arXiv:1802.05277v1 [astro-ph.EP] 14 Feb 2018

Preprint typeset using LATEX style emulateapj v. 12/16/11

275 CANDIDATES AND 149 VALIDATED PLANETS ORBITING BRIGHT STARS IN K2 CAMPAIGNS 0-10

Andrew W. Mayo1,2,3,†,‡,?, Andrew Vanderburg4,3,‡, 2, David W. Latham3, Allyson Bieryla3, Timothy D.Morton5, Lars A. Buchhave1,2, Courtney D. Dressing6,7,2, Charles Beichman8, Perry Berlind3, Michael L.

Calkins3, David R. Ciardi8, Ian J. M. Crossfield9, Gilbert A. Esquerdo3, Mark E. Everett10, Erica J.Gonzales11, ‡, Lea A. Hirsch6, Elliott P. Horch12, Andrew W. Howard13, Steve B. Howell14, John Livingston15,

Rahul Patel16 , Erik A. Petigura13, ††, Joshua E. Schlieder17, Nicholas J. Scott14, Clea F. Schumer3, EvanSinukoff13,18, Johanna Teske19,‡‡, Jennifer G. Winters3

ABSTRACT

Since 2014, NASA’s K2 mission has observed large portions of the ecliptic plane in search of transit-ing planets and has detected hundreds of planet candidates. With observations planned until at leastearly 2018, K2 will continue to identify more planet candidates. We present here 275 planet candi-dates observed during Campaigns 0-10 of the K2 mission that are orbiting stars brighter than 13thmagnitude (in Kepler band) and for which we have obtained high-resolution spectra (R = 44,000).These candidates are analyzed using the vespa package (Morton 2012, 2015b) in order to calculatetheir false positive probabilities (FPP). We find that 149 candidates are validated with a FPP lessthan 0.1%, 39 of which were previously only candidates and 56 of which were previously undetected.The processes of data reduction, candidate identification, and statistical validation are described, andthe demographics of the candidates and newly validated planets are explored. We show tentativeevidence of a gap in the planet radius distribution of our candidate sample. Comparing our sampleto the Kepler candidate sample investigated by Fulton et al. (2017), we conclude that more planetsare required to quantitatively confirm the gap with K2 candidates or validated planets. This work, inaddition to increasing the population of validated K2 planets by nearly 50% and providing new targetsfor follow-up observations, will also serve as a framework for validating candidates from upcoming K2campaigns and the Transiting Exoplanet Survey Satellite (TESS), expected to launch in 2018.

Keywords: methods: data analysis, planets and satellites: detection, techniques: photometric

† [email protected]‡ National Science Foundation Graduate Research Fellow? Fulbright Fellow2 NASA Sagan Fellow†† NASA Hubble Fellow‡‡ Carnegie Origins Fellow, jointly appointed by Carnegie DTM

& Carnegie Observatories1 DTU Space, National Space Institute, Technical University of

Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark2 Centre for Star and Planet Formation, Natural History Mu-

seum of Denmark & Niels Bohr Institute, University of Copen-hagen, Øster Voldgade 5-7, DK-1350 Copenhagen K., Denmark

3 Harvard–Smithsonian Center for Astrophysics, 60 Garden St.,Cambridge, MA 02138

4 Department of Astronomy, University of Texas at Austin,Austin, TX 76712

5 Department of Astrophysical Sciences, 4 Ivy Lane, Peyton Hall,Princeton University, Princeton, NJ 08544

6 Astronomy Department, University of California, Berkeley, CA94720

7 Division of Geological & Planetary Sciences, California Insti-tute of Technology, 1200 E California Blvd MC 150-21, Pasadena,CA 91125 USA

8 NASA Exoplanet Science Institute, California Institute ofTechnology, Pasadena, CA 91125

9 Department of Physics and Kavli Institute for Astrophysicsand Space Research, Massachusetts Institute of Technology, Cam-bridge, MA 02139

10 National Optical Astronomy Observatory, 950 North CherryAvenue, Tucson, AZ 85719

11 Department of Astronomy and Astrophysics, University ofCalifornia, Santa Cruz, CA 95064

12 Department of Physics, Southern Connecticut State Univer-sity, 501 Crescent Street, New Haven, CT 06515

13 Cahill Center for Astrophysics, California Institute of Tech-nology, Pasadena, CA 91125

14 Space Science and Astrobiology Division, NASA Ames Re-search Center, Moffett Field, CA 94035

1. INTRODUCTION

The field of exoplanets is relatively young compared tomost other disciplines of astronomy: the announcementof the first exoplanet orbiting a star similar to our ownwas only in 199526 (Mayor & Queloz 1995). Since then,the field has expanded rapidly, with several thousandexoplanets having now been discovered. With many up-coming extremely large telescopes, the number of knownexoplanets and our understanding of them will only in-crease.

One of the most important moments in the history ofexoplanet science was the beginning of the Kepler mission(Borucki et al. 2008). Launched in 2009, the Kepler spacetelescope observed over 100,000 stars in a single patch ofsky for four years in order to look for transits. Kepler hasbeen an overwhelming success. According to the NASAExoplanet Archive27 (accessed 2018 February 14), it iscurrently responsible for 2341 verified exoplanets, more

15 Department of Astronomy, The University of Tokyo, 7-3-1Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

16 Infrared Processing and Analysis Center, California Instituteof Technology, Pasadena, CA 91125

17 NASA Goddard Space Flight Center, Greenbelt, MD 2077118 Institute for Astronomy, University of Hawai‘i at Manoa, Hon-

olulu, HI 9682219 Carnegie Observatories, 813 Santa Barbara Street, Pasadena,

CA 9110126 The exoplanet, 51 Peg b, was not fully confirmed to be a

planet until the absolute mass was measured by Martins et al.(2015). Also, a reported brown dwarf discovered in 1989 (Lathamet al. 1989) may in fact be an exoplanet, depending on its inclina-tion.

27 https://exoplanetarchive.ipac.caltech.edu/

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2 Mayo et al.

than every other exoplanet survey combined.Unfortunately, in 2013 the second of four reaction

wheels on the Kepler spacecraft failed, preventing thespacecraft from looking at its designated field and bring-ing an end to the original mission. Fortunately, a fol-low up mission, called K2, was developed that used thespacecraft’s thrusters as a makeshift third reaction wheel(Howell et al. 2014). Unlike the original Kepler mission,the K2 mission must observe new fields roughly every83 days28. As a result, K2 observations are divided into“campaigns” each corresponding to a field.

With every new campaign, K2 observes more brightstars and finds more planets orbiting these stars, so thereare new bright targets available for follow-up (such as RVmeasurements or transmission spectroscopy). K2 has ledto the discovery of numerous candidate and confirmedplanets (Vanderburg et al. 2015b; Crossfield et al. 2015;Foreman-Mackey et al. 2015; Montet et al. 2015; Van-derburg et al. 2016a; Schlieder et al. 2016; Sinukoff et al.2016; Crossfield et al. 2016; Barros et al. 2016; Pope et al.2016; Adams et al. 2016; Dressing et al. 2017b; Martinezet al. 2017; Hirano et al. 2017), as well as the identifica-tion of planets orbiting rare types of stars, including par-ticularly bright nearby dwarf stars (Petigura et al. 2015;Vanderburg et al. 2016b; Rodriguez et al. 2017b; Cross-field et al. 2017; Christiansen et al. 2017; Rodriguez et al.2017a; Niraula et al. 2017), young, pre-main-sequencestars (Mann et al. 2016; David et al. 2016), and dis-integrating planetary material transiting a white dwarf(Vanderburg et al. 2015a).

Here, we take advantage of the large number of brightstars observed by K2 and present the identification andfollow-up of a sample of 275 exoplanet candidates orbit-ing stars (brighter than 13th magnitude) in the Keplerbandpass identified from K2 Campaigns 0 through 10.Since the beginning of the K2 mission, we have also ob-tained spectra for all of our candidates as well as manyhigh-resolution imaging observations, in order to mea-sure the candidate host stars’ parameters and identifynearby stars (both types of follow-up aid in identificationand ruling out of false positive scenarios). We also at-tempt to validate29 our candidates with vespa, a statis-tical validation tool developed by Morton (2012, 2015b),

28 Roughly 75 of those days are devoted to science.29 The difference between an exoplanet candidate and a val-

idated exoplanet is very important. During the original Keplermission, an exoplanet candidate was a transit signal that hadpassed a battery of astrophysical false positive and instrumentalfalse alarm tests. In K2, however, the usage is looser; the term iscommonly used to refer to any exoplanet signal that a particularteam has identified as a possible planet. So long as the reasoningis sound and the results are published, the signal is effectively acandidate. A validated planet is a candidate that has been vet-ted with follow-up observations and determined quantitatively tobe far more likely an exoplanet than a false positive (according tosome likelihood threshold). Validated planets, because confidencein their planethood is higher than for a regular candidate, are farmore promising targets than planet candidates for follow-up obser-vations, characterization, and eventual confirmation. We note thatvalidation is not the same thing as confirmation, which is ideallyattained through a reliable mass determination. In this work, weare in general not attempting to “confirm” planets. Confirmationis more rigorous than validation, in the same way that validationis more rigorous than candidacy. Confirmation is usually accom-plished via the RV method, the TTV method, or, less commonly,methods such as a full photo-dynamical modeling solution (e.g.Carter et al. 2011) or Doppler tomography (e.g. Zhou et al. 2016).

finding 149 to be validated with a false positive proba-bility less than 0.1%. Of these newly validated exoplan-ets, 39 were previously only exoplanet candidates and 56have not been previously detected (see Table 2). Thiswork will increase the validated K2 planet sample from212 (according to the Mikulski Archive for Space Tele-scopes30; accessed 2018 February 14) to 307, a nearly50% increase. Similarly, this work increases the K2 can-didate sample by ∼20%.

In this paper we describe the identification and analysisof our candidate sample, as well as our validation processand the resulting validated planet sample. Section 2 dis-cusses the process by which we use K2 data to identifyexoplanet candidates. Section 3 describes our ground-based observations of the planet candidate host stars de-tected by K2. Section 4 explains the analysis of the K2light curves and the follow-up spectroscopy and high-contrast imaging. Section 5 details how we use vespa tocalculate false positive probabilities for our planet candi-dates. Section 6 presents the results of the our candidateidentification, vetting, follow-up observations, and anal-ysis in detail for a single, instructive planet. Then theresults for the entire planet candidate sample are simi-larly presented. In Section 7, we discuss the results ofour work, including confirmation of features in the exo-planet population previously identified using data fromthe original Kepler mission. Finally, we summarize andconclude in Section 8.

2. PIXELS TO PLANETS

In this section, we first explain how K2 observationsare collected, then we describe the process by which sys-tematic errors are removed from K2 data, and finally wediscuss analysis of the systematics-corrected K2 data inorder to identify planet candidates.

2.1. K2 Observations

Since 2014, the K2 mission has served as the successorto the original Kepler mission. By observing fields alongthe ecliptic plane and firing its thrusters approximatelyonce every six hours, the probe can maintain an unstableequilibrium against solar radiation. However, the space-craft can only point toward a given field for roughly 83days before re-pointing (in order to keep sunlight on thespacecraft’s panels and out of its telescope).

Due to on-board data storage constraints, not all datacollected by the CCD array can be retained and transmit-ted to the ground. As a result, targets must be identifiedwithin each campaign field prior to observation so thatnon-target data can be discarded and a postage stamp(a small group of pixels) around each target can be savedand transmitted to the ground.

In the original Kepler mission, the primary objectivewas to determine the frequency of Earth-like planets or-biting Sun-like stars (Batalha et al. 2010b). Althoughsome planet search targets were selected during missionadjustments and others were selected through a GuestObserver program for secondary science objectives, mosttargets were selected pre-launch for the primary objec-tive. However, K2 operates in a very different manner.For each K2 campaign, targets are exclusively selected

30 https://archive.stsci.edu/k2/published planets/search.php

New Candidates and Planets Transiting Bright Stars 3

through the Guest Observer (GO) program, which eval-uates observing proposals submitted by the astronomicalcommunity for any scientific objective, not just exoplanetrelated objectives. Ideally, GO proposals have scientifi-cally compelling goals that can be achieved through K2observations and cannot easily be achieved with otherinstruments or facilities.

In a typical K2 campaign, the number of targets rangesbetween 10,000 and 40,000 with long cadence observa-tions (≈30 minute integration), and about 50 to 200 withshort cadence observations (≈1 minute integration). Ex-ceptions include C0, which served primarily as a proof-of-concept campaign to show that the K2 mission wasviable, and C9, which focused on microlensing targets inthe Galactic Bulge. Both C0 and C9 had fewer targetsthan normal in both long cadence and short cadence.It should also be noted that there are occasional over-laps between campaign fields. Despite fewer new tar-gets, overlaps provide a longer baseline of observationsfor targets of interest in the overlapping region.

This paper focuses on Campaigns 0 through 10 (ex-cluding Campaign 9). However, the process implementedin this research can easily be extended and applied to ad-ditional K2 campaigns.

2.2. K2 Data Reduction

Because of the loss of two reaction wheels, the Ke-pler telescope is perpetually drifting off target and mustbe regularly corrected by thruster fires, causing shifts inthe pixels that targets fall on. These shifts, coupled withvariable sensitivity between pixels on the telescope CCDsand variable amounts of starlight falling inside photomet-ric apertures, lead to systematic variations in the signalfrom K2 targets, introducing noise into the photometricmeasurements. Howell et al. (2014) estimated that rawK2 precision is roughly a factor of 3-4 times worse thanKeplers original precision (depending on stellar magni-tude). Fortunately, an understanding of the motion ofthe Kepler spacecraft allows for modeling and correctionof the induced systematic noise. In particular, we rely onthe method of systematic correction described by Van-derburg & Johnson (2014, hereafter referred to as VJ14),as well as the updates to the method described in Van-derburg et al. (2016a, hereafter referred to as V16). Webriefly describe here the method developed by VJ14.

First, 20 different aperture masks were chosen for eachtarget star, 10 circular masks of varying size and 10masks shaped liked the Kepler pixel response functionfor the target with varying sensitivity cutoffs. Thesemasks were used to perform simple aperture photometryto produce 20 different “raw” light curves. Then the mo-tion of the target star across the CCD was estimated bycalculating centroid position for each cadence31. Next,the recurrent path of the centroid across the CCD be-tween thruster fires was identified. Data collected dur-ing thruster fires were identified and removed. Then, foreach of the 20 raw light curves produced, low-frequencyvariations (> 1.5 days) were removed with a basis splineand the relationship between centroid position and flux

31 Although it is possible to produce light curves by decorre-lating with centroid positions measured from each star, we usedthe centroids measured from one hand-selected isolated, bright K2target per campaign, which we found gives better results.

was fit with a piecewise function. Because the centroidpath would shift on timescales longer than 5-10 days, theflux-centroid piecewise function was applied separatelyto each 5-10 day light curve segment. This function wasthen used to correct the raw data so that low-frequencyvariations could be recalculated. This process was thenrepeated iteratively until convergence. Finally, after all20 raw light curves per star were processed in this way,a “best” aperture was chosen to maximize photometricprecision. An example of a light curve before and afterthe full data reduction procedure can be seen in Fig. 1 forthe planet host EPIC 212521166. We note that light fromany nearby companion stars could potentially enter thebest aperture mask, which may lead to a diluted transitand an underestimated planet radius (Ciardi et al. 2015;Hirsch et al. 2017). However, we expected this effect tobe small even when present and therefore do not correctfor it.

2.3. Identifying Threshold Crossing Events

Once the roll systematics were removed from the pho-tometry according to the method described by VJ14, weconducted a transit search of each K2 target using themethod of Vanderburg et al. (2016a). We give a shortdescription of the transit search process here.

First, low-frequency variations were removed via a ba-sis spline and outliers were removed. Then a box-least-squares (BLS) periodogram (Kovacs et al. 2002) wascalculated over periods between 2.4 hours and half thelength of the campaign. All periodic decreases in bright-ness with SNR > 9 were investigated. If putative tran-sits lasted longer than 20% of their period, or were com-posed of a single data point, or changed depth by over50% when the lowest point was removed, the signal wasremoved and the BLS periodogram recalculated. Anydetection passing these tests was deemed a “ThresholdCrossing Event” (TCE). We identified ∼30, 000 TCEsacross C0-C10 in this manner.

Each TCE was fit with the Mandel & Agol (2002) tran-sit model to estimate transit parameters, then the TCEwas removed from the light curve, and the BLS peri-odogram was recalculated. Once all TCEs had been iden-tified, they subsequently underwent “triage”, in whicheach candidate was inspected by eye in order to removeobvious astrophysical false positives and instrumentalfalse alarms from subsequent analysis. TCEs identifiedas neither type of false signal passed the triage phase andmoved on to a “vetting” phase.

2.4. Identifying K2 Candidates

During vetting, we subjected the surviving TCEs to abattery of additional tests to identify astrophysical falsepositives and instrumental false alarms. Some of thesetests were identical or similar to the tests conducted forthe Kepler mission, while others are specific to K2 data.For each test we produced a diagnostic plot, examples ofwhich are shown in Figs. 2, 3, and 4. Here we describethe tests we conducted in more detail:

1. The times of a TCE’s “in transit” points were com-pared against the position of the Kepler spacecraftat those times, as many instrumental false alarmswere composed of data points near the edges ofKepler’s rolls where the K2 flat field is less well

4 Mayo et al.

Figure 1. Example of the K2 systematics reduction process on the light curve of the planet host EPIC 212521166. The blue points showthe light curve before correcting for the systematics induced by the roll motion of the Kepler spacecraft, while the yellow points show thesame light curve after those systematics have been removed via the data reduction process summarized in Section 2.2 and documentedin Vanderburg & Johnson (2014) and Vanderburg et al. (2016a). The remaining downward dips in the corrected (yellow) light curve aretransits of a mini-Neptune sized exoplanet, validated in this work and already confirmed in Osborn et al. (2017).

constrained, and our analysis method can leave insystematics. The plots we use to identify these falsealarms are shown in Figs. 2 and 3.

2. We compared the signal of a TCE in lightcurves produced using multiple different photomet-ric apertures. This test is a powerful way to iden-tify signals caused by instrumental systematics (asthese systematics present differently in differentphotometric apertures), as well as identifying as-trophysical false positives, such as when a candi-date transit signal was due to contamination froma nearby star. An example of these tests are shownin Fig. 3. We note that although this test rules outtransits or eclipses originating from a nearby com-panion, it does not rule out the possibility of lightcontamination from a nearby companion, whichcould dilute the observed transit and lead to an un-derestimation of the planetary radius (Ciardi et al.2015; Hirsch et al. 2017).

3. Individual transits of a TCE were visually in-spected, since instrumental false alarms were lesslikely to have consistent, planet-like transit depthsor shapes (see Fig. 2). This metric is qualitativelysimilar to the “transit patrol” metrics introduced inthe DR25 Kepler planet candidate catalog (in par-ticular the Rubble, Marshall, Chases, and Zumatests, Thompson et al. 2017).

4. Flux centroid motion, phase variations (possiblycaused by relativistic beaming, reflected light, or el-lipsoidal effects), differences in depth between oddand even numbered transits, and secondary eclipseswere all searched for as evidence of astrophysicalfalse positives. Similar tests have been used sincethe beginning of the Kepler mission (Batalha et al.

2010a). Example diagnostic plots for identifyingphase variations, the difference between even andodd numbered transits, and secondary eclipses nearphase 0.5 are shown in Fig. 2; flux-centroid shifttests are shown in Fig. 3. We searched for sec-ondary eclipses at arbitrary phases (not necessarilynear phase = 0.5) using the “model-shift unique-ness” test designed by Coughlin et al. (2016). Weshow diagnostic plots for the model-shift unique-ness test in Fig. 4.

5. We searched for astrophysical false positive scenar-ios by “ephemeris matching”. Sometimes the pix-els surrounding a target star can be contaminatedwith a small amount of light from other nearbystars. When those nearby stars are variable them-selves (like eclipsing binaries), the variability fromthe nearby stars can be introduced into the target’slight curve (Coughlin et al. 2014). We identifiedcases where this happened by searching for planetcandidates that have the same period (or integermultiples of the same period) and time of transitas eclipsing binaries observed by K2 using the samecriteria as Coughlin et al. (2014). We found no ex-amples of matched ephemerides due to direct PixelResponse Function (PRF) overlap that we had notalso identified in our tests with multiple photomet-ric apertures, but we did find two instances wherecandidate transit signals were caused by chargetransfer inefficiency along one of the columns ofthe Kepler detector. We excluded a candidatearound EPIC 212435047 caused by contaminationfrom the eclipsing binary EPIC 212409377 locatedalong the same CCD column about 2000 arcsec-onds away, and we excluded a candidate aroundEPIC 202710713 contaminated by the eclipsing bi-


nary EPIC 202685801 located along the same CCDcolumn at a distance of about 300 arcseconds.

6. We estimated the SNR of a TCE by taking thedifference between the mean baseline flux and thein-transit flux and dividing by the quadrature sumof the standard deviation of the flux in those tworegions. We defined the boundaries of the in-transitregion in two ways and calculated the SNR for bothchoices. In one case we used every data point col-lected between the second and third contact (mi-nus a single long-cadence Kepler exposure on ei-ther side). This estimate of SNR could sometimesnot be calculated if the transit was grazing. In theother case we used the central 20% of data collectedfrom the first to fourth contact (which could be cal-culated even if the transit was grazing). Followingstandard practice from the Kepler mission, if bothof these values (or just the latter in the grazingcase) were below 7.1σ the candidate was excluded(7.1σ is the minimum significance level for a signalto qualify as a TCE in the Kepler Science Pipeline;Jenkins et al. 2010). We only encountered two suchcandidates: EPIC 220474074 and EPIC 201289302.

Although it is possible to automate diagnostic testsof this type (see, for example, the Robovetter that wasdesigned for the main Kepler mission, Coughlin et al.2016), we performed vetting tests 1-4 by eye.

Any TCE surviving all of these vetting stages was pro-moted to “planet candidate” (∼1, 000 were promoted inthis way). All candidates orbiting sufficiently bright hoststars (see Section 3.1) were then subjected to our vali-dation process. Parameters for the 275 candidates thatsatisfied these requirements and were subjected to val-idation are listed in Table 4. Their associated stellarparameters are listed in Table 5.

3. SUPPORTING OBSERVATIONS

In this section, we describe follow-up observationswe conducted to better characterize the candidate hoststars. These observations are crucial for improving stel-lar parameters (e.g. Dressing et al. 2017a; Martinez et al.2017; Mann et al. 2017), which in turn can help differenti-ate between a transiting planet and various false positivescenarios (i.e. stellar binary configurations) that mightprefer different regions of stellar parameter space. Wefirst discuss high-resolution optical spectroscopy of theplanet candidate host stars from the Tillinghast Reflec-tor Echelle Spectrograph (TRES), followed by speckleimaging from the Differential Speckle Survey Instru-ment (DSSI) and the NASA Exoplanet Star and SpeckleImager (NESSI) at the WIYN telescope32, the GeminiSouth telescope, and the Gemini North telescope, thenlastly adaptive optics imaging from Keck Observatory,Palomar Observatory, Gemini South Observatory, Gem-ini North Observatory, and the Large Binocular Tele-scope Observatory.

3.1. The Tillinghast Reflector Echelle Spectrograph

32 The WIYN Observatory is a joint facility of the Universityof Wisconsin-Madison, Indiana University, the National OpticalAstronomy Observatory, and the University of Missouri.

All of the spectra used in this work were obtainedwith TRES, a spectrograph with a resolving power ofR = 44,000 and one of two spectrographs for the 1.5 me-ter Tillinghast telescope at the Whipple Observatory onMt. Hopkins in Arizona. We obtained at least one us-able TRES spectrum of each of the planet candidate hoststars that we consider in this work and that we subject toour validation process (see Section 4.2 for our definitionof “usable”). With a few exceptions, we only observedcandidates brighter than 13th magnitude in the Keplerband with TRES because of the lengthy integration timerequired to collect spectra of stars fainter than this andthe difficulty of subsequent follow-up observations (forexample, with precise radial velocities) at other facili-ties. This limitation reduced the number of candidateswe considered for validation significantly, from ∼1, 000to 275. In the future, observing these fainter candidates,either with TRES or other spectrographs on larger tele-scopes, could potentially more than double the numberof K2 planets for our analysis.

3.2. Speckle Observations

We observed many of our planet candidates withspeckle imaging from either the 3.5-m WIYN telescope,the Gemini-South 8.1-m telescope, or the Gemini-North8.1-m telescope. Together, the three telescopes collected162 speckle images of 73 stars with DSSI (Horch et al.2009). DSSI is a speckle imaging instrument that travelsbetween different telescopes. For each of the 73 targets,we collected DSSI speckle images at narrow band filterscentered at 6920 A and 8800 A (at least one of each forevery target). These observations were made in Septem-ber and October of 2015, as well as January, April, andJune of 2016.

Further, 160 speckle images were collected for a dis-tinct sample of 70 stars at the WIYN telescope usingNESSI, which is essentially a newer version of the DSSIinstrument. For each of the 70 targets, we collectedNESSI speckle images at narrow band filters centered at5620 A and 8320 A (at least one of each). These observa-tions were made in October through November of 2016and March through May of 2017. A list of the observedstars can be found in Table 7.

3.3. Adaptive Optics Observations

In addition to speckle imaging, we also observed manyof our planet candidate host stars with adaptive optics(AO) imaging.

We collected 47 AO images for 45 stars on the KeckII 10-m telescope in K filter with the Near Infra RedCamera 2 (NIRC2); 5 of those stars were also imagedusing NIRC2 in J band. All of these observations weremade during April, July, August, and October of 2015as well as January and February of 2016.

We collected 27 AO images for 27 stars on the Palomar5.1-m Hale telescope in K filter with the Palomar HighAngular Resolution Observer (PHARO, Hayward et al.2001); 6 of those stars were also imaged using PHAROin J band. All of these observations were made dur-ing February, May, and August of 2015 as well as June,September, and October of 2016.

We collected 19 AO images for 18 stars on the Gemini-North 8.1-m telescope in K band with the Near In-fraRed Imager and spectrograph (NIRI, Hodapp et al.

6 Mayo et al.

2400 2420 2440 2460BJD − 2454833

0.998

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1.001

1.002

2400 2420 2440 2460BJD − 2454833

0.9985

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−10 −5 0 5 10Days from Midtransit

0.9985

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0.9985

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0.9995

1.0000

1.0005Secondary

−5 0 5Hours from Phase = 0.5

0.9998

0.9999

1.0000

1.0001

1.0002

EP 212521166, Cand. 1 of 1Campaign 6Period = 13.863953 daysDuration = 3.2 hoursImpact = 0.31Rp/R* = 0.0331Depth = 0.133%sqrt(depth) = 0.0365

Kp = 11.6, CDPP6 ¾ 16.3 ppmRA: 13:49:23.9, Dec: -12:17:04J: 10.18, H: 9.64, K: 9.61B: 12.834, V: 11.915, R: 11.56PMRA: 42.6, PMDec: -101.2B-V =0.919 --> R* = 0.79 RO •

--> Rplanet = 2.8 Rearth

-5 0 5Hours from Midtransit

0.992

0.994

0.996

0.998

1.000

Even

-4 -2 0 2 4Hours from Midtransit

Odd

-4 -2 0 2 4Hours from Midtransit

0.9985

0.9990

0.9995

1.0000

1.0005

0 2 4 6 8 10Arclength [arcseconds]

0.997

0.998

0.999

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1.001

0 2 4 6 8 10Arclength [arcseconds]

0.9985

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EPIC 212521166, Candidate 1 of 1

Figure 2. Diagnostic plots for EPIC 212521166.01. Left column, first (top) and second rows: K2 light curves without and with lowfrequency variations removed, respectively. The low frequency variations alone are modeled in red in the first row, whereas the best-fittransit model is in red in the second row. Vertical, brown, dotted lines denote the regions into which the light curve was separated tocorrect roll systematics. Left column, third and fourth rows: phase-folded, low frequency corrected K2 light curves. In the third row,the full light curve is shown (points more than one half period from the transit are gray), whereas in the fourth row, only the light curvenear transit is shown. The red line is the best-fit model and the blue points are binned data points. Middle column, first and secondrows: arclength of centroid position of star versus brightness, after and before roll systematics correction respectively. Red points denotein-transit data. In the second row, small orange points denote the roll systematics correction made to the data. Middle column, third row:separate plotting and modeling of odd (left panel) and even (right panel) transits, with orange and blue data points respectively. The blackline is the best-fit model, the horizontal red line denotes the modeled transit depth, and the vertical red line denotes the mid-transit time(this is useful for detecting binary stars with primary and secondary eclipses). Middle column, fourth row: light curve data in and aroundthe expected secondary eclipse time (for zero eccentricity). Blue data points are binned data, the horizontal red line denotes a relativeflux = 1, and the two vertical red lines denote the expected beginning and end of the secondary eclipse. Right column: individual transits(vertically shifted from one another) with the best-fit model in red and the vertical blue lines denoting the beginning and end of transit.

2003). These observations were made during Octoberand November of 2015 as well as June and October of2016.

We collected a single AO image on the Large BinocularTelescope in K filter with the L/M-band mid-InfraRedCamera (LMIRCam, Leisenring et al. 2012). This obser-vation was made in January of 2015.

There was some overlap between instruments; overall,AO images were collected for a total of 80 systems. Alist of the observed stars can be found in Table 7.

4. DATA ANALYSIS

Once all of the photometry had been reduced and all ofthe necessary follow-up observations had been collected,the next step was to analyze the data, calculate relevantparameters, and prepare the results for the validationprocess. In this section, we explain the process of fittinga model to our reduced light curves (to determine transitparameters and create folded light curves), analyzing our

spectra (to calculate stellar parameters), and extractingand reducing data from our high-contrast images (to cre-ate contrast curves).

4.1. K2 light curves

4.1.1. Simultaneous Fitting of K2 Systematics and TransitParameters

In Sections 2.2, 2.3, and 2.4 we described the processof correcting K2 photometry for instrumental systemat-ics and exploring the reduced light curves for candidates.Once those steps were complete, the planet candidatesneeded to be more thoroughly characterized. In order toassess transit and orbital parameters, we re-produced theK2 light curves for these planet candidates, re-derivingthe systematics correction while simultaneously model-ing the transits in the light curve. As in our originalsystematics correction, the light curve was divided intomultiple sections and the systematics correction was ap-plied to each section separately. A piecewise linear func-


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Figure 3. Diagnostic plots for EPIC 212521166.01. Left column, first (top), second, and third rows: images from the first Digital SkySurvey, the second Digital Sky Survey, and K2 respectively, each with a scale bar near the top and an identical red polygon to show theshape of the photometric aperture chosen for reduction. The K2 image is rotated into the same orientation as the two archival images(north up). Middle column, top row: multiple panels of uncorrected brightness versus arclength, chronologically ordered and separated intothe divisions in which the roll systematics correction was calculated. In-transit data points are red, orange points denote the brightnesscorrection applied to remove systematics. Middle column, bottom row: variations in the centroid position of the K2 image. In-transitpoints are red. The discrepancy (in standard deviations) between the mean centroid position in-transit and out-of-transit is shown onthe right side of the plot. Right column, first row: the K2 light curve near transit as calculated using three differently sized apertures:“Small mask” (top panel), “Medium mask” (middle panel), and “Large mask” (bottom panel), each with the identical best-fit model inred. Aperture-size dependent discrepancies in depth could suggest background contamination from another star. Right column, third row:the K2 image overlaid with the three masks from the previous plot shown (in this figure, the large mask is fully outside the postage stampand is therefore not visible).

tion was fit with breaks roughly every 0.25 arcseconds(varying slightly by target) to the arclength v. brightnessrelationship described in section 2.2 (arclength is a one-dimensional measure of position along the path an imagecentroid traces out on the Kepler CCD camera). Thelow-frequency variations in the light curve were modeledwith a cubic spline (with breakpoints every 0.75 days),and the transits themselves were modeled with the Man-del & Agol (2002) transit model. The fit was performedusing a Levenberg-Marquardt optimization (Markwardt2009), and all of the parameters from the optimization(besides the transit parameters) were used in order tocorrect the systematics of the light curve (once again)and remove the low-frequency variations (once again).Since these parameters were determined in a simultane-ous fit with the transits, the quality of the resulting lightcurves reduction tended to be better than the originallight curves.

4.1.2. Final Estimation of Transit Parameters andUncertainties

After we produced the systematics-corrected, low-frequency-extracted light curves, we analyzed them fur-ther in order to estimate final transit parameter valuesand their uncertainties. We based our model on theBATMAN Python package (Kreidberg 2015), which we usedto calculate our synthetic transit light curves. We fitthe transit light curves of all planet candidates arounda given star simultaneously so that overlapping transitscould be modeled, assuming that each of the planets werenon-interacting and on circular orbits. For each planetcandidate, five parameters were included: the epoch (i.e.time of first transit), the period, the inclination, the plan-etary to stellar radius ratio (Rp/R∗), and the semi-majoraxis normalized to the stellar radius (a/R∗). Addition-ally, two parameters for a quadratic limb-darkening lawwere included (Kipping 2013), as well as a parameter toallow the baseline to vary (in case there was an erro-neous systematic offset from flux = 1 outside of transit),and a noise parameter that assigned the same uncertain-ties to each flux measurement (since flux error bars were

8 Mayo et al.

Figure 4. Model-shift uniqueness diagnostic plots for EPIC 212521166.01. We cross-correlated the phase-folded light curve of eachplanet candidate with the candidate’s best-fitting transit model. The two plots in the top row show the cross-correlation function as afunction of orbital phase with different scaling on the Y-axis. The tallest peak in the response is the primary transit, and the three verticallines show the phase of the highest significance putative secondary event (red) , the second highest significance putative secondary event(orange), and the highest significance “upside-down” secondary event (blue). The bottom row of plots show the three segments of thelight curve surrounding the highest and second highest significance putative secondary eclipses, and the highest significance “upside-down”event. Grey and purple data points are unbinned and binned observations respectively. Comparing the amplitudes of these three eventsgives an indication of their significance. Here, the two most significant putative secondary eclipses have a similar amplitude to the mostsignificant upside-down event, indicating that they are all likely spurious. We find no significant secondary eclipse in the light curve ofEPIC 212521166.01.

not calculated in the K2 data reduction process). Forall of these planet and system parameters we assumed auniform prior, except for the Rp/R∗ parameter for eachplanet, which we gave a log-uniform prior.

For each candidate system, the transit parametersin this model were estimated using emcee (Foreman-Mackey et al. 2013), a Python package that runs simula-tions using a Markov chain Monte Carlo (MCMC) algo-rithm with an affine invariant ensemble sampler (Good-man & Weare 2010). In each simulation, the parameterspace for a system with n candidates was sampled with8 + 10n chains (equal to twice the number of model pa-rameters). The MCMC process was ran for either 10,000steps or until convergence, whichever came last. Con-vergence was defined according to the scale-reductionfactor (Gelman & Rubin 1992), a diagnostic that com-pares variance for individual chains against variance ofthe whole ensemble. A simulation was considered con-verged when the scale reduction factor was less than 1.1for each parameter. The Gelman-Rubin scale-reductionfactor is properly defined for chains from distinct, non-communicating MCMC processes; however, we foundthat our simulations visually converged many times morequickly than the Gelman-Rubin diagnostic, so we decidedthe diagnostic would be sufficient for our purposes. Anexample of a converged model fit against transit data canbe seen in Fig. 5.

Additionally, each simulation was checked after the

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Figure 5. Fit of our transit model to corrected and normalizedlight curve data for EPIC 212521166.01. The yellow points are theobserved data, normalized and phase-folded to the orbital periodof the planet. The black line is our transit model with the medianparameter values determined from an MCMC process. The darkblue and light blue regions are 1σ and 3σ confidence intervals,respectively.

minimum number of steps (10,000) and at the end ofthe simulation for any chains in the ensemble that couldbe easily categorized as “bad”, i.e. trapped in a mini-


mum of parameter space with a poorer best fit than theminimum of the ensemble majority. In detail, a chainwas classified as “bad” if both of the following applied:

1. The Kolmogorov-Smirnov statistic between thechain with the highest likelihood step and the chainin question was greater than 0.5.

2. θl/θg < 1/(100n), where θl is the local maxi-mum likelihood (the maximum likelihood withinthe chain in question), θg is the global maximumlikelihood throughout the ensemble, and n is the to-tal number of steps. This test is our own invention,which is more likely to classify a chain as bad whenits maximum likelihood is further from the globalmaximum likelihood. This test also accounts forthe length of the simulation, since the maximumlikelihood within each chain should be closer to theglobal maximum likelihood for longer simulations.We include a factor of 100 in the denominator tomake the test sufficiently conservative, such thatit only finds bad chains very rarely and only thoseextremely unlikely to rejoin the ensemble in thelifetime of the simulation.

If a chain was deemed bad after 10,000 steps, its posi-tion in parameter space was updated to that of a goodchain from the previous step of the simulation. If a chainwas deemed bad at the end of the simulation, it was sim-ply removed and not replaced. Both after 10,000 stepsand at the end of the simulation, bad chains only oc-curred about 15% of the time, typically for only one ortwo chains in the ensemble.

A representative sample of the converged posteriors foreach exoplanet system transit fit has been archived athttps://zenodo.org/record/1164791.

4.2. TRES Spectroscopy

We first visually inspected each of the spectra collectedwith TRES for our candidate host stars. Our main goalin visually inspecting the spectra was to identify cases inwhich the spectra were composite or otherwise indicativeof multiple stars in the system. We looked at diagnos-tic plots produced by the TRES pipeline, which showedvarious echelle orders and a cross-correlation between asynthetic template spectrum and a single spectral orderaround 5280 A.

After identifying composite spectra and confirmingthat the others were apparently single-lined, we preparedthe spectra before determining the host stars’ parame-ters. In particular, we manually removed cosmic raysfrom the spectra that might bias or otherwise affect thespectroscopic parameters we measured. We focused onthree echelle orders in particular, orders 22, 23, and 24(covering 5059-5158, 5135-5236, and 5214-5317 A respec-tively), which are within the range we used to measurespectroscopic parameters.

Once we finished visually inspecting each spectrum andremoving cosmic rays, we analyzed each TRES spectrumusing the Stellar Parameter Classification (SPC) tool,developed by Buchhave et al. (2012). SPC determineskey stellar parameters through a comparison of the in-put spectrum (between 5050 and 5360 A) to a librarygrid of synthetic model spectra, developed by Kurucz

(1992). The library is 4-dimensional, varying in effec-tive temperature Teff , surface gravity log g, metallicity[m/H], and line broadening (a good proxy for projectedrotational velocity, or v sin i). [m/H] is estimated ratherthan [Fe/H] because all metallic absorption features areused to determine metallicity rather than just iron lines.(SPC assumes all relative metal abundances are the sameas in the Sun, and [m/H] simply scales all solar abun-dances by the same factor.) This library grid spans Teff

from 3500 K to 9750 K in 250 K increments, log g from0.0 to 5.0 (cgs) in 0.5 increments, [m/H] from -2.5 to +0.5in 0.5 dex increments, and line broadening from 0 km s−1

to 200 km s−1 in progressively spaced increments (from1 km s−1 up to 20 km s−1). In total, the library contains51,359 synthetic spectra. The stellar parameters derivedusing SPC can be found in Table 5.

We also calibrated TRES against Duncan et al. (1991)for the SHK stellar activity index, a measure of thestrength of emission in the cores of the H and K CaII spectral absorption features. Our calibration was onlyperformed over a range of 0.244 < B-V < 1.629, 0.055 <SHK < 2.070, and v sin i < 20 km s−1. Additionally, werequired a photon count of more than 250,000 in the Rand V continuum regions (3901.07±10 Aand 4001.07±10Arespectively). Within those ranges, we were able tocalculate SHK for 28 of our spectra collected for 4 stars.Although there are relatively few K2 planet candidatesbright enough for this measurement on a 1 meter tele-scope, it will be much more common with TESS. A notehas been made for the relevant stars in Table 5 and thefull results are listed in Table 3. There is also a detaileddescription of the SHK calibration process for TRES inthe Appendix.

In cases where we observed a candidate host star morethan once with TRES, we attempted to identify or ruleout large velocity variations indicating a stellar compan-ion to the host star. (For this purpose we collected onenew TRES spectrum each for EPIC 220250254 and EPIC210965800, but otherwise exclusively used the spectrafrom which we derived stellar parameters.) We phasedthe radial velocities to the photometric ephemeris and fita sinusoid to the velocities at the period and ephemeris ofeach candidate (and assuming a circular orbit) in orderto estimate the companion mass and mass uncertainty.If the companion mass was more than 3σ lower than 13Jupiter masses, we ruled out the eclipsing binary scenario(see Section 5.1 and Table 6). If the semi-amplitude ofthe companion mass was more than 1 km s−1 we labeledthe system as a binary. Five systems were labeled bina-ries in this manner (see Table 4). If neither of the abovecases was true, no action was taken.

Out of the 233 candidate host stars, 43 had more thanone TRES spectrum available. The stellar parameterscalculated for the spectra of such candidates were com-bined via a weighted average based on the peak heightof the cross-correlation function. The scatter betweenmultiple spectra for the same candidate was not largerelative to the assumed systematic errors. For example,Buchhave et al. (2012) set an internal error floor of 50 Kfor effective temperature; we found an average standarddeviation of 40 K between spectra of the same candidate,and the scatter was less 100 K for ∼90% of candidateswith multiple spectra.

10 Mayo et al.

There were some instances in which a TRES spectrumwas not considered good enough for stellar parameterestimation with SPC. In particular, we did not use anyspectrum for which the SNR per resolution element was< 20 or the cross-correlation function peak height of thespectrum was < 0.8. Further, we also did not use anyspectra that yielded SPC results outside of certain trust-worthy ranges. Specifically, we only used spectra thatyielded 4250 < Teff < 6500 and line broadening < 50km s−1. It should also be noted that all spectra used todetermine stellar parameters were collected with TRESon or before 2017 June 10 (although some usable spectrahave since been collected, they were not retroactively in-cluded in our stellar parameter analysis). No planet can-didate underwent the validation process unless their hoststar had at least one spectrum (collected with TRES)that satisfied these criteria.

4.3. Contrast Curves

We quantified the constraints placed on the presenceof additional companions in our high-resolution (speckleand adaptive optics) imaging by calculating “contrastcurves”. A contrast curve specifies at a given distancefrom the target star how bright a companion star wouldhave to be in order to be detected.

Once speckle observations were collected, the data werereduced according to method described in Furlan et al.(2017), yielding a high-contrast image of a candidate.Then local minima and maxima were analyzed relativeto the star’s peak brightness to determine ∆m (averagesensitivity) and its uncertainties within bins of radial dis-tance from the target star. The contrast curves used inthis research were the 5σ upper limit on ∆m as a func-tion of radial distance. A more detailed description ofthe data reduction process can be found in Howell et al.(2011). An example of a contrast curve can be seen inFig. 6.

As for AO observations, the creation of correspondingcontrast curves was performed by injecting fake sourcesinto the images and varying their brightness in order todetermine the brightness threshold for the detection al-gorithm being used. This process is described in greaterdetail in Crossfield et al. (2016); Ziegler et al. (2017)

Note that these processes of creating a contrast curvewere the same regardless of wavelength. So in the in-stances that multiple speckle or adaptive optics imagesat different wavelengths were available, multiple contrastcurves were created that were all used in the validationprocess for a given candidate.

5. FALSE POSITIVE PROBABILITY ANALYSIS

5.1. The Application of vespa to Planet Candidates

Our validation work relied primarily on a methodcalled Validation of Exoplanet Signals using a Proba-bilistic Algorithm, or vespa, a public package (Morton2015b) based on the work of Morton (2012). It operateswithin a Bayesian framework and calculates the FalsePositive Probability (FPP), the probability that a candi-date is an astrophysical false positive rather than a truepositive (i.e. a planet).

Once photometry, spectroscopy, and any availablehigh-contrast imaging had been collected and reducedfor a candidate system, that system underwent our val-

idation procedure using vespa. For each candidate, thefollowing information was supplied:

1. A folded light curve containing the planetary tran-sit and roughly one transit duration of baseline oneither side. Identical error bars were assigned toall data points based on the noise parameter deter-mined by our transit fitting procedure. This lightcurve had the presence of other planets in the sys-tem removed using the best-fit parameters deter-mined by the fitting procedure.

2. A secondary threshold limit. We calculate thislimit by first cutting out all transits from all can-didates in a system. Then, for a given candidate,we phase-fold the data to the candidate’s period,bin the baseline flux according to the transit du-ration of the candidate, calculate the standard de-viation between the bin averages, and multiply bythree. Effectively, we are asserting that a secondaryeclipse has not been detected at a 3σ level or higher.

3. A contrast curve. When available, this loweredthe FPP by eliminating the possibility of boundor background stars above a certain brightness ata given projected distance, thus reducing the pa-rameter space in which a false positive scenariocould exist. Note that vespa doesn’t require a con-trast curve to operate, and in many cases a candi-date host star had no contrast curve data available.However, contrast curves were collected from AOor speckle data and provided to vespa for 186 ofour 233 candidate host stars (see Table 7).

4. RA and Dec. The likelihood of a false positive sce-nario is calculated by vespa based on the targetstar’s location on the celestial sphere. For exam-ple, near the Galactic plane a target star’s FPPwill increase significantly due to the crowded field.

5. Teff , log g, and [m/H] (collected from SPC). Theseconstraints help rule out false positive scenariosthat would otherwise be allowed given only stellarmagnitude information. Although vespa could op-erate without these values, we did not apply vespato any candidate system for which stellar parame-ters could not be estimated from a TRES spectrum.

6. Stellar magnitudes. The K2 Ecliptic Plane InputCatalog (Huber et al. 2016) was queried to findmagnitude information on each target star in theKepler, J, H, and K band passes. The J, H, andK band passes originated from the 2MASS catalog(Cutri et al. 2003; Skrutskie et al. 2006). Mag-nitude uncertainties were not required or providedfor the Kepler band pass, while uncertainties for theJ, H, and K band passes were added in quadraturewith 0.02 magnitudes of systematic uncertainty tobe conservative.

7. Parallaxes. Whenever parallaxes were availablefrom HIPPARCOS (Perryman et al. 1997) or GAIA(Gaia Collaboration et al. 2016a,b) those were alsoincluded.


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12 Mayo et al.

Given all this input, vespa makes a representative pop-ulation for each false positive scenario (and the transitingplanet scenario). False positive scenarios considered byvespa include a background (or foreground) eclipsing bi-nary blended with the target star, a hierarchical eclipsingbinary system, or a single eclipsing binary system (as wellas each of those scenarios with twice the period). Thenvespa calculates a prior for each scenario by multiplyingtogether the probability that the scenario exists withinthe photometric aperture, the geometric probability thatthe scenario leads to an eclipse, and the fraction of in-stances in which the eclipse is appropriate. Here “appro-priate” means an instance’s eclipse takes place within thephotometric aperture, the secondary eclipse (if it exists)is not deep enough to cross the detection threshold, theinstance’s primary star has wavelength-dependent mag-nitudes within 0.1 magnitudes of those provided as in-put, and the instance’s primary star has Teff and log gthat agree with the input values to within 3σ.

Then the likelihood for each scenario is calculated us-ing the folded light curve by fitting against a distributionof transit durations, depths, and ingress/egress slopescalculated from each scenario. Once priors and likeli-hoods have been determined for each scenario, the laststep is simply to combine them for each scenario in or-der to determine an overall posterior likelihood for everyscenario. If the posterior likelihood for the planet sce-nario is exceedingly larger than all of the other scenarioscombined, then the candidate can be classified as a val-idated planet. In our case, we required the sum of allfalse positive scenario probabilities to be < 0.001.

The output from vespa includes simulation informa-tion from the underlying light curve fitting process, aswell as figures and text files conveying likelihood in-formation of various false positive scenarios and thetransiting planet scenario. Section 6.1 provides a con-crete validation example with characteristic input andoutput. Additionally, the full vespa input and out-put for each exoplanet candidate has been archived athttps://zenodo.org/record/1164791.

As we noted in Section 4.2, for systems where we hadcollected more than one good TRES spectrum, we phasedthe RVs to search for or eliminate the possibility of aneclipsing binary scenario. (Small RVs would not ruleout hierarchical or background eclipsing binary scenar-ios since large RVs would be reduced by the third starin the aperture.) In cases where the eclipsing binary sce-nario could be eliminated, we reduced the probability ofthe scenario (and the similar scenario analyzed by vespawith double the period) to zero. We then divided theprobability of all the remaining scenarios investigated byvespa by their sum so that the total probability was stillone. The values reported in Table 6 already have thisadjustment applied.

Systems with multiple planet candidates are morelikely to be hosting multiple planets than multiple falsepositive signals. In fact, the likelihood of the planetscenario for each individual candidate is consequentlyboosted relative to false positive scenarios in multiplanetcandidate systems (Latham et al. 2011). To account forthis effect, we apply a “multiplicity boost” to the planetscenario prior in such systems, deflating the FPP by themultiplicity boost factor to account for the nature ofthese systems. We choose a boost factor of 25 for double

candidate systems and a boost factor of 50 for systemswith 3+ candidates based on the values used by Lissaueret al. (2012), Vanderburg et al. (2016b), and Sinukoffet al. (2016). The FPP values reported in Table 4 alreadyhave the appropriate multiplicity boost factor applied.

5.2. Criteria for Planet Validation

Following standard practice, we only validated planetsfor which the following were true, since vespa assumeswe have checked for and ruled out each of them:

1. There is not a composite spectrum.

2. There is not a companion in the aperture. (Thiswas determined from archival imaging.)

3. There is not a companion in AO and/orspeckle images. (This was determined fromour AO and speckle images as well asany images for our candidates uploaded tohttps://exofop.ipac.caltech.edu/k2/ before 2017August 9.)

4. There is no evidence of a secondary eclipse (at anyarbitrary phase).

5. There is not an ephemeris match (see Section 2.4).

If any of the above were false, the FPP was not re-ported in Table 4 and the candidate was not validatedregardless of the FPP value vespa provided.

It is worth noting that recently there have been sixvalidated planets shown to be false positives by follow-upobservations and analysis (Cabrera et al. 2017; Shporeret al. 2017). We briefly examine whether these instancesare a cause for concern in our own results.

In the case of Cabrera et al. (2017), they found thattwo false positives exhibited increased transit depths forlarger aperture masks (suggesting a nearby star was re-sponsible for the eclipses) while the third showed a sec-ondary eclipse at phase = 0.62 when they used a differ-ent data reduction process. The first two false positiveswould have failed the variable-sized mask test we applyvia our diagnostic plots, while the secondary eclipse fromthe third false positive would have been caught througha combination of our data reduction process and the“model-shift uniqueness” test we apply (Coughlin et al.2016).

As for Shporer et al. (2017), the vespa fit to the avail-able photometry for each false positive was very poorand all three of the false positives were reported to bevery large “planets”. We addressed these concerns in twoways. First, we decided to only use 2MASS photometryin order to avoid systematic errors between photometricbands. Second, we chose not to validate any planet can-didates larger than 8 R⊕, since a candidate of that sizeor larger could actually be a small M dwarf. The only ex-ception to this rule is if there are RV measurements thatcan rule out the eclipsing binary scenario, in which casewe do report the FPP (and validate for FPP < 0.001)regardless of planet size.

6. RESULTS

The results section is divided into two parts. In thefirst part, the process of validation is described in detail


Table 1System and planetary parameters of EPIC 212521166

Parameter Unit This Paper Osborn et al. (2017)Orbital parameters

Period P days 13.86391+0.00022−0.00023 13.86375± 2.6×10−4

Time of first transita BJD-2454833 2386.87440+0.00072−0.00068 2442.32992± 6.1×104

Orbital eccentricity e - 0 (fixed) 0.079± 0.07Inclination degrees 89.36+0.43

−0.75 89.35+0.41−0.24

Transit parameters

System scale a/R∗ - 32.3+2.0−5.7 30.8± 1.0

Impact parameter b - 0.36+0.28−0.23 0.34+0.14

−0.22

Transit duration T14 hours 3.181+0.072−0.047 3.22± 0.03

Radius ratio Rp/R∗ - 0.0334+0.0018−0.0007 0.0333± 6.6×10−4

Planet parameters

Planet radius Rp R⊕ 2.52+0.16−0.10 2.592± 0.098

Stellar parameters

Stellar mass M∗ M� 0.724± 0.025 0.738± 0.018Stellar radius R∗ R� 0.692+0.025

−0.023 0.713± 0.020Effective temperature Teff K 4877± 50 5010± 50Surface gravity log g g cm−2 4.51± 0.10 4.60± 0.03Metallicity [m/H]a dex −0.30± 0.08 −0.34± 0.03

Validation parameters

FPP - 8.44×10−7 -

aOur reported transit time and that reported by Osborn et al.(2017) differ by 4 orbital periods.bOur reported metallicity is [m/H] (derived from many metal ab-

sorption features) while the metallicity reported in Osborn et al.(2017) is [Fe/H] (derived from iron absorption lines only).

for a single planet candidate, in order to explain preciselyhow the photometry and follow-up observations are used.In the second part, our validation process is more widelyapplied to every selected candidate and the results foreach candidate are reported.

6.1. Validating a single planet: EPIC 212521166.01

In order to understand the process that was applied toeach of our candidates, it is instructive to look at valida-tion for a single, concrete example. Here, we describe indetail the validation process for a typical planet candi-date system, EPIC 212521166 (K2-110). We chose thissystem because 1) it was detected in our pipeline, and2) Osborn et al. (2017) has already confirmed and char-acterized the planet, which allows us to compare someof the system parameters we calculated against their re-sults.

EPIC 212521166 was observed by K2 during Campaign6. After we produced a light curve from calibrated K2pixel data and removed systematics (as described in Sec-tion 2.2), we searched for transits in our processed lightcurve (as described in Section 2.3). Our transit searchpipeline detected a single, high signal-to-noise thresholdcrossing event with a period of 13.87 days and a depthof about 0.1%. The signal passed triage (see Section 2.3)and moved on to vetting (see Section 2.4). We confirmedthe signal was transit-like, and observed no significantsecondary eclipse, phase variations, differences in depthbetween odd and even transits, aperture-size dependent

transit depths, or other indications of a false positive orinstrumental false alarm (see Figs. 2, 3, and 4). As a re-sult, we promoted the EPIC 212521166 threshold cross-ing event to a planet candidate.

Upon its identification as a planet candidate, we ob-served EPIC 212521166 with the TRES spectrograph onthe Mt. Hopkins 1.5m Tillinghast reflector and with theDSSI speckle imaging camera on the 3.5m WIYN tele-scope at Kitt Peak National Observatory. Using the or-bital and transit parameters determined with our tran-sit model, the stellar parameters derived from SPC, afolded light curve of the planetary transit, and two con-trast curves in r-band and z-band collected via high-contrast speckle imaging from DSSI on the WIYN tele-scope (see Fig. 6), vespa was employed to determine theFPP for EPIC 212521166.01. The FPP was found to be8.44×10−7, which was well below the cutoff threshold, sothe planet candidate was classified as validated. The keyoutput figure of vespa can be seen in Fig. 7.

Like us, Osborn et al. (2017) found EPIC 212521166to be a metal-poor K-dwarf star hosting planet candi-date with P = 13.9d and Rp = 2.6 R⊕. A comparisonof planetary and system parameters can be see in Table1. Our analyses and theirs are in good agreement for allparameters. Additionally, Osborn et al. (2017) took thefurther step of obtaining precise radial velocity observa-tions to confirm the existence of EPIC 212521166.01, sowe can be confident that in this case, vespa’s assessmentof a low false positive probability was well justified.

14 Mayo et al.

Figure 7. False Positive Probability analysis of EPIC 212521166.01. HEB, EB, and BEB refer to a hierarchical eclipsing binary, eclipsingbinary, and background eclipsing binary scenario respectively. Combining the prior likelihood of a false positive scenario (given sky position,contrast curve data, and wavelength-dependent magnitudes), as well as the likelihood of the transit photometry under various scenarios,the posterior distribution highly favors the planet scenario, with FPP = 8.44×10−7. (Note: the true FPP value is always reported in asupplementary file, but for FPP < 1 in 1e6 the figure produced by vespa simply reports the FPP as < 1 in 1e6.)


6.2. Full Validation Results

The process of validation described for EPIC212521166.01 in the previous section was similarly ap-plied to the remaining candidates suitable for validation.We identified 275 candidates in 233 systems that hadat least one usable TRES spectrum, and the FPP wascalculated for each of these candidates (see Table 4).

Occasionally vespa failed to return a FPP; in suchcases, the lowest data point in the light curve was re-moved (to aid the initialization process for vespa’s trape-zoidal transit fit) and vespa was reran. This approachworked in most cases, but if it failed again the lowest twodata points were removed and vespa was reran. If thattoo was unsuccessful then the FPP was not reported.(Most of the time vespa only failed after these steps be-cause of a Roche lobe overflow error.) 149 candidates in111 systems had a FPP < 0.001 and were thus promotedto validated planet status.

To date, the largest single release of K2 validation re-sults has been Crossfield et al. (2016), with 197 candi-dates and 104 validated planets in C0-C4. In comparison,108 of our candidates are from C0-C4, 69 of which arevalidated. The two samples share 53 candidates in com-mon, 37 of which are validated and 9 of which remaincandidates in both analyses. (Additionally, 2 candidatesin common are only validated in this work while 5 areonly validated in Crossfield et al. 2016). That leaves 55candidates in our C0-C4 sample (30 of which are vali-dated) that were undetected by Crossfield et al. (2016),as well as 146 candidates (62 of which are validated) inthe Crossfield et al. (2016) sample undetected in our ownC0-C4 sample. Only ∼21% of the total candidates weredetected by both analyses, and only ∼26% of the totalvalidated planets were validated by both analyses.

Table 2Breakdown of Candidate Dispositions

Previous Updated DispositionDisposition1 VP PC All

VP 53 15 68PC 39 55 94FP 12 13 2UK 56 55 111All 149 126 275

1 VP = Validated Planet, PC = Planet Candidate, FP = False

Positive, UK = Unknown2 EPIC 210894022.01. See Section 6.23 EPIC 202900527.01. See Section 6.2

The sample overlap may seem surprisingly small, butit makes more sense when the candidate selection andvalidation processes are examined. For example, Cross-field et al. (2016) only considered candidates with 1d <P < 37d (19% of our C0-C4 sample was outside thatrange) and we only considered candidates with Kp < 13(48% of their sample was outside that range). If we onlyconsider C0-C4 candidates within those ranges (137 to-tal), both teams find over half of each other’s samples,and the overlap between samples rises to 39% (53 can-didates). Similarly, for validated planets within thoseranges (77 total), both teams find more than two thirds

of each other’s samples, and the overlap between samplesrises to 57% (44 validated planets).

There are many further examples of differences thatcreated discrepancies between the two samples. We re-quired that each planet candidate had at least one us-able TRES spectrum (see Sections 3.1 and 4.2), eventhough in early campaigns TRES spectra weren’t col-lected for all bright candidates. This led to the exclu-sion of many otherwise promising candidates that areincluded in Crossfield et al. (2016). Further discrepan-cies could have arisen from the temperature and planetradius cuts applied to our validated planet sample, theelimination of objects with companions closer than 4” inthe Crossfield et al. (2016) candidate sample, and a dif-ference in significance thresholds for TCEs (we used 9σwhile they used 12σ).

Table 2 compares the candidate dispositions found inthis work against their previous dispositions (accord-ing to the NASA Exoplanet Archive33 and the Mikul-ski Archive for Space Telescopes34 (both accessed 2018February 14). We should note that 15 of our candi-dates were not validated in this work even though theyhave been previously validated elsewhere. However, allof these candidates were either restricted from being vali-dated by our conservative criteria for validation (see Sec-tion 5.2), or had a FPP value close to our validation cut-off of FPP = 0.001, or were validated using different oradditional observations as input to vespa. We also notethat our work classifies two targets previously labeled asfalse positives: EPIC 202900527.01 (K2-51 b) and EPIC210894022.01 (K2-111 b). Shporer et al. (2017) clearlyshowed EPIC 202900527.01 to be a stellar binary. Wedon’t claim otherwise by labeling it a candidate (sincewe label all targets with FPP > 0.001 as candidates).On the other hand, Crossfield et al. (2016) previouslyidentified EPIC 210894022.01 as a false positive, but asubsequent, improved vespa run showed the target to infact be a planet (I. Crossfield, private communication).Therefore we do claim this target to be validated.

Another case worth mentioning is the multiplanet sys-tem EPIC 228725972, which hosts one validated planetand one candidate ruled out by a companion in the aper-ture and in a NESSI speckle image. The smallest aper-ture mask we tested excluded the companion (locatedapproximately 12 arcseconds from the primary) but onlyexhibited transits for one of the candidates, hence thedifference in flags for the two candidates.

In addition to the FPPs and other parameters derivedthrough the validation process described in previous sec-tions, we also calculated the radii and masses of thestars in our sample (having a stellar radius allowed usto calculate absolute planetary radius). We calculatedthese parameters by inputting stellar effective tempera-ture, metallicity, and surface gravity into the isochronesPython package (Morton 2015a). We also found that in-putting 2MASS photometry into isochrones along withthe aforementioned stellar parameters had no notice-able effect on the resulting stellar radius and mass val-ues (or their uncertainties). Although isochrones havebeen found to underestimate stellar radii before (Dress-ing et al. 2017a; Martinez et al. 2017; Dressing et al.

33 https://exoplanetarchive.ipac.caltech.edu/34 https://archive.stsci.edu/k2/published planets/search.php

16 Mayo et al.

2017b), this effect is confined to M dwarfs and late Kdwarfs, which are largely excluded from our host starsample since we do not consider stars with effective tem-peratures below 4250 K (see Section 4.2). The derivedstellar masses and radii are reported in Table 4. (Alsonote that all stellar parameters for each system are re-ported in Table 5).

7. DISCUSSION

7.1. Lessons Learned

There have been a few recent instances of false posi-tive misclassification (Cabrera et al. 2017; Shporer et al.2017), in which a target has been classified as a validatedplanet but later shown to be a false positive through sub-sequent analysis. Here, we discuss some of the pitfallsof statistical validation, and share some lessons we havelearned and solutions we have implemented to preventfalse positive misclassification.

First, spectroscopy is key. Stellar parameters are cru-cial to understanding the host star and correctly classify-ing the candidates. For example, identifying the star ashighly evolved can prevent an orbiting brown dwarf or Mdwarf from being incorrectly labeled as a smaller planetorbiting a main sequence star. One might attempt toavoid this issue by estimating stellar surface gravity viaphotometry alone, but that is notoriously difficult to doand can lead to incorrectly estimated stellar parameters.Collecting at least one spectrum from which to estimatespectroscopic parameters (including surface gravity) canavoid many issues like this. And collecting more spec-tra may exclude (or reveal) large RV variations from aneclipsing binary scenario.

Second, a search for secondary eclipses at all phasesshould be performed to exclude highly eccentric binaryscenarios. The search method used here was the “model-shift uniqueness” test designed by Coughlin et al. (2016).This method compared off-transit portions of the lightcurve against the transit portion of the best-fit transitmodel (and the transit model inverted, to provide a vi-sual comparison of detection significance). An even morerigorous method would consider secondary eclipses of du-ration and depth distinct from that of the transit.

Third, when validating exoplanets using vespa oneshould be very careful about what broadband photom-etry is used and what offsets and systematics there are.Statistical validation work on data from the original Ke-pler mission took advantage of high-quality and uniformbroadband photometry from the Kepler Input Catalog(KIC, Brown et al. 2011). The analogous EPIC cata-log for K2 is similarly vital to the analysis of the K2star and planet sample. However, it is approximatelyfour times larger and was produced by collecting archivalphotometric measurements; therefore, it is more hetero-geneous and more prone to systematic errors and offsetsthan the KIC. We have found that in some cases, thesesystematic errors or offsets in photometry can result inuntrustworthy FPP estimates, in particular, extremelylow FPP measurements for known or likely false posi-tives. For example, when we input to vespa all availablebroadband photometry from the EPIC catalog for thecandidate EPIC 211418290.01, vespa yields a FPP lessthan 10−6 because it is unable to find an acceptable fitto a binary star model due to underestimated photomet-

ric uncertainties and therefore incorrectly rules that falsepositive scenario out. However, inputting only 2MASSphotometry to vespa yields a better fit to the eclips-ing binary scenario, and vespa therefore returns a muchhigher FPP of about 0.6. Situations like this were notuncommon, which is why we ultimately decided to useonly photometry from the all sky 2MASS survey. Wechose to use only the 2MASS survey because it providesbroadband photometry for all of our candidates and op-erates in the infrared, reducing the effects of reddening.Including photometry from additional surveys that arecalibrated differently and have distinct systematic un-certainties would introduce non-uniformity that wouldbe difficult to quantify and could bias our results.

To be conservative, we also added 0.02 mags of sys-tematic error in quadrature with the reported error foreach 2MASS band we used. This will continue to be im-portant after the launch of TESS, which will observe tar-gets selected from the TESS Input Catalog (TIC, Stassunet al. 2017). The TIC will be very important for select-ing candidates for observation and follow-up; however, itis being assembled in a manner similar to the EPIC andis approximately ten times larger, so it may have similaror even greater photometric offsets.

Fourth, it is very important to make and remake acandidate’s light curve with multiple apertures of vary-ing sizes, in order to determine whether the transit signaloriginates from the target star or a nearby backgroundstar (and thus exclude background false positive scenar-ios). This test caught many false positives in our ownanalysis, and has been used successfully before in othercandidacy analyses (e.g. Dressing et al. 2017b).

Fifth, transiting giant planets are nearly indistinguish-able from eclipsing brown dwarfs or small M-dwarf stars,since they have roughly equal radii. Great care shouldbe taken when interpreting the output of vespa for gi-ant planets, and unless there is a clear way to distin-guish between the two scenarios (via RV measurements,secondary eclipse detection, composite spectra, etc.), at-tempts to validate large planets can be difficult and proneto error.

By considering each of the above lessons and incorpo-rating them into future validation analyses, misclassifi-cations of validated planets can be significantly reducedand hopefully eliminated in all but the most perversescenarios.

We will now investigate some of the individual vali-dated planets in our sample as well as the characteristicsof our sample as a whole.

7.2. A New Brightest Host Star in the K2 and KeplerPlanet Samples

One interesting target in our sample is EPIC205904628 (HIP 110758, HD 212657), a F7 star observedin Campaign 3. We detected and validated a 2.8 R⊕planet on a 10 day orbit. At a V magnitude of 8.24, EPIC205904628 is now the brightest star at optical wave-lengths in the entire Kepler and K2 samples to host a val-idated planet. EPIC 205904628 is just slightly brighterthan Kepler-21 (V = 8.25), a star of similar spectral typefound during the original Kepler mission to host a singleshort-period exoplanet (Lopez-Morales et al. 2016; How-ell et al. 2012). TESS is expected to discover planetsaround many stars this bright and brighter.


We note that due to its brightness, we applied somespecial care to this star. In particular, we re-reducedthe K2 light curve by extracting light curves from largerphotometric apertures than our standard pipeline uses.We also incorporated information from 2MASS J-bandimaging to rule out additional stars in the photometricaperture by calculating a contrast curve and inputting itto vespa to provide deeper imaging constraints than ourspeckle image.

7.3. Characteristics of the Sample

In addition to individual planets in our sample, it isinteresting to explore a few of the demographics of thenewly validated exoplanet population. Figs. 8-15 revealvarious aspects of the validated exoplanet sample andthe exoplanet candidate sample.

7.3.1. The Stellar Magnitude Distribution

Fig. 8 is a histogram of the distribution of brightnessesfor the host stars in our sample compared against bright-ness for stars hosting known Kepler planets (downloadedfrom https://exofop.ipac.caltech.edu/; accessed 2017 De-cember 4). Most of the candidates in our population areclustered near stellar magnitudes of Kp = 12 to Kp =13, and the cutoff we imposed at Kp = 13 is very evi-dent. Also in Fig. 8 is the distribution of brightnessesfor host stars to known Kepler planets. That distribu-tion peaks near Kp = 15 and drops rapidly at brightermagnitudes. It is more difficult to find planet candidatesaround faint targets for K2 than for Kepler since thebaseline is shorter. Therefore K2 candidates tend to or-bit very bright host stars relative to Kepler candidates,making K2 candidates excellent targets for follow-up ob-servations.

7.3.2. The Effective Temperature Distribution

Most of the validated planets and candidates we iden-tified orbit host stars with effective temperatures in the5000 − 6000 K range. However, out of 233 stars in oursample 41 are cooler than 5000 K and 25 are hotterthan 6000 K. No stars in our sample are cooler than4250 K or hotter than 6500 K. See Fig. 9 for a com-parison against the Kepler sample (downloaded fromhttps://exofop.ipac.caltech.edu/; accessed 2017 Decem-ber 4).

7.3.3. The Period Distribution

We also explored the period distribution of our candi-date population. As can be seen in Fig. 10, the typicalvalidated planet or candidate has an orbital period of 20days or less. This should come as no surprise, given the∼75 day baseline of K2 observations per campaign field.Of 275 candidates in our sample, only 46 have periodsover 20 days and only 10 have periods over 40 days.

7.3.4. The Multiplicity Distribution

Most of the candidates in our sample (validated or oth-erwise) are the only candidate in their system to havebeen detected. However, our sample does include 21 sys-tems with two candidates (15 of those have only vali-dated planets), 9 systems with three candidates (8 ofthose have only validated planets), and 1 system withfour candidates (EPIC 212157262; all candidates in this

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Figure 8. Histograms of Kepler magnitude for host stars to vali-dated planets (purple) and candidate planets (diagonal lines) fromC0-C10 of K2 that have been identified in this work, as well as acomparison against host stars to confirmed Kepler planets (pink).There is a fairly sharp cutoff in our sample near magnitude 13, sincevalidation was only conducted on stars for which we had a spectrumand almost all of the spectra we used were for targets brighter than13th magnitude. The typical Kepler host star is much fainter, withthe peak of the distribution near 15th magnitude, which makes K2target stars much more suitable for follow-up observations thanKepler stars. Also of note: the brightest star hosting a validatedplanet in our sample is EPIC 205904628, a V = 8.2 star with a2.8 R⊕ planet on a 10 day orbit. Validated in this work, EPIC205904628 is now the brightest host star for a validated planet ineither the Kepler or K2 samples.

system are validated). The full multiplicity distributioncan be seen in Fig. 11.

7.3.5. The Planet Radius Distribution

One of the more interesting features of our sample wasthe radius distribution. Fig. 12 demonstrates the fullplanetary radius distribution of our sample for both val-idated planets and candidates. As expected, there is asharp cutoff in planet radius for validated planets at Rp

= 8 R⊕ (since we generally chose not to validate largerplanets).

In order to investigate the radius distribution of theunderlying planet population, we adopted and applied arough completeness correction to our planet sample. Wedetermined the completeness of our K2 planet detectionpipeline by performing injection/recovery tests. We in-jected planet signals into K2 light curves over a rangeof expected signal-to-noise ratios (analogous to the in-jection/recovery tests performed by Christiansen et al.2016, Petigura et al. 2013, and Dressing & Charbonneau2015 on the Kepler pipeline). We then calculated for eachof our planet candidates the number of stars observed byK2 around which we could have detected the planet, andweighted the planet’s contribution to the histograms bythat factor and the geometric transit probability.

The uncorrected and corrected distributions for vali-dated planets and candidates can be seen in Fig. 13, while

18 Mayo et al.

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Figure 9. Histograms of effective temperature for host stars tovalidated planets (purple) and candidate planets (diagonal lines)from C0-C10 of K2 that have been identified in this work, as well asa comparison against host stars to confirmed Kepler planets (pink).Apart from the cutoffs we impose at Teff = 4250 K and 6500 K,our sample follows a similar effective temperature distribution asthe Kepler sample.

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Figure 10. Histogram of orbital period for the validated plan-ets (purple) and candidates (diagonal lines) in C0-C10 of K2 thathave been identified in this work. The steep drop off in validatedplanets and candidates around 20 days is due to the K2 strategyof observing each field for only ∼75 days.

a comparison of our corrected candidate sample to theFulton et al. (2017) sample and a log-uniform distribu-tion can be seen in Fig. 14. Additionally, a completeness-corrected contour plot of stellar incident flux versus plan-

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Figure 11. Histogram of multiplicity for the validated planet sys-tems (purple) and planet candidate systems (diagonal lines) in C0-C10 of K2 that have been identified in this work. (A validatedplanet system is a system for which all candidates have been val-idated.) Most validated planets and candidates have no detectedcandidate companions in their system. The largest system in thesample is EPIC 212157262, which hosts four validated planets.

etary radius for our candidate sample can be seen inFig. 15 (constructed in the same way as Fig. 10 fromFulton et al. 2017).

By visual inspection of these figures alone, our cor-rected candidate sample appears to exhibit a gap in theradius frequency around 1.8 to 2.0 R⊕, similar to thegap in the Kepler planet sample explored by Fulton et al.(2017). They argued that the underlying astrophysicaleffect could be photoevaporation, whereby stellar inci-dent flux strips a planet’s H/He atmosphere if the at-mosphere is not thick enough, leaving a population ofstripped, rocky planets and an untouched population oflarger, gaseous mini-Neptunes (Owen & Wu 2013; Lopez& Rice 2016; Owen & Wu 2017; Van Eylen et al. 2017).As an alternative hypothesis, they also suggested thatgas accretion could be delayed during planet formationuntil the protoplanetary disk is already gas poor, creat-ing a population of small, rocky planets (Lee et al. 2014;Lee & Chiang 2016).

We wanted to analyze in a more quantitative fash-ion how the completeness-corrected radius distributionof our K2 candidates compared to the completeness-corrected Kepler candidates from Fulton et al. (2017);we also decided to compare against a log-uniform distri-bution to probe the significance of a possible bimodalityFulton et al. (as 2017, does). We binned all three nor-malized distributions in 0.1 R⊕ intervals from 1.2 − 2.5R⊕. We assigned error bars to our own sample and theFulton et al. (2017) sample via Poisson statistics (forthe number of candidates in each bin) and then scaledthe uncertainty according to the completeness-correctionscaling applied to each bin.

We then calculated χ2reduced between our sample and

that of Fulton et al. (2017) as well as our sample and


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Figure 13. Left: Histogram of planetary radius for the validated planets (purple) and candidates (diagonal lines) in C0-C10 of K2 thathave been identified in this work (between 0.7 − 12 R⊕). Right: Same data as presented in the left panel, with a completeness-correctedapplied to estimate the underlying planet population. Error bars for each bin correspond to 1/

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bin) scaled according to the completeness correction subsequently performed. Through visual inspection, the full candidate sample appearsto exhibit a frequency gap centered near 1.8 to 2.0 R⊕.

20 Mayo et al.

the log-uniform distribution, finding values of 2.21 and2.34 respectively. Across all bin numbers from 5 to 20for which there were more than two candidates in every(equally sized and spaced) bin for all samples, the aver-age χ2

reduced was 2.21 between our sample and the Ful-ton et al. (2017) and 2.95 between our sample and thelog-uniform distribution. However, we note that a largeportion of the χ2

reduced between our sample and that ofFulton et al. (2017) is caused by only the smallest radiusbin. Still, the Fulton et al. (2017) sample did not pro-vide a significant improvement in goodness of fit than asimple log-uniform distribution. This suggests that thevisual gap in our candidate sample cannot be quantita-tively confirmed unless future observations and planetdetections are made to increase the sample size.

7.3.6. Future Applications

The K2 mission has thus far conducted observationsthrough more than 15 campaigns, and it will continueobservations for future campaigns until it expends all ofits fuel. Given that the validation infrastructure built forthis research is directly applicable to future campaigns,we will be able to identify and validate exoplanet candi-dates from upcoming campaigns as quickly as the neces-sary follow-up observations can be collected.

This research will also be useful even after the end ofthe K2 mission. The upcoming TESS mission (Rickeret al. 2015) is expected to yield more than 1500 totalexoplanet discoveries, but it is also estimated that TESSwill detect over 1000 false positive signals (Sullivan et al.2015). Even so, one (out of three) of the level one baselinescience requirements for TESS is to measure the massesof 50 planets with Rp < 4 R⊕. Therefore, there willneed to be an extensive follow-up program to the pri-mary photometric observations conducted by the space-craft, including careful statistical validation to aid in theselection of follow-up targets. The work presented herewill be extremely useful in that follow-up program, sinceonly modest adjustments will allow for the validation ofplanet candidate systems identified by TESS rather thanK2.

8. SUMMARY AND CONCLUSIONS

In this paper, we processed 208, 423 targets from C0-C10, removed instrumental systematics from the K2 pho-tomtry, and searched for threshold crossing events. Weidentified ∼30, 000 TCEs, which were subjected to triageand vetting. Of those, ∼1, 000 targets systems passedboth and were upgraded to candidates. And of those, 275candidates in 233 systems had at least one usable TRESspectrum. For each candidate, we also collected andanalyzed follow-up observations including spectroscopyand high-contrast imaging. We derived transit/orbitalparameters from the K2 photometry, stellar parametersfrom the spectra, and contrast curves from the high-contrast imaging. Then, using these results, we deter-mined the false positive probability (FPP) of each planetcandidate using the vespa validation procedure (Morton2012, 2015b), which calculates the likelihood of variousfalse positive scenarios as well as the true positive sce-nario. These FPP values were then adjusted appropri-ately for systems with radial velocity measurements andfor multiplanet systems (see Section 5.1). We reported

the resulting FPPs for our planet candidates (see Ta-ble 4) and classified candidates with FPP < 0.001 asvalidated planets.

149 of the 275 candidates had a FPP below the valida-tion threshold of 0.001, while 126 remained candidates(FPP > 0.001). According to the NASA ExoplanetArchive35 and the Mikulski Archive for Space Tele-scopes36 (both accessed 2018 February 14), of the 149newly validated exoplanets, 56 have not been previouslydetected, 39 have already been identified as candidates,53 have already been validated, and 1 has previouslybeen classified as a false positive (EPIC 210894022.01;see Section 6.2). As a result, this work will increase thevalidated K2 planet sample by nearly 50% (and increasethe K2 candidate sample by ∼20%. The full dispositionresults can be found in Table 2.

Most of the newly validated exoplanets orbited hoststars with 12 < Kp < 13 and 5000 K < Teff < 6000K. Additionally, the majority of validated planets hadorbital periods < 20d and planetary radii between 1− 4R⊕. Our complete candidate sample also shows signs ofa frequency gap in the radius distribution (see Fig 14),similar to the gap found by Fulton et al. (2017). However,further analysis with a larger planet sample is requiredto confirm the radius gap for K2 planets.

This work has clear broader implications. The abil-ity to validate planet candidates is vital to conductinga successful follow-up and confirmation program. Thewide applicability of the validation infrastructure devel-oped in this research is clear from the large number ofcandidates subjected to our validation process. By con-tinuing to apply the validation process described here,future K2 campaigns and the upcoming TESS missionwill benefit from a valuable source of validated planetsand a useful validation pipeline able to process the largeand constant supply of identified planet candidates.

Many thanks to Guillermo Torres and Dimitar Sasselovfor their review and grading of this work during its phaseas a thesis project. We thank Joey Rodriguez, GeorgeZhou, Sam Quinn, Jeff Coughlin, and Tom Barclay foruseful conversations and assistance vetting some of ourcandidates. We are grateful to BJ Fulton for providingus access to useful contour plotting tools, and also for al-lowing for the reproduction of a plot from another paper.Special thanks to Ellen Price for crucial assistance, time,and effort in setting up vespa. Finally, A.W.M. wishesto thank Prof. David Charbonneau and the classmatesof Astronomy 99 for their regular support and feedback.

A.W.M, A.V., and E.J.G are supported by the NSFGraduate Research Fellowship grant nos. DGE 1752814,1144152, and 1339067, respectively. This work was per-formed in part under contract with the California Insti-tute of Technology (Caltech)/Jet Propulsion Laboratory(JPL) funded by NASA through the Sagan FellowshipProgram executed by the NASA Exoplanet Science In-stitute. A.V. and D.W.L. acknowledge partial supportfrom the TESS mission through a sub-award from theMassachusetts Institute of Technology to the Smithso-nian Astrophysical Observatory.

35 https://exoplanetarchive.ipac.caltech.edu/36 https://archive.stsci.edu/k2/published planets/search.php


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Figure 14. Left: Completeness-corrected comparison of the radius distribution between 1.2− 12.0 R⊕ for all candidate planets identifiedin this work (thatched), the planet sample analyzed in Fulton et al. (2017, blue), and a normalized log-uniform distribution (dashed line).Right: Comparison of the same distributions as the left panel, now focused on planet candidates with radii between 1.2 − 2.5 R⊕. Thefrequency gap identified by Fulton et al. (2017) can clearly be seen in their distribution. A similar gap tentatively appears in our sample(near 1.8 to 2.0 R⊕), although a log-uniform distribution provides a fit to our sample roughly as good as the Fulton et al. (2017) distribution.

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17)

Figure 15. Left: Contour plot of incident stellar flux versus planetary radius. The black points are the 275 candidates in our sampleand the typical uncertainty is plotted in the top left. The contours are completeness-corrected and roughly scaled to the same height asthose in Fig. 10 from Fulton et al. (2017). The contours show tentative visual evidence of a gap in the radius frequency near 1.6 to 1.8 R⊕.Right: Top panel of Fig. 10 from Fulton et al. (2017, taken with permission), with a similar gap near 1.6 to 1.8 R⊕.

22 Mayo et al.

Some observations in the paper made use of theNN-EXPLORE Exoplanet and Stellar Speckle Imager(NESSI). NESSI was funded by the NASA Exoplanet Ex-ploration Program and the NASA Ames Research Cen-ter. NESSI was built at the Ames Research Center bySteve B. Howell, Nic Scott, Elliott P. Horch, and Em-mett Quigley. The NESSI data were obtained at theWIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the Na-tional Aeronautics and Space Administration, the Na-tional Science Foundation, and the National Optical As-tronomy Observatory.

This paper includes data collected by the Kepler/K2mission. Funding for the Kepler mission is provided bythe NASA Science Mission directorate. Some of the datapresented in this paper were obtained from the Mikul-ski Archive for Space Telescopes (MAST). STScI is op-erated by the Association of Universities for Researchin Astronomy, Inc., under NASA contract NAS5–26555.Support for MAST for non–HST data is provided by theNASA Office of Space Science via grant NNX13AC07Gand by other grants and contracts. Support from theKepler Participating Scientist Program was provided viaNASA grant NNX14AE11G. The authors are honoredto be permitted to conduct observations on Iolkam Duag(Kitt Peak), a mountain within the Tohono O’odham Na-tion with particular significance to the Tohono O’odhampeople. Some of the data presented herein were obtainedat the WM Keck Observatory (which is operated as ascientific partnership among Caltech, UC, and NASA).The authors wish to recognize and acknowledge the verysignificant cultural role and reverence that the summit ofMauna Kea has always had within the indigenous Hawai-ian community. We are most fortunate to have the op-portunity to conduct observations from this mountain.

Facilities: Kepler, FLWO:1.5m (TRES), WIYN (DSSI,NESSI), Gemini:Gillett (DSSI, NIRI), Gemini:South(DSSI), Keck:II (NIRC2), Hale (PHARO), LBT (LMIR-Cam), Gaia, HIPPARCOS, Exoplanet Archive, ADS,MAST

APPENDIX

CALIBRATING TRES TO MEASURE THE MT. WILSONSHK INDEX

Our work involved the analysis of many spectra col-lected with the Tillinghast Reflector Echelle Spectro-graph (TRES) on the 1.5-m Tillinghast telescope at theWhipple Observatory on Mt. Hopkins. In addition to us-ing TRES spectra to derive spectroscopic parameters andmeasure radial velocities, we also used TRES to measurethe Mt. Wilson SHK activity indicator. SHK is a ratiobetween the flux in the cores of the Calcium II H and Kspectral features (at 3933.66 ± 1.09 and 3968.47 ± 1.09A) and the flux in two nearby continuum regions (oneslightly redward of the Ca II lines called R and oneslightly blueward called V). SHK is commonly used asa proxy for a star’s chromospheric activity (Isaacson &Fischer 2010). Because SHK depends on ratios of fluxesat different wavelengths, it is sensitively affected by aspectrograph’s blaze function. The effect of the spectro-graph’s blaze function must therefore be carefully cali-brated and quantified in order to standardize measure-ments of SHK from different instruments. In this ap-

pendix, we describe how we calibrated the TRES spectro-graph to place measurements of SHK on the Mt. Wilsonscale, and present our measurements of SHK for a hand-ful of bright K2 planet candidate hosts for which we wereable to measure SHK reliably. These measurements arelisted in Table 3.

To calibrate TRES to measure SHK on the Mt. Wilsonscale, we closely followed the procedure of Isaacson &Fischer (2010). We based our calibration on a sample ofstars that were both observed by TRES (prior to 2016June 1) and were included in the Duncan et al. (1991)catalog of Mt. Wilson SHK measurements. Additionally,the following cuts were applied to improve the samplequality:

1. TRES spectra for the star in question were onlyused if the photon count in the R continuum region(4001.07 ± 10 A) was greater than 174,000. (Thecutoff is actually at 150,000 ADU, which is con-verted using a gain of 1.16 for TRES.) This conser-vative cutoff was imposed to remove spectra withonly low or moderate SNR from the calibration.

2. The star was not in a close binary or multiple sys-tem. We only included widely separated (& 5′′)visual binaries in order to prevent flux from thecompanion star(s) being blended with flux of theintended target.

3. One rapidly rotating star (HD 30780, or ‘VB123’in the TRES database) was removed from the cal-ibration set as the H and K emission cores wereclearly broadened and smeared with other spectralfeatures (v sin i ' 180 km s−1).

After these cuts, our calibration sample included 118stars with a total of 1204 individual TRES observations.The calibration was done in the same way as Isaacson &Fischer (2010), by determining values of Kcoeff , Vcoeff , m,and b that minimize the differences between the Mt. Wil-son survey’s measurement of SHK for each star (Duncanet al. 1991) and SHK calculated from the TRES spectrausing the following equation:

SHK,TRES = m× H +KcoeffK

R+ VcoeffV+ b (A1)

where H and K are fluxes in the cores of the Ca II H andK lines37, R and V are continuum fluxes 38, Kcoeff is acoefficient that scales the magnitude of K fluxes to matchthe magnitude of H fluxes, Vcoeff is a coefficient thatscales the magnitude of V fluxes to match the magnitudeof R fluxes, and m and b are free parameters.Kcoeff was calculated through a linear regression be-

tween H and K for our TRES spectra, so as to scale themagnitude of K to match that of H. The same processwas performed for R and V in order to calculate Vcoeff .This was done to mirror the approach taken by Isaacson

37 The H and K fluxes were calculated by integrating the spec-trum over triangular-shaped bandpasses centered at 3933.66 and3968.47 A respectively, each with a FWHM of 1.09 A.

38 The R and V fluxes were calculated by integrating the spec-trum over 20 A wide box-shaped bandpasses centered at 4001.07A and 3901.07 A, respectively, following Duncan et al. (1991).


& Fischer (2010) in their calibration of the Keck HIRESinstrument.

We estimated m and b by minimizing the differencesbetween SHK,Mt.Wilson from the Mt. Wilson survey (Dun-can et al. 1991) and SHK,TRES determined from TRESspectra with Equation A1 using a Markov chain MonteCarlo (MCMC) algorithm with affine invariant ensemblesampling (Foreman-Mackey et al. 2013). We calculatedthe likelihood, L, using the following function:

ln(L) = −0.5∑(

(SHK,TRES − SHK,Mt.Wilson)2

σ2+lnσ2

)(A2)

where σ is a “jitter” term that absorbs uncertainties inboth measurements of SHK as well as uncertainties dueto factors including astrophysical variability in the SHK

index of a single star over time. We imposed uniformpriors on m and b, and imposed a Jeffreys prior on σ.

It is important to note that for a given star, therecould be both multiple TRES spectra and multiple Mt.Wilson SHK measurements. So if a star had more thanone TRES spectrum or Mt. Wilson SHK measurementthat star was simply represented as a grid of TRES andMt. Wilson measurements in the MCMC process. Withthis in mind, the total number of data points in the fittingprocess was 3108. This implicitly gives higher weight inour calibration to stars with multiple observations, whichhelps average out astrophysical variability in SHK.

Our MCMC process used 200 chains of 50,000 stepseach in order to explore parameter space and determinebest-fit parameters and uncertainties. The resulting en-semble was well converged according to the Gelman-Rubin statistic (Gelman & Rubin 1992), which in thiscase was less than 1.04 for all parameters. The last 500samples of the MCMC process are visualized in Figure16 with a posterior corner plot (Foreman-Mackey 2016).We found the following parameter values from our modelfit:

Kcoeff = 0.876

Vcoeff = 0.775

m = 15.496+0.068−0.069

b = −0.0031± 0.0015

ln(jitter) = −3.119± 0.013

There was also significant covariance between m andb (see Fig. 16), which we estimated to be Cov(m, b) =−8.571× 10−5.

Statistical uncertainties, σrandom, for SHK were calcu-lated by propagating sample draws from four Poisson dis-tributions representing R, V , H, and K through drawsfrom the m and b posterior distributions and the Kcoeff

and Vcoeff values. We also included a systematic er-ror term, σsystematic, in our uncertainty estimates. Weestimated the systematic uncertainties for TRES SHK

measurements using 6 high signal-to-noise spectra of thebright star Tau Ceti collected with TRES on the nightof 2013 October 24. We assumed that SHK for Tau Cetiremained constant over the course of a single night, andestimated a systematic error term based on the scatter

0.009

0.006

0.003

0.000

0.003

b

15.30

15.45

15.60

15.75

m

3.16

3.14

3.12

3.10

3.08

ln(

)

0.009

0.006

0.003

0.000

0.003

b

3.16

3.14

3.12

3.10

3.08

ln( )

Figure 16. Corner plot for three parameters in our calibration ofthe Tillinghast Reflector Echelle Spectrograph for SHK, an indica-tor of stellar activity: a line slope (m) and a line y-intercept (b) inour SHK equation, as well as a noise parameter (ln (σ)) to accountfor error bars and stellar variability.

between individual SHK measurements. Our final er-ror estimates, σtotal came from assuming the statisticaluncertainties and systematic uncertainties were indepen-dent and could be added in quadrature as follows:

σ2total = σ2

systematic + σ2random (A3)

We note that our calibration for SHK is only validover specifics ranges in parameter values. Our calibra-tion was performed over a range of 0.244 to 1.629 in B-V and yielded SHK values ranging from 0.055 to 2.070.Based on tests with simulated data and with real lowsignal-to-noise data, we are cautious of SHK measure-ments on spectra with fewer than 290,000 photon counts(or 250,000 ADU) in the R and V continuum regionscombined. We also note that SHK measurements can beaffected by rapid stellar rotation. We found by artifi-cially broadening the lines of slowly rotating stars thatSHK measurements for stars with v sin i above 20 km s−1

can be skewed compared to the values that would havebeen measured if the stars were slowly rotating.

We tested our calibration by comparing SHK measure-ments derived from TRES with a “test set” of SHK mea-surements from literature (in particular, we focused onstars observed by Isaacson & Fischer 2010). We con-structed the test data set by identifying stars observedby TRES with the following properties:

1. The stars were not included in our calibration set(stars observed both by Duncan et al. 1991 andTRES).

2. The TRES spectra for the star in question havephoton counts in the R continuum region greaterthan 174,000 (or 150,000 ADU).

3. The star had at least one SHK measurement fromKeck HIRES that had been reported in Isaacson &Fischer (2010).

24 Mayo et al.

After applying these cuts we were left with a test set of121 stars, which had been observed a total of 4308 timesby TRES.

We show the results of our SHK calibration in Figure17, which compares TRES SHK measurements from ourcalibration set with measurements from the Mt. Wilsonsurvey, and in Figure 18, which compares TRES SHK

measurements from our test set with values from Isaacson& Fischer (2010).

0.0 0.5 1.0 1.5 2.0 2.5Mt. Wilson (Duncan et al. 1991) SHK values

0.0

0.5

1.0

1.5

2.0

2.5

Newl

y de

term

ined

TRE

S S H

K val

ues

RMS = 10.9%

Figure 17. A comparison of our SHK calibration for TRESagainst the Duncan et al. (1991) catalog for our calibration dataset of 118 stars (with 1204 TRES spectra). Each red point denotesa unique pair of observations from TRES and Mt. Wilson for agiven star. The fractional RMS scatter on the calibration set is11.0%.

0.0 0.5 1.0 1.5 2.0 2.5Isaacson & Fischer (2010) SHK values

0.0

0.5

1.0

1.5

2.0

2.5

Newl

y de

term

ined

TRE

S S H

K val

ues

RMS = 13.6%

Figure 18. A comparison of our SHK calibration for TRESagainst the Isaacson & Fischer (2010) catalog for our test dataset of 121 stars (with 4308 TRES spectra). Each red point denotesa unique pair of observations from TRES and Mt. Wilson for agiven star. The fractional RMS scatter on the calibration set is13.6%.

For the calibration set, there is an 10.9% fractionalRMS scatter about the one-to-one line. The only no-ticeable outlier appears to be at approximately (0.9,0.2),corresponding to the single TRES spectrum (and Mt.Wilson measurement) of HD 120477, a variable star ob-served in July 2015 by TRES and observed no later than1991 at Mt. Wilson. The reason for this outlier could not

be identified, but its presence in the calibration set didnot significantly change the calibration so it was left in(removing the point maintained a fractional RMS scatterof 10.9%.)

As for the test set, there is a 13.6% fractional RMSscatter about the one-to-one line, slightly larger than forthe calibration set (which is to be expected). There doesappear to a slight systematic offset between TRES andKeck HIRES such that SHK values from Keck HIREStend to be smaller than those from TRES. However, thisis to be expected, since the same systematic underesti-mation with Keck HIRES compared to Mt. Wilson canbe seen in Fig. 4 of Isaacson & Fischer (2010). There arealso a few obviously errant data points in this figure, cen-tered around (1.5, 0.5). These data points correspond tofour TRES spectra of the star GJ 570B, a spectroscopicbinary. The test data set, because it was not used forcalibration, was not clipped of binary stars; thus, GJ570B is a clear example of how calculating SHK for closebinaries can go wrong. However, the presence of thosefour spectra has very little effect on the results; removingthem only reduced the fractional RMS scatter of the testset to 13.5%.

Table 3Stellar SHK Activity Index

EPIC Date SHK

201437844 2017-01-08 0.1666+0.0030−0.0031

201437844 2017-03-09 0.1698± 0.0032201437844 2017-03-09 0.1589± 0.0031201437844 2017-03-09 0.1712± 0.0031201437844 2017-03-09 0.1651+0.0030

−0.0029201437844 2017-03-09 0.1624± 0.0030201437844 2017-03-09 0.1633+0.0030

−0.0029201437844 2017-03-09 0.1614± 0.0029201437844 2017-03-09 0.1692± 0.0029201437844 2017-03-09 0.1622+0.0030

−0.0029201437844 2017-03-09 0.1635± 0.0028201437844 2017-03-09 0.1593+0.0029

−0.0027

201437844 2017-03-09 0.1615+0.0028−0.0029

201437844 2017-03-09 0.1680+0.0028−0.0029

201437844 2017-03-09 0.1646± 0.0029201437844 2017-03-09 0.1639± 0.0028201437844 2017-03-09 0.1651± 0.0028201437844 2017-03-09 0.1656± 0.0029201437844 2017-03-09 0.1693± 0.0029201437844 2017-03-09 0.1641± 0.0029201437844 2017-03-09 0.1680± 0.0029205904628 2015-07-24 0.1550+0.0029

−0.0030

205904628 2015-09-06 0.1453+0.0031−0.0033

211424769 2015-12-09 0.3255+0.0040−0.0039

211424769 2016-01-01 0.3144+0.0040−0.0039

211993818 2015-11-27 0.4189+0.0044−0.0045

211993818 2016-02-29 0.3851+0.0031−0.0030

211993818 2016-03-02 0.3115+0.0027−0.0028


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New Candidates and Planets Transiting Bright Stars 27Table

4Pla

net

Candid

ate

Param

eters

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

K2-1

56

b201110617.0

12750.1

409

±0.0

028

0.8

13149+

0.0

00050

−0.0

00049

4.4

+0.7

−1.1

84.0

+4.3

−7.6

0.0

170+

0.0

014

−0.0

011

1.1

4+

0.1

0−

0.0

80.6

16+

0.0

19

−0.0

16

0.6

42+

0.0

22

−0.0

19

12.9

47

<1.0

0e

−04

Pla

net

201111557.0

12750.1

621

±0.0

021

2.3

0237+

0.0

0011

−0.0

0010

12.6

+2.8

−8.0

87.4

+1.9

−9.5

0.0

169+

0.0

067

−0.0

015

1.3

1+

0.5

2−

0.1

20.7

11+

0.0

19

−0.0

20

0.7

46

±0.0

23

11.3

63

1.2

2e

−03

Candid

ate

201127519.0

12752.5

513+

0.0

011

−0.0

012

6.1

7837+

0.0

0019

−0.0

0017

17.3

+1.1

−2.0

88.8

+0.8

−1.0

0.1

151+

0.0

049

−0.0

034

9.9

1+

0.5

3−

0.3

60.7

89+

0.0

25

−0.0

17

0.8

57+

0.0

21

−0.0

23

11.5

58

−Candid

ate

c

K2-1

57

b201130233.0

12749.8

239+

0.0

032

−0.0

033

0.3

65257

±0.0

00029

1.8

8+

0.3

2−

0.3

877.0

+10.0

−18.0

0.0

110+

0.0

014

−0.0

010

1.0

6+

0.1

5−

0.1

00.8

76+

0.0

45

−0.0

25

0.9

40+

0.0

23

−0.0

27

12.6

04

<1.0

0e

−04

Pla

net

K2-1

58

b201132684.0

12757.4

817+

0.0

096

−0.0

092

10.0

621+

0.0

023

−0.0

022

17.6

+2.9

−5.8

88.4

+1.2

−2.4

0.0

271+

0.0

027

−0.0

020

2.6

3+

0.3

5−

0.2

20.8

92+

0.0

74

−0.0

36

0.9

33+

0.0

27

−0.0

30

11.6

78

<1.0

0e

−04

Pla

net

201166680.0

12765.1

93+

0.0

21

−0.0

16

18.1

05+

0.0

10

−0.0

13

26.3

+5.3

−8.9

88.9

+0.8

−1.7

0.0

157+

0.0

017

−0.0

012

2.1

0+

0.3

1−

0.2

01.2

2+

0.1

2−

0.0

71.1

92+

0.0

33

−0.0

30

10.8

97

1.7

3e

−03

Candid

ate

201211526.0

12755.4

780

±0.0

040

21.0

702+

0.0

024

−0.0

023

34.0

+5.0

−11.0

89.2

+0.6

−1.2

0.0

170+

0.0

031

−0.0

013

1.6

5+

0.3

2−

0.1

40.8

91+

0.0

56

−0.0

37

0.9

36+

0.0

32

−0.0

31

11.6

96

2.1

0e

−03

Candid

ate

K2-1

59

b201225286.0

12753.5

147+

0.0

034

−0.0

037

12.4

211

±0.0

010

26.1

+2.8

−6.0

89.1

+0.7

−1.1

0.0

244+

0.0

023

−0.0

013

2.2

1+

0.2

4−

0.1

40.8

30+

0.0

45

−0.0

29

0.8

86+

0.0

27

−0.0

32

11.7

29

3.5

3e

−04

Pla

net

K2-1

60

b201227197.0

12752.6

6637+

0.0

0081

−0.0

0079

3.7

05871+

0.0

00074

−0.0

00076

14.7

+1.5

−3.7

88.3

+1.2

−2.1

0.0

319+

0.0

017

−0.0

011

3.1

8+

0.2

1−

0.1

50.9

14+

0.0

37

−0.0

26

0.9

83+

0.0

23

−0.0

25

12.4

86

7.5

4e

−04

Pla

net

K2-1

61

b201231064.0

12754.8

476+

0.0

077

−0.0

073

9.2

832+

0.0

021

−0.0

023

10.8

+1.8

−4.7

87.3

+2.0

−5.6

0.0

218+

0.0

052

−0.0

018

6.1

+1.6

−0.8

2.5

7+

0.3

1−

0.2

50.9

87+

0.0

82

−0.0

60

12.3

58

7.9

7e

−04

Pla

net

201295312.0

11978.7

201

±0.0

026

5.6

5630+

0.0

0037

−0.0

0032

9.4

+0.9

−2.3

87.4

+1.9

−3.3

0.0

1726+

0.0

0070

−0.0

0054

2.9

4+

0.5

0−

0.3

81.5

6+

0.2

6−

0.1

91.0

50+

0.0

68

−0.0

45

12.1

26

<1.0

0e

−04

Pla

net

201299088.0

12767.3

429+

0.0

081

−0.0

080

21.2

047+

0.0

053

−0.0

055

7.2

6+

0.9

0−

0.6

683.5

+1.1

−1.0

0.0

474+

0.0

020

−0.0

018

9.1

+1.2

−1.0

1.7

6+

0.2

1−

0.1

70.8

48+

0.0

23

−0.0

10

11.7

51

−Candid

ate

a

201352100.0

12761.7

920+

0.0

020

−0.0

021

13.3

8363+

0.0

0076

−0.0

0073

34.9

+4.0

−9.0

89.2

5+

0.5

3−

0.9

10.0

323+

0.0

019

−0.0

015

2.8

7+

0.1

9−

0.1

40.8

15+

0.0

27

−0.0

18

0.8

89+

0.0

19

−0.0

24

12.7

98

−Candid

ate

c

201384232.0

11994.4

972+

0.0

044

−0.0

043

30.9

446+

0.0

030

−0.0

032

41.6

+4.1

−9.9

89.4

2+

0.4

3−

0.7

40.0

246+

0.0

015

−0.0

009

2.3

1+

0.1

7−

0.1

20.8

63+

0.0

34

−0.0

30

0.9

30+

0.0

29

−0.0

30

12.5

10

<1.0

0e

−04

Pla

net

K2-1

62

b201390048.0

12750.9

089+

0.0

064

−0.0

054

9.4

577

±0.0

014

22.6

+3.8

−7.0

88.8

+0.9

−1.8

0.0

188+

0.0

021

−0.0

014

1.4

9+

0.1

7−

0.1

20.7

26

±0.0

20

0.7

77+

0.0

25

−0.0

26

11.9

61

<1.0

0e

−04

Pla

net

201403446.0

11982.3

364+

0.0

051

−0.0

052

19.1

545

±0.0

028

18.8

+2.1

−4.9

88.6

+1.0

−1.7

0.0

170+

0.0

013

−0.0

008

2.4

7+

0.3

5−

0.3

01.3

3+

0.1

6−

0.1

51.0

15+

0.0

54

−0.0

46

11.9

95

<1.0

0e

−04

Pla

net

K2-1

63

b201427874.0

12749.8

484

±0.0

019

6.6

7312+

0.0

0032

−0.0

0030

15.7

+2.1

−4.4

88.3

+1.3

−2.2

0.0

297+

0.0

030

−0.0

014

2.4

7+

0.2

6−

0.1

20.7

62+

0.0

18

−0.0

13

0.8

26+

0.0

19

−0.0

23

12.8

19

<1.0

0e

−04

Pla

net

201437844.0

12753.5

434

±0.0

044

9.5

545+

0.0

013

−0.0

014

18.3

+2.5

−6.8

88.5

+1.1

−2.7

0.0

168+

0.0

010

−0.0

007

2.3

3+

0.3

5−

0.2

61.2

7+

0.1

7−

0.1

31.1

19+

0.0

55

−0.0

43

9.2

34

<1.0

0e

−04

Pla

net

201437844.0

22757.0

745+

0.0

033

−0.0

035

21.0

575+

0.0

022

−0.0

020

33.0

+3.1

−7.2

89.2

6+

0.5

3−

0.8

30.0

3091+

0.0

0099

−0.0

0078

4.2

9+

0.6

0−

0.4

51.2

7+

0.1

7−

0.1

31.1

19+

0.0

55

−0.0

43

9.2

34

<1.0

0e

−04

Pla

net

201441872.0

11979.8

713+

0.0

067

−0.0

072

4.4

4126+

0.0

0088

−0.0

0094

11.0

+3.1

−7.8

87.0

+2.0

−15.0

0.0

124+

0.0

093

−0.0

013

1.1

2+

0.8

5−

0.1

30.8

34+

0.0

50

−0.0

31

0.8

85+

0.0

29

−0.0

31

12.0

88

−Candid

ate

b

K2-1

64

b201460826.0

11983.7

370+

0.0

084

−0.0

091

17.3

551+

0.0

041

−0.0

038

13.9

+2.3

−5.4

87.9

+1.5

−3.7

0.0

1357+

0.0

0097

−0.0

0074

3.2

5+

0.5

2−

0.4

12.2

0+

0.3

1−

0.2

51.1

81+

0.0

93

−0.0

61

11.1

30

<1.0

0e

−04

Pla

net

201505350.0

11984.2

7514

±0.0

0082

11.9

0762

±0.0

0024

23.4

+1.9

−4.0

89.0

4+

0.6

7−

0.9

50.0

445+

0.0

019

−0.0

009

4.0

5+

0.2

5−

0.1

50.8

34+

0.0

36

−0.0

26

0.8

95+

0.0

26

−0.0

30

12.8

06

<1.0

0e

−04

Pla

net

201505350.0

21980.3

8334

±0.0

0026

7.9

19493+

0.0

00047

−0.0

00049

19.6

+0.5

−1.2

89.3

7+

0.4

5−

0.6

80.0

742+

0.0

014

−0.0

010

6.7

5+

0.3

2−

0.2

30.8

34+

0.0

36

−0.0

26

0.8

95+

0.0

26

−0.0

30

12.8

06

<1.0

0e

−04

Pla

net

201505350.0

31978.4

307+

0.0

060

−0.0

065

2.5

0828+

0.0

0031

−0.0

0030

7.6

+1.3

−2.2

86.6

+2.5

−5.1

0.0

127+

0.0

011

−0.0

008

1.1

6+

0.1

1−

0.0

80.8

34+

0.0

36

−0.0

26

0.8

95+

0.0

26

−0.0

30

12.8

06

<1.0

0e

−04

Pla

net

K2-1

65

b201528828.0

12751.4

827+

0.0

047

−0.0

046

2.3

5499+

0.0

0025

−0.0

0026

9.2

+1.6

−2.9

87.1

+2.2

−4.4

0.0

145+

0.0

014

−0.0

010

1.2

7+

0.1

4−

0.1

00.8

04+

0.0

45

−0.0

29

0.8

35+

0.0

31

−0.0

30

11.4

15

<1.0

0e

−04

Pla

net

K2-1

65

c201528828.0

22751.2

131

±0.0

048

4.3

8274+

0.0

0051

−0.0

0054

10.5

+1.9

−4.2

87.1

+2.1

−5.0

0.0

177+

0.0

022

−0.0

011

1.5

5+

0.2

1−

0.1

10.8

04+

0.0

45

−0.0

29

0.8

35+

0.0

31

−0.0

30

11.4

15

<1.0

0e

−04

Pla

net

K2-1

65

d201528828.0

32753.7

581

±0.0

022

14.1

014

±0.0

011

27.7

+3.6

−7.4

89.0

+0.7

−1.2

0.0

302+

0.0

023

−0.0

013

2.6

5+

0.2

5−

0.1

50.8

04+

0.0

45

−0.0

29

0.8

35+

0.0

31

−0.0

30

11.4

15

<1.0

0e

−04

Pla

net

201546283.0

11979.8

4469+

0.0

0042

−0.0

0040

6.7

71389+

0.0

00059

−0.0

00062

18.2

+1.2

−2.5

88.9

+0.8

−1.0

0.0

491+

0.0

016

−0.0

009

4.5

8+

0.2

5−

0.1

60.8

55+

0.0

38

−0.0

25

0.9

20+

0.0

23

−0.0

25

12.4

28

−Candid

ate

c

201577035.0

11986.5

775+

0.0

011

−0.0

010

19.3

0704+

0.0

0057

−0.0

0060

38.6

+2.2

−5.5

89.5

0+

0.3

5−

0.5

30.0

380+

0.0

010

−0.0

007

3.7

3+

0.2

4−

0.1

50.9

02+

0.0

54

−0.0

32

0.9

58+

0.0

26

−0.0

29

12.2

96

<1.0

0e

−04

Pla

net

201595106.0

12750.0

454+

0.0

027

−0.0

026

0.8

77183

±0.0

00057

5.2

+1.0

−1.7

84.7

+3.8

−8.6

0.0

138+

0.0

018

−0.0

011

1.4

1+

0.2

1−

0.1

30.9

32+

0.0

64

−0.0

38

0.9

80+

0.0

26

−0.0

29

11.6

78

1.5

5e

−03

Candid

ate

201613023.0

11982.3

701+

0.0

028

−0.0

029

8.2

8246+

0.0

0052

−0.0

0051

13.0

+2.3

−6.3

87.6

+1.8

−5.4

0.0

200+

0.0

024

−0.0

009

2.1

9+

0.3

7−

0.2

21.0

1+

0.1

2−

0.0

90.9

36+

0.0

32

−0.0

33

12.1

37

<1.0

0e

−04

Pla

net

K2-1

66

b201615463.0

12753.7

668+

0.0

093

−0.0

086

8.5

272

±0.0

020

10.4

+1.3

−3.3

87.4

+1.9

−3.9

0.0

140+

0.0

011

−0.0

007

1.8

2+

0.3

0−

0.2

31.2

0+

0.1

8−

0.1

41.0

73

±0.0

34

11.9

64

<1.0

0e

−04

Pla

net

201713348.0

11979.8

4015+

0.0

0072

−0.0

0073

5.3

40883+

0.0

00088

−0.0

00089

12.0

+20.0

−3.0

85.5

+3.9

−3.3

0.0

4+

0.1

7−

0.0

14.0

+14.0

−1.0

0.7

46+

0.0

19

−0.0

21

0.8

00+

0.0

23

−0.0

27

11.5

31

7.0

0e

−03

Candid

ate

201713348.0

21977.8

914

±0.0

013

1.4

22619

±0.0

00039

8.0

+1.4

−3.0

86.3

+2.7

−6.2

0.0

180+

0.0

026

−0.0

013

1.4

7+

0.2

2−

0.1

10.7

46+

0.0

19

−0.0

21

0.8

00+

0.0

23

−0.0

27

11.5

31

<1.0

0e

−04

Pla

net

201828749.0

11980.1

544+

0.0

033

−0.0

031

33.5

136

±0.0

028

45.0

+9.0

−18.0

89.3

+0.5

−1.1

0.0

264+

0.0

034

−0.0

015

2.4

7+

0.3

4−

0.1

70.8

58+

0.0

45

−0.0

32

0.9

15+

0.0

29

−0.0

30

11.5

64

−Candid

ate

c

201855371.0

11984.9

438+

0.0

033

−0.0

034

17.9

691

±0.0

014

46.0

+7.0

−14.0

89.4

0+

0.4

2−

0.8

20.0

297+

0.0

030

−0.0

019

1.9

5+

0.2

1−

0.1

40.6

01+

0.0

17

−0.0

15

0.6

25+

0.0

20

−0.0

19

12.9

97

<1.0

0e

−04

Pla

net

201920032.0

12000.2

014+

0.0

048

−0.0

058

28.2

718+

0.0

037

−0.0

038

43.0

+8.0

−17.0

89.3

+0.5

−1.2

0.0

266+

0.0

046

−0.0

020

2.7

1+

0.5

3−

0.2

40.9

34+

0.0

90

−0.0

47

0.9

54

±0.0

27

12.8

90

9.7

3e

−03

Candid

ate

202089657.0

11939.7

758+

0.0

025

−0.0

026

1.3

1444+

0.0

0019

−0.0

0018

5.2

+0.8

−1.9

85.0

+3.7

−9.9

0.0

193+

0.0

037

−0.0

016

3.1

0+

0.7

6−

0.5

41.4

7±

0.2

21.1

16+

0.0

57

−0.0

74

11.6

00

−Candid

ate

b

202091388.0

11940.3

832

±0.0

026

6.4

797+

0.0

013

−0.0

012

15.5

+2.3

−5.4

88.1

+1.3

−2.9

0.0

331+

0.0

032

−0.0

019

3.3

3+

0.3

9−

0.2

30.9

22+

0.0

62

−0.0

32

0.9

76+

0.0

24

−0.0

26

13.5

00

−Candid

ate

f

202675839.0

12065.8

485+

0.0

036

−0.0

037

15.4

667+

0.0

015

−0.0

016

13.5

+5.2

−1.5

85.5

±1.8

0.1

2+

0.3

0−

0.0

616.0

+41.0

−8.0

1.2

3+

0.1

9−

0.1

31.1

41+

0.0

50

−0.0

39

12.3

62

−Candid

ate

a

202821899.0

12062.6

880+

0.0

029

−0.0

031

4.4

7451+

0.0

0030

−0.0

0031

13.5

+2.4

−5.1

87.8

+1.6

−3.6

0.0

337+

0.0

056

−0.0

025

8.2

+1.7

−1.3

2.2

2+

0.2

8−

0.3

01.5

3+

0.0

9−

0.1

012.5

77

−Candid

ate

b

202900527.0

12072.7

5711+

0.0

0057

−0.0

0053

13.0

0838

±0.0

0021

19.3

+0.9

−1.2

89.0

3+

0.5

9−

0.5

30.1

010+

0.0

022

−0.0

013

15.7

+3.0

−2.3

1.4

2+

0.2

7−

0.2

11.0

04+

0.0

86

−0.0

47

12.3

03

−Candid

ate

a,d

,e

203771098.0

12082.6

2484+

0.0

0057

−0.0

0055

42.3

6398+

0.0

0076

−0.0

0080

49.8

+3.3

−4.5

89.5

7+

0.2

8−

0.2

50.0

611+

0.0

017

−0.0

011

7.1

2+

0.6

8−

0.3

51.0

68+

0.0

97

−0.0

50

1.0

95+

0.0

28

−0.0

29

11.6

48

<1.0

0e

−04

Pla

net

203771098.0

22072.7

9594+

0.0

0087

−0.0

0080

20.8

8502+

0.0

0041

−0.0

0044

26.5

+3.6

−4.2

88.8

7+

0.7

1−

0.6

70.0

451+

0.0

023

−0.0

016

5.2

6+

0.5

5−

0.3

11.0

68+

0.0

97

−0.0

50

1.0

95+

0.0

28

−0.0

29

11.6

48

<1.0

0e

−04

Pla

net

203826436.0

12065.8

559+

0.0

021

−0.0

020

6.4

2958+

0.0

0029

−0.0

0031

15.3

+2.1

−4.9

88.2

+1.4

−2.7

0.0

291+

0.0

035

−0.0

014

2.6

0+

0.3

3−

0.1

50.8

18+

0.0

32

−0.0

25

0.8

87+

0.0

25

−0.0

31

12.2

41

<1.0

0e

−04

Pla

net

203826436.0

22074.2

360+

0.0

026

−0.0

024

14.0

910+

0.0

010

−0.0

011

34.0

+5.0

−11.0

89.2

+0.6

−1.2

0.0

270+

0.0

036

−0.0

015

2.4

1+

0.3

3−

0.1

50.8

18+

0.0

32

−0.0

25

0.8

87+

0.0

25

−0.0

31

12.2

41

<1.0

0e

−04

Pla

net

203826436.0

32065.1

129+

0.0

046

−0.0

042

4.4

4377+

0.0

0045

−0.0

0050

10.8

+1.4

−3.1

87.5

+1.8

−3.4

0.0

171+

0.0

019

−0.0

010

1.5

3+

0.1

8−

0.1

00.8

18+

0.0

32

−0.0

25

0.8

87+

0.0

25

−0.0

31

12.2

41

<1.0

0e

−04

Pla

net

204750116.0

12065.8

359+

0.0

040

−0.0

037

23.4

469+

0.0

019

−0.0

021

27.9

+3.8

−8.2

89.0

+0.7

−1.3

0.0

269+

0.0

026

−0.0

013

2.9

0+

0.3

2−

0.1

80.9

87+

0.0

51

−0.0

39

1.0

37+

0.0

26

−0.0

30

11.5

26

−Candid

ate

c

205029914.0

12061.7

314+

0.0

014

−0.0

015

4.9

8184

±0.0

0017

8.6

+1.4

−3.4

86.4

+2.6

−6.0

0.0

224+

0.0

026

−0.0

009

2.3

9+

0.3

8−

0.1

70.9

8+

0.1

1−

0.0

60.9

83+

0.0

29

−0.0

34

12.1

83

−Candid

ate

c

205071984.0

12067.9

2671+

0.0

0060

−0.0

0063

8.9

9194

±0.0

0016

20.2

+1.0

−2.3

89.1

2+

0.6

1−

0.8

60.0

565+

0.0

013

−0.0

010

5.1

7+

0.2

0−

0.1

60.8

39+

0.0

26

−0.0

21

0.9

16+

0.0

20

−0.0

26

12.0

05

<1.0

0e

−04

Pla

net

205071984.0

22070.7

929+

0.0

024

−0.0

025

31.7

151+

0.0

026

−0.0

022

45.0

+6.0

−15.0

89.3

5+

0.4

7−

0.9

10.0

373+

0.0

025

−0.0

013

3.4

1+

0.2

6−

0.1

40.8

39+

0.0

26

−0.0

21

0.9

16+

0.0

20

−0.0

26

12.0

05

<1.0

0e

−04

Pla

net

205071984.0

32066.4

221+

0.0

036

−0.0

039

20.6

616+

0.0

018

−0.0

017

33.5

+3.2

−8.0

89.2

7+

0.5

1−

0.9

10.0

340+

0.0

016

−0.0

010

3.1

2+

0.1

8−

0.1

20.8

39+

0.0

26

−0.0

21

0.9

16+

0.0

20

−0.0

26

12.0

05

<1.0

0e

−04

Pla

net

28 Mayo et al.Table

4—

Continued

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

K2-1

67

b205904628.0

12146.9

368+

0.0

025

−0.0

024

9.9

775

±0.0

010

19.4

+2.5

−5.9

88.6

+1.0

−2.0

0.0

141+

0.0

013

−0.0

007

2.8

2+

0.5

2−

0.4

51.8

3+

0.2

9−

0.2

81.0

2+

0.1

2−

0.0

98.2

20

8.6

4e

−04

Pla

net

205944181.0

12148.8

1517+

0.0

0094

−0.0

0085

2.4

75641+

0.0

00057

−0.0

00054

8.0

+15.0

−2.0

82.2

+6.9

−4.0

0.0

6+

0.1

9−

0.0

35.0

+17.0

−3.0

0.8

25+

0.0

46

−0.0

26

0.8

72+

0.0

26

−0.0

33

12.4

10

9.4

9e

−01

Candid

ate

K2-1

68

b205950854.0

12157.8

877+

0.0

027

−0.0

026

15.8

540

±0.0

014

27.9

+4.1

−8.6

88.9

+0.7

−1.3

0.0

225+

0.0

013

−0.0

010

2.1

4+

0.2

1−

0.1

40.8

74+

0.0

68

−0.0

39

0.9

07+

0.0

29

−0.0

32

12.1

05

7.1

0e

−04

Pla

net

205957328.0

12148.5

855+

0.0

035

−0.0

032

14.3

534+

0.0

014

−0.0

015

31.0

+6.0

−13.0

89.0

+0.7

−1.8

0.0

239+

0.0

044

−0.0

018

2.1

6+

0.4

1−

0.1

70.8

28+

0.0

33

−0.0

21

0.8

92+

0.0

22

−0.0

27

12.4

64

3.9

7e

−03

Candid

ate

K2-1

69

b206007892.0

12149.0

097+

0.0

036

−0.0

038

6.3

8080+

0.0

0078

−0.0

0070

13.6

+2.2

−5.1

87.8

+1.6

−3.6

0.0

1270+

0.0

0083

−0.0

0065

1.2

7+

0.1

1−

0.0

80.9

19+

0.0

49

−0.0

30

0.9

86+

0.0

28

−0.0

26

12.0

23

<1.0

0e

−04

Pla

net

K2-1

70

c206008091.0

12152.6

669+

0.0

047

−0.0

046

12.4

000+

0.0

017

−0.0

019

20.9

+3.0

−7.6

88.7

+1.0

−2.3

0.0

168+

0.0

013

−0.0

008

1.8

0+

0.2

5−

0.1

60.9

8+

0.1

1−

0.0

70.9

64

±0.0

32

12.5

06

<1.0

0e

−04

Pla

net

K2-1

70

b206008091.0

22153.1

855+

0.0

069

−0.0

074

7.5

765+

0.0

018

−0.0

017

14.3

+2.3

−5.3

88.0

+1.4

−3.3

0.0

132+

0.0

012

−0.0

008

1.4

2+

0.2

0−

0.1

30.9

8+

0.1

1−

0.0

70.9

64

±0.0

32

12.5

06

<1.0

0e

−04

Pla

net

206011496.0

12148.6

4577+

0.0

0095

−0.0

0098

2.3

69008+

0.0

00056

−0.0

00059

7.3

+0.7

−1.8

86.6

+2.4

−4.3

0.0

171+

0.0

011

−0.0

005

1.6

6+

0.1

6−

0.0

80.8

89+

0.0

61

−0.0

30

0.9

40+

0.0

25

−0.0

27

10.9

16

−Candid

ate

c

206026904.0

12146.9

2339+

0.0

0086

−0.0

0090

7.0

5248

±0.0

0016

24.8

+3.4

−7.8

88.9

+0.8

−1.6

0.0

296+

0.0

030

−0.0

013

2.5

9+

0.2

8−

0.1

30.8

03+

0.0

34

−0.0

20

0.8

58+

0.0

22

−0.0

27

12.1

50

<1.0

0e

−04

Pla

net

206026904.0

22146.5

862

±0.0

014

2.5

37071+

0.0

00096

−0.0

00093

7.9

+1.3

−3.4

86.1

+2.8

−7.3

0.0

185+

0.0

028

−0.0

009

1.6

3+

0.2

6−

0.0

90.8

03+

0.0

34

−0.0

20

0.8

58+

0.0

22

−0.0

27

12.1

50

<1.0

0e

−04

Pla

net

206026904.0

32165.0

672+

0.0

029

−0.0

028

22.8

816+

0.0

021

−0.0

022

49.0

+6.0

−15.0

89.4

3+

0.4

1−

0.8

10.0

200+

0.0

021

−0.0

009

1.7

5+

0.2

0−

0.0

90.8

03+

0.0

34

−0.0

20

0.8

58+

0.0

22

−0.0

27

12.1

50

<1.0

0e

−04

Pla

net

206044803.0

12147.6

401

±0.0

024

2.5

7341+

0.0

0016

−0.0

0017

6.6

+0.9

−2.1

86.0

+2.9

−6.4

0.0

174+

0.0

022

−0.0

009

1.9

3+

0.3

2−

0.1

51.0

2+

0.1

1−

0.0

61.0

30

±0.0

29

12.9

75

2.1

6e

−04

Pla

net

K2-1

71

b206049764.0

12146.4

671

±0.0

071

5.6

285+

0.0

017

−0.0

015

5.5

+0.7

−2.1

85.0

+3.7

−9.6

0.0

143+

0.0

011

−0.0

007

2.6

9+

0.4

0−

0.3

31.7

2+

0.2

2−

0.1

90.8

92+

0.0

60

−0.0

27

12.4

45

<1.0

0e

−04

Pla

net

K2-1

72

c206082454.0

12160.5

398+

0.0

011

−0.0

012

29.6

268

±0.0

016

44.2

+3.4

−7.8

89.5

0+

0.3

5−

0.5

30.0

338+

0.0

013

−0.0

009

3.2

1+

0.1

9−

0.1

40.8

69+

0.0

38

−0.0

29

0.9

34+

0.0

26

−0.0

27

12.3

08

<1.0

0e

−04

Pla

net

K2-1

72

b206082454.0

22149.2

949

±0.0

034

14.3

169

±0.0

014

25.1

+3.1

−8.5

88.9

+0.8

−1.7

0.0

176+

0.0

015

−0.0

008

1.6

7+

0.1

6−

0.1

00.8

69+

0.0

38

−0.0

29

0.9

34+

0.0

26

−0.0

27

12.3

08

<1.0

0e

−04

Pla

net

206096602.0

12149.6

8564+

0.0

0097

−0.0

0098

6.6

7177+

0.0

0018

−0.0

0017

29.9

+3.8

−8.6

89.1

+0.6

−1.2

0.0

272+

0.0

017

−0.0

011

1.9

3+

0.1

3−

0.1

00.6

48+

0.0

21

−0.0

18

0.6

84+

0.0

22

−0.0

23

12.0

45

<1.0

0e

−04

Pla

net

206096602.0

22158.5

448

±0.0

016

16.1

9720+

0.0

0083

−0.0

0082

77.0

+13.0

−32.0

89.6

1+

0.2

9−

0.7

10.0

268+

0.0

027

−0.0

014

1.8

9+

0.2

0−

0.1

10.6

48+

0.0

21

−0.0

18

0.6

84+

0.0

22

−0.0

23

12.0

45

<1.0

0e

−04

Pla

net

206114630.0

12152.3

896+

0.0

014

−0.0

013

7.4

4503

±0.0

0030

55.0

+18.0

−37.0

89.3

+0.5

−2.7

0.0

25+

0.0

34

−0.0

03

2.3

+3.1

−0.3

0.8

25+

0.0

30

−0.0

19

0.8

97+

0.0

21

−0.0

24

11.0

32

9.9

1e

−01

Candid

ate

206119924.0

12146.9

496

±0.0

043

4.6

5534

±0.0

0051

13.8

+2.9

−5.4

87.8

+1.6

−3.6

0.0

096+

0.0

012

−0.0

007

0.7

19+

0.0

89

−0.0

57

0.6

87+

0.0

15

−0.0

17

0.7

27+

0.0

20

−0.0

21

10.3

10

−Candid

ate

b

206144956.0

12153.3

277+

0.0

015

−0.0

016

12.6

4781+

0.0

0067

−0.0

0072

28.9

+3.0

−8.5

89.1

+0.6

−1.3

0.0

189+

0.0

033

−0.0

011

1.3

8+

0.2

5−

0.0

90.6

69+

0.0

23

−0.0

21

0.7

02+

0.0

25

−0.0

23

10.3

96

<1.0

0e

−04

Pla

net

206146957.0

12146.8

699

±0.0

033

5.7

6136

±0.0

0052

16.9

+2.5

−6.0

88.3

+1.2

−2.7

0.0

140+

0.0

013

−0.0

008

1.3

7+

0.1

5−

0.0

90.9

02+

0.0

48

−0.0

34

0.9

56+

0.0

31

−0.0

30

11.3

79

5.2

2e

−03

Candid

ate

206159027.0

12149.3

259+

0.0

019

−0.0

020

8.0

5479+

0.0

0045

−0.0

0044

19.9

+2.3

−4.2

88.7

+0.9

−1.3

0.0

239+

0.0

017

−0.0

011

1.8

3+

0.1

4−

0.1

00.7

02

±0.0

21

0.7

51+

0.0

25

−0.0

26

12.5

97

<1.0

0e

−04

Pla

net

206169375.0

12146.5

3588+

0.0

0072

−0.0

0069

0.3

674730

±0.0

000070

2.5

+1.4

−1.1

72.0

+15.0

−34.0

0.0

3+

0.1

5−

0.0

04.0

+20.0

−1.0

1.2

6+

0.2

2−

0.1

51.0

96+

0.0

56

−0.0

47

12.5

59

9.2

5e

−01

Candid

ate

206181769.0

12151.4

441+

0.0

012

−0.0

011

13.9

7852+

0.0

0056

−0.0

0057

29.6

+2.9

−7.8

89.1

+0.6

−1.1

0.0

3157+

0.0

0099

−0.0

0076

2.7

5+

0.1

5−

0.1

00.7

99+

0.0

34

−0.0

21

0.8

48+

0.0

23

−0.0

28

12.7

70

<1.0

0e

−04

Pla

net

206192335.0

12146.9

471

±0.0

020

3.5

9905+

0.0

0020

−0.0

0018

13.4

+2.1

−4.5

87.9

+1.4

−3.2

0.0

176+

0.0

015

−0.0

010

1.5

9+

0.1

6−

0.1

10.8

26+

0.0

39

−0.0

28

0.8

83+

0.0

29

−0.0

30

11.8

70

−Candid

ate

c

206245553.0

12147.1

766+

0.0

014

−0.0

013

7.4

9569

±0.0

0028

15.1

+1.4

−3.2

88.4

+1.1

−1.8

0.0

229+

0.0

013

−0.0

006

2.6

3+

0.3

6−

0.1

91.0

5+

0.1

3−

0.0

71.0

43+

0.0

26

−0.0

27

11.7

45

<1.0

0e

−04

Pla

net

206268299.0

12164.9

999+

0.0

023

−0.0

027

19.5

656+

0.0

019

−0.0

017

26.1

+3.3

−5.9

88.9

+0.7

−1.0

0.0

250+

0.0

018

−0.0

011

2.9

6+

0.4

3−

0.3

31.0

9+

0.1

4−

0.1

10.9

87

±0.0

40

12.4

30

5.1

7e

−04

Pla

net

206348688.0

12150.4

293+

0.0

037

−0.0

039

7.8

1795+

0.0

0078

−0.0

0075

10.6

+1.3

−4.1

87.4

+1.9

−5.0

0.0

189+

0.0

012

−0.0

007

2.5

5+

0.3

7−

0.2

31.2

4+

0.1

6−

0.1

11.1

74+

0.0

48

−0.0

41

12.5

66

<1.0

0e

−04

Pla

net

206348688.0

22159.7

472+

0.0

067

−0.0

097

18.2

861+

0.0

057

−0.0

046

21.4

+2.4

−6.3

88.8

+0.9

−1.8

0.0

194+

0.0

011

−0.0

008

2.6

3+

0.3

7−

0.2

51.2

4+

0.1

6−

0.1

11.1

74+

0.0

48

−0.0

41

12.5

66

<1.0

0e

−04

Pla

net

206439513.0

12159.8

681+

0.0

082

−0.0

080

18.4

151+

0.0

067

−0.0

065

2.7

2+

0.3

0−

0.2

264.3

+4.8

−7.2

0.1

8+

0.3

4−

0.1

169.0

+130.0

−42.0

3.4

7+

0.4

8−

0.4

41.6

2+

0.0

7−

0.1

011.4

37

−Candid

ate

a

206535016.0

12163.3

684+

0.0

028

−0.0

030

20.3

981

±0.0

019

73.0

+16.0

−39.0

89.6

+0.3

−1.2

0.0

304+

0.0

088

−0.0

026

2.5

8+

0.7

6−

0.2

40.7

77+

0.0

38

−0.0

28

0.8

15+

0.0

32

−0.0

29

11.6

44

1.9

2e

−01

Candid

ate

210363145.0

12237.8

065+

0.0

015

−0.0

014

8.1

9981+

0.0

0036

−0.0

0037

23.5

+2.5

−7.1

88.9

+0.8

−1.7

0.0

292+

0.0

012

−0.0

010

2.5

0+

0.1

3−

0.0

90.7

84+

0.0

24

−0.0

14

0.8

52+

0.0

19

−0.0

24

11.8

96

<1.0

0e

−04

Pla

net

210365511.0

12234.6

17

±0.0

10

3.9

520+

0.0

012

−0.0

013

1.4

7+

0.5

0−

0.1

138.9

±9.2

0.1

1+

0.3

8−

0.0

78.0

+29.0

−6.0

0.6

92+

0.0

20

−0.0

21

0.7

30+

0.0

24

−0.0

23

12.4

39

−Candid

ate

a

210402237.0

12237.2

465

±0.0

020

10.9

9395+

0.0

0060

−0.0

0063

17.7

+1.6

−4.1

88.6

+1.0

−1.7

0.0

278+

0.0

015

−0.0

009

3.1

5+

0.3

3−

0.1

81.0

38+

0.0

92

−0.0

50

1.0

62+

0.0

29

−0.0

26

11.8

01

<1.0

0e

−04

Pla

net

210403955.0

12244.5

926+

0.0

056

−0.0

055

19.0

999+

0.0

041

−0.0

040

29.0

+5.0

−11.0

89.0

+0.7

−1.6

0.0

230+

0.0

032

−0.0

013

2.1

1+

0.3

0−

0.1

30.8

41+

0.0

31

−0.0

22

0.9

13+

0.0

21

−0.0

24

12.3

88

<1.0

0e

−04

Pla

net

210403955.0

22233.4

860+

0.0

037

−0.0

038

5.6

0531+

0.0

0064

−0.0

0063

13.3

+1.9

−4.5

87.9

+1.5

−3.3

0.0

162+

0.0

020

−0.0

010

1.4

9+

0.1

9−

0.1

00.8

41+

0.0

31

−0.0

22

0.9

13+

0.0

21

−0.0

24

12.3

88

<1.0

0e

−04

Pla

net

K2-8

0d

210403955.0

32249.9

371+

0.0

036

−0.0

045

28.8

673+

0.0

051

−0.0

046

46.0

+6.0

−13.0

89.4

0+

0.4

3−

0.7

70.0

278+

0.0

028

−0.0

013

2.5

5+

0.2

8−

0.1

40.8

41+

0.0

31

−0.0

22

0.9

13+

0.0

21

−0.0

24

12.3

88

<1.0

0e

−04

Pla

net

210423938.0

12239.0

161+

0.0

043

−0.0

037

19.8

605+

0.0

020

−0.0

022

34.0

+9.0

−18.0

89.0

+0.8

−2.3

0.0

274+

0.0

071

−0.0

027

2.0

8+

0.5

4−

0.2

20.6

97+

0.0

21

−0.0

20

0.7

41+

0.0

24

−0.0

26

12.6

55

8.4

5e

−02

Candid

ate

K2-1

73

b210512842.0

12234.1

411+

0.0

029

−0.0

028

5.8

6870+

0.0

0045

−0.0

0041

13.0

+1.8

−3.9

87.8

+1.5

−2.9

0.0

175+

0.0

013

−0.0

008

1.6

1+

0.1

6−

0.1

10.8

43+

0.0

58

−0.0

39

0.8

82+

0.0

34

−0.0

36

12.1

06

7.2

0e

−04

Pla

net

K2-1

74

b210558622.0

12231.2

161+

0.0

011

−0.0

012

19.5

6274+

0.0

0076

−0.0

0073

23.5

+2.2

−4.2

88.9

4+

0.7

1−

0.9

60.0

357+

0.0

023

−0.0

009

2.4

9+

0.1

8−

0.1

00.6

39+

0.0

20

−0.0

19

0.6

68+

0.0

22

−0.0

21

12.0

34

<1.0

0e

−04

Pla

net

210609658.0

12241.4

056

±0.0

011

14.1

4524+

0.0

0044

−0.0

0047

8.0

7+

0.7

5−

0.5

186.5

+1.7

−0.9

0.0

633+

0.0

015

−0.0

019

14.9

+1.8

−1.5

2.1

5+

0.2

6−

0.2

11.0

09+

0.0

81

−0.0

49

12.5

87

−Candid

ate

a

210629082.0

12253.0

149+

0.0

051

−0.0

052

27.3

531+

0.0

073

−0.0

075

25.7

+3.1

−8.0

89.0

+0.7

−1.5

0.0

193+

0.0

029

−0.0

012

3.0

5+

0.6

9−

0.4

31.4

5+

0.2

5−

0.1

81.2

56+

0.0

78

−0.0

58

11.5

80

2.0

9e

−03

Candid

ate

K2-1

75

b210643811.0

12240.2

768+

0.0

045

−0.0

044

9.5

260+

0.0

012

−0.0

013

11.1

+1.3

−3.0

87.5

+1.7

−3.0

0.0

132+

0.0

013

−0.0

007

2.0

4+

0.3

6−

0.2

71.4

2+

0.2

1−

0.1

71.0

95+

0.0

57

−0.0

39

10.6

32

5.2

6e

−04

Pla

net

K2-1

76

b210667381.0

12233.7

859+

0.0

037

−0.0

038

5.3

2944+

0.0

0061

−0.0

0071

13.8

+2.0

−4.4

88.1

+1.4

−2.9

0.0

158+

0.0

012

−0.0

009

1.4

9+

0.1

2−

0.0

90.8

64+

0.0

33

−0.0

20

0.9

39+

0.0

20

−0.0

25

12.6

74

5.3

8e

−04

Pla

net

210707130.0

12231.6

8219+

0.0

0074

−0.0

0072

0.6

84553

±0.0

00013

5.7

+0.7

−1.5

85.5

+3.3

−6.1

0.0

181+

0.0

014

−0.0

010

1.2

8+

0.1

1−

0.0

80.6

47+

0.0

20

−0.0

19

0.6

78+

0.0

21

−0.0

22

12.0

99

<1.0

0e

−04

Pla

net

210718708.0

12237.0

169

±0.0

035

8.7

7586+

0.0

0090

−0.0

0089

20.3

+3.4

−7.2

88.6

+1.0

−2.2

0.0

251+

0.0

031

−0.0

017

1.9

8+

0.2

6−

0.1

50.7

22+

0.0

35

−0.0

25

0.7

57+

0.0

28

−0.0

29

12.8

01

<1.0

0e

−04

Pla

net

210775710.0

12231.6

9728

±0.0

0013

59.8

4857

±0.0

0018

114.7

+4.2

−6.7

89.8

54+

0.0

98

−0.0

90

0.1

008+

0.0

019

−0.0

011

10.8

+1.2

−0.6

0.9

8+

0.1

0−

0.0

51.0

03+

0.0

26

−0.0

27

11.8

27

1.5

5e

−03

Candid

ate

210848071.0

12235.5

288

±0.0

028

41.6

886

±0.0

034

55.0

+6.0

−13.0

89.5

3+

0.3

3−

0.5

40.0

226+

0.0

018

−0.0

009

2.3

6+

0.3

1−

0.1

70.9

56+

0.0

99

−0.0

55

0.9

64+

0.0

30

−0.0

32

11.0

40

1.6

2e

−03

Candid

ate

K2-1

77

b210857328.0

12237.0

802+

0.0

071

−0.0

069

14.1

552+

0.0

032

−0.0

030

10.6

+1.6

−3.4

87.2

+2.0

−3.7

0.0

160+

0.0

018

−0.0

009

2.1

2+

0.2

8−

0.1

61.2

14+

0.0

87

−0.0

61

1.2

11+

0.0

32

−0.0

38

12.5

84

1.1

9e

−04

Pla

net

210894022.0

12234.9

691+

0.0

046

−0.0

045

5.3

5140+

0.0

0060

−0.0

0061

10.4

+1.8

−3.7

87.0

+2.1

−4.3

0.0

121+

0.0

013

−0.0

007

1.2

2+

0.2

0−

0.1

20.9

2+

0.1

1−

0.0

80.8

77+

0.0

36

−0.0

41

12.3

00

<1.0

0e

−04

Pla

net

210957318.0

12234.9

0560+

0.0

0024

−0.0

0025

4.0

98492+

0.0

00027

−0.0

00028

11.7

1+

0.5

9−

0.5

086.5

6+

0.4

0−

0.3

70.1

276+

0.0

028

−0.0

034

12.6

5+

0.8

1−

0.5

30.9

09+

0.0

54

−0.0

29

0.9

70+

0.0

24

−0.0

27

13.1

71

−Candid

ate

a

K2-1

78

b210965800.0

12237.3

366

±0.0

015

8.7

4782

±0.0

0036

18.5

+1.9

−4.4

88.6

+1.0

−1.6

0.0

368+

0.0

011

−0.0

009

3.5

6+

0.2

0−

0.1

40.8

87+

0.0

44

−0.0

26

0.9

51+

0.0

23

−0.0

28

12.1

34

3.4

7e

−04

Pla

net


4—

Continued

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

K2-1

79

b211048999.0

12233.5

803+

0.0

014

−0.0

015

5.1

7219

±0.0

0020

20.1

+2.3

−5.1

88.8

+0.9

−1.6

0.0

300+

0.0

018

−0.0

013

2.5

1+

0.1

6−

0.1

20.7

68+

0.0

22

−0.0

18

0.8

24+

0.0

22

−0.0

27

12.6

59

4.9

7e

−04

Pla

net

211089792.0

12231.4

3152

±0.0

0010

3.2

588240

±0.0

000090

10.9

9+

0.6

1−

0.4

186.9

7+

0.6

2−

0.4

40.1

289

±0.0

035

12.0

6+

0.6

5−

0.4

70.8

58+

0.0

40

−0.0

24

0.9

23+

0.0

23

−0.0

26

12.9

14

−Candid

ate

b,c

211106187.0

12239.2

745+

0.0

030

−0.0

028

14.6

431+

0.0

013

−0.0

014

55.0

+15.0

−30.0

89.4

+0.5

−1.7

0.0

46+

0.0

26

−0.0

05

66.0

+43.0

−15.0

13.2

+4.6

−2.7

1.1

0+

0.4

7−

0.1

813.1

24

−Candid

ate

a,b

,d

211147528.0

12232.4

082+

0.0

012

−0.0

013

2.3

49515+

0.0

00080

−0.0

00077

6.4

+1.6

−1.1

84.1

+4.3

−3.0

0.0

905+

0.0

067

−0.0

078

53.0

+6.0

−11.0

5.4

+0.5

−1.0

2.0

2+

0.0

5−

0.1

311.8

32

−Candid

ate

a,c

K2-1

80

b211319617.0

12310.3

955

±0.0

016

8.8

6593+

0.0

0032

−0.0

0033

21.6

+2.8

−6.3

88.7

+1.0

−1.7

0.0

324+

0.0

026

−0.0

013

2.4

1+

0.2

1−

0.1

10.6

81+

0.0

21

−0.0

16

0.7

30+

0.0

20

−0.0

22

12.3

93

<1.0

0e

−04

Pla

net

211351816.0

12309.0

552+

0.0

052

−0.0

046

8.4

053

±0.0

012

8.7

+2.0

−3.8

85.9

+2.9

−6.4

0.0

250+

0.0

032

−0.0

016

8.0

+1.4

−1.0

2.9

5+

0.3

7−

0.3

01.0

54+

0.0

89

−0.0

67

12.4

09

−Candid

ate

a

K2-1

81

b211355342.0

12310.7

936+

0.0

026

−0.0

025

6.8

9425

±0.0

0043

18.4

+2.2

−4.8

88.6

+1.0

−1.8

0.0

248+

0.0

021

−0.0

013

2.7

1+

0.3

1−

0.1

80.9

99+

0.0

77

−0.0

41

1.0

44+

0.0

24

−0.0

29

12.6

37

9.9

5e

−04

Pla

net

K2-1

82

b211359660.0

12308.2

0586+

0.0

0064

−0.0

0065

4.7

36884+

0.0

00071

−0.0

00075

13.4

+1.1

−2.3

88.3

+1.2

−1.7

0.0

321+

0.0

015

−0.0

008

2.7

7+

0.1

7−

0.1

00.7

90+

0.0

32

−0.0

21

0.8

47+

0.0

24

−0.0

31

11.7

42

5.9

7e

−04

Pla

net

211391664.0

12312.9

800+

0.0

015

−0.0

016

10.1

3680+

0.0

0042

−0.0

0039

14.6

+1.0

−2.4

88.5

+1.0

−1.5

0.0

304+

0.0

012

−0.0

007

5.0

1+

0.7

6−

0.7

41.5

1±

0.2

21.1

56+

0.0

82

−0.0

69

12.1

02

2.6

5e

−04

Pla

net

211401787.0

12318.0

685+

0.0

025

−0.0

024

13.7

738

±0.0

011

20.1

+2.5

−7.5

88.6

+1.0

−2.4

0.0

180+

0.0

019

−0.0

007

3.2

9+

0.6

2−

0.4

71.6

8+

0.2

7−

0.2

31.2

0+

0.1

0−

0.0

99.7

09

3.6

5e

−03

Candid

ate

211418290.0

12308.8

0704+

0.0

0081

−0.0

0086

5.0

3207

±0.0

0010

4.9

2+

0.0

5−

0.1

188.4

+1.1

−1.4

0.0

9133+

0.0

0069

−0.0

0063

36.7

+5.4

−3.9

3.6

9+

0.5

4−

0.3

90.9

15+

0.0

68

−0.0

51

11.5

04

−Candid

ate

a

211424769.0

12311.4

9837

±0.0

0031

5.1

76243+

0.0

00040

−0.0

00041

12.5

+1.1

−0.9

85.1

+0.9

−1.2

0.1

6+

0.2

0−

0.0

619.0

+25.0

−8.0

1.1

2+

0.1

1−

0.0

71.1

02+

0.0

41

−0.0

37

9.4

38

−Candid

ate

a,e

211491383.0

12308.5

884+

0.0

074

−0.0

092

4.1

454+

0.0

010

−0.0

008

8.8

+1.9

−3.1

86.7

+2.4

−5.2

0.0

084+

0.0

012

−0.0

008

1.2

0+

0.2

6−

0.1

81.3

1+

0.2

2−

0.1

61.1

01+

0.0

53

−0.0

50

11.7

85

2.4

0e

−03

Candid

ate

211525389.0

12314.9

9178+

0.0

0064

−0.0

0068

8.2

6679+

0.0

0014

−0.0

0013

17.9

+1.1

−2.1

88.8

7+

0.7

4−

0.9

40.0

3437+

0.0

0086

−0.0

0066

3.4

1+

0.2

3−

0.1

50.9

09+

0.0

58

−0.0

36

0.9

65+

0.0

31

−0.0

29

11.6

87

<1.0

0e

−04

Pla

net

K2-1

83

c211562654.0

12314.7

749+

0.0

031

−0.0

028

10.7

9347+

0.0

0080

−0.0

0073

19.0

+3.0

−5.1

88.4

+1.1

−1.7

0.0

264+

0.0

025

−0.0

012

2.5

1+

0.2

6−

0.1

40.8

73+

0.0

37

−0.0

23

0.9

42+

0.0

21

−0.0

25

12.7

54

<1.0

0e

−04

Pla

net

K2-1

83

d211562654.0

22311.1

552+

0.0

034

−0.0

037

22.6

295+

0.0

018

−0.0

019

45.0

+6.0

−14.0

89.3

8+

0.4

5−

0.8

40.0

267+

0.0

027

−0.0

014

2.5

4+

0.2

8−

0.1

50.8

73+

0.0

37

−0.0

23

0.9

42+

0.0

21

−0.0

25

12.7

54

<1.0

0e

−04

Pla

net

K2-1

83

b211562654.0

32307.6

034+

0.0

019

−0.0

021

0.4

69269+

0.0

00026

−0.0

00024

1.4

0+

0.9

3−

0.2

925.0

+56.0

−10.0

0.0

3+

0.2

7−

0.0

13.0

+26.0

−1.0

0.8

73+

0.0

37

−0.0

23

0.9

42+

0.0

21

−0.0

25

12.7

54

<1.0

0e

−04

Pla

net

K2-1

84

b211594205.0

12315.5

008

±0.0

014

16.9

9344+

0.0

0079

−0.0

0078

48.0

+6.0

−13.0

89.4

7+

0.4

0−

0.7

10.0

184+

0.0

016

−0.0

009

1.5

4+

0.1

5−

0.0

90.7

64+

0.0

33

−0.0

25

0.8

19+

0.0

28

−0.0

30

10.6

80

<1.0

0e

−04

Pla

net

211606790.0

12317.0

8969+

0.0

0050

−0.0

0057

37.2

4687+

0.0

0085

−0.0

0069

32.3

+2.1

−1.9

88.2

0+

0.2

0−

0.2

30.1

48+

0.0

56

−0.0

31

23.8

+9.7

−5.6

1.4

8+

0.2

2−

0.1

70.9

47+

0.0

73

−0.0

32

12.6

73

−Candid

ate

a,e

K2-1

85

b211611158.0

12311.7

371+

0.0

060

−0.0

054

10.6

166+

0.0

016

−0.0

018

27.0

+5.0

−10.0

88.9

+0.8

−1.9

0.0

132+

0.0

021

−0.0

011

1.3

1+

0.2

2−

0.1

20.9

14+

0.0

44

−0.0

33

0.9

76

±0.0

28

12.4

14

7.2

4e

−04

Pla

net

211611158.0

22326.1

581+

0.0

025

−0.0

024

52.7

141+

0.0

038

−0.0

036

48.0

+33.0

−17.0

89.0

0+

0.7

9−

0.7

80.0

280+

0.0

044

−0.0

043

2.8

0+

0.4

6−

0.4

40.9

14+

0.0

44

−0.0

33

0.9

76

±0.0

28

12.4

14

4.1

6e

−03

Candid

ate

211682544.0

12312.5

676+

0.0

017

−0.0

018

50.8

193+

0.0

024

−0.0

025

104.0

+15.0

−34.0

89.7

2+

0.2

0−

0.4

00.0

237+

0.0

019

−0.0

010

2.1

7+

0.2

1−

0.1

20.8

37+

0.0

40

−0.0

27

0.8

98+

0.0

27

−0.0

31

11.4

07

2.9

2e

−03

Candid

ate

211733267.0

12311.9

3174

±0.0

0015

8.6

58168

±0.0

00030

23.0

+1.4

−1.0

87.3

6+

0.3

7−

0.3

90.1

9+

0.1

1−

0.0

617.0

+10.0

−5.0

0.8

19+

0.0

40

−0.0

28

0.8

72+

0.0

27

−0.0

29

12.1

50

4.4

0e

−01

Candid

ate

211736671.0

12312.0

974

±0.0

013

4.7

3379

±0.0

0015

8.6

+1.7

−2.6

86.1

+2.7

−4.0

0.0

301+

0.0

030

−0.0

014

7.6

+1.5

−1.2

2.3

1+

0.3

8−

0.3

51.2

9±

0.1

112.1

60

8.4

5e

−03

Candid

ate

211743874.0

12315.2

087+

0.0

051

−0.0

049

12.2

823+

0.0

017

−0.0

018

19.1

+2.7

−6.3

88.5

+1.1

−2.2

0.0

164+

0.0

013

−0.0

010

2.5

3±

0.3

81.4

1+

0.1

8−

0.1

91.1

28+

0.0

56

−0.0

40

12.4

86

−Candid

ate

c

211763214.0

12313.5

930+

0.0

056

−0.0

067

21.1

918+

0.0

033

−0.0

030

30.0

+5.0

−10.0

89.0

+0.7

−1.5

0.0

154+

0.0

016

−0.0

011

1.3

2+

0.1

6−

0.1

00.7

82+

0.0

43

−0.0

28

0.8

26+

0.0

30

−0.0

31

12.5

29

5.3

3e

−03

Candid

ate

211770696.0

12312.9

686+

0.0

051

−0.0

048

16.2

728

±0.0

024

14.8

+1.8

−4.1

88.1

+1.3

−2.3

0.0

182+

0.0

016

−0.0

009

2.1

1+

0.3

1−

0.2

51.0

6+

0.1

2−

0.1

10.8

72+

0.0

37

−0.0

35

12.2

53

−Candid

ate

c

211800191.0

12307.7

4930+

0.0

0036

−0.0

0035

1.1

061750

±0.0

000090

2.6

8+

0.2

6−

0.2

267.3

+3.1

−3.2

0.0

89+

0.0

60

−0.0

33

8.8

+6.0

−3.3

0.9

06+

0.0

91

−0.0

53

0.9

17+

0.0

36

−0.0

40

12.4

43

−Candid

ate

a

211818569.0

12310.5

6048

±0.0

0010

5.1

85759

±0.0

00014

20.1

+0.9

−1.3

89.0

3+

0.5

7−

0.5

40.1

021+

0.0

040

−0.0

023

7.6

4+

0.3

7−

0.2

90.6

86+

0.0

20

−0.0

21

0.7

27+

0.0

25

−0.0

24

12.9

35

<1.0

0e

−04

Pla

net

211886472.0

12319.3

7961+

0.0

0015

−0.0

0017

19.6

40123+

0.0

00091

−0.0

00083

36.4

+2.1

−1.8

88.3

3±

0.2

10.1

80+

0.0

79

−0.0

52

34.0

+16.0

−11.0

1.7

4+

0.3

2−

0.2

71.3

9+

0.1

1−

0.0

811.1

26

−Candid

ate

a,c

,e

K2-1

86

b211906650.0

12321.8

454+

0.0

019

−0.0

020

41.4

742+

0.0

033

−0.0

043

49.0

+4.0

−11.0

89.5

2+

0.3

3−

0.5

90.0

2965+

0.0

0093

−0.0

0087

3.1

7+

0.2

6−

0.1

60.9

81+

0.0

75

−0.0

41

1.0

19+

0.0

23

−0.0

27

12.1

93

<1.0

0e

−04

Pla

net

211913977.0

12319.6

820+

0.0

022

−0.0

023

14.6

7721+

0.0

0085

−0.0

0082

29.0

+6.0

−12.0

88.9

+0.8

−2.0

0.0

261+

0.0

036

−0.0

014

2.1

9+

0.3

1−

0.1

20.7

70+

0.0

22

−0.0

15

0.8

33+

0.0

20

−0.0

24

12.6

19

4.2

7e

−03

Candid

ate

211941472.0

12310.6

169+

0.0

079

−0.0

080

5.7

819

±0.0

013

10.2

+1.8

−2.7

87.6

+1.7

−3.5

0.0

096+

0.0

011

−0.0

008

1.4

4+

0.2

6−

0.2

11.3

8+

0.1

9−

0.1

61.0

20+

0.0

43

−0.0

33

11.7

88

−Candid

ate

c

211945201.0

12325.8

2591+

0.0

0066

−0.0

0067

19.4

9179+

0.0

0052

−0.0

0051

39.0

+4.2

−9.1

89.3

3+

0.4

9−

0.7

30.0

380+

0.0

026

−0.0

010

5.8

5+

0.9

5−

0.7

81.4

1+

0.2

1−

0.1

81.1

43+

0.0

59

−0.0

40

10.1

15

1.6

4e

−01

Candid

ate

211978988.0

12319.7

054+

0.0

031

−0.0

025

36.5

563+

0.0

036

−0.0

042

40.0

+5.0

−11.0

89.3

2+

0.4

7−

0.8

10.0

263+

0.0

020

−0.0

011

2.9

7+

0.4

4−

0.2

71.0

4+

0.1

3−

0.0

90.9

88+

0.0

28

−0.0

30

12.5

88

2.5

7e

−03

Candid

ate

211993818.0

12316.0

2846+

0.0

0028

−0.0

0029

8.9

86648+

0.0

00068

−0.0

00067

10.1

7+

0.3

1−

0.2

383.7

+1.0

−1.3

0.3

1+

0.2

3−

0.1

0143.0

+108.0

−50.0

4.2

6+

0.6

8−

0.5

21.1

1+

0.1

3−

0.0

67.2

18

−Candid

ate

d

212006318.0

12314.3

26+

0.0

11

−0.0

10

14.4

606+

0.0

037

−0.0

047

13.9

+2.2

−4.6

88.0

+1.5

−3.1

0.0

151+

0.0

017

−0.0

011

1.7

6+

0.3

1−

0.1

91.0

7+

0.1

4−

0.0

91.0

30+

0.0

27

−0.0

28

12.9

09

1.1

3e

−03

Candid

ate

212008766.0

12312.1

114+

0.0

026

−0.0

025

14.1

334

±0.0

010

26.6

+3.5

−9.8

89.0

+0.7

−1.9

0.0

285+

0.0

064

−0.0

019

2.3

2+

0.5

3−

0.1

70.7

48+

0.0

26

−0.0

21

0.8

05+

0.0

26

−0.0

27

12.8

02

1.5

0e

−03

Candid

ate

212012119.0

12309.1

345+

0.0

022

−0.0

021

3.2

8086

±0.0

0017

12.3

+1.4

−3.3

88.0

+1.4

−2.9

0.0

268+

0.0

017

−0.0

013

2.1

3+

0.1

5−

0.1

20.7

27+

0.0

23

−0.0

21

0.7

60+

0.0

28

−0.0

25

11.7

53

2.2

6e

−03

Candid

ate

212110888.0

12308.3

51088+

0.0

00090

−0.0

00088

2.9

956460

±0.0

000060

6.8

8+

0.1

6−

0.1

483.2

3+

0.2

7−

0.2

40.0

880+

0.0

017

−0.0

010

14.0

+2.0

−1.9

1.4

5+

0.2

1−

0.2

01.1

20+

0.0

53

−0.0

44

11.4

41

9.1

7e

−04

Pla

net

212132195.0

12331.3

908+

0.0

016

−0.0

017

26.1

970+

0.0

023

−0.0

022

55.0

+7.0

−18.0

89.5

2+

0.3

5−

0.7

70.0

313+

0.0

021

−0.0

014

2.3

6+

0.1

7−

0.1

30.6

92+

0.0

21

−0.0

20

0.7

37+

0.0

25

−0.0

24

11.6

70

2.2

9e

−03

Candid

ate

212138198.0

12309.3

7287+

0.0

0056

−0.0

0060

3.2

09149+

0.0

00047

−0.0

00042

15.0

+15.0

−5.0

86.5

+3.0

−3.3

0.0

6+

0.1

8−

0.0

15.0

+17.0

−1.0

0.8

39+

0.0

38

−0.0

28

0.8

98+

0.0

27

−0.0

29

12.9

02

−Candid

ate

c

K2-1

87

d212157262.0

12313.3

285

±0.0

020

7.1

4908+

0.0

0036

−0.0

0037

14.8

+4.2

−6.6

87.5

+1.9

−3.9

0.0

330+

0.0

050

−0.0

023

3.2

2+

0.5

1−

0.2

50.8

95+

0.0

41

−0.0

26

0.9

67+

0.0

25

−0.0

24

12.8

64

<1.0

0e

−04

Pla

net

K2-1

87

e212157262.0

22308.4

722+

0.0

050

−0.0

055

13.6

083+

0.0

017

−0.0

016

26.3

+3.4

−7.3

89.0

+0.8

−1.3

0.0

231+

0.0

020

−0.0

012

2.2

6+

0.2

2−

0.1

30.8

95+

0.0

41

−0.0

26

0.9

67+

0.0

25

−0.0

24

12.8

64

<1.0

0e

−04

Pla

net

K2-1

87

c212157262.0

32308.7

638+

0.0

036

−0.0

039

2.8

7179

±0.0

0026

7.6

+1.2

−3.0

86.1

+2.8

−7.0

0.0

174+

0.0

024

−0.0

011

1.7

0+

0.2

5−

0.1

10.8

95+

0.0

41

−0.0

26

0.9

67+

0.0

25

−0.0

24

12.8

64

<1.0

0e

−04

Pla

net

K2-1

87

b212157262.0

42308.0

935+

0.0

028

−0.0

030

0.7

73981+

0.0

00052

−0.0

00050

3.3

8+

0.4

8−

0.9

882.0

+6.0

−12.0

0.0

142+

0.0

015

−0.0

008

1.3

8+

0.1

6−

0.0

90.8

95+

0.0

41

−0.0

26

0.9

67+

0.0

25

−0.0

24

12.8

64

<1.0

0e

−04

Pla

net

K2-1

88

b212164470.0

12309.2

133+

0.0

050

−0.0

047

1.7

4298

±0.0

0026

4.7

+0.8

−1.7

83.9

+4.4

−9.9

0.0

1041+

0.0

0090

−0.0

0072

1.2

6+

0.1

6−

0.1

11.1

1+

0.1

1−

0.0

61.1

07+

0.0

31

−0.0

25

12.7

04

<1.0

0e

−04

Pla

net

K2-1

88

c212164470.0

22311.8

660

±0.0

026

7.8

0760+

0.0

0056

−0.0

0060

15.2

+2.1

−4.8

88.1

+1.4

−2.6

0.0

217+

0.0

014

−0.0

008

2.6

3+

0.3

1−

0.1

81.1

1+

0.1

1−

0.0

61.1

07+

0.0

31

−0.0

25

12.7

04

<1.0

0e

−04

Pla

net

212303338.0

12385.3

925+

0.0

034

−0.0

033

0.5

95621+

0.0

00044

−0.0

00046

4.7

+1.6

−1.7

84.0

+4.0

−10.0

0.0

062+

0.0

011

−0.0

007

0.5

8+

0.1

1−

0.0

70.8

63+

0.0

53

−0.0

30

0.9

15+

0.0

25

−0.0

29

9.9

57

−Candid

ate

c

212357477.0

12388.2

300+

0.0

013

−0.0

012

6.3

2667

±0.0

0020

21.9

+3.3

−7.6

88.7

+1.0

−2.0

0.0

205+

0.0

018

−0.0

009

2.1

2+

0.2

3−

0.1

20.9

47+

0.0

58

−0.0

33

1.0

00+

0.0

24

−0.0

28

10.2

15

3.0

4e

−03

Candid

ate

K2-1

89

b212394689.0

12420.2

044+

0.0

019

−0.0

017

5.1

7630+

0.0

0041

−0.0

0043

14.9

+2.3

−5.0

88.1

+1.4

−2.8

0.0

161+

0.0

015

−0.0

009

1.5

1+

0.1

5−

0.1

00.8

62+

0.0

38

−0.0

27

0.9

28+

0.0

24

−0.0

27

12.2

06

<1.0

0e

−04

Pla

net

K2-1

89

c212394689.0

22390.4

181+

0.0

014

−0.0

016

6.6

7934

±0.0

0024

17.0

+2.9

−7.3

88.2

+1.3

−3.3

0.0

264+

0.0

031

−0.0

012

2.4

8+

0.3

2−

0.1

40.8

62+

0.0

38

−0.0

27

0.9

28+

0.0

24

−0.0

27

12.2

06

<1.0

0e

−04

Pla

net

30 Mayo et al.Table

4—

Continued

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

212460519.0

12390.7

941+

0.0

016

−0.0

015

7.3

8707

±0.0

0028

20.3

+2.4

−5.3

88.7

+1.0

−1.6

0.0

280+

0.0

020

−0.0

011

1.8

0+

0.1

4−

0.0

80.5

89+

0.0

16

−0.0

14

0.6

10+

0.0

19

−0.0

18

12.4

45

<1.0

0e

−04

Pla

net

K2-1

90

b212480208.0

12391.7

679

±0.0

026

10.0

9886+

0.0

0062

−0.0

0064

17.2

+2.4

−5.5

88.4

+1.2

−2.3

0.0

136+

0.0

010

−0.0

006

1.3

6+

0.1

8−

0.1

00.9

12+

0.0

96

−0.0

58

0.9

05+

0.0

33

−0.0

36

10.8

92

<1.0

0e

−04

Pla

net

K2-1

90

c212480208.0

22395.6

926+

0.0

065

−0.0

073

21.5

740+

0.0

057

−0.0

043

28.0

+5.0

−10.0

89.0

+0.7

−1.6

0.0

110+

0.0

010

−0.0

006

1.0

9+

0.1

5−

0.0

90.9

12+

0.0

96

−0.0

58

0.9

05+

0.0

33

−0.0

36

10.8

92

<1.0

0e

−04

Pla

net

K2-1

91

b212496592.0

12386.5

570

±0.0

029

2.8

5865+

0.0

0017

−0.0

0018

8.6

+1.2

−2.7

87.1

+2.1

−4.9

0.0

172+

0.0

028

−0.0

013

1.5

8+

0.2

7−

0.1

30.8

40+

0.0

36

−0.0

26

0.9

01+

0.0

26

−0.0

28

12.9

66

<1.0

0e

−04

Pla

net

212521166.0

12386.8

7440+

0.0

0072

−0.0

0068

13.8

6391+

0.0

0022

−0.0

0023

32.3

+2.1

−5.7

89.3

6+

0.4

3−

0.7

50.0

334+

0.0

018

−0.0

007

2.5

2+

0.1

6−

0.1

00.6

92+

0.0

24

−0.0

23

0.7

24+

0.0

25

−0.0

24

11.5

90

<1.0

0e

−04

Pla

net

212534729.0

12390.5

239+

0.0

044

−0.0

056

13.4

850+

0.0

015

−0.0

014

31.6

+4.5

−7.5

89.3

+0.5

−1.0

0.0

170+

0.0

016

−0.0

012

1.5

7+

0.1

9−

0.1

30.8

43+

0.0

64

−0.0

34

0.8

79+

0.0

29

−0.0

32

13.0

66

−Candid

ate

c

K2-1

92

b212555594.0

12387.4

424+

0.0

020

−0.0

021

4.1

6322+

0.0

0021

−0.0

0020

17.4

+2.7

−5.2

88.4

+1.1

−2.1

0.0

174+

0.0

014

−0.0

011

1.5

7+

0.1

5−

0.1

10.8

28+

0.0

42

−0.0

27

0.8

73+

0.0

24

−0.0

31

12.4

82

1.7

1e

−04

Pla

net

212562715.0

12387.4

693+

0.0

028

−0.0

030

13.5

247+

0.0

011

−0.0

009

37.0

+6.0

−11.0

89.3

+0.5

−1.1

0.0

235+

0.0

019

−0.0

013

2.2

8+

0.2

1−

0.1

50.8

88+

0.0

38

−0.0

27

0.9

55+

0.0

22

−0.0

26

13.0

46

4.0

3e

−03

Candid

ate

212577658.0

12388.3

213+

0.0

022

−0.0

023

14.0

6976+

0.0

0072

−0.0

0071

31.0

+5.0

−11.0

89.0

+0.7

−1.4

0.0

192+

0.0

015

−0.0

009

1.8

7+

0.1

8−

0.1

10.8

90+

0.0

52

−0.0

33

0.9

45+

0.0

27

−0.0

31

11.5

41

−Candid

ate

c

K2-1

93

b212580872.0

12391.2

591

±0.0

011

14.7

8721+

0.0

0043

−0.0

0047

25.2

+1.6

−3.5

89.1

9+

0.5

6−

0.7

60.0

385+

0.0

014

−0.0

008

4.0

1+

0.3

4−

0.2

10.9

57+

0.0

74

−0.0

45

0.9

94+

0.0

29

−0.0

27

13.0

47

<1.0

0e

−04

Pla

net

212586030.0

12387.8

833+

0.0

035

−0.0

039

7.7

8523+

0.0

0075

−0.0

0065

9.0

+21.0

−2.0

83.5

+5.9

−4.5

0.0

4+

0.1

8−

0.0

28.0

+36.0

−3.0

1.8

2+

0.2

2−

0.1

51.0

07+

0.0

77

−0.0

43

11.6

89

−Candid

ate

c

212587672.0

12404.0

437+

0.0

037

−0.0

039

23.2

260+

0.0

031

−0.0

032

45.0

+7.0

−16.0

89.4

+0.4

−1.0

0.0

216+

0.0

036

−0.0

018

2.2

4+

0.4

0−

0.2

10.9

53+

0.0

57

−0.0

43

0.9

87+

0.0

34

−0.0

33

12.1

88

1.5

7e

−02

Candid

ate

212639319.0

12389.4

365+

0.0

028

−0.0

029

13.8

4372+

0.0

0095

−0.0

0087

29.0

+33.0

−13.0

88.2

+1.6

−2.9

0.0

4+

0.3

0−

0.0

17.0

+53.0

−2.0

1.6

4+

0.2

6−

0.2

31.0

51+

0.0

97

−0.0

73

12.4

71

9.9

6e

−01

Candid

ate

212645891.0

12385.0

4150

±0.0

0018

0.3

281520

±0.0

000010

1.4

41+

0.0

66

−0.0

48

41.6

+5.4

−4.9

0.1

4+

0.1

1−

0.0

615.0

+12.0

−6.0

0.9

90+

0.0

72

−0.0

40

1.0

33

±0.0

26

12.6

41

−Candid

ate

a

K2-1

94

b212672300.0

12410.0

070

±0.0

043

39.7

214+

0.0

057

−0.0

056

31.0

+4.0

−10.0

89.1

+0.6

−1.3

0.0

261+

0.0

025

−0.0

010

3.6

4+

0.6

2−

0.5

01.2

8+

0.1

8−

0.1

71.1

10+

0.0

46

−0.0

35

12.8

46

<1.0

0e

−04

Pla

net

212686205.0

12388.4

481+

0.0

034

−0.0

032

5.6

7581+

0.0

0041

−0.0

0043

20.5

+2.9

−7.1

88.7

+1.0

−2.2

0.0

170+

0.0

013

−0.0

009

1.2

0+

0.1

0−

0.0

70.6

51+

0.0

21

−0.0

17

0.6

87+

0.0

23

−0.0

22

12.2

56

<1.0

0e

−04

Pla

net

K2-1

95

b212689874.0

12392.0

460+

0.0

017

−0.0

018

15.8

5354+

0.0

0079

−0.0

0075

24.1

+2.0

−6.9

89.0

+0.7

−1.6

0.0

297+

0.0

013

−0.0

007

2.9

4+

0.2

0−

0.1

30.9

06+

0.0

47

−0.0

33

0.9

63+

0.0

28

−0.0

32

12.3

30

<1.0

0e

−04

Pla

net

K2-1

95

c212689874.0

22410.0

089+

0.0

061

−0.0

055

28.4

828+

0.0

064

−0.0

073

28.0

+10.0

−15.0

88.5

+1.1

−2.7

0.0

261+

0.0

024

−0.0

012

2.5

8+

0.2

7−

0.1

50.9

06+

0.0

47

−0.0

33

0.9

63+

0.0

28

−0.0

32

12.3

30

<1.0

0e

−04

Pla

net

K2-1

96

b212691422.0

12394.8

907

±0.0

051

48.3

242+

0.0

085

−0.0

087

23.0

+9.0

−10.0

88.3

+1.4

−2.3

0.0

214+

0.0

017

−0.0

013

3.6

0+

0.6

0−

0.5

01.5

4+

0.2

3−

0.1

91.1

62+

0.0

75

−0.0

45

11.9

23

<1.0

0e

−04

Pla

net

212697709.0

12385.2

8702

±0.0

0010

3.9

516260+

0.0

000080

−0.0

000090

10.2

7+

0.4

3−

0.3

585.0

9+

0.3

0−

0.2

80.0

949+

0.0

033

−0.0

030

10.7

7+

0.9

7−

0.6

61.0

40+

0.0

87

−0.0

54

1.0

68+

0.0

35

−0.0

32

12.1

93

3.4

9e

−04

Pla

net

212703473.0

12389.7

255

±0.0

023

6.7

8908+

0.0

0036

−0.0

0035

16.1

+2.3

−4.9

88.2

+1.3

−2.3

0.0

1507+

0.0

0082

−0.0

0053

1.6

1+

0.1

4−

0.0

90.9

78+

0.0

68

−0.0

39

1.0

20+

0.0

25

−0.0

27

10.7

29

−Candid

ate

c

212703473.0

22388.1

642

±0.0

025

18.5

1732+

0.0

0092

−0.0

0093

43.0

+8.0

−16.0

89.3

+0.5

−1.1

0.0

174+

0.0

012

−0.0

007

1.8

6+

0.1

8−

0.1

10.9

78+

0.0

68

−0.0

39

1.0

20+

0.0

25

−0.0

27

10.7

29

−Candid

ate

c

K2-1

97

b212735333.0

12385.1

830+

0.0

016

−0.0

017

8.3

5795

±0.0

0028

17.0

+1.8

−4.3

88.5

+1.1

−1.9

0.0

252+

0.0

015

−0.0

008

2.5

0+

0.1

9−

0.1

20.9

10+

0.0

42

−0.0

31

0.9

75+

0.0

25

−0.0

29

11.9

77

<1.0

0e

−04

Pla

net

K2-1

98

b212768333.0

12388.6

1179+

0.0

0073

−0.0

0074

17.0

4318+

0.0

0032

−0.0

0031

42.0

+4.1

−8.4

89.4

0+

0.4

1−

0.6

00.0

485+

0.0

023

−0.0

014

4.1

2+

0.2

6−

0.1

70.7

78+

0.0

31

−0.0

24

0.8

36

±0.0

29

11.0

22

2.7

4e

−04

Pla

net

212772313.0

12393.3

740+

0.0

090

−0.0

079

37.3

62+

0.0

15

−0.0

16

20.0

+33.0

−11.0

87.3

+2.4

−5.1

0.0

2+

0.2

4−

0.0

13.0

+30.0

−1.0

1.1

2+

0.1

6−

0.1

30.9

72

±0.0

26

10.4

71

3.2

3e

−02

Candid

ate

K2-1

99

b212779596.0

12385.7

3787+

0.0

0097

−0.0

0093

3.2

25423+

0.0

00067

−0.0

00071

10.7

+1.6

−3.8

87.2

+2.1

−4.2

0.0

259+

0.0

024

−0.0

009

1.8

8+

0.1

9−

0.0

90.6

67+

0.0

20

−0.0

19

0.7

06+

0.0

24

−0.0

23

11.9

30

<1.0

0e

−04

Pla

net

K2-1

99

c212779596.0

22389.9

3002+

0.0

0067

−0.0

0063

7.3

7450+

0.0

0012

−0.0

0013

22.1

+2.0

−4.8

88.9

+0.8

−1.3

0.0

390+

0.0

021

−0.0

011

2.8

4+

0.1

7−

0.1

10.6

67+

0.0

20

−0.0

19

0.7

06+

0.0

24

−0.0

23

11.9

30

<1.0

0e

−04

Pla

net

212803289.0

12400.8

260+

0.0

011

−0.0

012

18.2

4871+

0.0

0063

−0.0

0057

11.4

+1.3

−1.6

87.6

+1.6

−1.4

0.0

424+

0.0

012

−0.0

008

10.5

+1.5

−1.2

2.2

8+

0.3

2−

0.2

61.4

2+

0.1

0−

0.1

111.0

14

−Candid

ate

a

K2-2

00

b212828909.0

12385.5

609

±0.0

029

2.8

4988+

0.0

0019

−0.0

0018

13.2

+2.2

−4.3

88.0

+1.4

−3.2

0.0

158+

0.0

016

−0.0

011

1.3

6+

0.1

4−

0.1

10.7

92+

0.0

24

−0.0

22

0.8

60+

0.0

23

−0.0

27

12.2

44

1.1

1e

−04

Pla

net

213546283.0

12469.3

568

±0.0

015

9.7

7019+

0.0

0031

−0.0

0032

22.9

+2.4

−5.4

88.9

+0.8

−1.3

0.0

294+

0.0

015

−0.0

010

3.1

9+

0.4

2−

0.3

30.9

9+

0.1

2−

0.1

00.9

11

±0.0

35

12.0

31

−Candid

ate

c

213817056.0

12478.9

450+

0.0

048

−0.0

050

13.6

136+

0.0

017

−0.0

016

23.0

±13.0

88.0

+1.5

−4.5

0.0

4+

0.1

3−

0.0

13.0

+11.0

−1.0

0.7

81+

0.0

30

−0.0

22

0.8

17+

0.0

27

−0.0

26

12.9

64

3.6

0e

−01

Candid

ate

214234110.0

12470.8

794

±0.0

015

4.6

3791+

0.0

0016

−0.0

0015

28.8

+5.4

−9.5

89.0

+0.7

−1.4

0.0

174+

0.0

021

−0.0

015

1.8

7+

0.2

7−

0.1

80.9

85+

0.0

77

−0.0

42

1.0

32+

0.0

28

−0.0

31

11.6

24

2.4

7e

−01

Candid

ate

214254518.0

12471.2

170+

0.0

043

−0.0

045

5.0

5903

±0.0

0049

14.4

+2.3

−4.4

88.1

+1.4

−2.7

0.0

153+

0.0

015

−0.0

011

1.0

4+

0.1

0−

0.0

80.6

24+

0.0

19

−0.0

18

0.6

53+

0.0

22

−0.0

21

11.8

74

1.4

7e

−02

Candid

ate

215171927.0

12468.8

706+

0.0

037

−0.0

035

4.1

3571+

0.0

0031

−0.0

0034

13.1

+2.4

−4.7

87.7

+1.7

−3.5

0.0

192+

0.0

018

−0.0

012

1.6

0+

0.1

6−

0.1

10.7

64+

0.0

25

−0.0

18

0.8

11+

0.0

24

−0.0

26

12.6

92

−Candid

ate

b

215171927.0

22473.8

953+

0.0

068

−0.0

072

6.6

312

±0.0

011

17.8

+3.7

−5.8

88.4

+1.1

−2.3

0.0

163+

0.0

016

−0.0

013

1.3

6+

0.1

4−

0.1

10.7

64+

0.0

25

−0.0

18

0.8

11+

0.0

24

−0.0

26

12.6

92

−Candid

ate

b

215502661.0

12473.2

23+

0.0

11

−0.0

10

21.5

216+

0.0

051

−0.0

061

21.0

+15.0

−14.0

87.7

+1.9

−8.5

0.0

2+

0.1

9−

0.0

02.0

+24.0

−1.0

1.1

6+

0.1

7−

0.1

40.9

78+

0.0

29

−0.0

27

12.0

32

9.7

8e

−01

Candid

ate

215854715.0

12477.0

811+

0.0

046

−0.0

055

11.1

237+

0.0

015

−0.0

012

21.1

+2.9

−6.0

88.7

+0.9

−1.7

0.0

192+

0.0

014

−0.0

012

1.7

2+

0.1

4−

0.1

20.8

21+

0.0

29

−0.0

23

0.8

85+

0.0

23

−0.0

28

12.6

11

−Candid

ate

b

K2-2

01

b216008129.0

12468.9

841

±0.0

019

1.0

59790+

0.0

00043

−0.0

00044

4.7

+0.6

−1.1

84.4

+4.1

−6.7

0.0

146+

0.0

013

−0.0

007

1.4

0+

0.1

4−

0.0

80.8

78+

0.0

29

−0.0

21

0.9

56+

0.0

20

−0.0

21

11.9

66

<1.0

0e

−04

Pla

net

K2-2

01

c216008129.0

22486.7

830+

0.0

023

−0.0

022

22.7

799+

0.0

020

−0.0

019

41.0

+6.0

−13.0

89.2

7+

0.5

2−

0.9

20.0

343+

0.0

040

−0.0

017

3.2

9+

0.4

0−

0.1

80.8

78+

0.0

29

−0.0

21

0.9

56+

0.0

20

−0.0

21

11.9

66

2.7

1e

−04

Pla

net

216050437.0

12475.2

4064+

0.0

0083

−0.0

0082

14.9

4897

±0.0

0032

15.8

+1.4

−1.1

85.7

7+

0.8

2−

0.9

10.2

2+

0.2

3−

0.1

137.0

+39.0

−19.0

1.5

2+

0.2

8−

0.1

61.3

81+

0.0

94

−0.0

70

12.3

26

−Candid

ate

a,c

,d

216114172.0

12470.2

127+

0.0

081

−0.0

084

13.1

252+

0.0

022

−0.0

023

22.0

+3.7

−8.4

88.7

+0.9

−2.3

0.0

157+

0.0

026

−0.0

013

1.6

8+

0.2

9−

0.1

50.9

77+

0.0

61

−0.0

39

1.0

29+

0.0

28

−0.0

27

12.6

03

−Candid

ate

b

216166748.0

12470.3

619

±0.0

025

19.6

794+

0.0

011

−0.0

010

29.0

+6.0

−12.0

88.8

+0.9

−1.8

0.0

212+

0.0

036

−0.0

013

2.3

2+

0.4

2−

0.1

81.0

02+

0.0

61

−0.0

46

1.0

50+

0.0

30

−0.0

34

11.8

84

−Candid

ate

b,d

216387101.0

12470.0

120+

0.0

086

−0.0

079

9.7

619+

0.0

018

−0.0

017

12.7

+4.7

−9.0

87.0

+2.0

−15.0

0.0

18+

0.0

79

−0.0

02

3.0

+15.0

−1.0

1.7

7+

0.2

3−

0.2

10.9

90+

0.0

41

−0.0

38

12.8

97

3.0

0e

−02

Candid

ate

K2-2

02

b216405287.0

12471.2

515+

0.0

016

−0.0

017

3.4

0516+

0.0

0013

−0.0

0012

11.9

+1.5

−3.4

87.7

+1.6

−2.9

0.0

232+

0.0

013

−0.0

010

2.3

0+

0.1

8−

0.1

30.9

11+

0.0

51

−0.0

34

0.9

71+

0.0

30

−0.0

28

12.9

97

<1.0

0e

−04

Pla

net

216468514.0

12471.5

2446

±0.0

0013

3.3

13921

±0.0

00010

5.9

3+

0.1

4−

0.1

182.3

6+

0.3

4−

0.2

60.0

827+

0.0

017

−0.0

011

12.0

+1.6

−1.0

1.3

3+

0.1

8−

0.1

01.2

58+

0.0

51

−0.0

46

12.7

49

−Candid

ate

a,c

216494238.0

12474.5

834+

0.0

060

−0.0

056

19.8

946+

0.0

027

−0.0

029

17.5

+1.7

−3.7

88.6

+1.0

−1.5

0.0

479+

0.0

023

−0.0

019

5.5

5+

0.4

5−

0.3

31.0

64+

0.0

69

−0.0

47

1.1

01+

0.0

25

−0.0

28

12.3

02

−Candid

ate

c

217192839.0

12471.8

448+

0.0

041

−0.0

042

7.9

3926

±0.0

0080

29.0

+8.0

−20.0

88.9

+0.8

−5.4

0.0

15+

0.0

13

−0.0

02

1.0

8+

0.9

4−

0.1

30.6

46+

0.0

21

−0.0

19

0.6

78+

0.0

23

−0.0

22

12.6

01

−Candid

ate

c

217192839.0

22471.2

912

±0.0

018

16.0

3505+

0.0

0080

−0.0

0081

31.0

+9.0

−16.0

88.8

+0.9

−2.3

0.0

292+

0.0

081

−0.0

035

2.0

6+

0.5

7−

0.2

50.6

46+

0.0

21

−0.0

19

0.6

78+

0.0

23

−0.0

22

12.6

01

−Candid

ate

c

217192839.0

32474.9

123

±0.0

031

26.8

050

±0.0

024

56.0

+9.0

−18.0

89.4

8+

0.3

8−

0.7

30.0

217+

0.0

039

−0.0

017

1.5

3+

0.2

8−

0.1

30.6

46+

0.0

21

−0.0

19

0.6

78+

0.0

23

−0.0

22

12.6

01

−Candid

ate

c

217855533.0

12487.3

845+

0.0

063

−0.0

060

21.5

873+

0.0

047

−0.0

053

31.3

+4.7

−9.4

89.1

+0.6

−1.2

0.0

1113+

0.0

0095

−0.0

0070

1.7

8+

0.3

2−

0.2

51.4

7+

0.2

3−

0.1

81.2

03+

0.0

89

−0.0

62

10.0

43

1.2

4e

−03

Candid

ate

217941732.0

12470.2

003+

0.0

022

−0.0

021

2.4

9416

±0.0

0012

10.0

+1.5

−2.5

87.6

+1.7

−3.4

0.0

151+

0.0

016

−0.0

012

1.0

6+

0.1

2−

0.0

90.6

44+

0.0

20

−0.0

18

0.6

75

±0.0

21

12.2

83

<1.0

0e

−04

Pla

net

217977895.0

12481.3

702+

0.0

041

−0.0

042

21.6

976+

0.0

023

−0.0

022

26.0

+12.0

−16.0

88.3

+1.4

−4.7

0.0

29+

0.0

64

−0.0

06

2.8

+6.1

−0.6

0.8

82+

0.0

38

−0.0

28

0.9

48+

0.0

25

−0.0

28

12.7

45

4.0

0e

−02

Candid

ate


4—

Continued

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

218131080.0

12468.8

0843

±0.0

0026

3.1

42846

±0.0

00018

4.7

8+

0.2

9−

0.2

183.1

+1.4

−1.0

0.0

626+

0.0

008

−0.0

010

8.8

+1.6

−0.8

1.2

9+

0.2

4−

0.1

21.2

14+

0.0

64

−0.0

49

12.7

00

−Candid

ate

a,c

218170789.0

12470.4

022+

0.0

049

−0.0

051

3.0

4162

±0.0

0032

2.0

1+

0.2

6−

0.1

857.3

+6.2

−6.6

0.0

9+

0.1

6−

0.0

59.0

+15.0

−5.0

0.8

74+

0.0

51

−0.0

49

0.8

58+

0.0

28

−0.0

24

12.8

90

−Candid

ate

a

218304292.0

12473.8

158+

0.0

024

−0.0

023

8.4

2166+

0.0

0038

−0.0

0040

86.0

±29.0

89.6

8+

0.2

2−

0.5

30.0

258+

0.0

050

−0.0

026

3.4

6+

0.8

4−

0.5

31.2

3+

0.1

7−

0.1

40.9

18+

0.0

57

−0.0

43

12.5

11

8.3

2e

−01

Candid

ate

218668602.0

12469.0

913+

0.0

030

−0.0

031

1.8

6598

±0.0

0012

6.3

+1.1

−2.5

85.3

+3.4

−8.6

0.0

207+

0.0

032

−0.0

015

1.8

6+

0.3

0−

0.1

40.8

25+

0.0

27

−0.0

19

0.8

99+

0.0

21

−0.0

23

12.4

11

1.5

7e

−03

Candid

ate

218916923.0

12492.8

1728

±0.0

0036

28.3

8207+

0.0

0028

−0.0

0027

45.8

+2.1

−2.5

89.5

6+

0.2

6−

0.2

00.0

974+

0.0

023

−0.0

020

9.2

7+

0.4

2−

0.3

10.8

72+

0.0

34

−0.0

23

0.9

49+

0.0

24

−0.0

22

11.4

70

−Candid

ate

a,c

219388192.0

12470.9

8880

±0.0

0028

5.2

92605

±0.0

00031

13.3

5+

0.1

9−

0.4

389.3

0+

0.4

9−

0.6

60.0

9434+

0.0

0085

−0.0

0070

9.9

8+

0.9

1−

0.4

70.9

70+

0.0

88

−0.0

45

1.0

04+

0.0

26

−0.0

25

12.3

36

−Candid

ate

a

K2-2

03

b220170303.0

12563.6

388

±0.0

058

9.6

951

±0.0

013

19.0

+3.8

−8.5

88.4

+1.2

−3.3

0.0

165+

0.0

032

−0.0

014

1.3

7+

0.2

8−

0.1

20.7

63+

0.0

30

−0.0

24

0.7

94+

0.0

33

−0.0

28

12.1

14

<1.0

0e

−04

Pla

net

K2-2

04

b220186645.0

12563.5

086+

0.0

037

−0.0

038

7.0

5578+

0.0

0065

−0.0

0064

11.0

+1.3

−3.2

87.6

+1.7

−3.3

0.0

2371+

0.0

0094

−0.0

0082

3.0

5+

0.4

3−

0.3

71.1

8+

0.1

6−

0.1

41.0

09+

0.0

31

−0.0

27

12.9

61

<1.0

0e

−04

Pla

net

220192485.0

12576.2

2330+

0.0

0040

−0.0

0037

50.6

9364+

0.0

0057

−0.0

0055

75.6

+5.0

−3.4

89.4

81+

0.0

82

−0.0

54

0.1

004+

0.0

017

−0.0

025

8.6

8+

0.4

6−

0.3

80.7

93+

0.0

40

−0.0

28

0.8

40+

0.0

27

−0.0

31

11.7

58

−Candid

ate

c

220207765.0

12563.4

263+

0.0

041

−0.0

042

7.1

1986+

0.0

0062

−0.0

0064

27.7

+5.3

−7.5

89.1

+0.7

−1.3

0.0

202+

0.0

021

−0.0

016

1.8

8+

0.2

1−

0.1

60.8

52+

0.0

33

−0.0

23

0.9

27+

0.0

25

−0.0

23

12.1

70

5.2

7e

−03

Candid

ate

K2-2

05

b220211923.0

12580.4

191+

0.0

045

−0.0

061

26.6

723+

0.0

042

−0.0

037

31.0

+4.4

−9.3

89.1

+0.7

−1.2

0.0

170+

0.0

011

−0.0

009

2.0

0+

0.2

7−

0.2

31.0

8+

0.1

3−

0.1

10.9

51+

0.0

38

−0.0

36

12.2

50

<1.0

0e

−04

Pla

net

K2-2

06

b220216730.0

12563.5

766+

0.0

039

−0.0

043

18.2

945+

0.0

017

−0.0

016

28.3

+3.0

−7.6

89.1

+0.6

−1.2

0.0

338+

0.0

023

−0.0

014

2.8

0+

0.2

2−

0.1

50.7

58+

0.0

32

−0.0

27

0.7

89+

0.0

30

−0.0

28

12.8

26

<1.0

0e

−04

Pla

net

K2-2

07

b220218012.0

12570.6

446+

0.0

036

−0.0

039

12.4

875

±0.0

012

21.2

+3.2

−5.9

88.6

+1.0

−1.6

0.0

257+

0.0

026

−0.0

015

2.6

1+

0.3

7−

0.2

10.9

28+

0.0

92

−0.0

51

0.9

42

±0.0

28

12.9

71

1.8

6e

−04

Pla

net

K2-2

08

b220225178.0

12563.5

116+

0.0

025

−0.0

023

4.1

9095+

0.0

0023

−0.0

0025

14.2

+2.1

−4.0

88.0

+1.4

−2.5

0.0

178+

0.0

016

−0.0

012

1.6

8+

0.1

6−

0.1

20.8

62+

0.0

34

−0.0

30

0.9

25

±0.0

30

12.3

02

<1.0

0e

−04

Pla

net

K2-2

09

b220241529.0

12561.2

331+

0.0

027

−0.0

025

2.0

8061

±0.0

0013

8.5

+1.8

−3.5

86.2

+2.7

−6.3

0.0

112+

0.0

013

−0.0

007

0.8

7+

0.1

0−

0.0

60.7

12

±0.0

20

0.7

45+

0.0

26

−0.0

24

10.7

17

<1.0

0e

−04

Pla

net

220245303.0

12563.4

771+

0.0

038

−0.0

036

3.6

8034+

0.0

0036

−0.0

0032

12.9

+2.7

−4.3

87.9

+1.5

−3.3

0.0

126+

0.0

022

−0.0

012

1.0

6+

0.1

9−

0.1

00.7

75+

0.0

23

−0.0

21

0.8

37+

0.0

24

−0.0

28

11.8

21

1.2

2e

−03

Candid

ate

K2-2

10

b220250254.0

12560.9

580

±0.0

021

0.5

70233

±0.0

00028

4.3

+0.8

−1.3

84.1

+4.2

−9.0

0.0

088+

0.0

010

−0.0

007

0.8

2+

0.1

0−

0.0

70.8

52+

0.0

42

−0.0

25

0.9

12+

0.0

23

−0.0

28

11.5

07

2.3

1e

−04

Pla

net

K2-2

11

b220256496.0

12560.8

136+

0.0

021

−0.0

022

0.6

69558

±0.0

00032

3.4

+0.6

−1.1

82.0

+6.0

−13.0

0.0

155+

0.0

018

−0.0

011

1.3

7+

0.1

7−

0.1

00.8

16+

0.0

33

−0.0

19

0.8

82+

0.0

19

−0.0

27

12.8

72

2.1

6e

−04

Pla

net

220292715.0

12574.4

8548

±0.0

0056

41.5

5293+

0.0

0077

−0.0

0087

86.0

+26.0

−23.0

89.5

5±

0.3

20.0

526+

0.0

045

−0.0

033

4.1

6+

0.3

8−

0.2

90.7

24+

0.0

25

−0.0

22

0.7

62+

0.0

26

−0.0

25

12.2

13

1.1

1e

−01

Candid

ate

220294712.0

12580.7

194+

0.0

030

−0.0

027

23.6

079+

0.0

020

−0.0

023

27.7

+3.4

−7.5

89.0

+0.7

−1.2

0.0

256+

0.0

024

−0.0

011

3.1

2+

0.4

0−

0.2

11.1

15+

0.0

98

−0.0

58

1.1

21+

0.0

31

−0.0

30

12.2

64

−Candid

ate

c

220317172.0

12563.1

520

±0.0

028

4.4

3572+

0.0

0031

−0.0

0032

33.0

+7.0

−10.0

89.2

+0.6

−1.2

0.0

143+

0.0

016

−0.0

012

1.3

2+

0.1

6−

0.1

20.8

47+

0.0

36

−0.0

23

0.9

13+

0.0

21

−0.0

26

12.1

07

5.1

1e

−02

Candid

ate

K2-2

12

b220321605.0

12566.6

413

±0.0

011

9.7

9540

±0.0

0029

28.4

+2.5

−7.3

89.2

+0.6

−1.2

0.0

367+

0.0

019

−0.0

011

2.3

9+

0.1

4−

0.0

90.5

98+

0.0

17

−0.0

14

0.6

22+

0.0

20

−0.0

18

12.5

88

<1.0

0e

−04

Pla

net

K2-2

13

b220341183.0

12566.0

026+

0.0

066

−0.0

076

8.1

309

±0.0

018

13.2

+2.6

−5.0

87.9

+1.6

−3.7

0.0

115+

0.0

016

−0.0

010

1.5

1+

0.3

0−

0.2

11.2

0+

0.1

7−

0.1

31.0

70+

0.0

55

−0.0

38

12.0

43

<1.0

0e

−04

Pla

net

K2-2

14

b220376054.0

12563.5

994+

0.0

024

−0.0

028

8.5

9653+

0.0

0059

−0.0

0053

15.6

+2.3

−5.8

88.1

+1.3

−3.1

0.0

181+

0.0

020

−0.0

008

2.2

2+

0.3

8−

0.2

61.1

2+

0.1

5−

0.1

21.0

22+

0.0

31

−0.0

28

11.5

97

3.7

3e

−04

Pla

net

220383386.0

12561.3

7357+

0.0

0097

−0.0

0095

0.9

59665+

0.0

00020

−0.0

00021

4.1

+0.4

−1.0

83.8

+4.4

−8.2

0.0

178+

0.0

016

−0.0

007

1.6

2+

0.1

7−

0.0

80.8

37+

0.0

48

−0.0

27

0.8

90+

0.0

26

−0.0

29

8.9

45

2.9

0e

−04

Pla

net

220383386.0

22561.9

795

±0.0

016

29.8

450

±0.0

014

42.0

+6.0

−11.0

89.3

3+

0.4

9−

0.7

40.0

310+

0.0

029

−0.0

012

2.8

3+

0.3

1−

0.1

40.8

37+

0.0

48

−0.0

27

0.8

90+

0.0

26

−0.0

29

8.9

45

<1.0

0e

−04

Pla

net

220397060.0

12570.2

329

±0.0

011

12.0

9220+

0.0

0038

−0.0

0036

10.2

+0.8

−1.2

87.7

±1.5

0.0

541+

0.0

022

−0.0

013

5.8

+1.5

−0.5

0.9

9+

0.2

4−

0.0

90.8

69+

0.0

25

−0.0

20

12.8

35

−Candid

ate

c,e

220410754.0

12570.2

505+

0.0

073

−0.0

071

19.4

966+

0.0

045

−0.0

055

25.0

+6.0

−11.0

88.9

+0.8

−2.5

0.0

176+

0.0

027

−0.0

015

2.2

2+

0.4

9−

0.3

21.1

6+

0.1

8−

0.1

30.9

93+

0.0

32

−0.0

33

12.8

43

1.0

6e

−03

Candid

ate

K2-2

15

b220471666.0

12561.3

322+

0.0

023

−0.0

024

8.2

6965+

0.0

0047

−0.0

0046

28.1

+4.3

−9.0

89.0

+0.7

−1.4

0.0

200+

0.0

015

−0.0

011

2.1

2+

0.2

6−

0.1

60.9

74+

0.0

95

−0.0

49

1.0

00+

0.0

26

−0.0

27

12.7

98

3.7

6e

−04

Pla

net

K2-2

16

b220481411.0

12561.0

4171+

0.0

0075

−0.0

0081

2.1

74789+

0.0

00039

−0.0

00038

8.7

+0.9

−2.1

87.0

+2.1

−3.5

0.0

231+

0.0

012

−0.0

008

1.6

8+

0.1

0−

0.0

80.6

66+

0.0

22

−0.0

19

0.6

99

±0.0

23

12.1

00

<1.0

0e

−04

Pla

net

K2-2

17

b220487418.0

12562.0

045+

0.0

030

−0.0

029

14.0

7452+

0.0

0099

−0.0

0094

16.1

+2.8

−6.2

88.0

+1.4

−3.0

0.0

246+

0.0

031

−0.0

011

3.5

8+

0.7

0−

0.4

91.3

3+

0.2

0−

0.1

71.1

03+

0.0

46

−0.0

37

12.0

62

3.5

6e

−04

Pla

net

K2-2

18

b220503236.0

12563.4

591

±0.0

019

8.6

7989+

0.0

0042

−0.0

0043

16.0

+1.6

−3.8

88.5

+1.1

−1.8

0.0

234+

0.0

017

−0.0

009

2.5

7+

0.2

8−

0.1

51.0

08+

0.0

80

−0.0

46

1.0

47+

0.0

31

−0.0

28

12.7

13

<1.0

0e

−04

Pla

net

220555384.0

12564.7

712+

0.0

013

−0.0

014

4.2

8452

±0.0

0014

26.1

+3.8

−7.2

89.0

+0.7

−1.4

0.0

192+

0.0

017

−0.0

013

1.3

0+

0.1

2−

0.1

00.6

22+

0.0

20

−0.0

17

0.6

50+

0.0

21

−0.0

20

12.3

95

−Candid

ate

c

K2-2

19

b220592745.0

12563.7

453+

0.0

059

−0.0

065

3.9

0129+

0.0

0066

−0.0

0068

9.0

+1.5

−3.1

86.8

+2.3

−4.8

0.0

1039+

0.0

0072

−0.0

0059

1.3

5+

0.2

0−

0.1

81.1

9+

0.1

6−

0.1

41.0

22+

0.0

34

−0.0

30

11.9

23

<1.0

0e

−04

Pla

net

K2-2

19

c220592745.0

22565.4

157+

0.0

090

−0.0

075

6.6

677+

0.0

013

−0.0

016

10.3

+1.7

−3.9

87.3

+2.0

−4.9

0.0

1109+

0.0

0074

−0.0

0060

1.4

4+

0.2

1−

0.1

91.1

9+

0.1

6−

0.1

41.0

22+

0.0

34

−0.0

30

11.9

23

<1.0

0e

−04

Pla

net

K2-2

19

d220592745.0

32571.5

943+

0.0

023

−0.0

025

11.1

3728+

0.0

0081

−0.0

0079

15.8

+1.9

−4.1

88.3

+1.2

−2.0

0.0

1986+

0.0

0078

−0.0

0060

2.5

8+

0.3

6−

0.3

21.1

9+

0.1

6−

0.1

41.0

22+

0.0

34

−0.0

30

11.9

23

<1.0

0e

−04

Pla

net

K2-2

20

b220621788.0

12568.2

705+

0.0

020

−0.0

022

13.6

8251+

0.0

0072

−0.0

0069

28.0

+5.0

−11.0

88.9

+0.8

−1.9

0.0

218+

0.0

016

−0.0

009

2.2

1+

0.2

7−

0.1

40.9

30+

0.0

89

−0.0

44

0.9

60+

0.0

26

−0.0

29

11.7

52

3.7

8e

−04

Pla

net

220643470.0

12560.8

116

±0.0

015

2.6

53230+

0.0

00084

−0.0

00089

2.8

3+

0.3

7−

0.2

071.0

+2.9

−1.8

0.0

416+

0.0

027

−0.0

021

62.0

+11.0

−8.0

13.7

+2.3

−1.6

0.9

7+

0.2

2−

0.1

310.8

39

−Candid

ate

c,f

220648214.0

12583.6

486

±0.0

034

29.4

352+

0.0

053

−0.0

051

42.0

+6.0

−14.0

89.3

+0.5

−1.0

0.0

223+

0.0

018

−0.0

011

2.9

2+

0.4

8−

0.3

91.2

0+

0.1

7−

0.1

51.0

12+

0.0

33

−0.0

27

12.3

90

6.3

2e

−03

Candid

ate

K2-2

21

b220650439.0

12562.3

558+

0.0

023

−0.0

022

2.3

9909+

0.0

0013

−0.0

0012

6.5

+1.0

−2.0

85.4

+3.2

−5.8

0.0

162+

0.0

014

−0.0

008

1.6

8+

0.1

7−

0.1

00.9

48+

0.0

45

−0.0

29

1.0

11+

0.0

24

−0.0

25

12.2

32

<1.0

0e

−04

Pla

net

220674823.0

12561.0

108

±0.0

012

0.5

71299

±0.0

00015

2.6

5+

0.3

0−

0.6

680.0

+7.0

−13.0

0.0

169+

0.0

014

−0.0

007

1.6

7+

0.1

6−

0.0

90.9

06+

0.0

51

−0.0

29

0.9

67+

0.0

23

−0.0

28

11.9

58

<1.0

0e

−04

Pla

net

220674823.0

22572.7

341+

0.0

029

−0.0

027

13.3

397+

0.0

010

−0.0

011

23.7

+4.5

−9.9

88.6

+1.0

−2.3

0.0

274+

0.0

033

−0.0

014

2.7

0+

0.3

6−

0.1

60.9

06+

0.0

51

−0.0

29

0.9

67+

0.0

23

−0.0

28

11.9

58

<1.0

0e

−04

Pla

net

220679255.0

12567.9

859+

0.0

052

−0.0

051

8.1

332+

0.0

012

−0.0

013

26.0

+6.0

−11.0

88.9

+0.8

−2.1

0.0

174+

0.0

026

−0.0

016

2.0

5+

0.4

0−

0.2

31.0

8+

0.1

3−

0.0

71.0

71+

0.0

27

−0.0

32

11.9

75

2.5

6e

−02

Candid

ate

K2-2

22

b220709978.0

12566.0

599+

0.0

021

−0.0

022

15.3

8883+

0.0

0099

−0.0

0096

23.4

+3.2

−7.7

88.8

+0.9

−1.8

0.0

196+

0.0

018

−0.0

007

2.2

2+

0.3

4−

0.2

21.0

4+

0.1

3−

0.1

00.9

50+

0.0

40

−0.0

36

9.4

43

<1.0

0e

−04

Pla

net

K2-2

23

b228721452.0

12750.0

620

±0.0

031

0.5

05570+

0.0

00037

−0.0

00036

3.4

+0.7

−1.2

82.0

+6.0

−14.0

0.0

0823+

0.0

0077

−0.0

0061

0.9

10+

0.0

99

−0.0

74

1.0

13+

0.0

55

−0.0

35

1.0

67

±0.0

26

11.3

25

<1.0

0e

−04

Pla

net

K2-2

23

c228721452.0

22749.9

734+

0.0

028

−0.0

027

4.5

6417+

0.0

0028

−0.0

0030

10.8

+1.4

−3.6

87.5

+1.8

−3.9

0.0

1465+

0.0

0099

−0.0

0062

1.6

2+

0.1

4−

0.0

91.0

13+

0.0

55

−0.0

35

1.0

67

±0.0

26

11.3

25

<1.0

0e

−04

Pla

net

K2-2

24

b228725972.0

12752.6

741+

0.0

066

−0.0

063

4.4

7859+

0.0

0061

−0.0

0064

12.3

+1.7

−3.3

87.9

+1.5

−2.8

0.0

182+

0.0

025

−0.0

012

1.6

6+

0.2

4−

0.1

30.8

40+

0.0

38

−0.0

30

0.9

02+

0.0

28

−0.0

29

12.4

82

<1.0

0e

−04

Pla

net

228725972.0

22755.4

089+

0.0

023

−0.0

024

10.0

9607+

0.0

0064

−0.0

0062

19.4

+2.1

−4.7

88.7

+0.9

−1.6

0.0

273+

0.0

031

−0.0

015

2.5

1+

0.3

1−

0.1

60.8

40+

0.0

38

−0.0

30

0.9

02+

0.0

28

−0.0

29

12.4

82

−Candid

ate

b,c

228729473.0

12752.7

713+

0.0

039

−0.0

037

16.7

706

±0.0

016

7.8

+0.7

−1.0

86.7

±2.1

0.0

422+

0.0

017

−0.0

010

13.2

+1.8

−1.6

2.8

8+

0.3

8−

0.3

31.0

0+

0.1

1−

0.0

811.5

24

−Candid

ate

a

228732031.0

12749.9

3557+

0.0

0099

−0.0

0098

0.3

693110+

0.0

000080

−0.0

000090

2.3

0+

0.3

7−

0.6

277.0

+9.0

−17.0

0.0

211+

0.0

025

−0.0

014

1.7

6+

0.2

2−

0.1

30.7

65+

0.0

33

−0.0

26

0.8

03+

0.0

28

−0.0

30

11.9

37

<1.0

0e

−04

Pla

net

228734889.0

12800.0

7702

±0.0

0013

48.2

4955+

0.0

0016

−0.0

0017

67.9

6+

0.4

9−

0.4

889.5

54+

0.0

24

−0.0

21

0.1

726+

0.0

020

−0.0

025

18.0

+1.0

−0.7

0.9

56+

0.0

54

−0.0

37

1.0

08+

0.0

27

−0.0

29

12.5

9−

Candid

ate

a,d

K2-2

25

b228734900.0

12754.3

682+

0.0

040

−0.0

049

15.8

715+

0.0

021

−0.0

017

18.0

+2.3

−6.4

88.4

+1.1

−2.5

0.0

202+

0.0

011

−0.0

008

2.6

6+

0.4

6−

0.3

11.2

1+

0.2

0−

0.1

31.1

15+

0.0

54

−0.0

35

11.5

35

<1.0

0e

−04

Pla

net

32 Mayo et al.Table

4—

Continued

New

K2

Nam

eEPIC

T0

(BJD

-2454833)

P(d)

a/R

∗i

(deg)

Rp/R

∗R

p(R

⊕)

R∗

(R

�)

M∗

(M

�)

Kp

FPP

Dispositio

nNotes

228735255.0

12755.2

8503

±0.0

0012

6.5

69213+

0.0

00019

−0.0

00020

15.3

0+

0.0

8−

0.1

989.6

4+

0.2

5−

0.3

80.1

1417+

0.0

0056

−0.0

0043

13.0

+1.8

−1.0

1.0

5+

0.1

4−

0.0

81.0

17+

0.0

36

−0.0

34

12.4

83

−Candid

ate

a,c

K2-2

26

b228736155.0

12751.0

261

±0.0

044

3.2

7111

±0.0

0037

9.2

+1.4

−3.2

86.7

+2.1

−4.7

0.0

165+

0.0

019

−0.0

011

1.4

9+

0.1

8−

0.1

10.8

24+

0.0

34

−0.0

27

0.8

86+

0.0

28

−0.0

30

12.0

42

<1.0

0e

−04

Pla

net

228737155.0

12758.1

57+

0.0

17

−0.0

19

25.9

88+

0.0

12

−0.0

11

2.9

8+

0.3

7−

0.2

467.1

+3.8

−4.2

0.1

8+

0.2

1−

0.1

0317.0

+371.0

−179.0

16.0

+2.0

−1.4

0.8

74+

0.0

90

−0.0

46

11.0

81

−Candid

ate

f

228754001.0

12757.1

696+

0.0

062

−0.0

064

9.1

739+

0.0

015

−0.0

014

8.4

+0.8

−1.7

87.0

+2.1

−2.9

0.0

291+

0.0

015

−0.0

010

6.8

6+

0.8

9−

0.6

92.1

6+

0.2

6−

0.2

00.9

84+

0.0

72

−0.0

39

11.6

51

−Candid

ate

c

K2-2

27

b228760097.0

12759.2

383+

0.0

097

−0.0

094

13.6

218+

0.0

032

−0.0

033

21.0

+6.0

−15.0

88.4

+1.2

−7.3

0.0

17+

0.0

13

−0.0

02

1.7

+1.2

−0.2

0.8

91+

0.0

41

−0.0

31

0.9

51+

0.0

28

−0.0

30

11.5

12

<1.0

0e

−04

Pla

net

K2-2

28

b228798746.0

12750.1

928

±0.0

022

2.6

9837+

0.0

0013

−0.0

0014

11.4

+1.8

−3.6

87.5

+1.8

−3.4

0.0

182+

0.0

012

−0.0

010

1.3

8+

0.1

0−

0.0

90.6

99+

0.0

22

−0.0

20

0.7

42+

0.0

25

−0.0

23

12.6

6<

1.0

0e

−04

Pla

net

K2-2

29

b228801451.0

12749.8

861+

0.0

010

−0.0

011

0.5

84240

±0.0

00014

3.1

6+

0.3

5−

0.8

082.0

+6.0

−11.0

0.0

143+

0.0

015

−0.0

007

1.2

5+

0.1

4−

0.0

70.8

02+

0.0

34

−0.0

23

0.8

58+

0.0

25

−0.0

29

10.9

55

<1.0

0e

−04

Pla

net

K2-2

29

c228801451.0

22753.3

351+

0.0

017

−0.0

016

8.3

2801+

0.0

0040

−0.0

0039

22.0

+6.0

−11.0

88.3

+1.2

−3.1

0.0

248+

0.0

051

−0.0

019

2.1

6+

0.4

6−

0.1

80.8

02+

0.0

34

−0.0

23

0.8

58+

0.0

25

−0.0

29

10.9

55

<1.0

0e

−04

Pla

net

K2-2

30

b228804845.0

12752.4

496+

0.0

047

−0.0

050

2.8

6064+

0.0

0031

−0.0

0029

7.1

+1.2

−2.3

86.0

+2.8

−5.9

0.0

150+

0.0

015

−0.0

010

1.9

3+

0.3

0−

0.2

01.1

8+

0.1

4−

0.0

91.1

31+

0.0

41

−0.0

29

12.5

51

<1.0

0e

−04

Pla

net

228809391.0

12763.8

037+

0.0

041

−0.0

043

19.5

757+

0.0

030

−0.0

027

47.0

+10.0

−18.0

89.3

+0.5

−1.0

0.0

287+

0.0

042

−0.0

021

2.8

4+

0.4

4−

0.2

20.9

07+

0.0

46

−0.0

28

0.9

70+

0.0

22

−0.0

26

12.5

95

1.6

8e

−03

Candid

ate

228952747.0

12750.0

961+

0.0

015

−0.0

016

1.0

55785+

0.0

00040

−0.0

00043

36.0

+29.0

−22.0

89.1

+0.7

−3.6

0.0

24+

0.0

35

−0.0

06

1.5

+2.3

−0.4

0.5

93+

0.0

17

−0.0

15

0.6

15+

0.0

19

−0.0

18

12.2

24

3.5

4e

−01

Candid

ate

229004835.0

12764.6

247+

0.0

025

−0.0

027

16.1

404

±0.0

012

50.0

+7.0

−15.0

89.4

4+

0.4

0−

0.7

20.0

194+

0.0

013

−0.0

010

2.0

6+

0.2

3−

0.1

50.9

75+

0.0

88

−0.0

53

0.9

90+

0.0

34

−0.0

35

10.1

51

1.8

3e

−02

Candid

ate

229039390.0

12749.6

2123

±0.0

0011

0.2

516470

±0.0

000010

1.4

6+

0.2

2−

0.0

838.7

+5.0

−5.5

0.2

6+

0.2

5−

0.1

128.0

+27.0

−12.0

0.9

87+

0.0

88

−0.0

48

1.0

13+

0.0

29

−0.0

31

12.7

35

−Candid

ate

f

229131722.0

12752.7

053

±0.0

064

15.4

824

±0.0

022

26.1

+3.3

−7.0

89.0

+0.7

−1.3

0.0

178+

0.0

021

−0.0

013

2.1

0+

0.3

1−

0.1

91.0

78+

0.0

92

−0.0

53

1.1

00+

0.0

34

−0.0

28

12.5

15

2.5

2e

−03

Candid

ate

229133720.0

12750.9

645

±0.0

011

4.0

3679

±0.0

0011

11.2

+2.3

−4.3

87.0

+2.2

−4.3

0.0

294+

0.0

056

−0.0

023

2.3

4+

0.4

5−

0.1

90.7

28+

0.0

22

−0.0

21

0.7

78+

0.0

26

−0.0

27

11.4

77

−Candid

ate

c

aU

nle

ssth

ere

isa

dee

pse

con

dary

eclip

seor

ellip

soid

al

vari

ati

on

sin

the

light

curv

e,V

ES

PA

can

not

dis

tin

gu

ish

bet

wee

na

pla

net

-siz

edst

ar

an

da

pla

net

.In

this

case

,R

p>

8R⊕

an

dR

Vm

easu

rem

ents

can

not

rule

ou

tth

efo

regro

un

dec

lip

sin

gb

inary

scen

ari

o.

Th

eref

ore

,a

FP

Pvalu

eis

not

rep

ort

ed.

bC

om

pan

ion

inap

ertu

re,

ther

efore

aF

PP

isn

ot

rep

ort

edc

AO

/S

pec

kle

com

pan

ion

,th

eref

ore

aF

PP

isn

ot

rep

ort

edd

Com

posi

tesp

ectr

um

,th

eref

ore

aF

PP

isn

ot

rep

ort

ede

Larg

eR

Vam

plitu

de

vari

ati

on

sco

nfi

rma

bin

ary

inth

esy

stem

,th

eref

ore

aF

PP

isn

ot

rep

ort

edf

VE

SP

Afa

iled

tofi

nd

aF

PP


Table 5Stellar Parameters

EPIC Teff [m/H] log g R∗ (R�) M∗ (M�) Kp Notes

201110617 4460.0± 50.0 −0.33± 0.08 4.68± 0.1 0.616+0.019−0.016 0.642+0.022

−0.019 12.947201111557 4720.0± 50.0 −0.06± 0.08 4.5± 0.1 0.711+0.019

−0.020 0.746± 0.023 11.363201127519 5015.0± 50.0 0.24± 0.08 4.67± 0.1 0.789+0.025

−0.017 0.857+0.021−0.023 11.558

201130233 5456.0± 50.0 0.13± 0.08 4.55± 0.1 0.876+0.045−0.025 0.940+0.023

−0.027 12.604201132684 5489.0± 50.0 0.07± 0.08 4.46± 0.1 0.892+0.074

−0.036 0.933+0.027−0.030 11.678

201166680 6213.0± 50.0 0.14± 0.08 4.32± 0.1 1.22+0.12−0.07 1.192+0.033

−0.030 10.897201211526 5728.0± 50.0 −0.2± 0.08 4.51± 0.1 0.891+0.056

−0.037 0.936+0.032−0.031 11.696

201225286 5419.0± 50.0 −0.1± 0.08 4.57± 0.1 0.830+0.045−0.029 0.886+0.027

−0.032 11.729201227197 5649.0± 50.0 0.07± 0.08 4.61± 0.1 0.914+0.037

−0.026 0.983+0.023−0.025 12.486

201231064 4972.0± 50.0 −0.03± 0.08 3.63± 0.1 2.57+0.31−0.25 0.987+0.082

−0.060 12.358201295312 5722.0± 50.0 0.04± 0.08 4.02± 0.1 1.56+0.26

−0.19 1.050+0.068−0.045 12.126

201299088 5154.0± 50.0 −0.26± 0.08 3.91± 0.1 1.76+0.21−0.17 0.848+0.023

−0.010 11.751201352100 5216.0± 50.0 0.16± 0.08 4.7± 0.1 0.815+0.027

−0.018 0.889+0.019−0.024 12.798

201384232 5617.0± 53.0 −0.12± 0.08 4.67± 0.1 0.863+0.034−0.030 0.930+0.029

−0.030 12.510201390048 4885.0± 50.0 −0.09± 0.08 4.71± 0.1 0.726± 0.020 0.777+0.025

−0.026 11.961201403446 6114.0± 50.0 −0.32± 0.08 4.11± 0.1 1.33+0.16

−0.15 1.015+0.054−0.046 11.995

201427874 4937.0± 50.0 0.14± 0.08 4.71± 0.1 0.762+0.018−0.013 0.826+0.019

−0.023 12.819201437844 6321.0± 50.0 −0.23± 0.08 4.19± 0.1 1.27+0.17

−0.13 1.119+0.055−0.043 9.234 b

201441872 5450.0± 50.0 −0.13± 0.08 4.54± 0.1 0.834+0.050−0.031 0.885+0.029

−0.031 12.088201460826 5791.0± 50.0 −0.23± 0.08 3.81± 0.1 2.20+0.31

−0.25 1.181+0.093−0.061 11.130

201505350 5391.0± 50.0 −0.03± 0.08 4.6± 0.1 0.834+0.036−0.026 0.895+0.026

−0.030 12.806201528828 5185.0± 50.0 −0.05± 0.08 4.46± 0.1 0.804+0.045

−0.029 0.835+0.031−0.030 11.415

201546283 5368.0± 50.0 0.15± 0.08 4.58± 0.1 0.855+0.038−0.025 0.920+0.023

−0.025 12.428201577035 5638.0± 50.0 −0.03± 0.08 4.53± 0.1 0.902+0.054

−0.032 0.958+0.026−0.029 12.296

201595106 5705.0± 50.0 −0.01± 0.08 4.48± 0.1 0.932+0.064−0.038 0.980+0.026

−0.029 11.678201613023 5663.0± 50.0 −0.11± 0.08 4.3± 0.1 1.01+0.12

−0.09 0.936+0.032−0.033 12.137

201615463 5922.0± 57.0 0.05± 0.08 4.24± 0.102 1.20+0.18−0.14 1.073± 0.034 11.964

201713348 4944.0± 50.0 −0.03± 0.08 4.7± 0.1 0.746+0.019−0.021 0.800+0.023

−0.027 11.531201828749 5628.0± 50.0 −0.18± 0.08 4.57± 0.1 0.858+0.045

−0.032 0.915+0.029−0.030 11.564

201855371 4382.0± 50.0 −0.35± 0.08 4.71± 0.1 0.601+0.017−0.015 0.625+0.020

−0.019 12.997201920032 5548.0± 50.0 0.13± 0.08 4.42± 0.1 0.934+0.090

−0.047 0.954± 0.027 12.890202089657 6009.0± 53.0 −0.12± 0.08 4.09± 0.1 1.47± 0.22 1.116+0.057

−0.074 11.600202091388 5586.0± 50.0 0.15± 0.08 4.5± 0.1 0.922+0.062

−0.032 0.976+0.024−0.026 13.500

202675839 5807.0± 50.0 0.45± 0.08 4.25± 0.1 1.23+0.19−0.13 1.141+0.050

−0.039 12.362202821899 6081.0± 50.0 0.46± 0.08 3.88± 0.1 2.22+0.28

−0.30 1.53+0.09−0.10 12.577

202900527 5526.0± 58.0 0.44± 0.08 4.29± 0.1 1.42+0.27−0.21 1.004+0.086

−0.047 12.303203771098 5744.0± 50.0 0.44± 0.08 4.41± 0.1 1.068+0.097

−0.050 1.095+0.028−0.029 11.648

203826436 5382.0± 57.0 −0.07± 0.08 4.66± 0.1 0.818+0.032−0.025 0.887+0.025

−0.031 12.241204750116 5869.0± 53.0 0.02± 0.08 4.53± 0.1 0.987+0.051

−0.039 1.037+0.026−0.030 11.526

205029914 5774.0± 50.0 −0.08± 0.08 4.37± 0.1 0.98+0.11−0.06 0.983+0.029

−0.034 12.183205071984 5415.0± 50.0 0.03± 0.08 4.73± 0.1 0.839+0.026

−0.021 0.916+0.020−0.026 12.005

205904628 5908.0± 50.0 −0.45± 0.08 3.88± 0.1 1.83+0.29−0.28 1.02+0.12

−0.09 8.220 b205944181 5257.0± 50.0 0.03± 0.08 4.49± 0.1 0.825+0.046

−0.026 0.872+0.026−0.033 12.410

205950854 5554.0± 50.0 −0.13± 0.08 4.46± 0.1 0.874+0.068−0.039 0.907+0.029

−0.032 12.105205957328 5317.0± 50.0 0.04± 0.08 4.59± 0.1 0.828+0.033

−0.021 0.892+0.022−0.027 12.464

206007892 5548.0± 50.0 0.26± 0.08 4.56± 0.1 0.919+0.049−0.030 0.986+0.028

−0.026 12.023206008091 5748.0± 50.0 −0.11± 0.08 4.34± 0.1 0.98+0.11

−0.07 0.964± 0.032 12.506206011496 5509.0± 50.0 0.07± 0.08 4.49± 0.1 0.889+0.061

−0.030 0.940+0.025−0.027 10.916

206026904 5134.0± 50.0 0.11± 0.08 4.54± 0.1 0.803+0.034−0.020 0.858+0.022

−0.027 12.150206044803 5761.0± 50.0 0.17± 0.08 4.38± 0.1 1.02+0.11

−0.06 1.030± 0.029 12.975206049764 5250.0± 50.0 −0.09± 0.08 3.95± 0.1 1.72+0.22

−0.19 0.892+0.060−0.027 12.445

206082454 5569.0± 50.0 −0.06± 0.08 4.61± 0.1 0.869+0.038−0.029 0.934+0.026

−0.027 12.308206096602 4636.0± 50.0 −0.29± 0.08 4.7± 0.1 0.648+0.021

−0.018 0.684+0.022−0.023 12.045

206114630 5277.0± 50.0 0.12± 0.08 4.65± 0.1 0.825+0.030−0.019 0.897+0.021

−0.024 11.032206119924 4547.0± 50.0 0.01± 0.08 4.64± 0.1 0.687+0.015

−0.017 0.727+0.020−0.021 10.310

206144956 4799.0± 50.0 −0.34± 0.08 4.55± 0.1 0.669+0.023−0.021 0.702+0.025

−0.023 10.396206146957 5744.0± 50.0 −0.14± 0.08 4.57± 0.1 0.902+0.048

−0.034 0.956+0.031−0.030 11.379

34 Mayo et al.

Table 5 — Continued


206159027 4893.0± 50.0 −0.21± 0.08 4.74± 0.1 0.702± 0.021 0.751+0.025−0.026 12.597

206169375 6060.0± 50.0 −0.08± 0.08 4.19± 0.1 1.26+0.22−0.15 1.096+0.056

−0.047 12.559206181769 5131.0± 50.0 0.06± 0.08 4.53± 0.1 0.799+0.034

−0.021 0.848+0.023−0.028 12.770

206192335 5459.0± 50.0 −0.15± 0.08 4.59± 0.1 0.826+0.039−0.028 0.883+0.029

−0.030 11.870206245553 5844.0± 50.0 0.09± 0.08 4.35± 0.1 1.05+0.13

−0.07 1.043+0.026−0.027 11.745

206268299 5929.0± 60.0 −0.21± 0.08 4.24± 0.11 1.09+0.14−0.11 0.987± 0.040 12.430

206348688 6022.0± 51.0 0.3± 0.08 4.26± 0.1 1.24+0.16−0.11 1.174+0.048

−0.041 12.566206439513 6211.0± 59.0 −0.25± 0.08 3.56± 0.104 3.47+0.48

−0.44 1.62+0.07−0.10 11.437

206535016 5199.0± 50.0 −0.17± 0.08 4.52± 0.1 0.777+0.038−0.028 0.815+0.032

−0.029 11.644210363145 5070.0± 50.0 0.12± 0.08 4.67± 0.1 0.784+0.024

−0.014 0.852+0.019−0.024 11.896

210365511 4672.0± 50.0 −0.1± 0.08 4.63± 0.1 0.692+0.020−0.021 0.730+0.024

−0.023 12.439210402237 5839.0± 51.0 0.2± 0.08 4.41± 0.1 1.038+0.092

−0.050 1.062+0.029−0.026 11.801

210403955 5377.0± 50.0 0.07± 0.08 4.65± 0.1 0.841+0.031−0.022 0.913+0.021

−0.024 12.388210423938 4760.0± 50.0 −0.14± 0.08 4.69± 0.1 0.697+0.021

−0.020 0.741+0.024−0.026 12.655

210512842 5580.0± 70.0 −0.25± 0.08 4.52± 0.12 0.843+0.058−0.039 0.882+0.034

−0.036 12.106 a210558622 4500.0± 50.0 −0.24± 0.08 4.62± 0.1 0.639+0.020

−0.019 0.668+0.022−0.021 12.034

210609658 5016.0± 50.0 0.2± 0.08 3.81± 0.1 2.15+0.26−0.21 1.009+0.081

−0.049 12.587210629082 6148.0± 50.0 0.28± 0.08 4.15± 0.1 1.45+0.25

−0.18 1.256+0.078−0.058 11.580

210643811 5909.0± 50.0 0.05± 0.08 4.11± 0.1 1.42+0.21−0.17 1.095+0.057

−0.039 10.632210667381 5428.0± 50.0 0.15± 0.08 4.63± 0.1 0.864+0.033

−0.020 0.939+0.020−0.025 12.674

210707130 4441.0± 50.0 −0.14± 0.08 4.65± 0.1 0.647+0.020−0.019 0.678+0.021

−0.022 12.099210718708 5129.0± 50.0 −0.35± 0.08 4.52± 0.1 0.722+0.035

−0.025 0.757+0.028−0.029 12.801

210775710 5738.0± 50.0 0.07± 0.08 4.4± 0.1 0.98+0.10−0.05 1.003+0.026

−0.027 11.827210848071 5703.0± 50.0 −0.06± 0.08 4.38± 0.1 0.956+0.099

−0.055 0.964+0.030−0.032 11.040

210857328 6063.0± 50.0 0.41± 0.08 4.38± 0.1 1.214+0.087−0.061 1.211+0.032

−0.038 12.584210894022 5741.0± 50.0 −0.36± 0.08 4.36± 0.1 0.92+0.11

−0.08 0.877+0.036−0.041 12.300

210957318 5574.0± 50.0 0.13± 0.08 4.53± 0.1 0.909+0.054−0.029 0.970+0.024

−0.027 13.171210965800 5525.0± 50.0 0.09± 0.08 4.55± 0.1 0.887+0.044

−0.026 0.951+0.023−0.028 12.134

211048999 5015.0± 50.0 0.03± 0.08 4.63± 0.1 0.768+0.022−0.018 0.824+0.022

−0.027 12.659211089792 5392.0± 50.0 0.13± 0.08 4.59± 0.1 0.858+0.040

−0.024 0.923+0.023−0.026 12.914

211106187 4883.0± 98.0 −1.1± 0.092 2.27± 0.162 13.2+4.6−2.7 1.10+0.47

−0.18 13.124 a211147528 6254.0± 98.0 0.15± 0.092 3.19± 0.161 5.4+0.5

−1.0 2.02+0.05−0.13 11.832 a

211319617 5263.0± 50.0 −0.59± 0.08 4.7± 0.1 0.681+0.021−0.016 0.730+0.020

−0.022 12.393211351816 4836.0± 50.0 0.27± 0.08 3.5± 0.1 2.95+0.37

−0.30 1.054+0.089−0.067 12.409

211355342 5609.0± 50.0 0.42± 0.08 4.46± 0.1 0.999+0.077−0.041 1.044+0.024

−0.029 12.637211359660 5159.0± 50.0 −0.01± 0.08 4.59± 0.1 0.790+0.032

−0.021 0.847+0.024−0.031 11.742

211391664 6095.0± 50.0 −0.1± 0.08 4.09± 0.1 1.51± 0.22 1.156+0.082−0.069 12.102

211401787 6114.0± 50.0 −0.15± 0.08 4.01± 0.1 1.68+0.27−0.23 1.20+0.10

−0.09 9.709211418290 5070.0± 59.0 −0.43± 0.08 3.25± 0.104 3.69+0.54

−0.39 0.915+0.068−0.051 11.504

211424769 6185.0± 50.0 −0.12± 0.08 4.34± 0.1 1.12+0.11−0.07 1.102+0.041

−0.037 9.438 b211491383 6035.0± 50.0 −0.07± 0.08 4.16± 0.1 1.31+0.22

−0.16 1.101+0.053−0.050 11.785

211525389 5475.0± 50.0 0.26± 0.08 4.51± 0.1 0.909+0.058−0.036 0.965+0.031

−0.029 11.687211562654 5482.0± 50.0 0.09± 0.08 4.6± 0.1 0.873+0.037

−0.023 0.942+0.021−0.025 12.754

211594205 5252.0± 50.0 −0.22± 0.08 4.63± 0.1 0.764+0.033−0.025 0.819+0.028

−0.030 10.680211606790 5445.0± 50.0 0.07± 0.08 4.05± 0.1 1.48+0.22

−0.17 0.947+0.073−0.032 12.673

211611158 5722.0± 50.0 −0.05± 0.08 4.58± 0.1 0.914+0.044−0.033 0.976± 0.028 12.414

211682544 5410.0± 50.0 −0.04± 0.08 4.58± 0.1 0.837+0.040−0.027 0.898+0.027

−0.031 11.407211733267 5319.0± 50.0 −0.05± 0.08 4.55± 0.1 0.819+0.040

−0.028 0.872+0.027−0.029 12.150

211736671 5414.0± 53.0 0.48± 0.08 3.75± 0.1 2.31+0.38−0.35 1.29± 0.11 12.160

211743874 5985.0± 50.0 0.08± 0.08 4.14± 0.1 1.41+0.18−0.19 1.128+0.056

−0.040 12.486211763214 5277.0± 50.0 −0.2± 0.08 4.54± 0.1 0.782+0.043

−0.028 0.826+0.030−0.031 12.529

211770696 5656.0± 52.0 −0.28± 0.08 4.23± 0.1 1.06+0.12−0.11 0.872+0.037

−0.035 12.253211800191 5851.0± 70.0 −0.35± 0.08 4.43± 0.12 0.906+0.091

−0.053 0.917+0.036−0.040 12.443 a

211818569 4695.0± 50.0 −0.14± 0.08 4.68± 0.1 0.686+0.020−0.021 0.727+0.025

−0.024 12.935211886472 6398.0± 61.0 0.17± 0.08 4.03± 0.112 1.74+0.32

−0.27 1.39+0.11−0.08 11.126

211906650 5784.0± 50.0 0.06± 0.08 4.45± 0.1 0.981+0.075−0.041 1.019+0.023

−0.027 12.193211913977 4942.0± 53.0 0.14± 0.08 4.66± 0.1 0.770+0.022

−0.015 0.833+0.020−0.024 12.619

211941472 5739.0± 50.0 0.02± 0.08 4.11± 0.1 1.38+0.19−0.16 1.020+0.043

−0.033 11.788




211945201 6046.0± 50.0 0.05± 0.08 4.14± 0.1 1.41+0.21−0.18 1.143+0.059

−0.040 10.115211978988 5759.0± 50.0 −0.03± 0.08 4.31± 0.1 1.04+0.13

−0.09 0.988+0.028−0.030 12.588

211993818 5265.0± 50.0 −0.04± 0.08 3.2± 0.1 4.26+0.68−0.52 1.11+0.13

−0.06 7.218 b212006318 5838.0± 50.0 0.03± 0.08 4.32± 0.1 1.07+0.14

−0.09 1.030+0.027−0.028 12.909

212008766 5098.0± 50.0 −0.15± 0.08 4.7± 0.1 0.748+0.026−0.021 0.805+0.026

−0.027 12.802212012119 4822.0± 50.0 −0.08± 0.08 4.44± 0.1 0.727+0.023

−0.021 0.760+0.028−0.025 11.753

212110888 5990.0± 50.0 −0.01± 0.08 4.11± 0.1 1.45+0.21−0.20 1.120+0.053

−0.044 11.441212132195 4789.0± 50.0 −0.18± 0.08 4.71± 0.1 0.692+0.021

−0.020 0.737+0.025−0.024 11.670

212138198 5182.0± 50.0 0.29± 0.08 4.55± 0.1 0.839+0.038−0.028 0.898+0.027

−0.029 12.902212157262 5477.0± 50.0 0.26± 0.08 4.62± 0.1 0.895+0.041

−0.026 0.967+0.025−0.024 12.864

212164470 5982.0± 50.0 0.16± 0.08 4.36± 0.1 1.11+0.11−0.06 1.107+0.031

−0.025 12.704212303338 5338.0± 50.0 0.19± 0.08 4.51± 0.1 0.863+0.053

−0.030 0.915+0.025−0.029 9.957

212357477 5733.0± 50.0 0.04± 0.08 4.51± 0.1 0.947+0.058−0.033 1.000+0.024

−0.028 10.215212394689 5503.0± 50.0 −0.01± 0.08 4.61± 0.1 0.862+0.038

−0.027 0.928+0.024−0.027 12.206

212460519 4396.0± 50.0 −0.44± 0.08 4.73± 0.1 0.589+0.016−0.014 0.610+0.019

−0.018 12.445212480208 5631.0± 50.0 −0.19± 0.08 4.38± 0.1 0.912+0.096

−0.058 0.905+0.033−0.036 10.892

212496592 5176.0± 50.0 0.31± 0.08 4.57± 0.1 0.840+0.036−0.026 0.901+0.026

−0.028 12.966212521166 4877.0± 50.0 −0.3± 0.08 4.51± 0.1 0.692+0.024

−0.023 0.724+0.025−0.024 11.590

212534729 5378.0± 50.0 −0.06± 0.08 4.47± 0.1 0.843+0.064−0.034 0.879+0.029

−0.032 13.066212555594 5252.0± 50.0 0.05± 0.08 4.49± 0.1 0.828+0.042

−0.027 0.873+0.024−0.031 12.482

212562715 5570.0± 50.0 0.04± 0.08 4.59± 0.1 0.888+0.038−0.027 0.955+0.022

−0.026 13.046212577658 5343.0± 50.0 0.33± 0.08 4.51± 0.1 0.890+0.052

−0.033 0.945+0.027−0.031 11.541

212580872 5623.0± 50.0 0.21± 0.08 4.46± 0.1 0.957+0.074−0.045 0.994+0.029

−0.027 13.047212586030 5084.0± 50.0 0.36± 0.08 3.95± 0.1 1.82+0.22

−0.15 1.007+0.077−0.043 11.689

212587672 5928.0± 50.0 −0.21± 0.08 4.49± 0.1 0.953+0.057−0.043 0.987+0.034

−0.033 12.188212639319 5465.0± 50.0 0.29± 0.08 3.98± 0.1 1.64+0.26

−0.23 1.051+0.097−0.073 12.471

212645891 5759.0± 50.0 0.18± 0.08 4.46± 0.1 0.990+0.072−0.040 1.033± 0.026 12.641

212672300 5979.0± 52.0 0.1± 0.08 4.21± 0.1 1.28+0.18−0.17 1.110+0.046

−0.035 12.846212686205 4621.0± 50.0 −0.26± 0.08 4.7± 0.1 0.651+0.021

−0.017 0.687+0.023−0.022 12.256

212689874 5712.0± 50.0 −0.09± 0.08 4.55± 0.1 0.906+0.047−0.033 0.963+0.028

−0.032 12.330212691422 6045.0± 50.0 0.01± 0.08 4.08± 0.1 1.54+0.23

−0.19 1.162+0.075−0.045 11.923

212697709 5773.0± 50.0 0.31± 0.08 4.43± 0.1 1.040+0.087−0.054 1.068+0.035

−0.032 12.193212703473 5758.0± 50.0 0.11± 0.08 4.46± 0.1 0.978+0.068

−0.039 1.020+0.025−0.027 10.729

212735333 5675.0± 50.0 −0.01± 0.08 4.58± 0.1 0.910+0.042−0.031 0.975+0.025

−0.029 11.977212768333 5262.0± 50.0 −0.16± 0.08 4.63± 0.1 0.778+0.031

−0.024 0.836± 0.029 11.022212772313 5675.0± 50.0 0.03± 0.08 4.25± 0.1 1.12+0.16

−0.13 0.972± 0.026 10.471212779596 4681.0± 50.0 −0.23± 0.08 4.69± 0.1 0.667+0.020

−0.019 0.706+0.024−0.023 11.930

212803289 6033.0± 50.0 0.15± 0.08 3.78± 0.1 2.28+0.32−0.26 1.42+0.10

−0.11 11.014212828909 5233.0± 50.0 −0.04± 0.08 4.71± 0.1 0.792+0.024

−0.022 0.860+0.023−0.027 12.244

213546283 5631.0± 50.0 −0.15± 0.08 4.29± 0.1 0.99+0.12−0.10 0.911± 0.035 12.031

213817056 4863.0± 50.0 0.27± 0.08 4.38± 0.1 0.781+0.030−0.022 0.817+0.027

−0.026 12.964214234110 5608.0± 50.0 0.37± 0.08 4.46± 0.1 0.985+0.077

−0.042 1.032+0.028−0.031 11.624

214254518 4455.0± 50.0 −0.28± 0.08 4.68± 0.1 0.624+0.019−0.018 0.653+0.022

−0.021 11.874215171927 4972.0± 50.0 0.02± 0.08 4.52± 0.1 0.764+0.025

−0.018 0.811+0.024−0.026 12.692

215502661 5694.0± 50.0 −0.0± 0.08 4.22± 0.1 1.16+0.17−0.14 0.978+0.029

−0.027 12.032215854715 5310.0± 50.0 0.01± 0.08 4.63± 0.1 0.821+0.029

−0.023 0.885+0.023−0.028 12.611

216008129 5507.0± 50.0 0.13± 0.08 4.68± 0.1 0.878+0.029−0.021 0.956+0.020

−0.021 11.966216050437 6391.0± 101.0 0.45± 0.095 4.18± 0.166 1.52+0.28

−0.16 1.381+0.094−0.070 12.326 a

216114172 5742.0± 56.0 0.19± 0.08 4.5± 0.1 0.977+0.061−0.039 1.029+0.028

−0.027 12.603216166748 5679.0± 50.0 0.35± 0.08 4.49± 0.1 1.002+0.061

−0.046 1.050+0.030−0.034 11.884

216387101 5529.0± 50.0 −0.22± 0.08 3.91± 0.1 1.77+0.23−0.21 0.990+0.041

−0.038 12.897216405287 5491.0± 58.0 0.27± 0.08 4.55± 0.102 0.911+0.051

−0.034 0.971+0.030−0.028 12.997

216468514 6178.0± 50.0 0.35± 0.08 4.24± 0.1 1.33+0.18−0.10 1.258+0.051

−0.046 12.749216494238 5767.0± 50.0 0.44± 0.08 4.47± 0.1 1.064+0.069

−0.047 1.101+0.025−0.028 12.302

217192839 4661.0± 50.0 −0.33± 0.08 4.66± 0.1 0.646+0.021−0.019 0.678+0.023

−0.022 12.601217855533 6244.0± 50.0 −0.06± 0.08 4.11± 0.1 1.47+0.23

−0.18 1.203+0.089−0.062 10.043

217941732 4528.0± 50.0 −0.24± 0.08 4.62± 0.1 0.644+0.020−0.018 0.675± 0.021 12.283

217977895 5570.0± 50.0 0.0± 0.08 4.61± 0.1 0.882+0.038−0.028 0.948+0.025

−0.028 12.745

36 Mayo et al.



218131080 6235.0± 82.0 0.14± 0.08 4.22± 0.137 1.29+0.24−0.12 1.214+0.064

−0.049 12.700 a218170789 5250.0± 50.0 0.07± 0.08 4.31± 0.1 0.874+0.051

−0.049 0.858+0.028−0.024 12.890

218304292 5779.0± 51.0 −0.29± 0.08 4.13± 0.1 1.23+0.17−0.14 0.918+0.057

−0.043 12.511218668602 5231.0± 50.0 0.21± 0.08 4.68± 0.1 0.825+0.027

−0.019 0.899+0.021−0.023 12.411

218916923 5425.0± 50.0 0.23± 0.08 4.66± 0.1 0.872+0.034−0.023 0.949+0.024

−0.022 11.470219388192 5689.0± 50.0 0.16± 0.08 4.43± 0.1 0.970+0.088

−0.045 1.004+0.026−0.025 12.336

220170303 5000.0± 50.0 −0.07± 0.08 4.43± 0.1 0.763+0.030−0.024 0.794+0.033

−0.028 12.114220186645 5755.0± 50.0 0.07± 0.08 4.23± 0.1 1.18+0.16

−0.14 1.009+0.031−0.027 12.961

220192485 5220.0± 50.0 −0.1± 0.08 4.54± 0.1 0.793+0.040−0.028 0.840+0.027

−0.031 11.758220207765 5318.0± 50.0 0.26± 0.08 4.68± 0.1 0.852+0.033

−0.023 0.927+0.025−0.023 12.170

220211923 5890.0± 50.0 −0.26± 0.08 4.25± 0.1 1.08+0.13−0.11 0.951+0.038

−0.036 12.250220216730 5043.0± 50.0 −0.14± 0.08 4.46± 0.1 0.758+0.032

−0.027 0.789+0.030−0.028 12.826

220218012 5522.0± 50.0 0.11± 0.08 4.41± 0.1 0.928+0.092−0.051 0.942± 0.028 12.971

220225178 5582.0± 50.0 −0.11± 0.08 4.62± 0.1 0.862+0.034−0.030 0.925± 0.030 12.302

220241529 4720.0± 50.0 −0.06± 0.08 4.46± 0.1 0.712± 0.020 0.745+0.026−0.024 10.717

220245303 5121.0± 50.0 −0.03± 0.08 4.69± 0.1 0.775+0.023−0.021 0.837+0.024

−0.028 11.821220250254 5396.0± 50.0 0.05± 0.08 4.55± 0.1 0.852+0.042

−0.025 0.912+0.023−0.028 11.507

220256496 5221.0± 50.0 0.11± 0.08 4.6± 0.1 0.816+0.033−0.019 0.882+0.019

−0.027 12.872220292715 4895.0± 50.0 −0.15± 0.08 4.52± 0.1 0.724+0.025

−0.022 0.762+0.026−0.025 12.213

220294712 6057.0± 58.0 0.1± 0.08 4.38± 0.103 1.115+0.098−0.058 1.120+0.031

−0.030 12.264220317172 5374.0± 50.0 0.09± 0.08 4.59± 0.1 0.847+0.036

−0.023 0.913+0.021−0.026 12.107

220321605 4349.0± 50.0 −0.33± 0.08 4.72± 0.1 0.598+0.017−0.014 0.622+0.020

−0.018 12.588220341183 5794.0± 50.0 0.25± 0.08 4.25± 0.1 1.20+0.17

−0.13 1.070+0.055−0.038 12.043

220376054 5768.0± 50.0 0.12± 0.08 4.27± 0.1 1.12+0.15−0.12 1.022+0.031

−0.028 11.597220383386 5366.0± 50.0 −0.01± 0.08 4.54± 0.1 0.837+0.048

−0.027 0.890+0.026−0.029 8.945

220397060 5333.0± 51.0 0.05± 0.08 4.2± 0.101 0.99+0.24−0.09 0.869+0.025

−0.020 12.835220410754 5758.0± 50.0 −0.05± 0.08 4.22± 0.1 1.16+0.18

−0.13 0.993+0.032−0.033 12.843

220471666 5704.0± 50.0 0.11± 0.08 4.41± 0.1 0.974+0.095−0.049 1.000+0.026

−0.027 12.798220481411 4591.0± 50.0 −0.18± 0.08 4.59± 0.1 0.666+0.022

−0.019 0.699± 0.023 12.100220487418 5967.0± 50.0 0.04± 0.08 4.17± 0.1 1.33+0.20

−0.17 1.103+0.046−0.037 12.062

220503236 5757.0± 50.0 0.25± 0.08 4.45± 0.1 1.008+0.080−0.046 1.047+0.031

−0.028 12.713220555384 4360.0± 50.0 −0.2± 0.08 4.69± 0.1 0.622+0.020

−0.017 0.650+0.021−0.020 12.395

220592745 5753.0± 50.0 0.13± 0.08 4.23± 0.1 1.19+0.16−0.14 1.022+0.034

−0.030 11.923220621788 5599.0± 50.0 0.06± 0.08 4.43± 0.1 0.930+0.089

−0.044 0.960+0.026−0.029 11.752

220643470 4621.0± 50.0 −0.78± 0.08 2.17± 0.1 13.7+2.3−1.6 0.97+0.22

−0.13 10.839220648214 5785.0± 50.0 0.01± 0.08 4.21± 0.1 1.20+0.17

−0.15 1.012+0.033−0.027 12.390

220650439 5716.0± 50.0 0.13± 0.08 4.57± 0.1 0.948+0.045−0.029 1.011+0.024

−0.025 12.232220674823 5590.0± 50.0 0.08± 0.08 4.54± 0.1 0.906+0.051

−0.029 0.967+0.023−0.028 11.958

220679255 5966.0± 50.0 0.01± 0.08 4.33± 0.1 1.08+0.13−0.07 1.071+0.027

−0.032 11.975220709978 5934.0± 50.0 −0.3± 0.08 4.29± 0.1 1.04+0.13

−0.10 0.950+0.040−0.036 9.443

228721452 5859.0± 50.0 0.19± 0.08 4.54± 0.1 1.013+0.055−0.035 1.067± 0.026 11.325

228725972 5614.0± 50.0 −0.22± 0.08 4.63± 0.1 0.840+0.038−0.030 0.902+0.028

−0.029 12.482228729473 4939.0± 50.0 −0.04± 0.08 3.54± 0.1 2.88+0.38

−0.33 1.00+0.11−0.08 11.524

228732031 5113.0± 50.0 −0.15± 0.08 4.5± 0.1 0.765+0.033−0.026 0.803+0.028

−0.030 11.937228734889 5792.0± 50.0 0.0± 0.08 4.52± 0.1 0.956+0.054

−0.037 1.008+0.027−0.029 12.59

228734900 5733.0± 50.0 0.47± 0.08 4.26± 0.1 1.21+0.20−0.13 1.115+0.054

−0.035 11.535228735255 5637.0± 50.0 0.29± 0.08 4.33± 0.1 1.05+0.14

−0.08 1.017+0.036−0.034 12.483

228736155 5397.0± 50.0 −0.08± 0.08 4.62± 0.1 0.824+0.034−0.027 0.886+0.028

−0.030 12.042228737155 4382.0± 50.0 −0.72± 0.08 2.07± 0.1 16.0+2.0

−1.4 0.874+0.090−0.046 11.081

228754001 5035.0± 50.0 0.07± 0.08 3.8± 0.1 2.16+0.26−0.20 0.984+0.072

−0.039 11.651228760097 5673.0± 50.0 −0.1± 0.08 4.58± 0.1 0.891+0.041

−0.031 0.951+0.028−0.030 11.512

228798746 4764.0± 50.0 −0.13± 0.08 4.67± 0.1 0.699+0.022−0.020 0.742+0.025

−0.023 12.66228801451 5231.0± 50.0 −0.03± 0.08 4.59± 0.1 0.802+0.034

−0.023 0.858+0.025−0.029 10.955

228804845 6002.0± 50.0 0.21± 0.08 4.29± 0.1 1.18+0.14−0.09 1.131+0.041

−0.029 12.551228809391 5611.0± 50.0 0.06± 0.08 4.55± 0.1 0.907+0.046

−0.028 0.970+0.022−0.026 12.595

228952747 4315.0± 50.0 −0.33± 0.08 4.73± 0.1 0.593+0.017−0.015 0.615+0.019

−0.018 12.224229004835 5870.0± 50.0 −0.15± 0.08 4.4± 0.1 0.975+0.088

−0.053 0.990+0.034−0.035 10.151

229039390 5833.0± 50.0 −0.04± 0.08 4.41± 0.1 0.987+0.088−0.048 1.013+0.029

−0.031 12.735




229131722 5928.0± 50.0 0.23± 0.08 4.42± 0.1 1.078+0.092−0.053 1.100+0.034

−0.028 12.515229133720 4933.0± 50.0 −0.12± 0.08 4.65± 0.1 0.728+0.022

−0.021 0.778+0.026−0.027 11.477

a Stellar parameters for this star are derived from a single spectrum with a cross correlation function peak height < 0.9 (but> 0.8). We have decided the resulting stellar parameters are trustworthy for this analysis, but provide a note for the reader’sdiscretion.b SHK values have been determined for this star and can be found in Table 3.

38 Mayo et al.Table

6D

etailed

FPP

Table

New

K2

Nam

eE

PIC

Sec

on

dary

Ecl

ipse

Th

resh

old

(pp

m)

Ap

ertu

reR

ad

ius

(arc

sec)

AO

/S

pec

kle

P(E

clip

sin

gB

inary

)

P(E

clip

sin

gB

inary

)(x

2P

er.)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)(x

2P

er.)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)(x

2P

er.)

RV

Mass

Lim

it

VE

SP

AF

PP

Mu

lti-

plici

tyB

oost

Ad

op

ted

FP

PD

isp

osi

tion

K2-1

56

b201110617.0

128

14.7

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y2.1

8e

−08

-<

1e

−04

Pla

net

201111557.0

147

14.4

Y<

1e

−04

1.1

6e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

2e

−03

-1.2

2e

−03

Candid

ate

201127519.0

1813

17.9

Y-

--

--

-Y

--

-Candid

ate

K2-1

57

b201130233.0

15

12.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.8

1e

−08

-<

1e

−04

Pla

net

K2-1

58

b201132684.0

195

19.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.6

2e

−06

-<

1e

−04

Pla

net

201166680.0

164

17.9

Y1.7

0e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.7

3e

−03

-1.7

3e

−03

Candid

ate

201211526.0

140

17.3

Y<

1e

−04

2.0

3e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.1

0e

−03

-2.1

0e

−03

Candid

ate

K2-1

59

b201225286.0

185

19.9

Y<

1e

−04

3.4

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.5

3e

−04

-3.5

3e

−04

Pla

net

K2-1

60

b201227197.0

153

14.7

Y6.7

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N7.5

4e

−04

-7.5

4e

−04

Pla

net

K2-1

61

b201231064.0

188

16.3

Y<

1e

−04

7.9

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N7.9

7e

−04

-7.9

7e

−04

Pla

net

201295312.0

127

14.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

9e

−09

-<

1e

−04

Pla

net

201299088.0

177

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

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N6.1

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--

Candid

ate

201352100.0

195

15.0

Y-

--

--

-N

--

-Candid

ate

201384232.0

195

20.5

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

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N2.5

0e

−05

-<

1e

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Pla

net

K2-1

62

b201390048.0

1105

17.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.4

6e

−06

-<

1e

−04

Pla

net

201403446.0

147

16.3

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y2.3

8e

−06

-<

1e

−04

Pla

net

K2-1

63

b201427874.0

192

17.7

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.5

2e

−09

-<

1e

−04

Pla

net

201437844.0

1421

22.3

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y−

1.3

2e

−04

25

<1e

−04

Pla

net

201437844.0

2846

22.3

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y−

2.7

6e

−04

25

<1e

−04

Pla

net

201441872.0

121

18.8

N-

--

--

-N

--

-Candid

ate

K2-1

64

b201460826.0

140

17.3

N<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.7

6e

−06

-<

1e

−04

Pla

net

201505350.0

183

16.6

Y<

1e

−04

1.1

4e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.1

7e

−04

50

<1e

−04

Pla

net

201505350.0

263

16.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.5

4e

−07

50

<1e

−04

Pla

net

201505350.0

336

16.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.1

1e

−16

50

<1e

−04

Pla

net

K2-1

65

b201528828.0

148

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.5

7e

−06

50

<1e

−04

Pla

net

K2-1

65

c201528828.0

267

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.0

9e

−07

50

<1e

−04

Pla

net

K2-1

65

d201528828.0

3146

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.7

8e

−05

50

<1e

−04

Pla

net

201546283.0

137

15.8

Y-

--

--

-N

--

-Candid

ate

201577035.0

163

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.6

2e

−05

-<

1e

−04

Pla

net

201595106.0

126

21.6

Y2.9

4e

−04

1.1

9e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.5

5e

−03

-1.5

5e

−03

Candid

ate

201613023.0

142

19.0

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.5

4e

−08

-<

1e

−04

Pla

net

K2-1

66

b201615463.0

135

20.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.9

2e

−07

-<

1e

−04

Pla

net

201713348.0

1129

17.1

Y1.5

5e

−01

1.2

1e

−02

<1e

−04

<1e

−04

7.3

2e

−03

1.0

5e

−03

N1.7

5e

−01

25

7.0

0e

−03

Candid

ate

201713348.0

228

17.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.5

8e

−05

25

<1e

−04

Pla

net

201828749.0

183

18.2

Y-

--

--

-N

--

-Candid

ate

201855371.0

1160

22.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

8e

−06

-<

1e

−04

Pla

net

201920032.0

1200

17.9

Y7.7

8e

−03

1.6

6e

−03

<1e

−04

2.7

7e

−04

<1e

−04

<1e

−04

N9.7

3e

−03

-9.7

3e

−03

Candid

ate

202089657.0

181

19.0

Y-

--

--

-Y

--

-Candid

ate

202091388.0

1179

16.3

Y-

--

--

-N

--

-Candid

ate

202675839.0

1291

18.2

Y5.8

2e

−01

1.8

3e

−01

<1e

−04

<1e

−04

2.7

6e

−02

1.1

5e

−02

N8.0

3e

−01

--

Candid

ate

202821899.0

1184

21.1

N-

--

--

-Y

--

-Candid

ate

202900527.0

1251

18.2

Y-

--

--

-N

--

-Candid

ate

203771098.0

1109

16.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

3e

−07

25

<1e

−04

Pla

net

203771098.0

262

16.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.1

8e

−05

25

<1e

−04

Pla

net

203826436.0

172

15.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

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N4.7

3e

−07

50

<1e

−04

Pla

net

203826436.0

2110

15.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.4

4e

−05

50

<1e

−04

Pla

net

203826436.0

364

15.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

8e

−08

50

<1e

−04

Pla

net

204750116.0

182

19.9

N-

--

--

-N

--

-Candid

ate

205029914.0

130

16.8

Y-

--

--

-N

--

-Candid

ate

205071984.0

1107

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

2e

−16

50

<1e

−04

Pla

net

205071984.0

2186

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

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N2.2

4e

−09

50

<1e

−04

Pla

net

205071984.0

3153

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.0

4e

−09

50

<1e

−04

Pla

net

K2-1

67

b205904628.0

124

22.6

Y0.0

0e

+00

0.0

0e

+00

9.7

2e

−04

<1e

−04

<1e

−04

<1e

−04

Y8.6

4e

−04

-8.6

4e

−04

Pla

net

205944181.0

142

18.2

Y8.0

1e

−01

1.3

3e

−01

<1e

−04

<1e

−04

1.1

6e

−02

3.3

9e

−03

N9.4

9e

−01

-9.4

9e

−01

Candid

ate

K2-1

68

b205950854.0

178

18.2

N<

1e

−04

<1e

−04

7.0

6e

−04

<1e

−04

<1e

−04

<1e

−04

N7.1

0e

−04

-7.1

0e

−04

Pla

net

205957328.0

194

16.3

N<

1e

−04

<1e

−04

3.0

5e

−03

8.4

6e

−04

<1e

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<1e

−04

N3.9

7e

−03

-3.9

7e

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Candid

ate

K2-1

69

b206007892.0

130

15.3

N<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.9

5e

−05

-<

1e

−04

Pla

net

K2-1

70

c206008091.0

152

13.8

N<

1e

−04

<1e

−04

3.2

6e

−04

<1e

−04

<1e

−04

<1e

−04

N3.3

6e

−04

25

<1e

−04

Pla

net

K2-1

70

b206008091.0

245

13.8

N<

1e

−04

<1e

−04

1.0

1e

−03

3.3

2e

−04

<1e

−04

<1e

−04

N1.3

5e

−03

25

<1e

−04

Pla

net

206011496.0

121

19.7

Y-

--

--

-N

--

-Candid

ate

206026904.0

148

15.3

Y1.0

8e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.0

9e

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50

<1e

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Pla

net

206026904.0

225

15.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

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<1e

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<1e

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N3.4

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50

<1e

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Pla

net

206026904.0

3121

15.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

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<1e

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N3.4

6e

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50

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Pla

net

206044803.0

128

13.8

N<

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1.6

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-2.1

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Pla

net

K2-1

71

b206049764.0

133

16.1

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<1e

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N5.3

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1e

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Pla

net

K2-1

72

c206082454.0

187

13.8

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1e

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<1e

−04

<1e

−04

<1e

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<1e

−04

<1e

−04

N4.8

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25

<1e

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Pla

net

K2-1

72

b206082454.0

258

13.8

N<

1e

−04

<1e

−04

1.4

0e

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1.2

3e

−04

<1e

−04

<1e

−04

N1.5

2e

−03

25

<1e

−04

Pla

net

206096602.0

141

16.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.7

7e

−05

25

<1e

−04

Pla

net

206096602.0

283

16.6

Y5.4

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.4

1e

−04

25

<1e

−04

Pla

net

206114630.0

165

21.3

N4.1

1e

−01

4.3

4e

−02

2.3

1e

−01

1.9

6e

−01

1.0

3e

−01

7.7

1e

−03

N9.9

1e

−01

-9.9

1e

−01

Candid

ate

206119924.0

129

18.8

N-

--

--

-N

--

-Candid

ate

206144956.0

128

18.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

4e

−06

-<

1e

−04

Pla

net

206146957.0

137

21.3

N<

1e

−04

<1e

−04

4.8

4e

−03

3.7

1e

−04

<1e

−04

<1e

−04

N5.2

2e

−03

-5.2

2e

−03

Candid

ate


6—

Continued

New

K2

Nam

eE

PIC

Sec

on

dary

Ecl

ipse

Th

resh

old

(pp

m)

Ap

ertu

reR

ad

ius

(arc

sec)

AO

/S

pec

kle

P(E

clip

sin

gB

inary

)

P(E

clip

sin

gB

inary

)(x

2P

er.)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)(x

2P

er.)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)(x

2P

er.)

RV

Mass

Lim

it

VE

SP

AF

PP

Mu

lti-

plici

tyB

oost

Ad

op

ted

FP

PD

isp

osi

tion

206159027.0

149

14.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.8

1e

−09

-<

1e

−04

Pla

net

206169375.0

18

21.1

N0.0

0e

+00

0.0

0e

+00

1.3

9e

−04

9.2

4e

−01

<1e

−04

1.0

4e

−03

Y9.2

5e

−01

-9.2

5e

−01

Candid

ate

206181769.0

157

14.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.6

6e

−05

-<

1e

−04

Pla

net

206192335.0

147

16.3

Y-

--

--

-N

--

-Candid

ate

206245553.0

126

15.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.5

8e

−06

-<

1e

−04

Pla

net

206268299.0

149

16.3

Y4.0

4e

−04

1.1

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.1

7e

−04

-5.1

7e

−04

Pla

net

206348688.0

149

16.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.0

6e

−10

25

<1e

−04

Pla

net

206348688.0

265

16.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.3

0e

−04

25

<1e

−04

Pla

net

206439513.0

111

18.2

Y<

1e

−04

1.3

7e

−03

<1e

−04

9.9

9e

−01

<1e

−04

<1e

−04

N1.0

0e

+00

--

Candid

ate

206535016.0

1118

21.1

N1.0

6e

−01

6.7

9e

−03

4.8

4e

−02

2.7

3e

−02

3.1

8e

−03

4.6

4e

−04

N1.9

2e

−01

-1.9

2e

−01

Candid

ate

210363145.0

177

20.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.2

9e

−10

-<

1e

−04

Pla

net

210365511.0

156

18.2

N<

1e

−04

<1e

−04

<1e

−04

1.0

0e

+00

<1e

−04

<1e

−04

N1.0

0e

+00

--

Candid

ate

210402237.0

152

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N7.8

3e

−13

-<

1e

−04

Pla

net

210403955.0

173

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.2

2e

−07

50

<1e

−04

Pla

net

210403955.0

239

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.0

9e

−07

50

<1e

−04

Pla

net

K2-8

0d

210403955.0

390

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.6

3e

−05

50

<1e

−04

Pla

net

210423938.0

1184

16.6

N0.0

0e

+00

0.0

0e

+00

7.4

3e

−02

1.0

5e

−02

<1e

−04

<1e

−04

Y8.4

5e

−02

-8.4

5e

−02

Candid

ate

K2-1

73

b210512842.0

148

13.1

Y<

1e

−04

<1e

−04

6.5

6e

−04

<1e

−04

<1e

−04

<1e

−04

N7.2

0e

−04

-7.2

0e

−04

Pla

net

K2-1

74

b210558622.0

142

17.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.1

1e

−15

-<

1e

−04

Pla

net

210609658.0

185

13.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.3

5e

−07

--

Candid

ate

210629082.0

141

12.8

Y2.3

6e

−04

1.8

6e

−04

1.5

1e

−03

1.5

8e

−04

<1e

−04

<1e

−04

N2.0

9e

−03

-2.0

9e

−03

Candid

ate

K2-1

75

b210643811.0

121

18.2

Y<

1e

−04

<1e

−04

4.4

6e

−04

<1e

−04

<1e

−04

<1e

−04

N5.2

6e

−04

-5.2

6e

−04

Pla

net

K2-1

76

b210667381.0

131

12.8

Y<

1e

−04

<1e

−04

4.7

6e

−04

<1e

−04

<1e

−04

<1e

−04

N5.3

8e

−04

-5.3

8e

−04

Pla

net

210707130.0

118

14.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.4

0e

−06

-<

1e

−04

Pla

net

210718708.0

1111

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

6e

−06

-<

1e

−04

Pla

net

210775710.0

172

16.3

Y0.0

0e

+00

0.0

0e

+00

1.6

5e

−03

<1e

−04

<1e

−04

<1e

−04

Y1.5

5e

−03

-1.5

5e

−03

Candid

ate

210848071.0

145

17.7

Y6.5

6e

−04

<1e

−04

9.0

7e

−04

<1e

−04

<1e

−04

<1e

−04

N1.6

2e

−03

-1.6

2e

−03

Candid

ate

K2-1

77

b210857328.0

135

14.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.1

9e

−04

-1.1

9e

−04

Pla

net

210894022.0

127

13.5

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.6

2e

−08

-<

1e

−04

Pla

net

210957318.0

1132

15.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.0

0e

−05

--

Candid

ate

K2-1

78

b210965800.0

1117

18.2

Y0.0

0e

+00

0.0

0e

+00

6.5

4e

−04

<1e

−04

<1e

−04

<1e

−04

Y3.4

7e

−04

-3.4

7e

−04

Pla

net

K2-1

79

b211048999.0

166

16.3

Y<

1e

−04

<1e

−04

3.4

2e

−04

1.5

4e

−04

<1e

−04

<1e

−04

N4.9

7e

−04

-4.9

7e

−04

Pla

net

211089792.0

160

18.2

Y-

--

--

-Y

--

-Candid

ate

211106187.0

1479

16.3

N-

--

--

-N

--

-Candid

ate

211147528.0

1351

21.1

Y-

--

--

-N

--

-Candid

ate

K2-1

80

b211319617.0

171

24.9

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.6

2e

−10

-<

1e

−04

Pla

net

211351816.0

1112

21.1

Y1.5

3e

−01

6.3

6e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.5

3e

−01

--

Candid

ate

K2-1

81

b211355342.0

164

21.1

Y7.8

5e

−04

1.9

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.9

5e

−04

-9.9

5e

−04

Pla

net

K2-1

82

b211359660.0

130

19.9

N<

1e

−04

<1e

−04

5.9

6e

−04

<1e

−04

<1e

−04

<1e

−04

N5.9

7e

−04

-5.9

7e

−04

Pla

net

211391664.0

141

22.3

Y1.6

6e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.6

5e

−04

-2.6

5e

−04

Pla

net

211401787.0

128

31.6

Y3.6

3e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.6

5e

−03

-3.6

5e

−03

Candid

ate

211418290.0

1945

16.1

N1.3

0e

−01

5.0

4e

−01

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.3

5e

−01

--

Candid

ate

211424769.0

1286

22.3

N-

--

--

-N

--

-Candid

ate

211491383.0

122

15.0

N<

1e

−04

<1e

−04

9.2

1e

−04

1.4

7e

−03

<1e

−04

<1e

−04

N2.4

0e

−03

-2.4

0e

−03

Candid

ate

211525389.0

153

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.3

3e

−06

-<

1e

−04

Pla

net

K2-1

83

c211562654.0

1156

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.6

5e

−06

50

<1e

−04

Pla

net

K2-1

83

d211562654.0

2174

16.3

Y4.4

7e

−04

1.7

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.3

1e

−04

50

<1e

−04

Pla

net

K2-1

83

b211562654.0

313

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.4

0e

−08

50

<1e

−04

Pla

net

K2-1

84

b211594205.0

135

20.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.3

8e

−05

-<

1e

−04

Pla

net

211606790.0

1106

21.1

N-

--

--

-N

--

-Candid

ate

K2-1

85

b211611158.0

148

16.8

N1.9

0e

−04

<1e

−04

1.4

2e

−02

3.6

2e

−03

<1e

−04

<1e

−04

N1.8

1e

−02

25

7.2

4e

−04

Pla

net

211611158.0

2131

16.8

N2.0

7e

−02

2.2

8e

−03

7.9

3e

−02

1.4

5e

−03

2.8

9e

−04

<1e

−04

N1.0

4e

−01

25

4.1

6e

−03

Candid

ate

211682544.0

177

16.3

N2.6

2e

−03

<1e

−04

2.6

5e

−04

<1e

−04

<1e

−04

<1e

−04

N2.9

2e

−03

-2.9

2e

−03

Candid

ate

211733267.0

187

15.3

N0.0

0e

+00

0.0

0e

+00

5.6

4e

−02

1.4

3e

−03

3.7

5e

−01

6.9

0e

−03

Y4.4

0e

−01

-4.4

0e

−01

Candid

ate

211736671.0

134

18.2

Y8.4

3e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.4

5e

−03

-8.4

5e

−03

Candid

ate

211743874.0

143

14.7

N-

--

--

-N

--

-Candid

ate

211763214.0

149

16.3

N<

1e

−04

<1e

−04

4.2

3e

−03

1.1

0e

−03

<1e

−04

<1e

−04

N5.3

3e

−03

-5.3

3e

−03

Candid

ate

211770696.0

146

16.1

Y-

--

--

-N

--

-Candid

ate

211800191.0

168

14.1

Y4.9

1e

−01

4.6

4e

−01

<1e

−04

<1e

−04

2.7

6e

−02

1.7

6e

−02

N1.0

0e

+00

--

Candid

ate

211818569.0

151

15.0

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y1.5

0e

−05

-<

1e

−04

Pla

net

211886472.0

155

21.1

Y-

--

--

-N

--

-Candid

ate

K2-1

86

b211906650.0

155

18.2

N<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.4

8e

−05

-<

1e

−04

Pla

net

211913977.0

194

13.8

N0.0

0e

+00

0.0

0e

+00

4.1

2e

−03

<1e

−04

<1e

−04

<1e

−04

Y4.2

7e

−03

-4.2

7e

−03

Candid

ate

211941472.0

119

15.8

N-

--

--

-N

--

-Candid

ate

211945201.0

137

24.1

Y1.6

2e

−01

1.1

7e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.6

4e

−01

-1.6

4e

−01

Candid

ate

211978988.0

155

13.8

N<

1e

−04

<1e

−04

2.4

0e

−03

<1e

−04

<1e

−04

<1e

−04

N2.5

7e

−03

-2.5

7e

−03

Candid

ate

211993818.0

185

42.2

N-

--

--

-Y

--

-Candid

ate

212006318.0

153

14.1

N<

1e

−04

<1e

−04

8.7

8e

−04

2.5

5e

−04

<1e

−04

<1e

−04

N1.1

3e

−03

-1.1

3e

−03

Candid

ate

212008766.0

170

15.3

Y<

1e

−04

1.4

9e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.5

0e

−03

-1.5

0e

−03

Candid

ate

212012119.0

1152

19.0

N<

1e

−04

<1e

−04

2.2

0e

−03

<1e

−04

<1e

−04

<1e

−04

N2.2

6e

−03

-2.2

6e

−03

Candid

ate

212110888.0

132

19.5

Y0.0

0e

+00

0.0

0e

+00

1.2

3e

−03

<1e

−04

1.3

1e

−04

<1e

−04

Y9.1

7e

−04

-9.1

7e

−04

Pla

net

212132195.0

185

21.5

N<

1e

−04

<1e

−04

2.2

8e

−03

<1e

−04

<1e

−04

<1e

−04

N2.2

9e

−03

-2.2

9e

−03

Candid

ate

212138198.0

173

17.9

Y-

--

--

-N

--

-Candid

ate

K2-1

87

d212157262.0

1127

16.3

Y<

1e

−04

5.1

5e

−04

1.1

2e

−04

<1e

−04

<1e

−04

<1e

−04

N6.2

9e

−04

50

<1e

−04

Pla

net

40 Mayo et al.Table

6—

Continued

New

K2

Nam

eE

PIC

Sec

on

dary

Ecl

ipse

Th

resh

old

(pp

m)

Ap

ertu

reR

ad

ius

(arc

sec)

AO

/S

pec

kle

P(E

clip

sin

gB

inary

)

P(E

clip

sin

gB

inary

)(x

2P

er.)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)(x

2P

er.)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)(x

2P

er.)

RV

Mass

Lim

it

VE

SP

AF

PP

Mu

lti-

plici

tyB

oost

Ad

op

ted

FP

PD

isp

osi

tion

K2-1

87

e212157262.0

2118

16.3

Y<

1e

−04

1.7

8e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

5e

−04

50

<1e

−04

Pla

net

K2-1

87

c212157262.0

383

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.2

4e

−09

50

<1e

−04

Pla

net

K2-1

87

b212157262.0

425

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.6

6e

−07

50

<1e

−04

Pla

net

K2-1

88

b212164470.0

115

18.2

N<

1e

−04

<1e

−04

1.3

8e

−04

2.3

9e

−04

<1e

−04

<1e

−04

N3.7

7e

−04

25

<1e

−04

Pla

net

K2-1

88

c212164470.0

244

18.2

N1.3

0e

−04

<1e

−04

6.8

7e

−04

<1e

−04

<1e

−04

<1e

−04

N8.6

7e

−04

25

<1e

−04

Pla

net

212303338.0

110

24.3

Y-

--

--

-N

--

-Candid

ate

212357477.0

127

29.1

Y2.9

9e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.0

4e

−03

-3.0

4e

−03

Candid

ate

K2-1

89

b212394689.0

1177

16.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.0

5e

−06

25

<1e

−04

Pla

net

K2-1

89

c212394689.0

253

16.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.3

5e

−06

25

<1e

−04

Pla

net

212460519.0

143

17.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.5

6e

−10

-<

1e

−04

Pla

net

K2-1

90

b212480208.0

119

18.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.8

3e

−10

25

<1e

−04

Pla

net

K2-1

90

c212480208.0

225

18.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.7

3e

−07

25

<1e

−04

Pla

net

K2-1

91

b212496592.0

155

15.0

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.4

0e

−07

-<

1e

−04

Pla

net

212521166.0

137

17.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.4

4e

−07

-<

1e

−04

Pla

net

212534729.0

161

14.4

Y-

--

--

-N

--

-Candid

ate

K2-1

92

b212555594.0

155

13.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.7

1e

−04

-1.7

1e

−04

Pla

net

212562715.0

178

16.1

Y4.0

1e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.0

3e

−03

-4.0

3e

−03

Candid

ate

212577658.0

138

18.2

Y-

--

--

-N

--

-Candid

ate

K2-1

93

b212580872.0

162

13.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.9

7e

−05

-<

1e

−04

Pla

net

212586030.0

179

16.6

Y-

--

--

-N

--

-Candid

ate

212587672.0

171

15.0

Y1.3

4e

−02

1.9

5e

−03

<1e

−04

<1e

−04

2.6

5e

−04

<1e

−04

N1.5

7e

−02

-1.5

7e

−02

Candid

ate

212639319.0

184

17.5

Y8.6

6e

−01

6.0

3e

−02

<1e

−04

<1e

−04

6.1

1e

−02

8.0

6e

−03

N9.9

6e

−01

-9.9

6e

−01

Candid

ate

212645891.0

142

18.2

Y<

1e

−04

9.8

8e

−01

<1e

−04

<1e

−04

<1e

−04

1.2

2e

−02

N1.0

0e

+00

--

Candid

ate

K2-1

94

b212672300.0

145

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.7

9e

−05

-<

1e

−04

Pla

net

212686205.0

144

15.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.2

5e

−05

-<

1e

−04

Pla

net

K2-1

95

b212689874.0

153

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.9

9e

−10

25

<1e

−04

Pla

net

K2-1

95

c212689874.0

2104

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.9

1e

−05

25

<1e

−04

Pla

net

K2-1

96

b212691422.0

151

19.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.8

9e

−05

-<

1e

−04

Pla

net

212697709.0

177

16.8

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y3.4

9e

−04

-3.4

9e

−04

Pla

net

212703473.0

118

18.8

Y-

--

--

-N

--

-Candid

ate

212703473.0

239

18.8

Y-

--

--

-N

--

-Candid

ate

K2-1

97

b212735333.0

182

17.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.0

6e

−05

-<

1e

−04

Pla

net

K2-1

98

b212768333.0

1273

24.7

Y2.3

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.7

4e

−04

-2.7

4e

−04

Pla

net

212772313.0

1227

21.1

Y2.2

6e

−02

9.5

0e

−03

<1e

−04

<1e

−04

<1e

−04

1.6

5e

−04

N3.2

3e

−02

-3.2

3e

−02

Candid

ate

K2-1

99

b212779596.0

145

21.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

7e

−09

25

<1e

−04

Pla

net

K2-1

99

c212779596.0

269

21.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.7

2e

−10

25

<1e

−04

Pla

net

212803289.0

131

26.7

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.8

0e

−14

--

Candid

ate

K2-2

00

b212828909.0

156

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.1

1e

−04

-1.1

1e

−04

Pla

net

213546283.0

158

18.2

Y-

--

--

-N

--

-Candid

ate

213817056.0

1492

18.6

N3.9

9e

−03

9.0

3e

−03

2.0

7e

−01

1.4

0e

−01

3.2

3e

−04

2.6

4e

−04

N3.6

0e

−01

-3.6

0e

−01

Candid

ate

214234110.0

139

15.6

Y1.9

5e

−01

5.1

4e

−02

<1e

−04

<1e

−04

<1e

−04

6.6

0e

−04

N2.4

7e

−01

-2.4

7e

−01

Candid

ate

214254518.0

142

18.2

N<

1e

−04

<1e

−04

8.8

4e

−03

5.8

5e

−03

<1e

−04

<1e

−04

N1.4

7e

−02

-1.4

7e

−02

Candid

ate

215171927.0

178

18.2

Y-

--

--

-N

--

-Candid

ate

215171927.0

2104

18.2

Y-

--

--

-N

--

-Candid

ate

215502661.0

164

18.2

N5.8

6e

−04

2.3

7e

−02

2.1

9e

−01

7.3

5e

−01

<1e

−04

3.9

4e

−04

N9.7

8e

−01

-9.7

8e

−01

Candid

ate

215854715.0

186

18.2

Y-

--

--

-N

--

-Candid

ate

K2-2

01

b216008129.0

132

20.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.6

8e

−07

25

<1e

−04

Pla

net

K2-2

01

c216008129.0

2120

20.3

Y3.8

8e

−03

2.8

8e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.7

7e

−03

25

2.7

1e

−04

Pla

net

216050437.0

195

21.1

Y-

--

--

-N

--

-Candid

ate

216114172.0

171

21.1

Y-

--

--

-N

--

-Candid

ate

216166748.0

154

16.3

Y-

--

--

-N

--

-Candid

ate

216387101.0

156

15.0

N9.7

5e

−04

1.6

9e

−03

8.2

2e

−03

1.9

1e

−02

<1e

−04

<1e

−04

N3.0

0e

−02

-3.0

0e

−02

Candid

ate

K2-2

02

b216405287.0

153

13.5

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.9

3e

−06

-<

1e

−04

Pla

net

216468514.0

146

12.8

Y-

--

--

-N

--

-Candid

ate

216494238.0

139

15.3

Y-

--

--

-N

--

-Candid

ate

217192839.0

144

13.8

Y-

--

--

-Y

--

-Candid

ate

217192839.0

292

13.8

Y-

--

--

-Y

--

-Candid

ate

217192839.0

377

13.8

Y-

--

--

-Y

--

-Candid

ate

217855533.0

125

21.1

N0.0

0e

+00

0.0

0e

+00

8.4

2e

−04

1.0

3e

−04

<1e

−04

<1e

−04

Y1.2

4e

−03

-1.2

4e

−03

Candid

ate

217941732.0

123

15.6

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.3

6e

−07

-<

1e

−04

Pla

net

217977895.0

1101

13.8

Y1.7

5e

−04

3.9

2e

−02

<1e

−04

<1e

−04

<1e

−04

6.7

0e

−04

N4.0

0e

−02

-4.0

0e

−02

Candid

ate

218131080.0

125

15.6

Y-

--

--

-N

--

-Candid

ate

218170789.0

154

16.3

N<

1e

−04

<1e

−04

1.8

9e

−02

9.8

1e

−01

<1e

−04

<1e

−04

N1.0

0e

+00

--

Candid

ate

218304292.0

192

15.3

Y7.4

5e

−01

3.1

5e

−02

<1e

−04

<1e

−04

5.0

9e

−02

3.9

9e

−03

N8.3

2e

−01

-8.3

2e

−01

Candid

ate

218668602.0

166

15.8

N<

1e

−04

<1e

−04

1.1

8e

−03

3.8

6e

−04

<1e

−04

<1e

−04

N1.5

7e

−03

-1.5

7e

−03

Candid

ate

218916923.0

183

21.1

Y-

--

--

-N

--

-Candid

ate

219388192.0

181

18.8

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.8

2e

−08

--

Candid

ate

K2-2

03

b220170303.0

176

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.1

7e

−06

-<

1e

−04

Pla

net

K2-2

04

b220186645.0

170

19.7

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.5

7e

−05

-<

1e

−04

Pla

net

220192485.0

1190

20.6

Y-

--

--

-Y

--

-Candid

ate

220207765.0

1112

20.1

Y4.2

8e

−04

4.5

1e

−03

<1e

−04

<1e

−04

<1e

−04

2.9

0e

−04

N5.2

7e

−03

-5.2

7e

−03

Candid

ate

K2-2

05

b220211923.0

151

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N9.8

5e

−06

-<

1e

−04

Pla

net

K2-2

06

b220216730.0

1164

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.2

2e

−08

-<

1e

−04

Pla

net

K2-2

07

b220218012.0

1113

16.3

Y<

1e

−04

1.8

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.8

6e

−04

-1.8

6e

−04

Pla

net


6—

Continued

New

K2

Nam

eE

PIC

Sec

on

dary

Ecl

ipse

Th

resh

old

(pp

m)

Ap

ertu

reR

ad

ius

(arc

sec)

AO

/S

pec

kle

P(E

clip

sin

gB

inary

)

P(E

clip

sin

gB

inary

)(x

2P

er.)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)

P(B

ack

-gro

un

dE

clip

sin

gB

inary

)(x

2P

er.)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)

P(H

ier-

arc

hic

al

Ecl

ipsi

ng

Bin

ary

)(x

2P

er.)

RV

Mass

Lim

it

VE

SP

AF

PP

Mu

lti-

plici

tyB

oost

Ad

op

ted

FP

PD

isp

osi

tion

K2-2

08

b220225178.0

153

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.3

0e

−06

-<

1e

−04

Pla

net

K2-2

09

b220241529.0

114

19.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

1e

−06

-<

1e

−04

Pla

net

220245303.0

137

18.2

Y<

1e

−04

1.0

7e

−03

<1e

−04

<1e

−04

<1e

−04

1.4

5e

−04

N1.2

2e

−03

-1.2

2e

−03

Candid

ate

K2-2

10

b220250254.0

113

17.1

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y2.3

1e

−04

-2.3

1e

−04

Pla

net

K2-2

11

b220256496.0

136

18.4

Y<

1e

−04

1.5

9e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.1

6e

−04

-2.1

6e

−04

Pla

net

220292715.0

1136

15.8

Y1.0

8e

−01

<1e

−04

<1e

−04

<1e

−04

3.1

3e

−03

<1e

−04

N1.1

1e

−01

-1.1

1e

−01

Candid

ate

220294712.0

160

14.7

Y-

--

--

-N

--

-Candid

ate

220317172.0

150

16.3

Y4.0

5e

−02

8.7

3e

−03

<1e

−04

<1e

−04

3.7

9e

−04

1.4

3e

−03

N5.1

1e

−02

-5.1

1e

−02

Candid

ate

K2-2

12

b220321605.0

159

15.0

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.0

1e

−08

-<

1e

−04

Pla

net

K2-2

13

b220341183.0

139

16.3

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y2.1

0e

−05

-<

1e

−04

Pla

net

K2-2

14

b220376054.0

134

16.3

Y3.6

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.7

3e

−04

-3.7

3e

−04

Pla

net

220383386.0

113

25.5

N<

1e

−04

<1e

−04

7.2

0e

−03

<1e

−04

<1e

−04

<1e

−04

N7.2

6e

−03

25

2.9

0e

−04

Pla

net

220383386.0

272

25.5

N<

1e

−04

1.1

4e

−04

1.6

8e

−03

<1e

−04

<1e

−04

<1e

−04

N1.8

0e

−03

25

<1e

−04

Pla

net

220397060.0

156

18.2

Y-

--

--

-N

--

-Candid

ate

220410754.0

167

15.0

Y8.3

9e

−04

2.2

3e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.0

6e

−03

-1.0

6e

−03

Candid

ate

K2-2

15

b220471666.0

164

13.8

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y3.7

6e

−04

-3.7

6e

−04

Pla

net

K2-2

16

b220481411.0

130

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N4.5

6e

−09

-<

1e

−04

Pla

net

K2-2

17

b220487418.0

150

17.3

Y<

1e

−04

3.2

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.5

6e

−04

-3.5

6e

−04

Pla

net

K2-2

18

b220503236.0

135

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N7.9

1e

−07

-<

1e

−04

Pla

net

220555384.0

146

16.3

Y-

--

--

-N

--

-Candid

ate

K2-2

19

b220592745.0

126

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.8

2e

−07

50

<1e

−04

Pla

net

K2-2

19

c220592745.0

225

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.1

8e

−09

50

<1e

−04

Pla

net

K2-2

19

d220592745.0

329

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.8

6e

−07

50

<1e

−04

Pla

net

K2-2

20

b220621788.0

139

17.5

Y3.7

7e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.7

8e

−04

-3.7

8e

−04

Pla

net

220643470.0

1182

22.4

Y-

--

--

-Y

--

-Candid

ate

220648214.0

166

17.3

Y6.3

2e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N6.3

2e

−03

-6.3

2e

−03

Candid

ate

K2-2

21

b220650439.0

128

16.3

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.0

3e

−09

-<

1e

−04

Pla

net

220674823.0

18

20.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N5.9

0e

−10

25

<1e

−04

Pla

net

220674823.0

276

20.1

Y<

1e

−04

1.3

2e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.3

4e

−04

25

<1e

−04

Pla

net

220679255.0

199

18.2

Y2.3

5e

−02

1.4

9e

−03

<1e

−04

<1e

−04

4.8

3e

−04

<1e

−04

N2.5

6e

−02

-2.5

6e

−02

Candid

ate

K2-2

22

b220709978.0

131

23.3

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

<1e

−04

<1e

−04

Y6.9

2e

−05

-<

1e

−04

Pla

net

K2-2

23

b228721452.0

117

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.0

9e

−04

25

<1e

−04

Pla

net

K2-2

23

c228721452.0

234

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.8

8e

−08

25

<1e

−04

Pla

net

K2-2

24

b228725972.0

168

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.2

3e

−06

25

<1e

−04

Pla

net

228725972.0

277

18.2

Y-

--

--

-N

--

-Candid

ate

228729473.0

153

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N7.4

3e

−11

--

Candid

ate

228732031.0

119

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.6

3e

−08

-<

1e

−04

Pla

net

228734889.0

1534

19.9

Y-

--

--

-N

--

-Candid

ate

K2-2

25

b228734900.0

138

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N8.0

6e

−07

-<

1e

−04

Pla

net

228735255.0

160

19.7

Y-

--

--

-N

--

-Candid

ate

K2-2

26

b228736155.0

136

24.7

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

1e

−08

-<

1e

−04

Pla

net

228737155.0

151

24.7

N-

--

--

-Y

--

-Candid

ate

228754001.0

166

23.9

Y-

--

--

-N

--

-Candid

ate

K2-2

27

b228760097.0

159

21.1

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.1

5e

−05

-<

1e

−04

Pla

net

K2-2

28

b228798746.0

135

15.0

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.6

4e

−06

-<

1e

−04

Pla

net

K2-2

29

b228801451.0

116

18.4

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.0

7e

−07

25

<1e

−04

Pla

net

K2-2

29

c228801451.0

2128

18.4

Y2.5

8e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N3.6

7e

−04

25

<1e

−04

Pla

net

K2-2

30

b228804845.0

160

18.2

Y<

1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.2

0e

−07

-<

1e

−04

Pla

net

228809391.0

1125

15.8

Y0.0

0e

+00

0.0

0e

+00

<1e

−04

<1e

−04

1.5

7e

−03

<1e

−04

Y1.6

8e

−03

-1.6

8e

−03

Candid

ate

228952747.0

1224

15.3

Y2.6

9e

−01

7.3

8e

−02

<1e

−04

<1e

−04

6.6

0e

−03

4.6

9e

−03

N3.5

4e

−01

-3.5

4e

−01

Candid

ate

229004835.0

148

20.5

Y1.8

2e

−02

<1e

−04

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N1.8

3e

−02

-1.8

3e

−02

Candid

ate

229039390.0

124

15.3

Y-

--

--

-Y

--

-Candid

ate

229131722.0

163

20.5

Y6.8

4e

−04

1.8

4e

−03

<1e

−04

<1e

−04

<1e

−04

<1e

−04

N2.5

2e

−03

-2.5

2e

−03

Candid

ate

229133720.0

139

17.3

Y-

--

--

-N

--

-Candid

ate

42 Mayo et al.

Table 7High-resolution Imaging

EPIC Filter Instrument

201110617 562 NESSI201110617 832 NESSI201111557 562 NESSI201111557 832 NESSI201127519 562 NESSI201127519 832 NESSI201130233 562 NESSI201130233 832 NESSI201132684 562 NESSI201132684 832 NESSI201132684 562 NESSI201132684 832 NESSI201166680 562 NESSI201166680 832 NESSI201211526 562 NESSI201211526 832 NESSI201225286 562 NESSI201225286 832 NESSI201227197 562 NESSI201227197 832 NESSI201231064 562 NESSI201231064 832 NESSI201295312 K PHARO201295312 K NIRC2201299088 562 NESSI201299088 832 NESSI201352100 562 NESSI201352100 832 NESSI201384232 K NIRC2201390048 562 NESSI201390048 832 NESSI201403446 K NIRC2201427874 562 NESSI201427874 832 NESSI201437844 562 NESSI201437844 832 NESSI201505350 K PHARO201505350 K NIRC2201528828 562 NESSI201528828 832 NESSI201546283 K NIRC2201577035 K PHARO201577035 K NIRC2201595106 562 NESSI201595106 832 NESSI201613023 K PHARO201613023 K NIRC2201615463 562 NESSI201615463 832 NESSI201713348 K PHARO201713348 K NIRC2201828749 J PHARO201828749 K PHARO201828749 J NIRC2201828749 K NIRC2201855371 K NIRC2201920032 K NIRC2202089657 K LMIRcam202089657 K PHARO202089657 692 DSSI202089657 880 DSSI202091388 692 DSSI202091388 880 DSSI202675839 K NIRC2202900527 K NIRC2203771098 K NIRC2203826436 K NIRC2205029914 K NIRC2205071984 K NIRC2205904628 J Unknown205904628 692 DSSI205904628 880 DSSI205944181 K NIRC2205944181 692 DSSI205944181 880 DSSI




206011496 J NIRC2206011496 K NIRC2206026904 K NIRC2206096602 K NIRC2206144956 K NIRC2206159027 K NIRI206159027 K PHARO206159027 K NIRC2206181769 K NIRC2206192335 K NIRI206192335 K PHARO206245553 K NIRC2206268299 K NIRC2206348688 K NIRC2206439513 K NIRC2210363145 K NIRI210363145 692 DSSI210363145 880 DSSI210363145 692 DSSI210363145 880 DSSI210363145 692 DSSI210363145 880 DSSI210402237 K NIRI210402237 692 DSSI210402237 880 DSSI210403955 K NIRI210512842 692 DSSI210512842 880 DSSI210558622 K NIRC2210558622 K NIRC2210558622 692 DSSI210558622 880 DSSI210558622 692 DSSI210558622 880 DSSI210609658 K NIRI210609658 692 DSSI210609658 880 DSSI210629082 692 DSSI210629082 880 DSSI210643811 692 DSSI210643811 880 DSSI210667381 692 DSSI210667381 880 DSSI210707130 K NIRC2210707130 K NIRC2210707130 692 DSSI210707130 880 DSSI210718708 K NIRI210718708 692 DSSI210718708 880 DSSI210775710 692 DSSI210775710 880 DSSI210848071 692 DSSI210848071 880 DSSI210857328 692 DSSI210857328 880 DSSI210894022 K NIRI210957318 K NIRI210965800 692 DSSI210965800 880 DSSI211048999 692 DSSI211048999 880 DSSI211089792 K NIRI211147528 K NIRC2211147528 692 DSSI211147528 880 DSSI211147528 692 DSSI211147528 880 DSSI211319617 K NIRC2211319617 692 DSSI211319617 880 DSSI211351816 K NIRC2211351816 K PHARO211355342 K NIRC2211391664 K NIRC2211401787 K PHARO211525389 J NIRC2

44 Mayo et al.



211525389 K NIRC2211525389 692 DSSI211525389 880 DSSI211562654 K NIRC2211594205 K PHARO211736671 K NIRC2211736671 692 DSSI211736671 880 DSSI211770696 K PHARO211800191 K NIRC2211818569 K PHARO211886472 J NIRC2211886472 K NIRC2211886472 692 DSSI211886472 880 DSSI211945201 K NIRC2211945201 692 DSSI211945201 880 DSSI212008766 K NIRC2212110888 692 DSSI212110888 880 DSSI212138198 J NIRC2212138198 K NIRC2212138198 692 DSSI212138198 880 DSSI212157262 K NIRC2212303338 692 DSSI212303338 880 DSSI212357477 692 DSSI212357477 880 DSSI212394689 K NIRC2212394689 692 DSSI212394689 880 DSSI212460519 692 DSSI212460519 880 DSSI212480208 692 DSSI212480208 880 DSSI212496592 692 DSSI212496592 880 DSSI212521166 692 DSSI212521166 880 DSSI212534729 692 DSSI212534729 880 DSSI212555594 692 DSSI212555594 880 DSSI212562715 692 DSSI212562715 880 DSSI212577658 692 DSSI212577658 880 DSSI212580872 692 DSSI212580872 880 DSSI212580872 692 DSSI212580872 880 DSSI212586030 J PHARO212586030 K PHARO212586030 692 DSSI212586030 880 DSSI212587672 692 DSSI212587672 880 DSSI212639319 692 DSSI212639319 880 DSSI212645891 692 DSSI212645891 880 DSSI212672300 692 DSSI212672300 880 DSSI212686205 692 DSSI212686205 880 DSSI212689874 692 DSSI212689874 880 DSSI212689874 692 DSSI212689874 880 DSSI212691422 692 DSSI212691422 880 DSSI212697709 692 DSSI212697709 880 DSSI212697709 692 DSSI212697709 880 DSSI




212703473 J PHARO212703473 K PHARO212703473 692 DSSI212703473 880 DSSI212735333 K PHARO212735333 692 DSSI212735333 880 DSSI212768333 692 DSSI212768333 880 DSSI212772313 692 DSSI212772313 880 DSSI212779596 692 DSSI212779596 880 DSSI212779596 692 DSSI212779596 880 DSSI212803289 692 DSSI212803289 880 DSSI212828909 692 DSSI212828909 880 DSSI213546283 K NIRI213546283 692 DSSI213546283 880 DSSI214234110 692 DSSI214234110 880 DSSI215171927 692 DSSI215171927 880 DSSI215854715 692 DSSI215854715 880 DSSI216008129 692 DSSI216008129 880 DSSI216050437 K NIRI216050437 692 DSSI216050437 880 DSSI216114172 692 DSSI216114172 880 DSSI216166748 692 DSSI216166748 880 DSSI216405287 692 DSSI216405287 880 DSSI216468514 K NIRI216468514 K NIRI216468514 692 DSSI216468514 880 DSSI216494238 K NIRI216494238 692 DSSI216494238 880 DSSI217192839 K NIRI217192839 692 DSSI217192839 880 DSSI217941732 692 DSSI217941732 880 DSSI217977895 692 DSSI217977895 880 DSSI218131080 K NIRI218131080 692 DSSI218131080 880 DSSI218304292 692 DSSI218304292 880 DSSI218916923 K PHARO218916923 692 DSSI218916923 880 DSSI219388192 K NIRI219388192 692 DSSI219388192 880 DSSI220170303 562 NESSI220170303 832 NESSI220170303 562 NESSI220170303 832 NESSI220186645 562 NESSI220186645 832 NESSI220186645 562 NESSI220186645 832 NESSI220192485 562 NESSI220192485 832 NESSI220192485 562 NESSI220192485 832 NESSI220207765 562 NESSI

46 Mayo et al.



220207765 832 NESSI220211923 562 NESSI220211923 832 NESSI220216730 562 NESSI220216730 832 NESSI220218012 562 NESSI220218012 832 NESSI220225178 562 NESSI220225178 832 NESSI220241529 562 NESSI220241529 832 NESSI220245303 562 NESSI220245303 832 NESSI220250254 562 NESSI220250254 832 NESSI220256496 562 NESSI220256496 832 NESSI220292715 562 NESSI220292715 832 NESSI220292715 562 NESSI220292715 832 NESSI220292715 562 NESSI220292715 832 NESSI220294712 562 NESSI220294712 832 NESSI220294712 K PHARO220317172 562 NESSI220317172 832 NESSI220321605 562 NESSI220321605 832 NESSI220321605 K PHARO220341183 562 NESSI220341183 832 NESSI220376054 562 NESSI220376054 832 NESSI220397060 562 NESSI220397060 832 NESSI220397060 J PHARO220397060 K PHARO220410754 562 NESSI220410754 832 NESSI220471666 562 NESSI220471666 832 NESSI220481411 562 NESSI220481411 832 NESSI220481411 562 NESSI220481411 832 NESSI220481411 562 NESSI220481411 832 NESSI220481411 K PHARO220487418 562 NESSI220487418 832 NESSI220487418 K PHARO220503236 562 NESSI220503236 832 NESSI220555384 562 NESSI220555384 832 NESSI220555384 J PHARO220555384 K PHARO220555384 K NIRI220592745 562 NESSI220592745 832 NESSI220621788 562 NESSI220621788 832 NESSI220643470 562 NESSI220643470 832 NESSI220643470 J PHARO220643470 K PHARO220648214 562 NESSI220648214 832 NESSI220650439 562 NESSI220650439 832 NESSI220650439 K PHARO220674823 562 NESSI220674823 832 NESSI220679255 562 NESSI220679255 832 NESSI




220709978 562 NESSI220709978 832 NESSI220709978 K PHARO228721452 562 NESSI228721452 832 NESSI228725972 562 NESSI228725972 832 NESSI228729473 562 NESSI228729473 832 NESSI228729473 562 NESSI228729473 832 NESSI228732031 562 NESSI228732031 832 NESSI228734889 562 NESSI228734889 832 NESSI228734900 562 NESSI228734900 832 NESSI228735255 562 NESSI228735255 832 NESSI228736155 562 NESSI228736155 832 NESSI228754001 562 NESSI228754001 832 NESSI228760097 562 NESSI228760097 832 NESSI228798746 562 NESSI228798746 832 NESSI228801451 562 NESSI228801451 832 NESSI228804845 562 NESSI228804845 832 NESSI228809391 562 NESSI228809391 832 NESSI228952747 562 NESSI228952747 832 NESSI229004835 562 NESSI229004835 832 NESSI229039390 562 NESSI229039390 832 NESSI229131722 562 NESSI229131722 832 NESSI229131722 562 NESSI229131722 832 NESSI229133720 562 NESSI229133720 832 NESSI

Documents

arXiv:1802.05277v1 [astro-ph.EP] 14 Feb 2018