Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data

Natalie M. Batalha; Jason F. Rowe; Stephen T. Bryson; Thomas Barclay; Christopher J. Burke; Douglas A. Caldwell; Jessie L. Christiansen; Fergal Mullally; Susan E. Thompson; Timothy M. Brown; Andrea K. Dupree; Daniel C. Fabrycky; Eric B. Ford; Jonathan J. Fortney; Ronald L. Gilliland; Howard Isaacson; David W. Latham; Geoffrey W. Marcy; Samuel N. Quinn; Darin Ragozzine; Avi Shporer; William J. Borucki; David R. Ciardi; Thomas N. Gautier; Michael R. Haas; Jon M. Jenkins; David G. Koch; Jack J. Lissauer; William Rapin; Gibor S. Basri; Alan P. Boss; Lars A. Buchhave; Joshua A. Carter; David Charbonneau; Jørgen Christensen-Dalsgaard; Bruce D. Clarke; William D. Cochran; Brice-Olivier Demory; Jean-Michel Desert; Edna Devore; Laurance R. Doyle; Gilbert A. Esquerdo; Mark Everett; Francois Fressin; John C. Geary; Forrest R. Girouard; Alan Gould; Jennifer R. Hall; Matthew J. Holman; Andrew W. Howard; Steve B. Howell; Khadeejah A. Ibrahim; Karen Kinemuchi; Hans Kjeldsen; Todd C. Klaus; Jie Li; Philip W. Lucas; Søren Meibom; Robert L. Morris; Andrej Prša; Elisa Quintana; Dwight T. Sanderfer; Dimitar Sasselov; Shawn E. Seader; Jeffrey C. Smith; Jason H. Steffen; Martin Still; Martin C. Stumpe; Jill C. Tarter; Peter Tenenbaum; Guillermo Torres; Joseph D. Twicken; Kamal Uddin; Jeffrey van Cleve; Lucianne Walkowicz; William F. Welsh

doi:10.1088/0067-0049/204/2/24

Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data

Natalie M. Batalha, Jason F. Rowe, Stephen T. Bryson, Thomas Barclay, Christopher J. Burke, Douglas A. Caldwell, Jessie L. Christiansen, Fergal Mullally, Susan E. Thompson, Timothy M. Brown, Andrea K. Dupree, Daniel C. Fabrycky, Eric B. Ford, Jonathan J. Fortney, Ronald L. Gilliland, Howard Isaacson, David W. Latham, Geoffrey W. Marcy, Samuel N. Quinn, Darin RagozzineAvi Shporer, William J. Borucki, David R. Ciardi, Thomas N. Gautier, Michael R. Haas, Jon M. Jenkins, David G. Koch, Jack J. Lissauer, William Rapin, Gibor S. Basri, Alan P. Boss, Lars A. Buchhave, Joshua A. Carter, David Charbonneau, Jørgen Christensen-Dalsgaard, Bruce D. Clarke, William D. Cochran, Brice-Olivier Demory, Jean-Michel Desert, Edna Devore, Laurance R. Doyle, Gilbert A. Esquerdo, Mark Everett, Francois Fressin, John C. Geary, Forrest R. Girouard, Alan Gould, Jennifer R. Hall, Matthew J. Holman, Andrew W. Howard, Steve B. Howell, Khadeejah A. Ibrahim, Karen Kinemuchi, Hans Kjeldsen, Todd C. Klaus, Jie Li, Philip W. Lucas, Søren Meibom, Robert L. Morris, Andrej Prša, Elisa Quintana, Dwight T. Sanderfer, Dimitar Sasselov, Shawn E. Seader, Jeffrey C. Smith, Jason H. Steffen, Martin Still, Martin C. Stumpe, Jill C. Tarter, Peter Tenenbaum, Guillermo Torres, Joseph D. Twicken, Kamal Uddin, Jeffrey van Cleve, Lucianne Walkowicz, William F. Welsh

Astrophysics and Planetary Science

694 Citations (Scopus)

Abstract

New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T ₀, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R _P/R*), reduced semimajor axis (d/R *), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2 R⊕ compared to 53% for candidates larger than 2 R⊕) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant.

Original language	English
Article number	24
Journal	Astrophysical Journal Supplement Series
Volume	204
Issue number	2
Number of pages	21
ISSN	0067-0049
DOIs	https://doi.org/10.1088/0067-0049/204/2/24
Publication status	Published - 1 Feb 2013

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Batalha, N. M., Rowe, J. F., Bryson, S. T., Barclay, T., Burke, C. J., Caldwell, D. A., Christiansen, J. L., Mullally, F., Thompson, S. E., Brown, T. M., Dupree, A. K., Fabrycky, D. C., Ford, E. B., Fortney, J. J., Gilliland, R. L., Isaacson, H., Latham, D. W., Marcy, G. W., Quinn, S. N., ... Welsh, W. F. (2013). Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data. Astrophysical Journal Supplement Series, 204(2), [24]. https://doi.org/10.1088/0067-0049/204/2/24

Batalha, NM, Rowe, JF, Bryson, ST, Barclay, T, Burke, CJ, Caldwell, DA, Christiansen, JL, Mullally, F, Thompson, SE, Brown, TM, Dupree, AK, Fabrycky, DC, Ford, EB, Fortney, JJ, Gilliland, RL, Isaacson, H, Latham, DW, Marcy, GW, Quinn, SN, Ragozzine, D, Shporer, A, Borucki, WJ, Ciardi, DR, Gautier, TN, Haas, MR, Jenkins, JM, Koch, DG, Lissauer, JJ, Rapin, W, Basri, GS, Boss, AP, Buchhave, LA, Carter, JA, Charbonneau, D, Christensen-Dalsgaard, J, Clarke, BD, Cochran, WD, Demory, B-O, Desert, J-M, Devore, E, Doyle, LR, Esquerdo, GA, Everett, M, Fressin, F, Geary, JC, Girouard, FR, Gould, A, Hall, JR, Holman, MJ, Howard, AW, Howell, SB, Ibrahim, KA, Kinemuchi, K, Kjeldsen, H, Klaus, TC, Li, J, Lucas, PW, Meibom, S, Morris, RL, Prša, A, Quintana, E, Sanderfer, DT, Sasselov, D, Seader, SE, Smith, JC, Steffen, JH, Still, M, Stumpe, MC, Tarter, JC, Tenenbaum, P, Torres, G, Twicken, JD, Uddin, K, van Cleve, J, Walkowicz, L & Welsh, WF 2013, 'Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data', Astrophysical Journal Supplement Series, vol. 204, no. 2, 24. https://doi.org/10.1088/0067-0049/204/2/24

@article{14d0d2accc5b493a8560c288092c2c3e,

title = "Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data",

abstract = "New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T 0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R P/R*), reduced semimajor axis (d/R *), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2 R⊕ compared to 53% for candidates larger than 2 R⊕) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant.",

author = "Batalha, {Natalie M.} and Rowe, {Jason F.} and Bryson, {Stephen T.} and Thomas Barclay and Burke, {Christopher J.} and Caldwell, {Douglas A.} and Christiansen, {Jessie L.} and Fergal Mullally and Thompson, {Susan E.} and Brown, {Timothy M.} and Dupree, {Andrea K.} and Fabrycky, {Daniel C.} and Ford, {Eric B.} and Fortney, {Jonathan J.} and Gilliland, {Ronald L.} and Howard Isaacson and Latham, {David W.} and Marcy, {Geoffrey W.} and Quinn, {Samuel N.} and Darin Ragozzine and Avi Shporer and Borucki, {William J.} and Ciardi, {David R.} and Gautier, {Thomas N.} and Haas, {Michael R.} and Jenkins, {Jon M.} and Koch, {David G.} and Lissauer, {Jack J.} and William Rapin and Basri, {Gibor S.} and Boss, {Alan P.} and Buchhave, {Lars A.} and Carter, {Joshua A.} and David Charbonneau and J{\o}rgen Christensen-Dalsgaard and Clarke, {Bruce D.} and Cochran, {William D.} and Brice-Olivier Demory and Jean-Michel Desert and Edna Devore and Doyle, {Laurance R.} and Esquerdo, {Gilbert A.} and Mark Everett and Francois Fressin and Geary, {John C.} and Girouard, {Forrest R.} and Alan Gould and Hall, {Jennifer R.} and Holman, {Matthew J.} and Howard, {Andrew W.} and Howell, {Steve B.} and Ibrahim, {Khadeejah A.} and Karen Kinemuchi and Hans Kjeldsen and Klaus, {Todd C.} and Jie Li and Lucas, {Philip W.} and S{\o}ren Meibom and Morris, {Robert L.} and Andrej Pr{\v s}a and Elisa Quintana and Sanderfer, {Dwight T.} and Dimitar Sasselov and Seader, {Shawn E.} and Smith, {Jeffrey C.} and Steffen, {Jason H.} and Martin Still and Stumpe, {Martin C.} and Tarter, {Jill C.} and Peter Tenenbaum and Guillermo Torres and Twicken, {Joseph D.} and Kamal Uddin and {van Cleve}, Jeffrey and Lucianne Walkowicz and Welsh, {William F.}",

year = "2013",

month = feb,

day = "1",

doi = "10.1088/0067-0049/204/2/24",

language = "English",

volume = "204",

journal = "Astrophysical Journal, Supplement Series",

issn = "0067-0049",

publisher = "Institute of Physics Publishing, Inc",

number = "2",

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TY - JOUR

T1 - Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data

AU - Batalha, Natalie M.

AU - Rowe, Jason F.

AU - Bryson, Stephen T.

AU - Barclay, Thomas

AU - Burke, Christopher J.

AU - Caldwell, Douglas A.

AU - Christiansen, Jessie L.

AU - Mullally, Fergal

AU - Thompson, Susan E.

AU - Brown, Timothy M.

AU - Dupree, Andrea K.

AU - Fabrycky, Daniel C.

AU - Ford, Eric B.

AU - Fortney, Jonathan J.

AU - Gilliland, Ronald L.

AU - Isaacson, Howard

AU - Latham, David W.

AU - Marcy, Geoffrey W.

AU - Quinn, Samuel N.

AU - Ragozzine, Darin

AU - Shporer, Avi

AU - Borucki, William J.

AU - Ciardi, David R.

AU - Gautier, Thomas N.

AU - Haas, Michael R.

AU - Jenkins, Jon M.

AU - Koch, David G.

AU - Lissauer, Jack J.

AU - Rapin, William

AU - Basri, Gibor S.

AU - Boss, Alan P.

AU - Buchhave, Lars A.

AU - Carter, Joshua A.

AU - Charbonneau, David

AU - Christensen-Dalsgaard, Jørgen

AU - Clarke, Bruce D.

AU - Cochran, William D.

AU - Demory, Brice-Olivier

AU - Desert, Jean-Michel

AU - Devore, Edna

AU - Doyle, Laurance R.

AU - Esquerdo, Gilbert A.

AU - Everett, Mark

AU - Fressin, Francois

AU - Geary, John C.

AU - Girouard, Forrest R.

AU - Gould, Alan

AU - Hall, Jennifer R.

AU - Holman, Matthew J.

AU - Howard, Andrew W.

AU - Howell, Steve B.

AU - Ibrahim, Khadeejah A.

AU - Kinemuchi, Karen

AU - Kjeldsen, Hans

AU - Klaus, Todd C.

AU - Li, Jie

AU - Lucas, Philip W.

AU - Meibom, Søren

AU - Morris, Robert L.

AU - Prša, Andrej

AU - Quintana, Elisa

AU - Sanderfer, Dwight T.

AU - Sasselov, Dimitar

AU - Seader, Shawn E.

AU - Smith, Jeffrey C.

AU - Steffen, Jason H.

AU - Still, Martin

AU - Stumpe, Martin C.

AU - Tarter, Jill C.

AU - Tenenbaum, Peter

AU - Torres, Guillermo

AU - Twicken, Joseph D.

AU - Uddin, Kamal

AU - van Cleve, Jeffrey

AU - Walkowicz, Lucianne

AU - Welsh, William F.

PY - 2013/2/1

Y1 - 2013/2/1

N2 - New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T 0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R P/R*), reduced semimajor axis (d/R *), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2 R⊕ compared to 53% for candidates larger than 2 R⊕) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant.

AB - New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T 0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R P/R*), reduced semimajor axis (d/R *), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2 R⊕ compared to 53% for candidates larger than 2 R⊕) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant.

U2 - 10.1088/0067-0049/204/2/24

DO - 10.1088/0067-0049/204/2/24

M3 - Journal article

SN - 0067-0049

VL - 204

JO - Astrophysical Journal, Supplement Series

JF - Astrophysical Journal, Supplement Series

IS - 2

M1 - 24

ER -

Planetary candidates observed by Kepler. III. Analysis of the first 16 months of data

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