EXONEST: The Exoplanetary Explorer
Multiple Star Systems
Exoplanet Orbit Viewer
Kepler Data Viewer
UNL Radial Velocity Simulator
Exoplanet Exploration (top)
The fields of astronomy and astrophysics are presently engaged in an unprecedented era of discovery as recent missions, such as NASA’s Kepler mission, have produced data sets that are revealing the presence of thousands of planets orbiting other stars. As of May 2014, PlanetQuest indicates that over 4600 exoplanet candidates have been detected mostly by relying on the transit method. The transit method aims to detect planets that eclipse their host stars with respect to our point of view on Earth. We are working to develop methods that detect more subtle photometric effects that will extend the both detection and characterization capabilities. These methods will be developed to extend the capabilities of future missions as well, such as NASA's K2 Mission, which came online in June 2014, and the Transiting Exoplanet Survey Satellite (TESS) to be launched in 2017.
Photometric Effects (top)
Transiting Kepler and CoRoT exoplanets have been observed to exhibit photometric variations not associated with the transiting events. Such variations are due to numerous effects such as: reflected light and thermal emission (Seager et al. 2000; Jenkins and Doyle, 2003; Brown, 2009; Snellen, 2009; Cowan and Agol, 2011; Knuth, Placek, Richards 2012; Placek, Knuth, Angerhausen, 2014; Placek & Knuth, 2014), tidal distortion of the host star and Doppler beaming or boosting of starlight due to the stellar wobble induced by planetary companions (Rybicki, 1979; Loeb and Gaudi, 2003; Faigler and Mazeh, 2011; Shporer, 2011; Mislis and Hodgkin 2012; Faigler et al. 2012; Knuth, Placek, Richards 2012; Placek, Richards, Knuth, 2012; Placek, Knuth, Angerhausen, 2014; Placek & Knuth, 2014).
Considering these photometric effects in addition to transits provides more precise characterization of transiting exoplanets and improved estimates of the stellar mass, which is typically estimated by spectroscopy and often with significant uncertainty. In addition, it is potentially more interesting to note that these effects provide information about the scattering and emissive properties of exoplanetary atmospheres (Seager et al. 2000; Charbonneau et al., 2002; Hood et al. 2008; Rowe et al. 2008), which complements information obtained via absorption spectra recorded during transits. Consideration of these factors promises to provide both greater return and higher precision from both the Kepler database and future missions.
EXONEST: The Exoplanetary Explorer (top)
We have been developing the EXONEST algorithm (Placek, Knuth, Angerhausen, 2014; Placek & Knuth, 2014), which utilizes advanced Bayesian machine learning methods to perform both parameter estimation and statistical model testing of photometric exoplanet models. EXONEST advances the state of the art in utilizing exoplanet photometric effects, such as BEER (Faigler and Mazeh, 2011), as well as other efforts (Shporer, 2011; Esteves et al., 2013), by including transits, and going beyond first-order approximations associated with circular orbits and accommodating elliptical orbits, which we demonstrate is critical since planets closely orbiting their host stars are not always in circularized orbits as previously imagined (Johnson et al., 2006; Fischer et al., 2007; Placek, Knuth, Angerhausen, 2014). In addition, the Bayesian machine learning methods we utilize employ advanced Markov chain Monte Carlo techniques, such as Nested Sampling (Skilling, 2004; Sivia and Skilling, 2006) and its more recent cousin MultiNest (Feroz and Hobson, 2008; Feroz et al. 2009). In addition to enabling one to perform parameter estimation using multiple data sets from multiple sources (data fusion), it also enables one to perform statistical model testing via the computation of the Bayesian evidence (Sivia and Skilling, 2006; Knuth, 2014). This allows one to test one photometric model against another. This is a significant advance since it may provide the ability to confirm the presence or absence of an exoplanet by computing the probabilities of independent photometric effects in a single data set without relying on secondary observations.
Not only does EXONEST have the capability to characterize both transiting and non-transiting exoplanets in situations where photometric effects are detectable, but these effects can provide better estimates of the stellar mass, which is critical in obtaining precise orbital elements, as well as valuable information about the planetary atmosphere, through the albedo and reflectance phase function, the planet’s day- and night-side temperatures, and the planet’s effects on the host star/s.
Placek B., Knuth K.H., Angerhausen D. 2016. Combining Photometry From Kepler and TESS to Improve Short-Period Exoplanet Characterization. In Press at the Publications of the Astronomical Society of the Pacific. arXiv:1511.01082 [astro-ph.IM]
Placek B., Knuth K.H. 2016. The detection and characterization of exoplanets with EXONEST. A. Giffin (ed.) Bayesian Inference and Maximum Entropy Methods in Science and Engineering (MaxEnt 2015), Potsdam, NY, USA, July 2015, AIP Conference Proceedings, American Institute of Physics, Melville NY. In press.
Placek B., Knuth K.H., Angerhausen D. 2015. Characterization of Kepler-91b and the Investigation of a Potential Trojan Companion Using EXONEST, The Astrophysical Journal, 814(2): 147; doi: 10.1088/0004-637X/814/2/147 , arXiv:1511.01068 [astro-ph.EP]
Placek B., Knuth K.H., Angerhausen D. 2014. EXONEST: Bayesian model selection applied to the detection and characterization of exoplanets via photometric variations, Astrophysical Journal, 795(2): 112. doi:10.1088/0004-637X/795/2/112, arXiv:1310.6764 [astro-ph.EP]
Placek B., Knuth K.H. 2014. A Bayesian Analysis of HAT-P-7b using the EXONEST Algorithm, to be published in Bayesian Inference and Maximum Entropy Methods in Science and Engineering 2014, Amboise, France, AIP Conference Proceedings, American Institute of Physics, Melville NY. arXiv:1409.4152 [astro-ph.EP]
Placek B., Knuth K.H., Angerhausen D. 2014. EXONEST: Bayesian model selection applied to the detection and characterization of exoplanets via photometric variations, Astrophysical Journal, 795(2): 112. arXiv:1310.6764 [astro-ph.EP], doi:0.1088/0004-637X/795/2/112
Knuth K.H., Placek B., Richards Z. 2012. Detection and characterization of non-transiting extra-solar planets in Kepler data using reflected light variations. N. Chawla and A.N. Srivastava (eds.) Proceedings of the Conference on Intelligent Data Understanding 2012, IEEE Explore, 31 - 38. doi: 10.1109/CIDU.2012.6382198
Placek B., Richards Z., Knuth K.H. 2012. Detecting non-transiting exoplanets. U. von Toussaint (ed.) Bayesian Inference and Maximum Entropy Methods in Science and Engineering, Garching, Germany, July 2012, AIP Conference Proceedings 1553, American Institute of Physics, Melville NY, 23-29.
Knuth K.H., Placek B. 2014. EXONEST: The Exoplanetary Explorer. 7th International Conference on Computational and Methodological Statistics (ERCIM 2014), Pisa, ITALY, 6 Dec 2014 (Presented by Ercan Kuruoglu)
Knuth K.H. 2013. Detection and characterization of non-transiting extra-solar planets in Kepler data using reflected light variations. Space Sciences Division, NASA Ames Research Center, Mountain View CA, 12 Apr 2013
- Ames Center for Exoplanet Studies (ACES) Seminar Announcement
- Slides: http://knuthlab.rit.albany.edu/talks/knuth---nasa-exo-2013---final.pdf
Orbiting planets reflect light, and from the perspective of a distant observer an illuminated planet undergoes phases resulting in a periodically-varying reflected light flux. While such reflected light is generally expected to be weak with the magnitude of the flux being well below noise level, in some cases reflected light variations are detectable with today's technology in the Kepler dataset. For example, a sinusoidal variation is visibly apparent along with a secondary eclipse in the HAT-P-7 light curve recorded by Kepler. In this talk I will discuss the problem of detecting extra-solar planets in Kepler data by modeling reflected light variations within a Bayesian estimation paradigm. We demonstrate that such detections are possible for a class of non-transiting planets using data from the Kepler Data Archive. The development of this computational technology could significantly increase the number of detectable planets within the Kepler dataset. Furthermore, an understanding of the potential capabilities of this technology could influence the design of future missions.
Knuth K.H., Placek B., Richards Z. 2012. Detection and characterization of non-transiting extra-solar planets in Kepler data using reflected light variations. N. Chawla and A.N. Srivastava (eds.) Conference on Intelligent Data Understanding 2012, Oct 2012, Boulder CO.
- Program: CIDU 2012 Program
- Paper: Proceedings of the Conference on Intelligent Data Understanding 2012, IEEE Explore, 31 - 38. (Digital Object Identifier: 10.1109/CIDU.2012.6382198 )
Placek B., Richards Z., Knuth K.H. 2012. Detecting non-transiting exoplanets. U. von Toussaint (ed.) Bayesian Inference and Maximum Entropy Methods in Science and Engineering, Garching, Germany, July 2012.
- Abstract: (MaxEnt 2012 pdf)
Developer: Placek B., KnuthLab, 2012.
OrbitViewer is a MatLab GUI that allows the user to adjust the orbital parameters of a planetary system and visualize both the reflected light curve and the orientation of the system.
Developer: Placek B., KnuthLab, 2013.
KepViewer is a Matlab GUI that allows the user to easily examine (Pre-Downloaded) Kepler light curves.
Developers: Placek B., Knuth K.H., KnuthLab, 2012-2014.
EXONEST: The Exoplanetary Explorer is a Bayesian Exoplanetary Inference Engine, which enables a host of exoplanetary (and stellar) photometric models to be tested against Kepler and CoRoT data. EXONEST, which was originally developed to rely on Nested Sampling, currently relies on MultiNest, which enables estimation of the Bayesian evidence for statistical model testing.
See EXONEST discussion above for additional details.