Validation of small Kepler transiting planet candidates in or near the habitable zone

Guillermo Torres; Stephen R. Kane; Jason F. Rowe; Natalie M. Batalha; Christopher E. Henze; David R. Ciardi; Thomas Barclay; William J. Borucki; Lars A. Buchhave; Justin R. Crepp; Mark E. Everett; Elliott P. Horch; Andrew W. Howard; Steve B. Howell; Howard T. Isaacson; Jon M. Jenkins; David W. Latham; Erik A. Petigura; Elisa V. Quintana

doi:10.3847/1538-3881/aa984b

Validation of small Kepler transiting planet candidates in or near the habitable zone

Guillermo Torres, Stephen R. Kane, Jason F. Rowe, Natalie M. Batalha, Christopher E. Henze, David R. Ciardi, Thomas Barclay, William J. Borucki, Lars A. Buchhave, Justin R. Crepp, Mark E. Everett, Elliott P. Horch, Andrew W. Howard, Steve B. Howell, Howard T. Isaacson, Jon M. Jenkins, David W. Latham, Erik A. Petigura, Elisa V. Quintana

Astrophysics and Planetary Science

9 Citations (Scopus)

Abstract

A main goal of NASA's Kepler Mission is to establish the frequency of potentially habitable Earth-size planets (). Relatively few such candidates identified by the mission can be confirmed to be rocky via dynamical measurement of their mass. Here we report an effort to validate 18 of them statistically using the BLENDER technique, by showing that the likelihood they are true planets is far greater than that of a false positive. Our analysis incorporates follow-up observations including high-resolution optical and near-infrared spectroscopy, high-resolution imaging, and information from the analysis of the flux centroids of the Kepler observations themselves. Although many of these candidates have been previously validated by others, the confidence levels reported typically ignore the possibility that the planet may transit a star different from the target along the same line of sight. If that were the case, a planet that appears small enough to be rocky may actually be considerably larger and therefore less interesting from the point of view of habitability. We take this into consideration here and are able to validate 15 of our candidates at a 99.73% (3σ) significance level or higher, and the other three at a slightly lower confidence. We characterize the GKM host stars using available ground-based observations and provide updated parameters for the planets, with sizes between 0.8 and 2.9 R _⊕. Seven of them (KOI-0438.02, 0463.01, 2418.01, 2626.01, 3282.01, 4036.01, and 5856.01) have a better than 50% chance of being smaller than 2 R _⊕ and being in the habitable zone of their host stars.

Original language	English
Article number	264
Journal	The Astronomical Journal
Volume	154
Issue number	6
Number of pages	19
ISSN	0004-6256
DOIs	https://doi.org/10.3847/1538-3881/aa984b
Publication status	Published - 1 Dec 2017

Keywords

methods: statistical
planetary systems
stars: individual (KOI-0172.02 = Kepler-69c ...)
techniques: photometric

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10.3847/1538-3881/aa984b

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Torres, G., Kane, S. R., Rowe, J. F., Batalha, N. M., Henze, C. E., Ciardi, D. R., Barclay, T., Borucki, W. J., Buchhave, L. A., Crepp, J. R., Everett, M. E., Horch, E. P., Howard, A. W., Howell, S. B., Isaacson, H. T., Jenkins, J. M., Latham, D. W., Petigura, E. A., & Quintana, E. V. (2017). Validation of small Kepler transiting planet candidates in or near the habitable zone. The Astronomical Journal, 154(6), Article 264. https://doi.org/10.3847/1538-3881/aa984b

Torres, G, Kane, SR, Rowe, JF, Batalha, NM, Henze, CE, Ciardi, DR, Barclay, T, Borucki, WJ, Buchhave, LA, Crepp, JR, Everett, ME, Horch, EP, Howard, AW, Howell, SB, Isaacson, HT, Jenkins, JM, Latham, DW, Petigura, EA & Quintana, EV 2017, 'Validation of small Kepler transiting planet candidates in or near the habitable zone', The Astronomical Journal, vol. 154, no. 6, 264. https://doi.org/10.3847/1538-3881/aa984b

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abstract = "A main goal of NASA's Kepler Mission is to establish the frequency of potentially habitable Earth-size planets (). Relatively few such candidates identified by the mission can be confirmed to be rocky via dynamical measurement of their mass. Here we report an effort to validate 18 of them statistically using the BLENDER technique, by showing that the likelihood they are true planets is far greater than that of a false positive. Our analysis incorporates follow-up observations including high-resolution optical and near-infrared spectroscopy, high-resolution imaging, and information from the analysis of the flux centroids of the Kepler observations themselves. Although many of these candidates have been previously validated by others, the confidence levels reported typically ignore the possibility that the planet may transit a star different from the target along the same line of sight. If that were the case, a planet that appears small enough to be rocky may actually be considerably larger and therefore less interesting from the point of view of habitability. We take this into consideration here and are able to validate 15 of our candidates at a 99.73% (3σ) significance level or higher, and the other three at a slightly lower confidence. We characterize the GKM host stars using available ground-based observations and provide updated parameters for the planets, with sizes between 0.8 and 2.9 R ⊕. Seven of them (KOI-0438.02, 0463.01, 2418.01, 2626.01, 3282.01, 4036.01, and 5856.01) have a better than 50% chance of being smaller than 2 R ⊕ and being in the habitable zone of their host stars.",

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AU - Batalha, Natalie M.

AU - Henze, Christopher E.

AU - Ciardi, David R.

AU - Barclay, Thomas

AU - Borucki, William J.

AU - Buchhave, Lars A.

AU - Crepp, Justin R.

AU - Everett, Mark E.

AU - Horch, Elliott P.

AU - Howard, Andrew W.

AU - Howell, Steve B.

AU - Isaacson, Howard T.

AU - Jenkins, Jon M.

AU - Latham, David W.

AU - Petigura, Erik A.

AU - Quintana, Elisa V.

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N2 - A main goal of NASA's Kepler Mission is to establish the frequency of potentially habitable Earth-size planets (). Relatively few such candidates identified by the mission can be confirmed to be rocky via dynamical measurement of their mass. Here we report an effort to validate 18 of them statistically using the BLENDER technique, by showing that the likelihood they are true planets is far greater than that of a false positive. Our analysis incorporates follow-up observations including high-resolution optical and near-infrared spectroscopy, high-resolution imaging, and information from the analysis of the flux centroids of the Kepler observations themselves. Although many of these candidates have been previously validated by others, the confidence levels reported typically ignore the possibility that the planet may transit a star different from the target along the same line of sight. If that were the case, a planet that appears small enough to be rocky may actually be considerably larger and therefore less interesting from the point of view of habitability. We take this into consideration here and are able to validate 15 of our candidates at a 99.73% (3σ) significance level or higher, and the other three at a slightly lower confidence. We characterize the GKM host stars using available ground-based observations and provide updated parameters for the planets, with sizes between 0.8 and 2.9 R ⊕. Seven of them (KOI-0438.02, 0463.01, 2418.01, 2626.01, 3282.01, 4036.01, and 5856.01) have a better than 50% chance of being smaller than 2 R ⊕ and being in the habitable zone of their host stars.

AB - A main goal of NASA's Kepler Mission is to establish the frequency of potentially habitable Earth-size planets (). Relatively few such candidates identified by the mission can be confirmed to be rocky via dynamical measurement of their mass. Here we report an effort to validate 18 of them statistically using the BLENDER technique, by showing that the likelihood they are true planets is far greater than that of a false positive. Our analysis incorporates follow-up observations including high-resolution optical and near-infrared spectroscopy, high-resolution imaging, and information from the analysis of the flux centroids of the Kepler observations themselves. Although many of these candidates have been previously validated by others, the confidence levels reported typically ignore the possibility that the planet may transit a star different from the target along the same line of sight. If that were the case, a planet that appears small enough to be rocky may actually be considerably larger and therefore less interesting from the point of view of habitability. We take this into consideration here and are able to validate 15 of our candidates at a 99.73% (3σ) significance level or higher, and the other three at a slightly lower confidence. We characterize the GKM host stars using available ground-based observations and provide updated parameters for the planets, with sizes between 0.8 and 2.9 R ⊕. Seven of them (KOI-0438.02, 0463.01, 2418.01, 2626.01, 3282.01, 4036.01, and 5856.01) have a better than 50% chance of being smaller than 2 R ⊕ and being in the habitable zone of their host stars.

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KW - planetary systems

KW - stars: individual (KOI-0172.02 = Kepler-69c ...)

KW - techniques: photometric

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Validation of small Kepler transiting planet candidates in or near the habitable zone

Abstract

Keywords

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