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Planetary Candidates Observed by Kepler. VIII. a Fully Automated Catalog with Measured Completeness and Reliability Based on Data Release 25

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Planetary Candidates Observed by Kepler. VIII. a Fully Automated Catalog with Measured Completeness and Reliability Based on Data Release 25 The Astrophysical Journal Supplement Series, 235:38 (49pp), 2018 April https://doi.org/10.3847/1538-4365/aab4f9 © 2018. The American Astronomical Society. All rights reserved. Planetary Candidates Observed by Kepler. VIII. A Fully Automated Catalog with Measured Completeness and Reliability Based on Data Release 25 Susan E. Thompson1,2,3 , Jeffrey L. Coughlin1,2 , Kelsey Hoffman1, Fergal Mullally1,2,4, Jessie L. Christiansen5 , Christopher J. Burke1,2,6, Steve Bryson2, Natalie Batalha2, Michael R. Haas2,33, Joseph Catanzarite1,2, Jason F. Rowe7 , Geert Barentsen8, Douglas A. Caldwell1,2, Bruce D. Clarke1,2, Jon M. Jenkins2 , Jie Li1, David W. Latham9 , Jack J. Lissauer2, Savita Mathur10, Robert L. Morris1,2, Shawn E. Seader11, Jeffrey C. Smith1,2, Todd C. Klaus2, Joseph D. Twicken1,2 , Jeffrey E. Van Cleve1, Bill Wohler1,2, Rachel Akeson5, David R. Ciardi5, William D. Cochran12 , Christopher E. Henze2, Steve B. Howell2 , Daniel Huber1,13,14,15 , Andrej Prša16 , Solange V. Ramírez5, Timothy D. Morton17 , Thomas Barclay18 , Jennifer R. Campbell2,19, William J. Chaplin15,20 , David Charbonneau9 , Jørgen Christensen-Dalsgaard15 , Jessie L. Dotson2 , Laurance Doyle1,21, Edward W. Dunham22, Andrea K. Dupree9 , Eric B. Ford23,24,25,26 , John C. Geary9, Forrest R. Girouard2,27, Howard Isaacson28 , Hans Kjeldsen15, Elisa V. Quintana18, Darin Ragozzine29 , Megan Shabram2,34 , Avi Shporer30 , Victor Silva Aguirre15 , Jason H. Steffen31, Martin Still8, Peter Tenenbaum1,2, William F. Welsh32 , Angie Wolfgang23,24,35 , Khadeejah A Zamudio2,19, David G. Koch2,36, and William J. Borucki2,33 1 SETI Institute, 189 Bernardo Ave., Suite 200, Mountain View, CA 94043, USA; [email protected] 2 NASA Ames Research Center, Moffett Field, CA 94035, USA 3 Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA 4 Orbital Insight, 100 W. Evelyn Ave. #110, Mountain View, CA 94041, USA 5 IPAC-NExScI, Mail Code 100-22, Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA 6 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Ave., 37-241, Cambridge, MA 02139, USA 7 Department of Physics and Astronomy, Bishop’s University, 2600 College St., Sherbrooke, QC, J1M 1Z7, Canada 8 Bay Area Environmental Research Institute, 625 2nd St., Ste. 209, Petaluma, CA 94952, USA 9 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA 10 Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA 11 Rincon Research Corporation, 101 N. Wilmot Rd., Tucson, AZ 85711, USA 12 McDonald Observatory and Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA 13 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Dr., Honolulu, HI 96822, USA 14 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia 15 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 16 Villanova University, Department of Astrophysics and Planetary Science, 800 Lancaster Ave., Villanova, PA 19085, USA 17 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 18 NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA 19 KRBwyle, 2400 Nasa Pkwy, Houston, TX 77058, USA 20 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK 21 Institute for the Metaphysics of Physics, Principia College, One Maybeck Place, Elsah, IL 62028, USA 22 Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USA 23 Department of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA 24 Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA 25 Center for Astrostatistics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA 26 Institute for CyberScience, The Pennsylvania State University, University Park, PA 16802, USA 27 Orbital Sciences Corporation, 2401 East El Segundo Blvd., Suite 200, El Segundo, CA 90245, USA 28 Department of Astronomy, UC Berkeley, Berkeley, CA 94720, USA 29 Brigham Young University, Department of Physics and Astronomy, N283 ESC, Provo, UT 84602, USA 30 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 31 University of Nevada, Las Vegas, 4505 S. Maryland Pkwy., Las Vegas, NV 89154, USA 32 Department of Astronomy, San Diego State University, 5500 Campanile Dr., San Diego, CA 92182-1221, USA Received 2017 October 13; revised 2018 February 18; accepted 2018 March 1; published 2018 April 9 Abstract We present the Kepler Object of Interest (KOI) catalog of transiting exoplanets based on searching 4 yr of Kepler time series photometry (Data Release 25, Q1–Q17). The catalog contains 8054 KOIs, of which 4034 are planet candidates with periods between 0.25and 632days. Of these candidates, 219 are new, including two in multiplanet systems (KOI-82.06 and KOI-2926.05) and 10 high-reliability, terrestrial-size, habitable zone candidates. This catalog was created using a tool called the Robovetter, which automatically vets the DR25 threshold crossing events (TCEs). The Robovetter also vetted simulated data sets and measured how well it was able to separate TCEs caused by noise from those caused by low signal-to-noise transits. We discuss the Robovetter and the metrics it uses to sort TCEs. For orbital periods less than 100 days the Robovetter completeness (the fraction of simulated transits that are determined to be planet candidates) across all observed stars is greater 33 NASA Ames Associate. 34 NASA Postdoctoral Program Fellow, Administered by Universities Space Research Association. 35 NSF Astronomy & Astrophysics Postdoctoral Fellow. 36 Deceased. 1 The Astrophysical Journal Supplement Series, 235:38 (49pp), 2018 April Thompson et al. than 85%. For the same period range, the catalog reliability (the fraction of candidates that are not due to instrumental or stellar noise) is greater than 98%. However, for low signal-to-noise candidates between 200 and 500 days around FGK-dwarf stars, the Robovetter is 76.7% complete and the catalog is 50.5% reliable. The KOI catalog, the transit fits, and all of the simulated data used to characterize this catalog are available at the NASA Exoplanet Archive. Key words: catalogs – planetary systems – stars: general – surveys Supporting material: machine-readable tables 1. Introduction found orbiting binary stars, e.g., Kepler-16(AB)b (Doyle et al. 2011). Kepler’s mission to measure the frequency of Earth-size Other authors have taken advantage of the long time series, planets in the Galaxy is an important step toward understanding near-continuous data set of 206,15037 stars to advance our the Earth’s place in the universe. Launched in 2009, the Kepler understanding of stellar physics through the use of asteroseis- mission (Koch et al. 2010; Borucki 2016) stared almost fi ( mology. Of particular interest to this catalog is the improve- continuously at a single eld for 4 yr or 17 quarters of ment in the determination of stellar radius (e.g., Huber ≈90 days each), recording the brightness of ≈200,000 stars ) (≈ ) et al. 2014; Mathur et al. 2017 , which can be one of the 160,000 stars at a time at a cadence of 29.4 minutes over the most important sources of error when calculating planetary course of the mission. Kepler detected transiting planets by radii. Kepler data were also used to track the evolution of observing the periodic decrease in the observed brightness of a starspots created from magnetic activity and thus enabled the star when an orbiting planet crossed the line of sight from the ( ’ measurement of stellar rotation rates e.g., García et al. 2014; telescope to the star. Kepler s prime-mission observations McQuillan et al. 2014; Aigrain et al. 2015; Zimmerman et al. concluded in 2013 when it lost a second of four reaction 2017). Studying stars in clusters enabled Meibom et al. (2011) wheels, three of which were required to maintain the stable to map out the evolution of stellar rotation as stars age. Kepler pointing. From the ashes of Kepler rose the K2 mission, which also produced light curves of 287638 eclipsing binary stars fi continues to nd exoplanets in addition to a whole host of (Prša et al. 2011; Kirk et al. 2016), including unusual binary fi astrophysics enabled by its observations of elds in the ecliptic systems, such as the eccentric, tidally distorted, Heartbeat stars ( ) fi Howell et al. 2014; Van Cleve et al. 2016b . While not the rst (Welsh et al. 2011; Thompson et al. 2012; Shporer et al. 2016) to obtain high-precision, long-baseline photometry to look for that have opened the doors to understanding the impact of tidal ( ’ transiting exoplanets see, e.g., O Donovan et al. 2006; Barge forces on stellar pulsations and evolution (e.g., Fuller et al. et al. 2008), Kepler and its plethora of planet candidates 2017; Hambleton et al. 2017). revolutionized exoplanet science. The large number of Kepler The wealth of astrophysics, as well as the size of the Kepler planet detections from the same telescope opened the door for community, is in part due to the rapid release of Kepler data to occurrence rate studies and has enabled some of the first the NASA Archives: the Exoplanet Archive (Akeson et al. measurements of the frequency of planets similar to Earth in 2013) and the MAST (Mikulski Archives for Space Tele- our Galaxy. To further enable those types of studies, we present scopes). The Kepler mission released data from every step of here the planet catalog that resulted from the final search of the the processing (Bryson et al. 2010; Stumpe et al. 2014; Data Release 25 (DR25) Kepler mission data, along with the Thompson et al. 2016b), including its planet searches. The tools provided to understand the biases inherent in the search results of both the original searches for periodic signals (known and vetting done to create that catalog.
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