KEPLER ECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND DATA RELEASE

By R. Slawson, A. Prša, W. Welsh, J. Orosz, Michael Rucker, N. Batalha, L. Doyle, S. Engle, K. Conroy, J. Coughlin and 14 more. 2011

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The Kepler Mission provides nearly continuous monitoring of ∼156,000 objects with unprecedented photometric precision. Coincident with the first data release, we presented a catalog of 1879 eclipsing binary systems identified within the 115 deg2 Kepler field of view (FOV). Here, we provide an updated catalog augmented with the second Kepler data release which increases the baseline nearly fourfold to 125 days. Three hundred and eighty-six new systems have been added, ephemerides and principal parameters have been recomputed. We have removed 42 previously cataloged systems that are now clearly recognized as short-period pulsating variables and another 58 blended systems where we have determined that the Kepler target object is not itself the eclipsing binary. A number of interesting objects are identified. We present several exemplary cases: four eclipsing binaries that exhibit extra (tertiary) eclipse events; and eight systems that show clear eclipse timing variations indicative of the presence of additional bodies bound in the system. We have updated the period and galactic latitude distribution diagrams. With these changes, the total number of identified eclipsing binary systems in the Kepler FOV has increased to 2165, 1.4% of the Kepler target stars. An online version of this catalog is maintained at http://keplerEBs.villanova.edu.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8a511bbb1c2aaf2d541c31c2c383d3185d55370d

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Citations in the corpus

They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, background): “…of our sample and identified 13 that are known or likely FPs (a rate of 11%): KOI 256.01 which is a known post-common envelope binary with a white dwarf (Muirhead et al. 2013): KOI 950.01 is also listed as a EB in Slawson et al. (2011) and has significant flux-weight centroid motion statistic.”
The Kepler characterization of the variability among A- and F-type stars I. General overview (2011, background): “Sixty-two stars are known to belong to multiple systems, including at least fourteen eclipsing binaries (EB; KIC 1432149, Hartman et al. 2004; KIC 10206340, Malkov et al. 2006; catalogues by Prša et al. 2011 and Slawson et al. 2011).”
KEPLER ECLIPSING BINARY STARS. III. CLASSIFICATION OF KEPLER ECLIPSING BINARY LIGHT CURVES WITH LOCALLY LINEAR EMBEDDING (2012, methodology): “The data classified in this paper are a part of the second Kepler catalog of EB stars (Slawson et al. 2011).”
PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, methodology): “Previous catalogs excluded all eclipsing binary (EB) candidates identified by Prša et al. (2011) and Slawson et al. (2011).”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, methodology): “In the Kepler FOV, it has been estimated to be 0.79 ± 0.02 % using the second version of the Kepler EB catalog (Slawson et al. 2011).”
PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1–Q8 (22 MONTHS) (2013, background): “0 (Prša et al. 2011; Slawson et al. 2011) and ground-based surveys (Coughlin et al., in preparation).”
THE OCCURRENCE OF POTENTIALLY HABITABLE PLANETS ORBITING M DWARFS ESTIMATED FROM THE FULL KEPLER DATASET AND AN EMPIRICAL MEASUREMENT OF THE DETECTION SENSITIVITY (2015, methodology): “We examined both the published Version 2 (Slawson et al. 2011) and the online beta version of the Third Revision4.”
ROTATION PERIODS OF 34,030 KEPLER MAIN-SEQUENCE STARS: THE FULL AUTOCORRELATION SAMPLE (2014, methodology): “The EB list was downloaded from the Villanova Eclipsing Binary web site2 which has an up-to-date and extended version of the Kepler EB catalogs of Prša et al. (2011) and Slawson et al. (2011).”
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “We also report observations for 23 stars that were subsequently identified as likely false positives (e.g., Slawson et al. 2011; Mann et al. 2012; Huber et al. 2013) after we observed them, since high-resolution imaging is useful for further confirming their non-planetary nature, but do not use…”
A comprehensive study of the Kepler triples via eclipse timing (2015, methodology): “They are: KIC 05897826 (=KOI-126) (Carter et al. 2011), KIC 05952403 (=HD 181068) (Derekas et al. 2011), KICs 06543674, 07289157 (Slawson et al. 2011), KIC 02856960 (Armstrong et al. 2012), KIC 02835289 (Conroy et al. 2014), and KICs 05255552, 06964043, 07668648 (Borkovits et al. 2015).”
PLANETARY CANDIDATES OBSERVED BY KEPLER. III. ANALYSIS OF THE FIRST 16 MONTHS OF DATA (2012, methodology): “This target has been included in the Eclipsing Binary Catalog (Prša et al. 2011; Slawson et al. 2011).”
ARCHITECTURE OF KEPLER'S MULTI-TRANSITING SYSTEMS. II. NEW INVESTIGATIONS WITH TWICE AS MANY CANDIDATES (2012, background): “To explore this, we selected Mp/M? as above (a reflection of the distribution of observed depths) but replaced the periods by two draws from the list of eclipsing binaries labeled “detached” by Slawson et al. (2011).”
LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, methodology): “This rate has been measured in the Kepler field (Prša et al. 2011; Slawson et al. 2011).”
REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1–16 TRANSIT DETECTION RUN (2013, background): “…time, Kepler data allowed key discoveries in stellar astrophysics such as the detection of more than 2000 eclipsing binary stars (Prša et al. 2011; Slawson et al. 2011; Matijevič et al. 2012) including eclipsing triple systems (Carter et al. 2011; Derekas et al. 2011), the 19 Center for High…”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, methodology): “These estimates make use of the frequencies of eclipsing binaries generated by the Kepler team (Slawson et al. 2011) as well as the frequencies of transiting planets of the specific size required to produce the above blends, based on the available sample of KOIs from the NASA Exoplanet Archive.”
Target Selection for the SDSS-IV APOGEE-2 Survey (2017, methodology): “The Kepler targets are selected from the Kepler EB Catalogs list of detached EBs (Prša et al. 2011; Slawson et al. 2011), using a magnitude limit of H ≤ 13.”
KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, background): “We note that for our search for transiting CBP we do this for the entire EB catalog listed in Slawson et al. (2011); Kirk et al. (2014).”
Statistical properties of superflares on solar-type stars based on 1-min cadence data (2015, methodology): “We checked the Kepler Eclipsing Binary Catalog (Kirk 2013; Prša A et al. 2011; Slawson et al. 2011) and removed all flare candidates which occurred on the eclipsing binary (14 stars).”