The Neptune-sized circumbinary planet kepler-38b

Jerome A. Orosz; William F. Welsh; Joshua A. Carter; Erik Brugamyer; Lars A. Buchhave; William D. Cochran; Michael Endl; Eric B. Ford; Phillip MacQueen; Donald R. Short; Guillermo Torres; Gur Windmiller; Eric Agol; Thomas Barclay; Douglas A. Caldwell; Bruce D. Clarke; Laurance R. Doyle; Daniel C. Fabrycky; John C. Geary; Nader Haghighipour; Matthew J. Holman; Khadeejah A. Ibrahim; Jon M. Jenkins; Karen Kinemuchi; Jie Li; Jack J. Lissauer; Andrej Prša; Darin Ragozzine; Avi Shporer; Martin Still; Richard A. Wade

doi:10.1088/0004-637X/758/2/87

The Neptune-sized circumbinary planet kepler-38b

Jerome A. Orosz, William F. Welsh, Joshua A. Carter, Erik Brugamyer, Lars A. Buchhave, William D. Cochran, Michael Endl, Eric B. Ford, Phillip MacQueen, Donald R. Short, Guillermo Torres, Gur Windmiller, Eric Agol, Thomas Barclay, Douglas A. Caldwell, Bruce D. Clarke, Laurance R. Doyle, Daniel C. Fabrycky, John C. Geary, Nader HaghighipourMatthew J. Holman, Khadeejah A. Ibrahim, Jon M. Jenkins, Karen Kinemuchi, Jie Li, Jack J. Lissauer, Andrej Prša, Darin Ragozzine, Avi Shporer, Martin Still, Richard A. Wade

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Abstract

We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8days, and consists of a moderately evolved main-sequence star (M_A = 0.949 ± 0.059 M _⊙ and R_A = 1.757 ± 0.034 R _⊙) paired with a low-mass star (M_B = 0.249 ± 0.010 M _⊙ and R_B = 0.2724 ± 0.0053 R _⊙) in a mildly eccentric (e = 0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1-11), from which a planetary period of 105.595 ± 0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35 ± 0.11 R _⊕, or equivalently 1.12 ± 0.03 R _Nep. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 M _⊕ (7.11 M _Nep or equivalently 0.384 M _Jup) at 95% confidence. This upper limit should decrease as more Kepler data become available.

Original language	English (US)
Article number	87
Journal	Astrophysical Journal
Volume	758
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/758/2/87
State	Published - Oct 20 2012

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/758/2/87

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Orosz, J. A., Welsh, W. F., Carter, J. A., Brugamyer, E., Buchhave, L. A., Cochran, W. D., Endl, M., Ford, E. B., MacQueen, P., Short, D. R., Torres, G., Windmiller, G., Agol, E., Barclay, T., Caldwell, D. A., Clarke, B. D., Doyle, L. R., Fabrycky, D. C., Geary, J. C., ... Wade, R. A. (2012). The Neptune-sized circumbinary planet kepler-38b. Astrophysical Journal, 758(2), Article 87. https://doi.org/10.1088/0004-637X/758/2/87

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title = "The Neptune-sized circumbinary planet kepler-38b",

abstract = "We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8days, and consists of a moderately evolved main-sequence star (MA = 0.949 ± 0.059 M ⊙ and RA = 1.757 ± 0.034 R ⊙) paired with a low-mass star (MB = 0.249 ± 0.010 M ⊙ and RB = 0.2724 ± 0.0053 R ⊙) in a mildly eccentric (e = 0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1-11), from which a planetary period of 105.595 ± 0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35 ± 0.11 R ⊕, or equivalently 1.12 ± 0.03 R Nep. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 M ⊕ (7.11 M Nep or equivalently 0.384 M Jup) at 95% confidence. This upper limit should decrease as more Kepler data become available.",

author = "Orosz, {Jerome A.} and Welsh, {William F.} and Carter, {Joshua A.} and Erik Brugamyer and Buchhave, {Lars A.} and Cochran, {William D.} and Michael Endl and Ford, {Eric B.} and Phillip MacQueen and Short, {Donald R.} and Guillermo Torres and Gur Windmiller and Eric Agol and Thomas Barclay and Caldwell, {Douglas A.} and Clarke, {Bruce D.} and Doyle, {Laurance R.} and Fabrycky, {Daniel C.} and Geary, {John C.} and Nader Haghighipour and Holman, {Matthew J.} and Ibrahim, {Khadeejah A.} and Jenkins, {Jon M.} and Karen Kinemuchi and Jie Li and Lissauer, {Jack J.} and Andrej Pr{\v s}a and Darin Ragozzine and Avi Shporer and Martin Still and Wade, {Richard A.}",

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doi = "10.1088/0004-637X/758/2/87",

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Orosz, JA, Welsh, WF, Carter, JA, Brugamyer, E, Buchhave, LA, Cochran, WD, Endl, M, Ford, EB, MacQueen, P, Short, DR, Torres, G, Windmiller, G, Agol, E, Barclay, T, Caldwell, DA, Clarke, BD, Doyle, LR, Fabrycky, DC, Geary, JC, Haghighipour, N, Holman, MJ, Ibrahim, KA, Jenkins, JM, Kinemuchi, K, Li, J, Lissauer, JJ, Prša, A, Ragozzine, D, Shporer, A, Still, M & Wade, RA 2012, 'The Neptune-sized circumbinary planet kepler-38b', Astrophysical Journal, vol. 758, no. 2, 87. https://doi.org/10.1088/0004-637X/758/2/87

TY - JOUR

T1 - The Neptune-sized circumbinary planet kepler-38b

AU - Orosz, Jerome A.

AU - Welsh, William F.

AU - Carter, Joshua A.

AU - Brugamyer, Erik

AU - Buchhave, Lars A.

AU - Cochran, William D.

AU - Endl, Michael

AU - Ford, Eric B.

AU - MacQueen, Phillip

AU - Short, Donald R.

AU - Torres, Guillermo

AU - Windmiller, Gur

AU - Agol, Eric

AU - Barclay, Thomas

AU - Caldwell, Douglas A.

AU - Clarke, Bruce D.

AU - Doyle, Laurance R.

AU - Fabrycky, Daniel C.

AU - Geary, John C.

AU - Haghighipour, Nader

AU - Holman, Matthew J.

AU - Ibrahim, Khadeejah A.

AU - Jenkins, Jon M.

AU - Kinemuchi, Karen

AU - Li, Jie

AU - Lissauer, Jack J.

AU - Prša, Andrej

AU - Ragozzine, Darin

AU - Shporer, Avi

AU - Still, Martin

AU - Wade, Richard A.

PY - 2012/10/20

Y1 - 2012/10/20

N2 - We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8days, and consists of a moderately evolved main-sequence star (MA = 0.949 ± 0.059 M ⊙ and RA = 1.757 ± 0.034 R ⊙) paired with a low-mass star (MB = 0.249 ± 0.010 M ⊙ and RB = 0.2724 ± 0.0053 R ⊙) in a mildly eccentric (e = 0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1-11), from which a planetary period of 105.595 ± 0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35 ± 0.11 R ⊕, or equivalently 1.12 ± 0.03 R Nep. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 M ⊕ (7.11 M Nep or equivalently 0.384 M Jup) at 95% confidence. This upper limit should decrease as more Kepler data become available.

AB - We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8days, and consists of a moderately evolved main-sequence star (MA = 0.949 ± 0.059 M ⊙ and RA = 1.757 ± 0.034 R ⊙) paired with a low-mass star (MB = 0.249 ± 0.010 M ⊙ and RB = 0.2724 ± 0.0053 R ⊙) in a mildly eccentric (e = 0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1-11), from which a planetary period of 105.595 ± 0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35 ± 0.11 R ⊕, or equivalently 1.12 ± 0.03 R Nep. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 M ⊕ (7.11 M Nep or equivalently 0.384 M Jup) at 95% confidence. This upper limit should decrease as more Kepler data become available.

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U2 - 10.1088/0004-637X/758/2/87

DO - 10.1088/0004-637X/758/2/87

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SN - 0004-637X

VL - 758

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 87

ER -

The Neptune-sized circumbinary planet kepler-38b

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