ner_tags: O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O B-Telescope O O B-Telescope O O O O O O O O O B-CelestialRegion O B-CelestialRegion I-CelestialRegion O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Dataset I-Dataset I-Dataset I-Dataset I-Dataset B-Dataset B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software I-Software I-Software I-Software B-Software B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O B-Software B-Citation I-Citation I-Citation O O B-Software O O O O O O O O O O O O O O O O O O O O B-Software O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O B-Software I-Software O B-Software I-Software I-Software I-Software O B-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope I-Telescope I-Telescope I-Telescope I-Telescope B-Telescope B-Citation I-Citation I-Citation I-Citation O O B-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation O B-Citation I-Citation O O O O O O O O B-Telescope I-Telescope I-Telescope I-Telescope B-Telescope B-Citation I-Citation I-Citation I-Citation O O B-Survey I-Survey I-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O B-Model I-Model O O O O B-Telescope B-Citation I-Citation I-Citation I-Citation O O B-Telescope I-Telescope I-Telescope I-Telescope B-Telescope B-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software O
tokens: a new era of research on eclipsing binary systems (EBs). The mission was designed with the main objective of searching for transiting planets (Borucki et al. 2011 ). As a by-product, the Kepler satellite provides the detection and monitoring of variable stars, most of which are EBs. This is an interesting fact, because EBs are important astronomical targets for determining the orbital and physical parameters of component stars from the geometry of their light curves (LCs) (Deb Singh 2011 ). The Kepler space mission Kepler was originally designed to investigate a region located between Swan and Lyre constellations, having a telescope with an aperture of 0.95 m and a field of view of 115.6° squares. Equipped with a photometer containing 42 CCDs with 2200 × 1024 pixels, where each pixel covers a region of 4 s of arc, Kepler provides unprecedented quality and quantity photometric data (e.g. Thompson et al. 2016 ). Details on the instrumentation of the mission can be found in Koch et al. ( 2010 ). The Kepler Eclipsing Binary Catalog 1 (KEBC; Prša et al. 2011 ; Slawson et al. 2011 ; Kirk et al. 2016 ) is an excellent bridge between the eclipsing binary data of the mission and the scientific community. In the catalogue versions, the parameters of the systems were determined by the method of Eclipsing Binaries via ArtificialIntelligence (EBAI; Prša et al. 2008 ), a computational tool for data mining of large volumes of data. Trained with synthetic LCs generated by the PHOEBE (Prša Zwitter 2005 ), the EBAI uses polynomial adjustment and does not aim at the precise and individual adjustment of LCs. On the other hand, the JKTEBOP code (Southworth, Maxted Smalley 2004a ; Southworth et al. 2004b ), based on the EBOP code ( Eclipsing Binary Orbit Program ; Etzel 1981 ; Popper Etzel 1981 ), is an efficient alternative for individual and precise analysis of LCs, obtaining more exact adjustments by allowing the parameters of interest to be free. The larger Kepler data set is a challenge for analysis tools. Consequently, a test of the fidelity of data mining tools for different processes is crucial, since the large observational programme such as Convection, Rotation and planetary Transits (CoRoT; Baglin et al. 2006 ) and All Sky Automated Survey (ASAS; Pojmanski 1997 ; Pojmański 2001 ), and in the future, programs such as Transiting Exoplanet Survey Satellite (TESS; Ricker et al. 2014 ) and PLAnetary Transits and Oscillations of stars (PLATO; Catala et al. 2010 ) will discover a lot of EBs and surely have data studied by powerful instruments such as neural networks. Furthermore, missions such as Gaia (Perryman et al. 2001 ) and Large Synoptic Survey Telescope (LSST; Tyson 2002 ) will discover millions of EBs but obtain LCs with few points (Southworth 2012 ), requiring more accurate and appropriate analysis tools. In this paper, we present the orbital and physical parameters of 78 EBs and investigate possible discrepancies between the results found by EBAI and