Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-29T08:42:03.016Z Has data issue: false hasContentIssue false
  • English
  • Français

Auto-Vetting Transiting Planet Candidates Identified by the Kepler Pipeline

Published online by Cambridge University Press:  29 April 2014

Jon M. Jenkins ,
Sean McCauliff ,
Christopher Burke ,
Shawn Seader ,
Joseph Twicken ,
Todd Klaus ,
Dwight Sanderfer ,
Ashok Srivastava  and
Michael R. Haas
Jon M. Jenkins
Affiliation:
SETI Institute/NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035 email: [email protected]
Sean McCauliff
Affiliation:
Orbital Sciences Corp./NASA Ames Research Center, Moffett Field, CA 94035
Christopher Burke
Affiliation:
SETI Institute/NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035 email: [email protected]
Shawn Seader
Affiliation:
SETI Institute/NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035 email: [email protected]
Joseph Twicken
Affiliation:
SETI Institute/NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035 email: [email protected]
Todd Klaus
Affiliation:
Orbital Sciences Corp./NASA Ames Research Center, Moffett Field, CA 94035
Dwight Sanderfer
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035
Ashok Srivastava
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035
Michael R. Haas
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The Kepler Mission simultaneously measures the brightness of more than 150,000 stars every 29.4 minutes primarily for the purpose of transit photometry. Over the course of its 3.5-year primary mission Kepler has observed over 190,000 distinct stars, announcing 2,321 planet candidates, 2,165 eclipsing binaries, and 105 confirmed planets. As Kepler moves into its 4-year extended mission, the total number of transit-like features identified in the light curves has increased to as many as ~18,000. This number of signals has become intractable for human beings to inspect by eye in a thorough and timely fashion. To mitigate this problem we are developing machine learning approaches to perform the task of reviewing the diagnostics for each transit signal candidate to establish a preliminary list of planetary candidates ranked from most credible to least credible. Our preliminary results indicate that random forests can classify potential transiting planet signatures with an accuracy of more than 98.6% as measured by the area under a receiver-operating curve.

Keywords

methods: data analysismethods: statisticalinstrumentation: photometers(stars:) planetary systemscatalogs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 94 - 99
Copyright
Copyright © International Astronomical Union 2014 

References

Batalha, N. M., Rowe, J. F., Bryson, S. T., et al., ApJS 204 article id. 24Google Scholar
Breiman, L., Friedman, J., Olshen, R., & Stone, C. 1984 Classification and Regression Trees. Boca Raton, FL: CRC Press.Google Scholar
Breiman, L. 2001 Machine Learning, 45, 1Google Scholar
Borucki, W. J., Koch, D. G., Basri, G., et al. 2011a, ApJ 728, 117CrossRefGoogle Scholar
Borucki, W. J., Koch, D. G., Basri, G., et al. 2011b, ApJ 736, 19CrossRefGoogle Scholar
Doyle, L. R., Carter, J. A., Fabrycky, D. C., et al. 2011 Science 333, 6049Google Scholar
Jenkins, J. M. 2002, ApJ 575, 493Google Scholar
Jenkins, J. M., Hema Chandrasekarana, H., McCauliff, S. D., et al. 2010, Proc. SPIE 7740.Google Scholar
Slawson, R. W., Prša, A., Welsh, W. F., et al. 2011, AJ, 142, 160CrossRefGoogle Scholar
Tenenbaum, P., Christiansen, Jessie L., Jenkins, J. M., et al. 2012, ApJS 199, 24CrossRefGoogle Scholar
Twicken, J. D., Wu, H., Wohler, B., et al. 2012, AAS Meeting 220, abstract #330.05.Google Scholar
Van Cleve, J. & Caldwell, D. A., 2009, Kepler Instrument Handbook, KSCI 19033-001, (Moffett Field, CA: NASA Ames Research Center)Google Scholar
Wu, H., Twicken, J. D., Tenenbaum, P.et al. 2010, Proc. SPIE, 7740, 774019CrossRefGoogle Scholar