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Cited by 228

The DOI matches its Crossref record; 5 of the 5 references it cites were found in a registry or an index.

PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1-Q8 (22 MONTHS)

Open access
Burke, Christopher J., Bryson, Stephen T., Mullally, F., Rowe, Jason F., Christiansen, Jessie L., Thompson, Susan E., Coughlin, Jeffrey L., Haas, Michael R., Batalha, Natalie M., Caldwell, Douglas A., Jenkins, Jon M., Still, Martin, Barclay, Thomas, Borucki, William J., Chaplin, William J., Ciardi, David R., Clarke, Bruce D., Cochran, William D., Demory, Brice-Olivier, Esquerdo, Gilbert A., Gautier, Thomas N., Gilliland, Ronald L., Girouard, Forrest R., Havel, Mathieu, Henze, Christopher E., Howell, Steve B., Huber, Daniel, Latham, David W., Li, Jie, Morehead, Robert C., Morton, Timothy D., Pepper, Joshua, Quintana, Elisa, Ragozzine, Darin, Seader, Shawn E., Shah, Yash, Shporer, Avi, Tenenbaum, Peter, Twicken, Joseph D., Wolfgang, Angie·2014·The Astrophysical Journal Supplement Series

Abstract

We provide updates to the Kepler planet candidate sample based upon nearly two years of high-precision photometry (i.e., Q1–Q8). From an initial list of nearly 13,400 threshold crossing events, 480 new host stars are identified from their flux time series as consistent with hosting transiting planets. Potential transit signals are subjected to further analysis using the pixel-level data, which allows background eclipsing binaries to be identified through small image position shifts during transit. We also re-evaluate Kepler Objects of Interest (KOIs) 1-1609, which were identified early in the mission, using substantially more data to test for background false positives and to find additional multiple systems. Combining the new and previous KOI samples, we provide updated parameters for 2738 Kepler planet candidates distributed across 2017 host stars. From the combined Kepler planet candidates, 472 are new from the Q1–Q8 data examined in this study. The new Kepler planet candidates represent ∼40% of the sample with R P ∼ 1 R ⊕ and represent ∼40% of the low equilibrium temperature ( T eq < 300 K) sample. We review the known biases in the current sample of Kepler planet candidates relevant to evaluating planet population statistics with the current Kepler planet candidate sample.

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Metadata

Authors
Burke, C. J., Bryson, S. T., Mullally, F., Rowe, J. F., Christiansen, J. L., Thompson, S. E., Coughlin, J. L., Haas, M. R., Batalha, N. M., Caldwell, D. A., Jenkins, J. M., Still, M., Barclay, T., Borucki, W. J., Chaplin, W. J., Ciardi, D. R., Clarke, B. D., Cochran, W. D., Demory, B.-O., Esquerdo, G. A., Gautier, T. N., Gilliland, R. L., Girouard, F. R., Havel, M., Henze, C. E., Howell, S. B., Huber, D., Latham, D. W., Li, J., Morehead, R. C., Morton, T. D., Pepper, J., Quintana, E., Ragozzine, D., Seader, S. E., Shah, Y., Shporer, A., Tenenbaum, P., Twicken, J. D., & Wolfgang, A.
Venue
The Astrophysical Journal Supplement Series
Published
2014-01-10
Volume
210
Issue
2
Pages
19
ISSN
  • 0067-0049 (ISSN-L)
  • 1538-4365
OpenAlex
W4231351050
Cited by
228
References
5
FWCI
27.65
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1-Q8 (22 MONTHS). https://app.cochat.ai/papers/10.1088/0067-0049/210/2/19
The paper
Burke, C. J., Bryson, S. T., Mullally, F., Rowe, J. F., Christiansen, J. L., Thompson, S. E., Coughlin, J. L., Haas, M. R., Batalha, N. M., Caldwell, D. A., Jenkins, J. M., Still, M., Barclay, T., Borucki, W. J., Chaplin, W. J., Ciardi, D. R., Clarke, B. D., Cochran, W. D., Demory, B.-O., . . . Wolfgang, A. (2014). PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1-Q8 (22 MONTHS). The Astrophysical Journal Supplement Series. https://doi.org/10.1088/0067-0049/210/2/19

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.