Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets

Geoffrey W. Marcy; Howard Isaacson; Andrew W. Howard; Jason F. Rowe; Jon M. Jenkins; Stephen T. Bryson; David W. Latham; Steve B. Howell; Thomas N., III Gautier; Natalie M. Batalha; Leslie Rogers; David Ciardi; Debra A. Fischer; Ronald L. Gilliland; Hans Kjeldsen; Jørgen Christensen-Dalsgaard; Daniel Huber; William J. Chaplin; Sarbani Basu; Lars A. Buchhave; Samuel N. Quinn; William J. Borucki; David G. Koch; Roger Hunter; Douglas A. Caldwell; Jeffrey Van Cleve; Rea Kolbl; Lauren M. Weiss; Erik Petigura; Sara Seager; Timothy Morton; John Asher Johnson; Sarah Ballard; Chris Burke; William D. Cochran; Michael Endl; Phillip MacQueen; Jack J. Lissauer; Eric B. Ford; Guillermo Torres; Francois Fressin; Jason H. Steffen; David Charbonneau; Gibor S. Basri; Dimitar D. Sasselov; Joshua Winn; Roberto Sanchis-Ojeda; Jessie Christiansen; Christopher Henze; Andrea Dupree; Daniel C. Fabrycky; Jonathan J. Fortney; Jill Tarter; Matthew J. Holman; Peter Tenenbaum; Avi Shporer; Philip W. Lucas; William F. Welsh; Jerome A. Orosz; T. R. Bedding; T. L. Campante; G. R. Davies; Y. Elsworth; Rasmus Handberg; S. Hekker; C. Karoff; S. D. Kawaler; M. N. Lund; M. Lundkvist; A. Miglio; Victor Silva Aguirre; D. Stello; T. R. White; Alan Boss; Edna Devore; Andrej Prsa; Eric Agol; Erik Brugamyer; Fergal Mullally; Elisa V. Quintana; Susan E. Thompson; David Morrison; Joseph D. Twicken; Jean-Michel Désert; Josh Carter; Justin R. Crepp; Alexandre Santerne; Charlie Sobeck; Douglas Hudgins; Michael R. Haas; Paul Robertson; Jorge Lillo-Box; David Barrado

doi:10.1088/0067-0049/210/2/20

Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets

Geoffrey W. Marcy, Howard Isaacson, Andrew W. Howard, Jason F. Rowe, Jon M. Jenkins, Stephen T. Bryson, David W. Latham, Steve B. Howell, Thomas N., III Gautier, Natalie M. Batalha, Leslie Rogers, David Ciardi, Debra A. Fischer, Ronald L. Gilliland, Hans Kjeldsen, Jørgen Christensen-Dalsgaard, Daniel Huber, William J. Chaplin, Sarbani Basu, Lars A. BuchhaveSamuel N. Quinn, William J. Borucki, David G. Koch, Roger Hunter, Douglas A. Caldwell, Jeffrey Van Cleve, Rea Kolbl, Lauren M. Weiss, Erik Petigura, Sara Seager, Timothy Morton, John Asher Johnson, Sarah Ballard, Chris Burke, William D. Cochran, Michael Endl, Phillip MacQueen, Jack J. Lissauer, Eric B. Ford, Guillermo Torres, Francois Fressin, Jason H. Steffen, David Charbonneau, Gibor S. Basri, Dimitar D. Sasselov, Joshua Winn, Roberto Sanchis-Ojeda, Jessie Christiansen, Christopher Henze, Andrea Dupree, Daniel C. Fabrycky, Jonathan J. Fortney, Jill Tarter, Matthew J. Holman, Peter Tenenbaum, Avi Shporer, Philip W. Lucas, William F. Welsh, Jerome A. Orosz, T. R. Bedding, T. L. Campante, G. R. Davies, Y. Elsworth, Rasmus Handberg, S. Hekker, C. Karoff, S. D. Kawaler, M. N. Lund, M. Lundkvist, A. Miglio, Victor Silva Aguirre, D. Stello, T. R. White, Alan Boss, Edna Devore, Andrej Prsa, Eric Agol, Erik Brugamyer, Fergal Mullally, Elisa V. Quintana, Susan E. Thompson, David Morrison, Joseph D. Twicken, Jean-Michel Désert, Josh Carter, Justin R. Crepp, Alexandre Santerne, Charlie Sobeck, Douglas Hudgins, Michael R. Haas, Paul Robertson, Jorge Lillo-Box, David Barrado

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Abstract

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology.

Original language	English
Journal	Astrophysical Journal Supplement Series
Volume	210
Issue	2
Pages (from-to)	20
ISSN	1538-4365
DOIs	https://doi.org/10.1088/0067-0049/210/2/20
Publication status	Published - 1 Feb 2014

Keywords

planetary systems
planets and satellites: detection
stars: individual: Kepler-25 Kepler-37 Kepler-48 Kepler-68 Kepler-93 Kepler-94 Kepler-95 Kepler-96 Kepler-97 Kepler-98 Kepler-99 Kepler-100 Kepler-102 Kepler-103 Kepler-106 Kepler-109 Kepler-113 Kepler-131 Kepler-406 Kepler-407 Kepler-409
techniques: photometric
techniques: radial velocities

Access to Document

10.1088/0067-0049/210/2/20

http://adsabs.harvard.edu/abs/2014ApJS..210...20M

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Marcy, G. W., Isaacson, H., Howard, A. W., Rowe, J. F., Jenkins, J. M., Bryson, S. T., Latham, D. W., Howell, S. B., Gautier, T. N. . III., Batalha, N. M., Rogers, L., Ciardi, D., Fischer, D. A., Gilliland, R. L., Kjeldsen, H., Christensen-Dalsgaard, J., Huber, D., Chaplin, W. J., Basu, S., ... Barrado, D. (2014). Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets. Astrophysical Journal Supplement Series, 210(2), 20. https://doi.org/10.1088/0067-0049/210/2/20

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title = "Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets",

abstract = "We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1\%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than \textasciitilde{}2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology.",

keywords = "planetary systems, planets and satellites: detection, stars: individual: Kepler-25 Kepler-37 Kepler-48 Kepler-68 Kepler-93 Kepler-94 Kepler-95 Kepler-96 Kepler-97 Kepler-98 Kepler-99 Kepler-100 Kepler-102 Kepler-103 Kepler-106 Kepler-109 Kepler-113 Kepler-131 Kepler-406 Kepler-407 Kepler-409, techniques: photometric, techniques: radial velocities",

author = "Marcy, \{Geoffrey W.\} and Howard Isaacson and Howard, \{Andrew W.\} and Rowe, \{Jason F.\} and Jenkins, \{Jon M.\} and Bryson, \{Stephen T.\} and Latham, \{David W.\} and Howell, \{Steve B.\} and Gautier, \{Thomas N., III\} and Batalha, \{Natalie M.\} and Leslie Rogers and David Ciardi and Fischer, \{Debra A.\} and Gilliland, \{Ronald L.\} and Hans Kjeldsen and J{\o}rgen Christensen-Dalsgaard and Daniel Huber and Chaplin, \{William J.\} and Sarbani Basu and Buchhave, \{Lars A.\} and Quinn, \{Samuel N.\} and Borucki, \{William J.\} and Koch, \{David G.\} and Roger Hunter and Caldwell, \{Douglas A.\} and \{Van Cleve\}, Jeffrey and Rea Kolbl and Weiss, \{Lauren M.\} and Erik Petigura and Sara Seager and Timothy Morton and Johnson, \{John Asher\} and Sarah Ballard and Chris Burke and Cochran, \{William D.\} and Michael Endl and Phillip MacQueen and Lissauer, \{Jack J.\} and Ford, \{Eric B.\} and Guillermo Torres and Francois Fressin and Steffen, \{Jason H.\} and David Charbonneau and Basri, \{Gibor S.\} and Sasselov, \{Dimitar D.\} and Joshua Winn and Roberto Sanchis-Ojeda and Jessie Christiansen and Christopher Henze and Andrea Dupree and Fabrycky, \{Daniel C.\} and Fortney, \{Jonathan J.\} and Jill Tarter and Holman, \{Matthew J.\} and Peter Tenenbaum and Avi Shporer and Lucas, \{Philip W.\} and Welsh, \{William F.\} and Orosz, \{Jerome A.\} and Bedding, \{T. R.\} and Campante, \{T. L.\} and Davies, \{G. R.\} and Y. Elsworth and Rasmus Handberg and S. Hekker and C. Karoff and Kawaler, \{S. D.\} and Lund, \{M. N.\} and M. Lundkvist and A. Miglio and \{Silva Aguirre\}, Victor and D. Stello and White, \{T. R.\} and Alan Boss and Edna Devore and Andrej Prsa and Eric Agol and Erik Brugamyer and Fergal Mullally and Quintana, \{Elisa V.\} and Thompson, \{Susan E.\} and David Morrison and Twicken, \{Joseph D.\} and Jean-Michel D{\'e}sert and Josh Carter and Crepp, \{Justin R.\} and Alexandre Santerne and Charlie Sobeck and Douglas Hudgins and Haas, \{Michael R.\} and Paul Robertson and Jorge Lillo-Box and David Barrado",

year = "2014",

month = feb,

day = "1",

doi = "10.1088/0067-0049/210/2/20",

language = "English",

volume = "210",

pages = "20",

journal = "Astrophysical Journal Supplement Series",

issn = "1538-4365",

publisher = "Institute of Physics Publishing",

number = "2",

}

Marcy, GW, Isaacson, H, Howard, AW, Rowe, JF, Jenkins, JM, Bryson, ST, Latham, DW, Howell, SB, Gautier, TNIII, Batalha, NM, Rogers, L, Ciardi, D, Fischer, DA, Gilliland, RL, Kjeldsen, H , Christensen-Dalsgaard, J, Huber, D, Chaplin, WJ, Basu, S, Buchhave, LA, Quinn, SN, Borucki, WJ, Koch, DG, Hunter, R, Caldwell, DA, Van Cleve, J, Kolbl, R, Weiss, LM, Petigura, E, Seager, S, Morton, T, Johnson, JA, Ballard, S, Burke, C, Cochran, WD, Endl, M, MacQueen, P, Lissauer, JJ, Ford, EB, Torres, G, Fressin, F, Steffen, JH, Charbonneau, D, Basri, GS, Sasselov, DD, Winn, J, Sanchis-Ojeda, R, Christiansen, J, Henze, C, Dupree, A, Fabrycky, DC, Fortney, JJ, Tarter, J, Holman, MJ, Tenenbaum, P, Shporer, A, Lucas, PW, Welsh, WF, Orosz, JA, Bedding, TR, Campante, TL, Davies, GR, Elsworth, Y, Handberg, R, Hekker, S, Karoff, C, Kawaler, SD, Lund, MN , Lundkvist, M, Miglio, A, Silva Aguirre, V, Stello, D, White, TR, Boss, A, Devore, E, Prsa, A, Agol, E, Brugamyer, E, Mullally, F, Quintana, EV, Thompson, SE, Morrison, D, Twicken, JD, Désert, J-M, Carter, J, Crepp, JR, Santerne, A, Sobeck, C, Hudgins, D, Haas, MR, Robertson, P, Lillo-Box, J & Barrado, D 2014, 'Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets', Astrophysical Journal Supplement Series, vol. 210, no. 2, pp. 20. https://doi.org/10.1088/0067-0049/210/2/20

Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets. / Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew W. et al.
In: Astrophysical Journal Supplement Series, Vol. 210, No. 2, 01.02.2014, p. 20.

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaper › Journal article › Research › peer-review

TY - JOUR

T1 - Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets

AU - Marcy, Geoffrey W.

AU - Isaacson, Howard

AU - Howard, Andrew W.

AU - Rowe, Jason F.

AU - Jenkins, Jon M.

AU - Bryson, Stephen T.

AU - Latham, David W.

AU - Howell, Steve B.

AU - Gautier, Thomas N., III

AU - Batalha, Natalie M.

AU - Rogers, Leslie

AU - Ciardi, David

AU - Fischer, Debra A.

AU - Gilliland, Ronald L.

AU - Kjeldsen, Hans

AU - Christensen-Dalsgaard, Jørgen

AU - Huber, Daniel

AU - Chaplin, William J.

AU - Basu, Sarbani

AU - Buchhave, Lars A.

AU - Quinn, Samuel N.

AU - Borucki, William J.

AU - Koch, David G.

AU - Hunter, Roger

AU - Caldwell, Douglas A.

AU - Van Cleve, Jeffrey

AU - Kolbl, Rea

AU - Weiss, Lauren M.

AU - Petigura, Erik

AU - Seager, Sara

AU - Morton, Timothy

AU - Johnson, John Asher

AU - Ballard, Sarah

AU - Burke, Chris

AU - Cochran, William D.

AU - Endl, Michael

AU - MacQueen, Phillip

AU - Lissauer, Jack J.

AU - Ford, Eric B.

AU - Torres, Guillermo

AU - Fressin, Francois

AU - Steffen, Jason H.

AU - Charbonneau, David

AU - Basri, Gibor S.

AU - Sasselov, Dimitar D.

AU - Winn, Joshua

AU - Sanchis-Ojeda, Roberto

AU - Christiansen, Jessie

AU - Henze, Christopher

AU - Dupree, Andrea

AU - Fabrycky, Daniel C.

AU - Fortney, Jonathan J.

AU - Tarter, Jill

AU - Holman, Matthew J.

AU - Tenenbaum, Peter

AU - Shporer, Avi

AU - Lucas, Philip W.

AU - Welsh, William F.

AU - Orosz, Jerome A.

AU - Bedding, T. R.

AU - Campante, T. L.

AU - Davies, G. R.

AU - Elsworth, Y.

AU - Handberg, Rasmus

AU - Hekker, S.

AU - Karoff, C.

AU - Kawaler, S. D.

AU - Lund, M. N.

AU - Lundkvist, M.

AU - Miglio, A.

AU - Silva Aguirre, Victor

AU - Stello, D.

AU - White, T. R.

AU - Boss, Alan

AU - Devore, Edna

AU - Prsa, Andrej

AU - Agol, Eric

AU - Brugamyer, Erik

AU - Mullally, Fergal

AU - Quintana, Elisa V.

AU - Thompson, Susan E.

AU - Morrison, David

AU - Twicken, Joseph D.

AU - Désert, Jean-Michel

AU - Carter, Josh

AU - Crepp, Justin R.

AU - Santerne, Alexandre

AU - Sobeck, Charlie

AU - Hudgins, Douglas

AU - Haas, Michael R.

AU - Robertson, Paul

AU - Lillo-Box, Jorge

AU - Barrado, David

PY - 2014/2/1

Y1 - 2014/2/1

N2 - We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology.

AB - We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology.

KW - planetary systems

KW - planets and satellites: detection

KW - stars: individual: Kepler-25 Kepler-37 Kepler-48 Kepler-68 Kepler-93 Kepler-94 Kepler-95 Kepler-96 Kepler-97 Kepler-98 Kepler-99 Kepler-100 Kepler-102 Kepler-103 Kepler-106 Kepler-109 Kepler-113 Kepler-131 Kepler-406 Kepler-407 Kepler-409

KW - techniques: photometric

KW - techniques: radial velocities

U2 - 10.1088/0067-0049/210/2/20

DO - 10.1088/0067-0049/210/2/20

M3 - Journal article

SN - 1538-4365

VL - 210

SP - 20

JO - Astrophysical Journal Supplement Series

JF - Astrophysical Journal Supplement Series

IS - 2

ER -

Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets

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Keywords

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