Abstract

We produce light curves for all ~34,000 targets observed with K2 in Campaign 17 (C17), identifying 34 planet candidates, 184 eclipsing binaries, and 222 other periodic variables. The location of the C17 field means follow-up can begin immediately now that the campaign has concluded and interesting targets have been identified. The C17 field has a large overlap with C6, so this latest campaign also offers a rare opportunity to study a large number of targets already observed in a previous K2 campaign. The timing of the C17 data release, shortly before science operations begin with the Transiting Exoplanet Survey Satellite (TESS), also lets us exercise some of the tools and methods developed for identification and dissemination of planet candidates from TESS. We find excellent agreement between these results and those identified using only K2-based tools. Among our planet candidates are several planet candidates with sizes < 4 R_E and orbiting stars with KepMag < 10 (indicating good RV targets of the sort TESS hopes to find) and a Jupiter-sized single-transit event around a star already hosting a 6 d planet candidate.

Highlights

  • Launched in 2009, the success of Kepler and its extended mission, K2, is unprecedented

  • Numerous spectra have been acquired with the Tillinghast Reflector Echelle Spectrograph (TRES; Fűrész 2008) and uploaded to the Exoplanet Follow-up Observing Program (ExoFOP)-K2 website; we describe these observations below

  • We report the radial velocities derived from the crosscorrelation of a single spectral order against the best-matched synthetic spectrum, shifted to the absolute IAU scale

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Summary

A TESS Dress Rehearsal

Chelsea Huang , Liang Yu1 , Karen A. Fulton , Björn Benneke, Merrin Peterson, Allyson Bieryla , Joshua E. Kosiarek8,16 , Makennah Bristow, Elisabeth Newton1,17 , Megan Bedell , David W. Calkins , Avi Shporer , Jennifer Burt , Sarah Ballard, Joseph E. Petigura8,18 , Sara Seager, Jason Dittmann , David Berardo , Lizhou Sha, Zahra Essack, Zhuchang Zhan, Martin Owens, Isabel Kain, Howard Isaacson , David R. Howard , and José Vinícius de Miranda Cardoso

Introduction
Identifying Planet Candidates
TESS-like Vetting
Stellar and Planetary Candidate Parameters
K2-like Vetting
Ground-based Spectroscopy
Purifying the Sample
Multicolor Photometry and Gaia DR2
Comparing Planet Candidates
Individual Systems
75 RÅ L L L L contact L L contact
Discussion and Conclusion
Full Text
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