayor, M, Micela, G, Molinari, E, Pepe, F, Piotto, G, Phillips, DF, Queloz, D, Rice, K, Sasselov, D, Ségransan, D, Sozzetti, A, Udry, S & Watson, C 2016, 'The orbit and mass of the third planet in the Kepler-56 system', Astronomical Journal, vol. 152, no. 6, 165. https://doi.org/10.3847/0004-6256/152/6/165

TY - JOUR

T1 - The orbit and mass of the third planet in the Kepler-56 system

AU - Otor, Oderah Justin

AU - Montet, Benjamin T.

AU - Johnson, John Asher

AU - Charbonneau, David

AU - Collier Cameron, Andrew

AU - Howard, Andrew W.

AU - Isaacson, Howard

AU - Latham, David W.

AU - Lopez-Morales, Mercedes

AU - Lovis, Christophe

AU - Mayor, Michel

AU - Micela, Giusi

AU - Molinari, Emilio

AU - Pepe, Francesco

AU - Piotto, Giampaolo

AU - Phillips, David F.

AU - Queloz, Didier

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Ségransan, Damien

AU - Sozzetti, Alessandro

AU - Udry, Stéphane

AU - Watson, Chris

PY - 2016/12/1

Y1 - 2016/12/1

N2 - While the vast majority of multiple-planet systems have orbital angular momentum axes that align with the spin axis of their host star, Kepler-56 is an exception: its two transiting planets are coplanar yet misaligned by at least 40° with respect to the rotation axis of their host star. Additional follow-up observations of Kepler-56 suggest the presence of a massive, non-transiting companion that may help explain this misalignment. We model the transit data along with Keck/HIRES and HARPS-N radial velocity data to update the masses of the two transiting planets and infer the physical properties of the third, non-transiting planet. We employ a Markov Chain Monte Carlo sampler to calculate the best-fitting orbital parameters and their uncertainties for each planet. We find the outer planet has a period of 1002 ± 5 days and minimum mass of 5.61 ± 0.38 MJup . We also place a 95% upper limit of 0.80 m s-1 yr-1 on long-term trends caused by additional, more distant companions.

AB - While the vast majority of multiple-planet systems have orbital angular momentum axes that align with the spin axis of their host star, Kepler-56 is an exception: its two transiting planets are coplanar yet misaligned by at least 40° with respect to the rotation axis of their host star. Additional follow-up observations of Kepler-56 suggest the presence of a massive, non-transiting companion that may help explain this misalignment. We model the transit data along with Keck/HIRES and HARPS-N radial velocity data to update the masses of the two transiting planets and infer the physical properties of the third, non-transiting planet. We employ a Markov Chain Monte Carlo sampler to calculate the best-fitting orbital parameters and their uncertainties for each planet. We find the outer planet has a period of 1002 ± 5 days and minimum mass of 5.61 ± 0.38 MJup . We also place a 95% upper limit of 0.80 m s-1 yr-1 on long-term trends caused by additional, more distant companions.

KW - Planets and satellites: fundamental parameters

KW - Planets and satellites: individual (Kepler-56)

KW - Techniques: radial velocities

U2 - 10.3847/0004-6256/152/6/165

DO - 10.3847/0004-6256/152/6/165

M3 - Article

AN - SCOPUS:85009105037

SN - 0004-6256

VL - 152

JO - Astronomical Journal

JF - Astronomical Journal

IS - 6

M1 - 165

ER -

The orbit and mass of the third planet in the Kepler-56 system

Abstract

Keywords

Access to Document

Handle.net

Fingerprint

Projects

Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

EU FP7 Space ETAEARTH: ETAEARTH

Cite this