Robo-AO Kepler Planetary Candidate Survey III: Adaptive Optics Imaging of 1629 Kepler Exoplanet Candidate Host Stars
Carl Ziegler, Nicholas M. Law, Tim Morton, Christoph Baranec, Reed Riddle, Dani Atkinson, Anna Baker, Sarah Roberts, David R. Ciardi
RR evision draft Preprint typeset using L A TEX style emulateapj v. 01 / / ROBO-AO KEPLER PLANETARY CANDIDATE SURVEY III: ADAPTIVE OPTICS IMAGING OF 1629 KEPLEREXOPLANET CANDIDATE HOST STARS C arl Z iegler , N icholas M. L aw , T im M orton , C hristoph B aranec , R eed R iddle , D ani A tkinson , A nna B aker ,S arah R oberts , and D avid R. C iardi Revision draft
ABSTRACTThe Robo-AO
Kepler
Planetary Candidate Survey is observing every
Kepler planet candidate host star withlaser adaptive optics imaging to search for blended nearby stars, which may be physically associated compan-ions and / or responsible for transit false positives. We present in this paper the results of our search for starsnearby 1629 Kepler planet candidate hosts. With survey sensitivity to objects as close as ∼ . (cid:48)(cid:48)
15 and magnitudedi ff erences ∆ m ≤
6, we find 223 stars in the vicinity of 206 target KOIs; 209 of these nearby stars have notpreviously been imaged in high resolution. We measure an overall nearby-star probability for
Kepler planetcandidates of 12.6% ± . (cid:48)(cid:48)
15 and 4 . (cid:48)(cid:48)
0. Particularly interesting KOI systems arediscussed, including 26 stars with detected companions which host rocky, habitable zone candidates, and fivenew candidate planet-hosting quadruple star systems. We explore the broad correlations between planetarysystems and stellar binarity using the combined dataset of Baranec et al. (2016) and this paper. Our previous2 σ result of a low detected nearby star fraction of KOIs hosting close-in giant planets is less apparent in thislarger dataset. We also find a significant correlation between detected nearby star fraction and KOI number,suggesting possible variation between early and late Kepler data releases.
Keywords: binaries: close - instrumentation: adaptive optics - techniques: high angular resolution - methods:data analysis - methods: observational - planets and satellites: detection - planets and satellites:fundamental parameters INTRODUCTION
The primary
Kepler mission vastly increased the tally ofknown extrasolar planets, discovering over 2300 confirmedplanets and approximately 4700 planet candidates (Boruckiet al. 2010, 2011a,b; Batalha et al. 2013; Burke et al. 2014;Rowe et al. 2014; Coughlin et al. 2015; Morton et al. 2016).Using high-precision photometry to detect the periodic dipin stellar brightness consistent with a transiting planet,
Ke-pler exoplanet candidates (
Kepler
Objects of Interests, orKOIs) require follow-up observations to rule out astrophys-ical false positives and for host star characterization (Brownet al. 2011).Most solar-type stars, which comprise the majority of
Ke-pler targets (Batalha et al. 2013), form with at least onecompanion star (Duquennoy & Mayor 1991; Raghavan et al.2010). The large e ff ective point-spread function (6-10 (cid:48)(cid:48) ) andcoarse resolution (pixel size of ∼ (cid:48)(cid:48) ) (Haas et al. 2010) of Ke-pler allow these companion stars and background objects tobe blended with the host candidate, illustrated in Figure 1.High-angular-resolution follow-up imaging is crucial to dis-tinguish these blended multiple stellar systems and identifyfalse transit signals. Even when the candidates are bona fide [email protected] Department of Physics and Astronomy, University of North Carolinaat Chapel Hill, Chapel Hill, NC 27599-3255, USA Department of Astrophysical Sciences, Princeton University, Prince-ton, NJ 08544, USA Institute for Astronomy, University of Hawai‘i at M¯anoa, Hilo, HI96720-2700, USA Division of Physics, Mathematics, and Astronomy, California Instituteof Technology, Pasadena, CA 91125, USA Durham Academy Upper School, 3601 Ridge Road, Durham, NC27705, USA Juniata College, 1700 Moore St, Huntingdon, PA 16652, USA NASA Exoplanet Science Institute, California Institute of Technology,Pasadena, CA 91125, USA planets, the planet radius measurements based on the dilutedtransit signal are underestimated due to the presence of mul-tiple stars in the system or unbounded stars within the
Kepler aperture (Ciardi et al. 2015).Before being elevated to planet candidate status, each KOIis vetted for clear signatures of being an astrophysical falsepositive: center-of-light shifts during transit, an identifiablesecondary eclipse signal indicating the eclipsing object is self-luminous, or sharing the exact ephemeris as another KOI.While these vetting e ff orts on early catalogs were largelybased on human inspection (Batalha et al. 2010), the most re-cent DR24 catalog has fully automated this process (Cough-lin et al. 2015). Notably, the candidate status of a KOI is not a function of its depth or shape (i.e., whether it is V-shaped), which means that a large fraction of the deepersignals ( ∼ ∼ Spitzer space tele-scope (D´esert et al. 2015). Nevertheless, even if a large frac-tion of the candidate signals are real planets, many of the in-ferred properties of these planets are a ff ected by the presenceof blended sources (Dressing & Charbonneau 2013; Santerneet al. 2013). Therefore to fully characterize individual Kepler planets and to measure any possible biasing e ff ects of stellarmultiplicity on the planetary populations, every KOI needs tobe searched for stellar companions .There has been considerable e ff ort by the community to per-form high-resolution imaging surveys of the KOIs (Howellet al. 2011; Adams et al. 2012, 2013; Lillo-Box et al. 2012, For brevity we denote stars which we found within our detection radiusof KOIs as “companions,” in the sense that they are asterisms associated onthe sky. a r X i v : . [ a s t r o - ph . E P ] S e p Z iegler et al . Figure 1.
On the left, the full-frame Robo-AO reduced image of KOI-4418 (KIC2859893) rotated and scaled to match the
Kepler view of the same field,displayed on the right, each pixel colored by the mean flux in Quarter 4. KICs in the field are marked on both images, as well as K P magnitude in the Kepler image. The 1 . (cid:48)(cid:48)
41 binary to KOI-4418 is not visible in the ∼ (cid:48)(cid:48) pixels of Kepler , illustrating how real companions and background stars can blend with the KOIs,resulting in astrophysical false positives or inaccurate planetary characteristics. High resolution follow-ups are a crucial step in the validation and characterizationof
Kepler planetary systems.
Kepler planetary candidates. This piecemeal ap-proach leads to inconsistent vetting, while limiting the com-prehensive statistics and correlations that can be derived froma large dataset of high resolution images of multiple stellarsystems hosting planetary systems. In addition, target lists ofpast surveys are often biased towards brighter targets, possi-bly skewing any interpretations drawn from the data.A complete, consistent high-resolution survey of all thethe KOIs with ground-based adaptive optics (AO) is limitedby the typical overheads required with traditional systems.Taking advantage of the order-of-magnitude increase in time-e ffi ciency provided by Robo-AO, the first robotic laser adap-tive optics system, we are performing high-resolution imag-ing of every KOI system. The first paper in this survey, Lawet al. (2014, hereafter Paper I), observed 715 Kepler plane-tary candidates, identifying 53 companions, with 43 new dis-coveries, for a detected companion fraction of 7.4% ± . (cid:48)(cid:48)
15 to 2 . (cid:48)(cid:48)
5. The second paper in thissurvey, Baranec et al. (2016, hereafter Paper II), observed969
Kepler planetary candidates, identifying 202 companions,with 139 new discoveries, for a detected companion frac-tion of 11.0% ± . (cid:48)(cid:48)
15 to 2 . (cid:48)(cid:48) ± . (cid:48)(cid:48)
15 to 4 . (cid:48)(cid:48) ± . (cid:48)(cid:48) ff ects on the planetary characteristics of the survey’sdiscoveries and looking at the overall binarity statistics of the Kepler planet candidates. We conclude in Section 6. SURVEY TARGETS AND OBSERVATIONS
Target Selection
KOI targets were selected from the KOI catalog based onQ1-Q17
Kepler data (Borucki et al. 2010, 2011a,b; Batalhaet al. 2013; Burke et al. 2014; Rowe et al. 2014; Coughlinet al. 2015). We selected targets not observed in Paper I andPaper II, with the objective of completing the Robo-AO sur-vey of all KOIs, including those with already detected com-panions. Observations in this paper are primarily from the2014-15 observing seasons; residual observations of dim tar-gets from 2012-13 are also included, their analysis now pos-sible using our improved binary detection and characteriza-tion pipeline. KOIs flagged as false positives using
Kepler data were removed. In Figure 2 the properties of the targetedKOIs in this work as well as for the full Robo-AO surveyas of the end of the 2015 observing season are compared tothe set of all KOIs from Q1-Q17 with CANDIDATE disposi-tions based on
Kepler data. The Robo-AO target distributionclosely matches the full KOI list in magnitude, planetary ra-dius, planetary orbital period, and stellar temperature. On-skypositions of all targeted KOIs in the complete survey are dis-played in Figure 3.
Observations
Robo-AO
We obtained high-angular-resolution images of the 1629KOIs during 55 separate nights of observations between 2012July 16 and 2015 June 12 (UT), detailed in Table 9 in the Ap-pendix. The observations were performed using the Robo-AOlaser adaptive optics system (Baranec et al. 2013, 2014b; Rid-dle et al. 2012) mounted on the Palomar 1.5-m telescope. Thefirst robotic laser guide star adaptive optics system, the au-tomatic Robo-AO system can e ffi ciently perform large, highangular resolution surveys. The AO system runs at a looprate of 1.2 kHz to correct high-order wavefront aberrations,delivering a median Strehl ratio of 9% in the i (cid:48) -band. Obser-vations were taken in either a i (cid:48) -band filter or a long-pass filtercutting on at 600 nm (LP600 hereafter). The LP600 filter ap- obo -AO Kepler P lanetary C andidate S urvey III 3
Figure 2.
Comparison of the distribution of the Robo-AO sample in this paper as well as the combined Robo-AO survey (Paper I, Paper II, and this work) to thecomplete set of KOIs from Q1-Q17 (Borucki et al. 2010, 2011a,b; Batalha et al. 2013; Burke et al. 2014; Rowe et al. 2014; Coughlin et al. 2015). proximates the
Kepler passband at redder wavelengths, whilealso suppressing blue wavelengths that reduce adaptive opticsperformance.Typical seeing at the Palomar Observatory is between 0 . (cid:48)(cid:48) . (cid:48)(cid:48)
8, with median around 1 . (cid:48)(cid:48) ff raction limited) resolution of the Robo-AO system is 0 . (cid:48)(cid:48)
15. Images are recorded on an electron-multiplying CCD (EMCCD), allowing short frame rates fortip and tilt correction in software using a natural guide star( m V <
16) in the field of view. Specifications of the Robo-AOKOI survey are summarized in Table 1.
Keck LGS-AO
Eight candidate multiple systems were selected for re-imaging by the NIRC2 camera behind the Keck-II laser guidestar adaptive optics system (Wizinowich et al. 2006; van Damet al. 2006), on 2015 July 25 (UT) to confirm possible com-panions. The targets were selected for their low signifi-cance of detectability, either because of low contrast ratio orsmall angular separation. Observations were performed inthe K prime filter using the narrow mode of NIRC2 (9.952 maspixel − ; Yelda et al. 2010), dithering the primary target at in-tervals of 30 s into the 3 lowest noise quadrants, for a total ex-posure time of 90 s. The images were corrected for geometricdistortion using the NIRC2 distortion solution of Yelda et al.(2010). Targets observed with Keck are detailed in Table 2.Further follow-up observations of low-significance compan- ion detections are ongoing and will appear in future papers inthis survey. Gemini LGS-AO
Seven candidate multiple systems from this work and threefrom Paper I and Paper II, again selected for their low de-tection significance, were re-imaged with the adaptive opticsassisted NIRI instrument (Hodapp et al. 2003) on the GeminiNorth telescope. Three targets were observed on 2015 July 31(UT) and seven targets were observed on 2015 August 27, us-ing Band 3 allocated time. Targets observed with Gemini aredetailed in Table 3. Observations were performed with theF /
32 camera, providing resolution of 21.9 mas pixel − acrossa field of view of 22 (cid:48)(cid:48) × (cid:48)(cid:48) . Total integration times were90 s in the K prime band across three dithered images, used toincrease dynamic range and allow sky subtraction. The com-mon striping pattern found in NIRI images was removed usingthe cleanir.py script provided by the Gemini sta ff . The imageswere flat fielded, bad pixel corrected, and sky subtracted. Thedistortion solution provided by the Gemini sta ff was used tocorrect the images for distortion. DATA REDUCTION
With the largest adaptive optics dataset yet assembled byRobo-AO, the data reduction process was automated as muchas possible for e ffi ciency and consistency. As in Paper Iand Ziegler et al. (2015), after initial pipeline reductions de-scribed in Section 3.1, the target stars were identified (Section Z iegler et al . Table 1
The specifications of the Robo-AO KOI surveyKOI targets 1629FWHM resolution ∼ . (cid:48)(cid:48)
15 (@600-750 nm)Observation wavelengths 600-950 nmField size 44 (cid:48)(cid:48) × (cid:48)(cid:48) Detector format 1024 pixelsPixel scale 43.1 mas / pixExposure time 90 secondsTargets observed / hour 20Observation dates 2012 July 16 –2015 June 12 Figure 3.
Location on sky of targeted KOIs from Paper I (L14), Paper II(B16), and this work (TW). The median coordinates of the targeted KOIs isdesignated by an ‘ × ’. A projection of the Kepler field of view is provided forreference.
Imaging Pipeline
The Robo-AO imaging pipeline (Law et al. 2009, 2014) re-duced the images: the raw EMCCD output frames are dark-subtracted and flat-fielded and then stacked and aligned usingthe Drizzle algorithm (Fruchter & Hook 2002), which alsoup-samples the images by a factor of two. To avoid tip / tiltanisoplanatasism e ff ects, the image motion was corrected byusing the KOI itself as the guide star in each observation. Target Verification
To verify that the star viewed in the image is the desiredKOI target, we created Digital Sky Survey cutouts of similarangular size around the target coordinates. Each image wasmanually checked to assure no ambiguity in the target starwith images with either poor performance or incorrect fieldsremoved. These bad images made up approximately 2% of allour images, and for all but 2 of the targets additional imageswere available.
Image Preparation
Figure 4.
Example of PSF subtraction on KOI-5762 with companion sep-aration of 0 . (cid:48)(cid:48)
34. The yellow circle marks the position of the primary star’sPSF peak. Both images have been scaled and smoothed for clarity. Success-ful removal of the PSF leaves residuals consistent with photon noise. The2 (cid:48)(cid:48) square field shown here is approximately equal to half the
Kepler pixelsize. The close companion to KOI-5762 was confirmed with NIRC2 / Keckimages, shown in Figure 7.
To facilitate the automation of the data reduction, centered8 . (cid:48)(cid:48) (cid:48)(cid:48) separation cuto ff for our companionsearch to detect all nearby stars that would blend with the tar-get KOI in a Kepler pixel.
PSF Subtraction
To identify close companions, a custom locally optimizedpoint spread function (PSF) subtraction routine based onthe Locally Optimized Combination of Images algorithm(Lafreni`ere et al. 2007) was applied to centered cutouts ofall stars. Detailed in Paper I, the code uses a set of twentyKOI observations, selected from the observations within thesame filter closest to the target observation in time, as refer-ence PSFs, as it is improbable that a companion would ap-pear at the same position in two di ff erent images. A locallyoptimized PSF is generated and subtracted from the originalimage, leaving residuals consistent with photon noise.This procedure was performed on all KOI images out to2 (cid:48)(cid:48) , and the results visually checked for companions. Figure 4shows an example of the PSF subtraction performance. ThePSF subtracted images were subsequently run through the au-tomated companion finding routine, as described in Section3.5. Companion Detection obo -AO
Kepler P lanetary C andidate S urvey III 5An initial visual companion search was performed redun-dantly by three of the authors. This search yielded a prelimi-nary companion list, and filtered out bad images.Continuing the companion search, we ran all imagesthrough a custom automated search algorithm, based on thecode described in Paper I. The algorithm slides a 5-pixel di-ameter aperture within concentric annuli centered on the tar-get star. Any aperture with > + σ outlier to the local noiseis considered a potential astrophysical source. These are sub-sequently checked manually, eliminating spurious detectionswith dissimilar PSFs to the target star and those having char-acteristics of a cosmic ray hit, such as a single bright pixel orbright streak. The detection significance of ‘secure’ compan-ions are listed in Tables 4 and 5.Many possible companions were visually identified but fellbeneath the formal 5 σ required for a discovery. Despite notreaching our formal significance level required for a discov-ery, previous results suggest that all but a small fraction arelikely real: Keck / NIRC2 observations have confirmed all 15‘likely’ detections in Paper I and all 38 re-observed ‘likely’companions in Paper II. The detection significance of these‘likely’ companions are listed in Tables 6 and 7.
Imaging Performance Metrics
The two dominant factors that a ff ect the image performanceof the Robo-AO system are seeing and target brightness. Anautomated routine was used to classify the image performancefor each target. Described in detail in Paper I, the code usesPSF core size as a proxy for image performance. Observa-tions were binned into three performance groups, with 31%fall in the low performance group, 41% in the medium perfor-mance group, and 28% in the high performance group.We determine the angular separation and contrast consis-tent with a 5 σ detection by injecting artificial companions, aclone of the primary PSF. For concentric annuli of 0 . (cid:48)(cid:48) σ magnitudes are averaged. For clarity,these average magnitudes for all radii measurements are fit-ted with functions of the form a ∗ sinh ( b ∗ r + c ) + d (where r is the radius from the target star and a, b, c and d are fittingvariables). Contrast curves for the three performance groupsare shown in Section 4 in Figure 5. Companion Characterization
Contrast Ratios
For wide, resolved companions with little PSF overlap, thecompanion to primary star contrast ratio was determined us-ing aperture photometry on the original images. The apertureradius was cycled in one-pixel increments from 1-5 FWHMfor each system, with background measured opposite the pri-mary from the companion (except in the few cases where an-other object falls near or within this region in the image). Pho-tometric uncertainties are estimated from the standard devia-tion of the contrast ratios measured for the various aperturesizes.For close companions, the estimated PSF was used to re-move the blended contributions of each star before aperturephotometry was performed. The locally optimized PSF sub-traction algorithm can attempt to remove the flux from com-panions using other reference PSFs with excess brightness in those areas. For detection purposes, we use many PSFcore sizes for optimization, and the algorithm’s ability to re-move the companion light is reduced. However, the compan-ion is artificially faint as some flux has still been subtracted.To avoid this, the PSF fit was redone excluding a six-pixel-diameter region around the detected companion. The largePSF regions allow the excess light from the primary star to beremoved, while not reducing the brightness of the companion.
Separation and Position Angles
Separation and position angles were determined from theraw pixel positions. Uncertainties were found using estimatedsystematic errors due to blending between components. Typ-ical uncertainty in the position for each star was 1-2 pixels.Position angles and the plate scale were calculated using adistortion solution produced using Robo-AO measurementsfor the globular cluster M15. Companion Spectral Types
The approximate spectral type of the detected companions,assuming that they are bound to the primary and all stars aremain sequence dwarfs, were estimated using an SED model(Kraus & Hillenbrand 2007) and the estimated stellar e ff ectivetemperatures reported on the NASA Exoplanet Archive. Withthe LP600 band closely matching the Kepler bandpass, themagnitude di ff erences between the primary star and nearbystars were converted to i (cid:48) -band when necessary using the lin-ear correlation found by Lillo-Box et al. (2014): ∆ m i (cid:48) = . · ∆ m LP (1)In addition, we estimate the latest spectral type companionconsistent with a 5 σ detection for each observed target basedon the typical contrast curve for the three image performancegroups (see Section 3 . ∼
12% by Ciardi et al. (2011). In addition, the use of a lin-ear correlation in converting between passbands will result inan error with varying spectral types. We estimate this error bycalculating the flux of F0V to M5V stars (Pickles 1998) in theLP600 and i (cid:48) -band inlcuding quantum e ffi ciencies and instru-mental e ff ects (see Figure 2 in Paper I). The maximum di ff er-ence between the flux of spectral types in the two passbandsresults in an error of ∼ DISCOVERIES
Of the 1629 KOI targets observed, 206 are apparent inmultiple star systems for a nearby star fraction within 4 (cid:48)(cid:48) of12.6% ± . We also found 15 triple systems for a tripletfraction of 0 . + . − . % , and 1 quadruple system for a quadru-plet fraction of 0 . + . − . % . Cutouts of the triple and quadru-ple systems are shown in Figure 6. One quarter (25.8%) of thecompanions would only be observable in a high-resolutionsurvey ( < . (cid:48)(cid:48) < . (cid:48)(cid:48)
0) for many seeing limited surveysto accurately measure binary properties (e.g. contrast ratios).The detected companion separations and contrast ratios are S. Hildebrandt (2013, private communication) Error based on Poissonian statistics (Burgasser et al. 2003) Error based on binomial statistics (Burgasser et al. 2003) Z iegler et al . Figure 5.
Separations and magnitude di ff erences of the detected companions in Paper II and this work, with the color and shape of each star denoting theassociated typical low-, medium- and high-performance 5 σ contrast curve during the observation (as described in Section 3.6). plotted in Figure 5, along with the calculated 5 σ detectionlimits as detailed in Section 3 .
6. Cutouts of all multiple starsystems are shown in Figures 18, 19, 20, and 21. For compan-ions within 2 . (cid:48)(cid:48)
5, measured properties are detailed in Tables 4and 6. For companions outside 2 . (cid:48)(cid:48) . (cid:48)(cid:48)
0, measuredproperties are detailed in Tables 5 and 7.We confirmed six companions to eight Robo-AO detectionswith NIRC2 and AO on Keck-II (Wizinowich et al. 2000). Inaddition, two new companions were found around KOIs 2554and 3020. These targets were selected for followup becauseof their faintness and / or closely separated detected compan-ion. Low-sigma, visually detected companions to KOIs 1873and 5257 were not detected. These non-detected companionsare possibly a result of non-common path aberrations, as de-scribed in Section 5.1 of Paper II. These spurious detectionsall have similar separations and position angles with respectto the target star, facilitating their identification and manualremoval. The PSF subtraction routine usually does not re-move these false companions, as another star exhibiting theNCP error is unlikely to be within the set of twenty referenceimages. The Keck-II observations are listed in Table 2, withthe measured separations and position angles of the confirmedcompanions using Keck-II images listed in Tables 4 and 6,and the follow-up images are shown in Figure 7.We confirmed five companions to seven KOIs observed inthis paper with NIRI and AO on Gemini North. We did notdetect a possible companion to KOI-2198 that was visuallydetected, manifesting as an elongated PSF in the Robo-AOimage. We observed three KOIs targeted in Paper I (KOI-327) and Paper II (KOIs 2833 and 4301) which displayednon-common path error aberrations. No companions were ob-served to these three targets in the follow-up observations. Anew companion outside our separation cuto ff ( ρ = . (cid:48)(cid:48)
24) wasobserved nearby KOI-4131. The Gemini observations arelisted in Table 3, and the follow-up images are shown inFigure 8.
Table 2
Full Keck-AO Observation ListKOI m v ObsID Companion? ∆ K p ± ± ± a yes 2.96 ± b ± c yes 5.01 ± d ± ± a Companion at ρ = . (cid:48)(cid:48) b New companion at ρ = . (cid:48)(cid:48) c Companion at ρ = . (cid:48)(cid:48) d New companion at ρ = . (cid:48)(cid:48) Comparison to Other Surveys
Two detected companions (KOI-326 and KOI-841) in oursurvey were previously found in Lillo-Box et al. (2012), whoobserved 98 KOIs using the AstraLux Lucky Imaging sys-tem on the 2.2m telescope at the Calar Alto Observatory.Lillo-Box et al. (2014) also previously detected companionsto KOI-3263, 3649, and 3886 in a survey of 174 KOIs. Adamset al. (2012) and Adams et al. (2013) observed 87 and 13KOIs, respectively, with the instruments ARIES and PHAROon the MMT and Palomar telescopes, respectively. They de-tect companions to KOI-126 and 266 that are fainter than oursurvey sensitivity. Observing 87 KOIs with ARIES at theMMT, Dressing et al. (2014) previously detected companionsto KOI-2813 and KOI-3111 and also detected a companion toKOI-266 ( ∆ m K s = Hubble Space Telescope (HST) with ∆ m K p of 2.4 obo -AO Kepler P lanetary C andidate S urvey III 7
Figure 6.
Normalized log-scale cutouts of 16 KOIs with multiple companions with separations < (cid:48)(cid:48) resolved with Robo-AO. The angular scale and orientation(displayed in the first frame) is similar for each cutout, and circles are centered on the detected nearby stars. Three targets (KOIs 3214, 3463, and 6800) have apossible third companion, marked with arrows, outside our 4 (cid:48)(cid:48) separation cuto ff , as described in Section 5 . . and 6.0 and separations of 0 . (cid:48)(cid:48)
11 and 3 . (cid:48)(cid:48)
31, respectively, whichwere outside the detection limits of our Robo-AO image.Wang et al. (2015a) observed 84 KOIs using the PHARO andNIRC2 instruments at Palomar and Keck, respectively, withone discovered companion (KOI-3678) appearing in our sur-vey. Two of our targets (KOI-1411 and KOI-3823) have com-panions detected by Wang et al., both with ∆ m K >
5, whichfall outside our detection sensitivity. Wang et al. (2015b) ob-served 73 multiple transiting planet KOI systems at Palomarand Keck, with the only overlapping system being a compan-ion observed near KOI-1806 which we did not detect. Thecompanion to KOI-1806, measured by Wang et al. (2015b) as ∆ K = . (cid:48)(cid:48)
43 separation, is well within out survey sen-sitivity, and the reason for the non-detection is unclear. Thereported companion is also not visible in UKIRT images, al- though it would be detectable. We detected companions toKOI-126 and 200 not detected by Howell et al. (2011); bothcompanions are within the stated sensitivity limits for their re-spective targets, so the reason for the earlier non-detection isunclear. None of our nearby-star detections overlap with thediscoveries of Everett et al. (2015).Kraus et al. (2016) observed 382 KOIs with AO on theKeck-II telescope. They detected single companions to KOI-255, 1908, 2705, and 2813, and both companions to KOI-1201 that were detected in our survey. They also detectedsingle companions to KOI-1298, 1681, 2179 2453, and 2862,and double companions to KOI-1361 and 2813, that all falloutside of our reported sensitivity.Kolbl et al. (2015) searched for the blended spectra of KOIswith secondary stars within ∼ . (cid:48)(cid:48) iegler et al . Figure 7.
Normalized log-scale cutouts of 8 KOIs observed with the NIRC2 instrument on Keck-II, as described in Section 2.2.2. The angular scale andorientation (displayed in the first frame) is similar for each cutout, and circles are centered on the detected nearby stars.
Table 3
Full Gemini Observation ListKOI m v ObsID Companion? ∆ K p
327 13.1 2015 Aug 272198 12.8 2015 Aug 272833 12.8 2015 Aug 274131 13.2 2015 Jul 31 yes 4.41 ± a yes 4.96 ± b ± ± c yes 4.11 ± d ± a Companion at ρ = . (cid:48)(cid:48) b New companion at ρ = . (cid:48)(cid:48) c Companion at ρ = . (cid:48)(cid:48) d Companion at ρ = . (cid:48)(cid:48) cal echelle spectra of 1160 California Kepler
Survey KOIs.Of the 63 KOIs the authors found with evidence of a sec-ondary star, we found companions to seven (KOIs 1137, 2813,3161, 3415, 3471, 4345, 4713) and did not detect companionsto eight (KOIs 1121, 1326, 1645, 3515, 3527, 3605, 3606,3853). The companions we did not detect likely lie at smallseparations inside the limits of our survey sensitivity. Two ofour companions (KOIs 1137 and 3415) fall within their cal-culated flux ratio uncertainty and within their ∼ . (cid:48)(cid:48) ρ > (cid:48)(cid:48) )nearby star detections are noted on the Kepler
CommunityFollow-up Observing Program (CFOP) using J-band, ∼ (cid:48)(cid:48) seeing-limited imaging from United Kingdom InfraRed Tele-scope (UKIRT) (Lawrence et al. 2007). However, with high-acuity imaging to resolve blended companions, providinggreater precision photometry, and a filter that better simulatesthe Kepler bandpass, the Robo-AO survey can better evaluate the e ff ect of the companion on the observed transit signal. Multiplicity and Other Surveys
There have been multiple past high-resolution surveys ofKOIs performed, allowing our results to be put into contextwith the overall community follow-up program. A compar-ison of the observed nearby-star rates from various surveyswith di ff ering methodologies may also provide convergenceon the intrinsic multiplicity rate of planet hosting stars. Withvarying sensitivities between surveys, we use a lower sepa-ration cuto ff than in this paper for a uniform comparison be-tween surveys. This also has the added benefit of using onlythe nearest stars that have the highest probability of associa-tion. An exact comparison between surveys is still hindered,however, by the use of dissimilar instruments, passbands, andtarget selection criteria; in comparing results in this sectionwe attempt to highlight major di ff erences when comparingmultiplicity rates, however we caution that in each case thereare inherent biases in the coverage of the di ff erent surveyswhich requires detailed analysis not covered in this work.We find that 6.8% of KOIs have nearby stars within 2 (cid:48)(cid:48) , inagreement with other visible light surveys: 6.4% in Paper I,8.2% in Paper II, and 6.4% (Howell et al. 2011). Horch et al.(2014) found 7.0% of KOI targets had nearby stars within 1 (cid:48)(cid:48) separation, a range where we showed a 3.4% nearby star rate.Horch et al. (2014) do not report their target list, so it is notpossible to identify the source of this discrepancy. It is pos-sible that this is a result of our target selection of every KOI,resulting in a dimmer overall sample than surveys which pri-oritize brighter targets. The targets in this paper have a me-dian K p , med = K p , med = K p , med = K p < p , med = p , med = Kepler targets mainly are between 11th and14th magnitude. There are several reasons a brighter overalltarget list will inflate binarity rates: the target stars are intrin-sically more luminous, which results in more physically as-sociated companion stars as binarity correlates with luminos-ity (Duchˆene & Kraus 2013); the target stars are less distant,so physically associated companion of a given spectral typeis brighter, thus easier to detect; brighter stars tend to have obo -AO
Kepler P lanetary C andidate S urvey III 9
Table 4
Secure Detections of Objects within 2 . (cid:48)(cid:48) Kepler
Planet CandidatesKOI m i (cid:48) ObsID Filter Det. Significance Separation P.A. Mag. Di ff . Approx. Comp. Prev. High Res. Prev. Low Res. False Positive? a N KOI b (mag) σ ( (cid:48)(cid:48) ) (deg.) (mag) Spectral Type c Detection? Detection?163 13.3 2012 Jul 18 LP600 17 1.22 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± i (cid:48)
13 0.50 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± Notes. — References for previous detections are denoted using the following codes: Dressing et al. 2014 (D14), Lillo-Box et al. 2014 (LB14),Kraus et al. 2016 (K16), Wang et al. 2015a (W15), visible in United Kingdom InfraRed Telescope images (UKIRT), high angular resolutionimages available on
Kepler
Community FollowUp Observing Program (CFOP). a Probability that planetary transit signal is a false positive based on
Kepler data. b Number of planet candidates detected orbiting KOI. c Estimation method described in Section 3 . . d From Keck follow-up, described in Section 4. deeper detectable contrast ratios.The disparity in multiplicity between papers in the Robo-AO survey was explored in Section 6 of Paper II as a pos-sible result of the bias in the KOI selection process betweendata releases, with the median observed KOI in Paper II lo-cated nearer the Galactic plane than in Paper I. KOIs near theGalactic plane lie in denser stellar fields, increasing the likeli-hood of unassociated nearby stars with the separation cuto ff .Plotting the Kepler field of view with our targeted KOIs in Figure 3, the median position of KOIs in this work is closerto the center of the field than in Paper II, and further from theGalactic plane than Paper I or Paper II.Surveys in the NIR find higher multiplicity rates within 2 (cid:48)(cid:48) :13% (Dressing et al. 2014), 17% (Adams et al. 2012), 20%(Adams et al. 2013). This is likely caused by many compan-ions being cool, red dwarf stars that are faint in the optical(Ngo et al. 2015), and deeper, higher angular resolution imag-ing.0 Z iegler et al . Table 5
Secure Detections of Objects outside 2 . (cid:48)(cid:48) . (cid:48)(cid:48) Kepler
Planet CandidatesKOI m i (cid:48) ObsID Filter Det. Significance Separation P.A. Mag. Di ff . Approx. Comp. Prev. High Res. Prev. Low Res. False Positive? a N KOI b (mag) σ ( (cid:48)(cid:48) ) (deg.) (mag) Spectral Type c Detection? Detection?255 14.5 2014 Jul 17 LP600 5.8 3.41 ± ± ± ± ± ± ± ± ± + ± ± ± ± ± ± + ± ± ± + ± ± ± i (cid:48) ± ± ± ± ± ± ± ± ± ± ± ± + ± ± ± ± ± ± ± ± ± ± ± ± + ± ± ± + ± ± ± ± ± ± ± ± ± Notes. — References for previous detections are denoted using the following codes: Kraus et al. 2016 (K16), visible in United KingdomInfraRed Telescope images (UKIRT), high angular resolution images available on
Kepler
Community FollowUp Observing Program (CFOP),companions visible in UKIRT and with 2MASS designations (J*). a Probability that planetary transit signal is a false positive based on
Kepler data. b Number of planet candidates detected orbiting KOI. c Estimation method described in Section 3 . . Figure 8.
Normalized log-scale cutouts of 10 KOIs observed with the NIRI instrument on Gemini North, as described in Section 2.2.3. The angular scale andorientation (displayed in the first frame) is similar for each cutout, and circles are centered on the detected nearby stars. DISCUSSION
In this section, we delve further into the combined datasetsof Paper II and this work to further explore the implications ofstellar multiplicity on the planetary candidates (Section 5.1),expand on the planetary candidates found in higher order mul-tiple systems or orbiting within the habitable zone (Section5.2), and search for insight into the role that multiple stel-lar bodies play on planetary formation and evolution (Section5.3).
Implications for Kepler Planet Candidates
When a close companion is detected near a KOI host star,there are several potential implications. If the planet does in-deed transit the purported target star, the consequences maybe relatively mild: the planet’s radius will be slightly largerthan had previously been thought—at most by a factor of √ Kepler stellar cat-alog are based on broad-band photometry assuming that theyare single, the derived stellar radii may well be incorrect if thesystem actually contains multiple stars. Re-fitting the stellarproperties of all the companion stars, as well as for the
Kepler target stars accounting for the presence of the companions,is beyond the scope of this work, but will be addressed in afuture paper in this series.Finally, if a KOI system has multiple transiting planets de-tected, it might be the case that the planets are distributedaround multiple stars in the system. KOI-284 / Kepler-132 isa good example of such a case (Fabrycky et al. 2012; Lissaueret al. 2014): its multiple planets would be unstable if they all obo -AO
Kepler P lanetary C andidate S urvey III 11
Table 6
Likely Detections of Objects within 2 . (cid:48)(cid:48) Kepler
Planet CandidatesKOI m i (cid:48) ObsID Filter Det. Significance Separation P.A. Mag. Di ff . Approx. Comp. Prev. High Res. Prev. Low Res. False Positive? a N KOI b (mag) σ ( (cid:48)(cid:48) ) (deg.) (mag) Spectral Type c Detection? Detection?126 13.1 2015 Jun 08 LP600 3.3 0.34 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± i (cid:48) ± ± ± i (cid:48) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± i (cid:48) ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± d ± d ± ± ± ± i (cid:48) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± Notes. — References for previous detections are denoted using the following codes: Lillo-Box et al. 2012 (LB12), Lillo-Box et al. 2014(LB14), Kraus et al. 2016 (K16), visible in United Kingdom InfraRed Telescope images (UKIRT). a Probability that planetary transit signal is a false positive based on
Kepler data. b Number of planet candidates detected orbiting KOI. c Estimation method described in Section 3 . . d From Keck follow-up, described in Section 4. iegler et al . Table 7
Likely Detections of Objects outside 2 . (cid:48)(cid:48) . (cid:48)(cid:48) Kepler
Planet CandidatesKOI m i (cid:48) ObsID Filter Det. Significance Separation P.A. Mag. Di ff . Approx. Comp. Prev. High Res. Prev. Low Res. False Positive? a N KOI b (mag) σ ( (cid:48)(cid:48) ) (deg.) (mag) Spectral Type c Detection? Detection?51 13.4 2013 Jul 25 LP600 2.6 3.51 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± + ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± i (cid:48) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± + ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± + ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± Notes. — References for previous detections are denoted using the following codes: Lillo-Box et al. 2012 (LB12), Dressing et al. 2014 (D14),Kraus et al. 2016 (K16), visible in United Kingdom InfraRed Telescope images (UKIRT), companions visible in UKIRT and with 2MASSdesignations (J*). a Probability that planetary transit signal is a false positive based on
Kepler data. b Number of planet candidates detected orbiting KOI. c Estimation method described in Section 3 . . obo -AO Kepler P lanetary C andidate S urvey III 13orbited a single star, but it turns out to be a close visual bi-nary, with the only sensible interpretation being that some ofthe planets transit one star and some transit the other. Whilesuch “split multiple” systems are predicted to be relativelyrare among the population of
Kepler multiple stellar systems(Fabrycky et al. 2012), any multi-planet system with a closecompanion has a higher chance of being split, and thus de-serves close consideration. Barclay et al. (2015) presents amodel of how such systems might be analyzed, investigatingthe KOI-1422 / Kepler-296.
Particularly Interesting Systems
Several KOIs with detected companions are of particularinterest, either for displaying unusual system characteristics,rare false-positive scenarios, or planetary attributes that sat-isfy habitability requirements.
Possible Quadruple Systems
KOI-5327 hosts a 2.24 R ⊕ planetary candidate on a 5.4 dayorbit. We detect two nearby stellar companions, with angu-lar separations of 1 . (cid:48)(cid:48)
88 and 3 . (cid:48)(cid:48)
63 and magnitude di ff erencesof 3.43 and 3.92, respectively. A possible fourth componentof the system lies at 3 . (cid:48)(cid:48)
96 and is 0.12 mags brighter than theKOI target. Further multiple passband observations and radialvelocity measurements are needed to understand the hierar-chy of this system. In the full 44 (cid:48)(cid:48) square image, a total of8 stars appear, including the target and possible companions.With nearly equal brightness, the third companion has a highprobability of being associated. With few stars found in thefull field, it is unlikely that any unassociated stars would befound within 4 (cid:48)(cid:48) of the KOI. The likelihood that the other twostars are in fact bound is 97%. If physical association is con-firmed for all four components, KOI-5327 would be the thirdknown planet residing in a quadruple star system (Schwambet al. 2013; Roberts et al. 2015). Following the analysis ofSection 5.1 in Paper I, with the planet assumed to orbit thebright target star, the updated planetary radius estimate forthe planetary candidate with all three stars in the aperture is3.3 R ⊕ . Without the 0.12 mags brighter star in the photomet-ric aperture, the updated radius estimate is 2.3 R ⊕ . The secondscenario detailed in Paper I, with the planet orbiting one of thefainter companions, will be further explored in future papersin this survey for all detected companions. KOI-4495 , first detected in Paper II, has three nearby stars,with angular separations of 3 . (cid:48)(cid:48)
04, 3 . (cid:48)(cid:48)
06, and 3 . (cid:48)(cid:48)
41 and mag-nitude di ff erences of 4.73, 3.90, and 2.68, respectively. Thesystem hosts a planetary candidate with period of 5.92 daysand estimated radius of 1.49 R ⊕ . The system lies in a rela-tively dense stellar field, thus it is probable that at least one ofthe stars is an unassociated asterism. The Robo-AO discov-ery image is available in Figure 5 of Paper II. With all threestars in the photometric aperture diluting the transit signal,and assuming the planet does indeed orbit the bright star, theupdated planetary radius estimate is 1.6 R ⊕ . KOI-3214 hosts planetary candidates with radii of 2.59 R ⊕ and 2.02 R ⊕ on 11.5 and 25.1 day orbits, respectively. We de-tect two nearby stellar companions, with angular separationsof 0 . (cid:48)(cid:48)
49 and 1 . (cid:48)(cid:48)
41 and magnitude di ff erences of 0.73 and 2.50,respectively. Outside our 4 (cid:48)(cid:48) separation cuto ff , another 5.33mag dimmer star appears at and 4 . (cid:48)(cid:48)
34. With multiple starsin the same
Kepler pixel, the probability of an eclipsing bi-nary resulting in a false planetary transit signal is increased.KOI-3214 lies in a relatively sparse stellar field, with only 6 additional stars in the full 44 (cid:48)(cid:48) square image, including thetarget and possible companions. The probability based on thebackground star density that all three stars are bound is ap-proximately 98%. Assuming the planets orbit the brighteststar, the two close stars likely dilute the observed transit sig-nal, leading to updated planetary radii estimates of 3.3 R ⊕ and2.6 R ⊕ for the planet candidates on orbits with periods of 11.5and 25.1 days, respectively. KOI-3463 hosts a 1.3 R ⊕ planetary candidate on a 32.5 dayorbit. We detect two nearby stellar companions, with angularseparations of 2 . (cid:48)(cid:48)
74 and 3 . (cid:48)(cid:48)
67 and magnitude di ff erences of4.79 and 4.41, respectively. Just outside our 4 (cid:48)(cid:48) separation cut-o ff , another 2.44 mag dimmer star appears at 4 . (cid:48)(cid:48)
11. KOI-3463lies in a relatively dense stellar field, with at least 16 stars inthe full 44 (cid:48)(cid:48) square image, including the target and possiblecompanions. The probability based on the background stardensity that all three stars are bound is approximately 86%. Ifthe planet candidate orbits the bright star, the additional twonearby stars in the photometric aperture only marginally di-lute the transit signal, leading to an updated planetary radiusestimate of 1.3 R ⊕ . KOI-6800 hosts a 27.5 R ⊕ planetary candidate on a 2.5 dayorbit. We detect two nearby stellar companions, with angularseparations of 2 . (cid:48)(cid:48)
62 and 3 . (cid:48)(cid:48)
11 and magnitude di ff erences of5.10 and 5.41, respectively. Outside our 4 (cid:48)(cid:48) separation cuto ff ,another 5.27 mag dimmer object appears at 4 . (cid:48)(cid:48)
13, althoughUKIRT photometry suggests that this is highly likely ( > (cid:48)(cid:48) square image of KOI-6800, 9 stars are visible, including the target and possiblecompanions. The probability based on the background stardensity that all three stars are bound is approximately 97%.The two dim nearby stars within the photometric apertureonly slightly increases the estimated planetary radius to 27.7 R ⊕ , assuming the planet orbits the brightest star. If the planetcandidate orbits one of the fainter stars, the corrected plane-tary radius would be large enough to make it highly probablethe transiting event is in fact a background eclipsing binary.The Robo-AO images of the four possible quadruple sys-tems from this work are displayed in Figure 6. Habitable Zone Candidates
The discovery of habitable exoplanets is a major goal of the
Kepler mission, and an accurate knowledge of the host star’sproperties is required to establish unambiguously whether anexoplanet possesses the two habitability conditions – rockyand in a location where water can be found in a liquid state onthe surface (habitable zone; HZ). The exact requirements forhabitability are still debated (Kasting et al. 1993; Selsis et al.2007; Seager 2013; Zsom et al. 2013), however it has beenshown that the transition between “rocky” and “non-rocky”occurs rather sharply at R P = R ⊕ (Rogers 2015). For thisanalysis, we will use a large cuto ff of 4 R ⊕ , as the presenceof a stellar companion may dramatically alter the estimatedradius, and even a gaseous planet in the HZ may host a rockyexomoon (Heller 2012). Overall, the existence of an unknownstellar companion within the same photometric aperture as theKOI will increase the calculated radius of the planet, as theobserved transit signal will be diluted by the constant light ofthe nearby star.In Paper II and this work, we detected companions to 26KOIs which host planetary candidates with equilibrium tem-peratures, from the NEA, in the HZ range (273 K ≤ T eq ≤ < R ⊕ , displayed in Table 8. All are newly de-tected in this survey. Corrected planetary radii estimates are4 Z iegler et al . Table 8
Habitable Zone Candidates with Robo-AO Detected CompanionsPlanet Period R p , i a R p , c b Equil. Temp. Sep ∆ mcandidate (d) (R ⊕ ) (R ⊕ ) (K) ( (cid:48)(cid:48) ) (mag)227.01 c c c c c c c c a Initial planetary radius estimate b Corrected planetary radius estimate c Detected in Paper II of this survey. included, as described in Section 5.1 of Paper I, with the as-sumption that the planet orbits the bright star.KOI-2926 hosts two planetary candidates within the HZ,and KOI-6745 is a possible triple system hosting a planet inthe HZ. The equilibrium temperature calculation is based onan estimate of the stellar e ff ective temperature of the host star,thus if the planet orbits the dimmer companion it is unlikelyto be in the HZ.KOI-1503 hosts a planetary candidate with initial dilutedradius estimate of 3.79 R ⊕ in a 0.51 AU orbit. If the planetorbits the primary star, the corrected radius of the planet is4.23 ± R ⊕ , decreasing the probability that it is rocky.KOI-5101, a sun-like star, hosts a near-Earth analog, with acalculated radius 64% larger than Earth and an orbit of 1.12AU. With a 3.33 magnitude dimmer companion at 1 . (cid:48)(cid:48)
22, theKOI is likely a 1.68 R ⊕ rocky planet if it orbits the primary. Stellar Multiplicity and Kepler Planet Candidates
We detect 206 planetary candidate hosts with nearby starsfrom 1629 targets, for an overall multiplicity fraction of12.6% ± ∼ . (cid:48)(cid:48) . (cid:48)(cid:48) ∆ m ≤ Figure 9.
The cumulative distribution of nearby stars within a given sep-aration from our observations in Paper II and this work, and the expecteddistribution from a set of the same number of unassociated stars. For allseparations, the observed number of companions we detected is above theexpected number if all stars were unassociated. evolution models.Any individual companion found may not be physicallybound, however we expect a small number of unassociatedasterisms within our complete set of observed targets. An ar-gument for the majority of nearby stars being associated isderived from the observed distribution of companion sepa-rations: if all companions were unassociated background orforeground stars, we would expect a quadratic distribution ofcompanions (i.e., ∼ × the number of objects at 4 (cid:48)(cid:48) as at 2 (cid:48)(cid:48) ).Instead we find a near linear distribution. The dissimilaritybetween the observed distribution and the distribution of allunassociated objects is shown in Figure 9. In addition, a re-cent follow-up study with the NIRC2 instrument on the Keck-II telescope (Atkinson et al. 2016) observed 84 KOI systems,finding that at least 14 . + . − . % of companions within ∼ (cid:48)(cid:48) areinconsistent with being physically associated based on multi-band photometric parallax. We therefore expect the overallmultiplicity trends to remain relatively unchanged when theunassociated objects are removed.A summary and analysis paper in the Robo-AO survey willinvestigate the multiplicity properties of Kepler candidates inmore detail, including quantifying the e ff ects of associationprobability and incompleteness.All stellar and planetary properties for the KOIs in this sec-tion were obtained from the cumulative planet candidate list atthe NASA Exoplanet Archive and have not been correctedfor possible dilution due to the presence of nearby stars. Stellar Multiplicity and KOI Number
The early and late public releases of KOIs (Borucki et al.2011c; Batalha et al. 2013; Burke et al. 2014; Coughlin et al.2015) could conceivably have a built-in bias, either astrophys-ical in origin or as a result of the initial vetting process by the
Kepler team. This bias might appear as a variation in multi-plicity with respect to KOI number. With a target list of KOIsin Paper II and this work widely dispersed in the full KOIdataset, we can search for such a trend. The fraction of KOIswith companions as a function of KOI number, as displayedin Figure 10, shows a sharp decrease at approximately KOI-5000. We find KOI numbers less than 5000 have a nearby starfraction of 16.1% ± ± σ disparity.The exact mechanism for this is unclear, however this may http://exoplanetarchive.ipac.caltech.edu/ obo -AO Kepler P lanetary C andidate S urvey III 15
Figure 10.
Multiplicity fraction within 4 (cid:48)(cid:48) of KOIs as a function of KOI num-ber. A 2.9 σ decrease in the fraction of nearby stars between KOIs numberedless than 5000 and greater than 5000 is apparent. Figure 11.
Fraction of KOIs with detected nearby ( ≤ (cid:48)(cid:48) ) stars as a functionof stellar e ff ective temperature. be a result of better false positive detection in the later datareleases due to automation of the vetting process (Mullallyet al. 2015). There is no significant corresponding variationin the separations or contrasts of stellar companions betweenthe two populations. Stellar Multiplicity Rates and Host-star TemperatureRevisited
It has been well established that stellar multiplicity corre-lates with stellar mass and temperature (Duchˆene & Kraus2013). In Paper I, it was found at low significance that thistrend appears to also be true for the observed KOIs. Ngoet al. (2015) found in a sample of stars hosting close-in gi-ant planets that, with 2.9 σ significance, stars hotter than 6200K have a companion rate two times larger than their coolcounterparts. We find in the combined target sample of Pa-per II and this work that 14.7% ± ± Stellar Multiplicity and Multiple-planet Systems Revisited
Figure 12.
The multiplicity fraction within 4 (cid:48)(cid:48) of KOIs hosting detectedsingle- and multiple-planetary systems.
Multiple star systems are thought to more commonly hostsingle transiting planets than multiple planet systems. Per-turbations from the companion star will change the mutualinclinations of planets in the same system (Wang et al. 2014),therefore a lower number of multiple transiting planet systemsare expected to have stellar companions. Multiple planet sys-tems are also subject to planet-planet e ff ects (Rasio & Ford1996; Wang et al. 2015a).In Paper I, we found a low-sigma disparity in multiplic-ity rates between single- and multiple-planet systems, withsingle-planet systems exhibiting a slightly higher nearby starfraction. With our combined sample from Paper II and thiswork, we revisit this result with over three times more tar-gets. We find a slightly higher nearby star fraction for multipleplanetary systems, displayed in Figure 12. A Fisher exact testgives an 8.7% probability of this being a chance di ff erence.With the expectation, given the e ff ects of stellar perturbationsand the higher false positive rate for single star systems, of ahigher nearby-star fraction for single-planet candidate hostingstars, even this low-significance result is surprising. A possi-ble explanation is that the additional stellar body in the systemis causing orbital migration of outer planets, moving them toshorter period orbits where Kepler has higher sensitivity totransit events. Also, multiple star systems have at least twiceas many stars that could host transiting planets, resulting ina higher probability of observing multiple planetary transits.Lastly, with relatively low-significance, this result could alsobe a consequence of the “look-elsewhere” e ff ect inherent toany multi-comparison study (Gross & Vitells 2010); with theparameter space explored in this section, a result of this sig-nificance is expected to arise approximately 50% of the timeout of per chance.Wang et al. (2015b) studied the influence of stellar com-panions on multiple-planet systems, finding a 3.2 σ deficit inmultiplicity rate in multi-planet systems compared to a con-trol sample of field stars. However, they also found no signif-icant disparity in multiplicity rates between single- and multi-planet systems. Stellar Multiplicity and Close-in Planets Revisited
The presence of stellar companions is hypothesized toshape the formation and evolution of planetary systems. Over-all, there is evidence that planetary formation is disruptedin close binary systems (Fragner et al. 2011; Roell et al.2012). The third body in the system can lead to Kozai oscil-lations causing orbital migration of the planets (Fabrycky &Tremaine 2007; Katz et al. 2011; Naoz et al. 2012) or tilt thecircumstellar disk (Batygin 2012). Smaller planets are also6 Z iegler et al . Figure 13. σ uncertainty regions for the binarity fraction as a function ofKOI period for two di ff erent planetary populations. Figure 14. σ uncertainty regions for the binarity fraction as a function ofKOI period for two di ff erent planetary populations, with only companionswith separations < . (cid:48)(cid:48) more prone to the influence of a stellar companion because ofweaker planet-planet dynamical coupling (Wang et al. 2015a).These dynamical interactions between small and large planetsin the same system tend to di ff erentially eject small planetsmore frequently than large planets (Xie et al. 2014). The pres-ence of a stellar companion increases the frequency of theseinteractions, leading to higher loss of small planets. Conse-quently, we would expect a correlation between binarity andplanetary period for di ff erent sized planets.We previously reported a low-significance result of stellarthird bodies increasing the rate of close-in giant planets, pos-sible evidence of orbital migration of the planet caused bythe stellar companion. We revisit the discussion and analysisfrom Paper I in search of this correlation using the results ofPaper II and this work. This analysis splits the “small” and“giant” planets at the arbitrary value of Neptune’s radius (3.9R ⊕ ). The exact value does not significantly a ff ect the resultsas just 11 of the detected systems have planetary radii within20% of the cuto ff value, with 1635 small and 395 giant planetsin total.In Figure 13 the fraction of Kepler planet candidates withnearby stars is shown, with planets grouped into two di ff erentsize ranges. We again see a small increase in the nearby starfraction for giants with periods <
15 days, however the > σ spike at periods of 2-4 days seen in Paper I is not present. Ifour sample is reduced to correspond to the separation rangeof Paper I ( ρ< . (cid:48)(cid:48)
5) in Figure 14, again no binarity spike atperiods <
10 days is apparent.Binning our targets into four population groups in Figure 15suggests no significant di ff erence in the binarity rate of shortperiod giants. We also attempt to decrease the occurrence Figure 15.
Multiplicity fraction of KOIs with four planetary populations,with all contrast ratios and separations ≤ (cid:48)(cid:48) . A planet is considered giantif its radius is equal to or larger to that of Neptune (3.9 R ⊕ ). Multi-planetsystems can be assigned to multiple populations. of unassociated asterisms by only using close, bright com-panions ( ∆ m ≤ ρ ≤ . (cid:48)(cid:48) ff erences between the four populations is evident.Any real disparity between the populations would also man-ifest in the physical orbital semi-major axis, which is relatedto the observable periods by the stellar mass. In Figure 17we plot the two population’s binarity fraction as a functionof the calculated semi-major axis of the planetary candidatesbetween 0.01 and 1.0 AU. No significant giant planet binarityspike is observed as in the periods plot.Our updated study using the targets in Paper II and thiswork suggests that the presence of a second stellar body inplanetary systems does not appreciably a ff ect the number ofclose-in giant planets. This agrees with the analysis of Wanget al. (2015a) who find a relatively uniform multiplicity ratefor planets with short and long periods. They note that ourprevious tentative result may have been due to short-periodgiants with brighter stellar companions in the visible biasingour detections. Subject to the same potential biases, the largersurvey in this analysis does not indicate a period-multiplicitycorrelation for the two planetary populations, suggesting thatour previous low-sigma result may have instead been an arti-fact of small-number statistics.Kraus et al. (2016) find a 6.6 σ deficit in binary stars withseparation ρ<
50 AU in KOIs compared to field stars, againsuggesting that close-in stellar companions disrupt the forma-tion and / or evolution of planets, as had been previously hy-pothesized (Wang et al. 2014). Indeed, a quarter of all solar-type stars in the Milky Way are disallowed from hosting plan-etary systems due to the influence of binary companions.Some evidence remains, however, that stellar binarity mayencourage the presence of hot Jupiters. A recent NIR survey(Ngo et al. 2015) of exoplanetary systems with known close-in giants finds that hot Jupiter hosts are twice as likely as fieldstars to be found in a multiple star system, with a significanceof 2.8 σ . However, the binarity rates of systems containinghot Jupiters remains unclear: 12% (Roell et al. 2012), 38%(Evans et al. 2016), 51% (Ngo et al. 2015).We will revisit this discussion in the last paper in this serieswhere we will combine the full Robo-AO KOI survey dataset. CONCLUSION obo -AO
Kepler P lanetary C andidate S urvey III 17
Figure 16.
Multiplicity fraction of KOIs with four planetary populations,with only companions with ∆ m ≤ ≤ . (cid:48)(cid:48)
5, removing the faintnearby stars that are less likely to be physically associated.
Figure 17. σ uncertainty regions for the binarity fraction as a function ofKOI semi-major axis between 0.01 and 1.0 AU for two di ff erent planetarypopulations. We observed 1629
Kepler planetary candidates with theRobo-AO robotic laser adaptive optics system. We detected206 planetary candidates with nearby stars, implying an over-all nearby-star probability of 12.6% ± ∼ . (cid:48)(cid:48)
15 and 4 . (cid:48)(cid:48) ∆ m ≤ ∼
500 objects per nightand have access to three-quarters of the sky over the courseof a year. A southern analog to Robo-AO, mounted on theSouthern Astrophysical Research Telescope (SOAR) at CTIOand capable of twice HST resolution imaging, is also in de-velopment. With unmatched e ffi ciency, Robo-AO and its lin-eage of instruments are uniquely able to perform high-acuity imaging of the hundreds of K2 (Howell et al. 2014) plane-tary candidates, ground-based transit surveys such as MEarth(Nutzman & Charbonneau 2008), KELT (Pepper et al. 2007,2012), HATNet (Bakos et al. 2004), SuperWASP (Pollaccoet al. 2006), NGTS (Wheatley et al. 2013), XO (McCulloughet al. 2005), and the Evryscope (Law et al. 2015), as wellas the thousands of expected exoplanet hosts discovered bythe forthcoming NASA Transiting Exoplanet Survey Satellite(TESS, Ricker et al. 2015) and ESA PLAnetary Transits andOscillations of stars 2.0 (PLATO, Rauer et al. 2014) missions.The Robo-AO survey has completed observations of over90% of the Kepler planet candidates, with the remaining tar-gets to be observed at the Kitt Peak telescope. Future papersin this survey will present these final KOI targets, and per-form a full probability of association analysis. With the entiresurvey soon to be completed, providing us with an unprece-dented dataset of thousands of high angular resolution imagedplanetary candidates, we can continue our search for clues toplanetary formation and evolution.
ACKNOWLEDGEMENTS
We thank the anonymous referee for careful analysis anduseful comments on the manuscript.This research is supported by the NASA Exoplanets Re-search Program, grant ff fortheir ongoing support of Robo-AO on the 1.5-m telescope,particularly S. Kunsman, M. Doyle, J. Henning, R. Walters,G. Van Idsinga, B. Baker, K. Dunscombe and D. Roderick.Some of the data presented herein were obtained at theW.M. Keck Observatory, which is operated as a scientificpartnership among the California Institute of Technology, theUniversity of California and the National Aeronautics andSpace Administration. The Observatory was made possibleby the generous financial support of the W.M. Keck Foun-dation. Some of the data presented herein is based on ob-servations obtained at the Gemini Observatory, operated bythe Association of Universities for Research in Astronomy,Inc., under a cooperative agreement with the NSF on behalf ofthe Gemini partnership. We recognize and acknowledge thevery significant cultural role and reverence that the summitof Maunakea has always had within the indigenous Hawaiiancommunity. We are most fortunate to have the opportunity toconduct observations from this mountain.We thank Adam Kraus et al. for sharing a preprint of theirpaper.This research has made use of the SIMBAD database, op-erated by Centre des Donn´ees Stellaires (Strasbourg, France),and bibliographic references from the Astrophysics Data Sys-tem maintained by SAO / NASA. This research has made useof the
Kepler
Community FollowUp Observing Program Website (https: // cfop.ipac.caltech.edu) and the NASA ExoplanetArchive, which is operated by the California Institute of Tech-8 Z iegler et al .nology, under contract with the National Aeronautics andSpace Administration under the Exoplanet Exploration Pro-gram. This work used the K2fov (Mullally 2016) Pythonpackage. Facilities:
PO:1.5m (Robo-AO), Keck:II (NIRC2-LGS),Gemini:Gillett (NIRI) REFERENCES
Adams, E. R., Ciardi, D. R., Dupree, A. K., Gautier, III, T. N., Kulesa, C., &McCarthy, D. 2012, AJ, 144, 42Adams, E. R., Dupree, A. K., Kulesa, C., & McCarthy, D. 2013, AJ, 146, 9Atkinson, D., Baranec, C., Ziegler, C., Law, N. M., Riddle, R., & Morton, T.2016Bakos, G., Noyes, R. W., Kov´acs, G., Stanek, K. Z., Sasselov, D. D., &Domsa, I. 2004, PASP, 116, 266Baranec, C., Riddle, R., Law, N. M., Chun, M. R., Lu, J. R., Connelley,M. S., Hall, D., Atkinson, D., & Jacobson, S. 2014a, in Proc. SPIE, Vol.9148, Adaptive Optics Systems IV, 914812Baranec, C., Riddle, R., Law, N. M., Ramaprakash, A. N., Tendulkar, S. P.,Bui, K., Burse, M. P., Chordia, P., Das, H. K., Davis, J. T. C., Dekany,R. G., Kasliwal, M. M., Kulkarni, S. R., Morton, T. D., Ofek, E. O., &Punnadi, S. 2013, Journal of Visualized Experiments, 72, e50021Baranec, C., Riddle, R., Law, N. M., Ramaprakash, A. N., Tendulkar, S. P.,Hogstrom, K., Bui, K., Burse, M., Chordia, P., Das, H., Dekany, R. G.,Kulkarni, S., & Punnadi, S. 2014b, ApJL, 790, L8Baranec, C., Ziegler, C., Law, N. M., Morton, T., Riddle, R., Atkinson, D.,Schonhut, J., & Crepp, J. 2016, ArXiv e-printsBarclay, T., Quintana, E. V., Adams, F. C., Ciardi, D. R., Huber, D.,Foreman-Mackey, D., Montet, B. T., & Caldwell, D. 2015, ApJ, 809, 7Batalha, N. M., Borucki, W. J., Koch, D. G., Bryson, S. T., Haas, M. R.,Brown, T. M., Caldwell, D. A., Hall, J. R., Gilliland, R. L., Latham,D. W., Meibom, S., & Monet, D. G. 2010, ApJL, 713, L109Batalha, N. M., Rowe, J. F., Bryson, S. T., Barclay, T., Burke, C. J.,Caldwell, D. A., Christiansen, J. L., Mullally, F., Thompson, S. E.,Brown, T. M., Dupree, A. K., Fabrycky, D. C., Ford, E. B., Fortney, J. J.,Gilliland, R. L., Isaacson, H., Latham, D. W., Marcy, G. W., Quinn, S. N.,Ragozzine, D., Shporer, A., Borucki, W. J., Ciardi, D. R., Gautier, III,T. N., Haas, M. R., Jenkins, J. M., Koch, D. G., Lissauer, J. J., Rapin, W.,Basri, G. S., Boss, A. P., Buchhave, L. A., Carter, J. A., Charbonneau, D.,Christensen-Dalsgaard, J., Clarke, B. D., Cochran, W. D., Demory, B.-O.,Desert, J.-M., Devore, E., Doyle, L. R., Esquerdo, G. A., Everett, M.,Fressin, F., Geary, J. C., Girouard, F. R., Gould, A., Hall, J. R., Holman,M. J., Howard, A. W., Howell, S. B., Ibrahim, K. A., Kinemuchi, K.,Kjeldsen, H., Klaus, T. C., Li, J., Lucas, P. W., Meibom, S., Morris, R. L.,Prˇsa, A., Quintana, E., Sanderfer, D. T., Sasselov, D., Seader, S. E.,Smith, J. C., Ste ff en, J. H., Still, M., Stumpe, M. C., Tarter, J. C.,Tenenbaum, P., Torres, G., Twicken, J. D., Uddin, K., Van Cleve, J.,Walkowicz, L., & Welsh, W. F. 2013, ApJS, 204, 24Batygin, K. 2012, Nature, 491, 418Borucki, W. J., Koch, D. G., Basri, G., Batalha, N., Boss, A., Brown, T. M.,Caldwell, D., Christensen-Dalsgaard, J., Cochran, W. D., DeVore, E.,Dunham, E. W., Dupree, A. K., Gautier, III, T. N., Geary, J. C., Gilliland,R., Gould, A., Howell, S. B., Jenkins, J. M., Kjeldsen, H., Latham, D. W.,Lissauer, J. J., Marcy, G. W., Monet, D. G., Sasselov, D., Tarter, J.,Charbonneau, D., Doyle, L., Ford, E. B., Fortney, J., Holman, M. J.,Seager, S., Ste ff en, J. H., Welsh, W. F., Allen, C., Bryson, S. T.,Buchhave, L., Chandrasekaran, H., Christiansen, J. L., Ciardi, D., Clarke,B. D., Dotson, J. L., Endl, M., Fischer, D., Fressin, F., Haas, M., Horch,E., Howard, A., Isaacson, H., Kolodziejczak, J., Li, J., MacQueen, P.,Meibom, S., Prsa, A., Quintana, E. V., Rowe, J., Sherry, W., Tenenbaum,P., Torres, G., Twicken, J. D., Van Cleve, J., Walkowicz, L., & Wu, H.2011a, ApJ, 728, 117 Borucki, W. J., Koch, D. G., Basri, G., Batalha, N., Brown, T. M., Bryson,S. T., Caldwell, D., Christensen-Dalsgaard, J., Cochran, W. D., DeVore,E., Dunham, E. W., Gautier, III, T. N., Geary, J. C., Gilliland, R., Gould,A., Howell, S. B., Jenkins, J. M., Latham, D. W., Lissauer, J. J., Marcy,G. W., Rowe, J., Sasselov, D., Boss, A., Charbonneau, D., Ciardi, D.,Doyle, L., Dupree, A. K., Ford, E. B., Fortney, J., Holman, M. J., Seager,S., Ste ff en, J. H., Tarter, J., Welsh, W. F., Allen, C., Buchhave, L. A.,Christiansen, J. L., Clarke, B. D., Das, S., D´esert, J.-M., Endl, M.,Fabrycky, D., Fressin, F., Haas, M., Horch, E., Howard, A., Isaacson, H.,Kjeldsen, H., Kolodziejczak, J., Kulesa, C., Li, J., Lucas, P. W., Machalek,P., McCarthy, D., MacQueen, P., Meibom, S., Miquel, T., Prsa, A., Quinn,S. N., Quintana, E. V., Ragozzine, D., Sherry, W., Shporer, A.,Tenenbaum, P., Torres, G., Twicken, J. D., Van Cleve, J., Walkowicz, L.,Witteborn, F. C., & Still, M. 2011b, ApJ, 736, 19—. 2011c, ApJ, 736, 19Borucki, W. J., Koch, D. G., Brown, T. M., Basri, G., Batalha, N. M.,Caldwell, D. A., Cochran, W. D., Dunham, E. W., Gautier, III, T. N.,Geary, J. C., Gilliland, R. L., Howell, S. B., Jenkins, J. M., Latham,D. W., Lissauer, J. J., Marcy, G. W., Monet, D., Rowe, J. F., & Sasselov,D. 2010, ApJL, 713, L126Brown, T. M., Latham, D. W., Everett, M. E., & Esquerdo, G. A. 2011, AJ,142, 112Burgasser, A. J., Kirkpatrick, J. D., Reid, I. N., Brown, M. E., Miskey, C. L.,& Gizis, J. E. 2003, ApJ, 586, 512Burke, C. J., Bryson, S. T., Mullally, F., Rowe, J. F., Christiansen, J. L.,Thompson, S. E., Coughlin, J. L., Haas, M. R., Batalha, N. M., Caldwell,D. A., Jenkins, J. M., Still, M., Barclay, T., Borucki, W. J., Chaplin, W. J.,Ciardi, D. R., Clarke, B. D., Cochran, W. D., Demory, B.-O., Esquerdo,G. A., Gautier, III, T. N., Gilliland, R. L., Girouard, F. R., Havel, M.,Henze, C. E., Howell, S. B., Huber, D., Latham, D. W., Li, J., Morehead,R. C., Morton, T. D., Pepper, J., Quintana, E., Ragozzine, D., Seader,S. E., Shah, Y., Shporer, A., Tenenbaum, P., Twicken, J. D., & Wolfgang,A. 2014, ApJS, 210, 19Ciardi, D. R., Beichman, C. A., Horch, E. P., & Howell, S. B. 2015, ApJ,805, 16Ciardi, D. R., von Braun, K., Bryden, G., van Eyken, J., Howell, S. B., Kane,S. R., Plavchan, P., Ram´ırez, S. V., & Stau ff er, J. R. 2011, AJ, 141, 108Coughlin, J. L., Mullally, F., Thompson, S. E., Rowe, J. F., Burke, C. J.,Latham, D. W., Batalha, N. M., Ofir, A., Quarles, B. L., Henze, C. E.,Wolfgang, A., Caldwell, D. A., Bryson, S. T., Shporer, A., Catanzarite, J.,Akeson, R., Barclay, T., Borucki, W. J., Boyajian, T. S., Campbell, J. R.,Christiansen, J. L., Girouard, F. R., Haas, M. R., Howell, S. B., Huber, D.,Jenkins, J. M., Li, J., Patil-Sabale, A., Quintana, E. V., Ramirez, S.,Seader, S., Smith, J. C., Tenenbaum, P., Twicken, J. D., & Zamudio, K. A.2015, ArXiv e-printsD´esert, J.-M., Charbonneau, D., Torres, G., Fressin, F., Ballard, S., Bryson,S. T., Knutson, H. A., Batalha, N. M., Borucki, W. J., Brown, T. M.,Deming, D., Ford, E. B., Fortney, J. J., Gilliland, R. L., Latham, D. W., &Seager, S. 2015, ApJ, 804, 59Dressing, C. D., Adams, E. R., Dupree, A. K., Kulesa, C., & McCarthy, D.2014, AJ, 148, 78Dressing, C. D. & Charbonneau, D. 2013, ApJ, 767, 95Duchˆene, G. & Kraus, A. 2013, ARA&A, 51, 269Duquennoy, A. & Mayor, M. 1991, A&A, 248, 485Evans, D. F., Southworth, J., Maxted, P. F. L., Skottfelt, J., Hundertmark,M., Jørgensen, U. G., Dominik, M., Alsubai, K. A., Andersen, M. I.,Bozza, V., Bramich, D. M., Burgdorf, M. J., Ciceri, S., D’Ago, G.,Figuera Jaimes, R., Gu, S. H., Haugbølle, T., Hinse, T. C., Juncher, D.,Kains, N., Kerins, E., Korhonen, H., Ku ff meier, M., Peixinho, N.,Popovas, A., Rabus, M., Rahvar, S., Schmidt, R. W., Snodgrass, C.,Starkey, D., Surdej, J., Tronsgaard, R., von Essen, C., Wang, Y.-B., &Wertz, O. 2016, ArXiv e-printsEverett, M. E., Barclay, T., Ciardi, D. R., Horch, E. P., Howell, S. B., Crepp,J. R., & Silva, D. R. 2015, AJ, 149, 55Fabrycky, D. & Tremaine, S. 2007, ApJ, 669, 1298Fabrycky, D. C., Ford, E. B., Ste ff en, J. H., Rowe, J. F., Carter, J. A.,Moorhead, A. V., Batalha, N. M., Borucki, W. J., Bryson, S., Buchhave,L. A., Christiansen, J. L., Ciardi, D. R., Cochran, W. D., Endl, M., Fanelli,M. N., Fischer, D., Fressin, F., Geary, J., Haas, M. R., Hall, J. R., Holman,M. J., Jenkins, J. M., Koch, D. G., Latham, D. W., Li, J., Lissauer, J. J.,Lucas, P., Marcy, G. W., Mazeh, T., McCauli ff , S., Quinn, S., Ragozzine,D., Sasselov, D., & Shporer, A. 2012, ApJ, 750, 114Fragner, M. M., Nelson, R. P., & Kley, W. 2011, A&A, 528, A40Fressin, F., Torres, G., Charbonneau, D., Bryson, S. T., Christiansen, J.,Dressing, C. D., Jenkins, J. M., Walkowicz, L. M., & Batalha, N. M.2013, ApJ, 766, 81Fruchter, A. S. & Hook, R. N. 2002, PASP, 114, 144 obo -AO Kepler P lanetary C andidate S urvey III 19
Gilliland, R. L., Cartier, K. M. S., Adams, E. R., Ciardi, D. R., Kalas, P., &Wright, J. T. 2015, AJ, 149, 24Gross, E. & Vitells, O. 2010, European Physical Journal C, 70, 525Haas, M. R., Batalha, N. M., Bryson, S. T., Caldwell, D. A., Dotson, J. L.,Hall, J., Jenkins, J. M., Klaus, T. C., Koch, D. G., Kolodziejczak, J.,Middour, C., Smith, M., Sobeck, C. K., Stober, J., Thompson, R. S., &Van Cleve, J. E. 2010, ApJL, 713, L115Heller, R. 2012, A&A, 545, L8Hodapp, K. W., Jensen, J. B., Irwin, E. M., Yamada, H., Chung, R., Fletcher,K., Robertson, L., Hora, J. L., Simons, D. A., Mays, W., Nolan, R., Bec,M., Merrill, M., & Fowler, A. M. 2003, PASP, 115, 1388Horch, E. P., Howell, S. B., Everett, M. E., & Ciardi, D. R. 2012, AJ, 144,165—. 2014, ApJ, 795, 60Howell, S. B., Everett, M. E., Sherry, W., Horch, E., & Ciardi, D. R. 2011,AJ, 142, 19Howell, S. B., Sobeck, C., Haas, M., Still, M., Barclay, T., Mullally, F.,Troeltzsch, J., Aigrain, S., Bryson, S. T., Caldwell, D., Chaplin, W. J.,Cochran, W. D., Huber, D., Marcy, G. W., Miglio, A., Najita, J. R., Smith,M., Twicken, J. D., & Fortney, J. J. 2014, PASP, 126, 398Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108Katz, B., Dong, S., & Malhotra, R. 2011, Physical Review Letters, 107,181101Kolbl, R., Marcy, G. W., Isaacson, H., & Howard, A. W. 2015, AJ, 149, 18Kraus, A. L. & Hillenbrand, L. A. 2007, AJ, 134, 2340Kraus, A. L., Ireland, M. J., Huber, D., Mann, A. W., & Dupuy, T. J. 2016,AJ, 152, 8Lafreni`ere, D., Marois, C., Doyon, R., Nadeau, D., & Artigau, ´E. 2007, ApJ,660, 770Law, N. M., Fors, O., Ratzlo ff , J., Wulfken, P., Kavanaugh, D., Sitar, D. J.,Pruett, Z., Birchard, M. N., Barlow, B. N., Cannon, K., Cenko, S. B.,Dunlap, B., Kraus, A., & Maccarone, T. J. 2015, PASP, 127, 234Law, N. M., Mackay, C. D., Dekany, R. G., Ireland, M., Lloyd, J. P., Moore,A. M., Robertson, J. G., Tuthill, P., & Woodru ff , H. C. 2009, ApJ, 692,924Law, N. M., Morton, T., Baranec, C., Riddle, R., Ravichandran, G., Ziegler,C., Johnson, J. A., Tendulkar, S. P., Bui, K., Burse, M. P., Das, H. K.,Dekany, R. G., Kulkarni, S., Punnadi, S., & Ramaprakash, A. N. 2014,ApJ, 791, 35Lawrence, A., Warren, S. J., Almaini, O., Edge, A. C., Hambly, N. C.,Jameson, R. F., Lucas, P., Casali, M., Adamson, A., Dye, S., Emerson,J. P., Foucaud, S., Hewett, P., Hirst, P., Hodgkin, S. T., Irwin, M. J.,Lodieu, N., McMahon, R. G., Simpson, C., Smail, I., Mortlock, D., &Folger, M. 2007, MNRAS, 379, 1599Lillo-Box, J., Barrado, D., & Bouy, H. 2012, A&A, 546, A10—. 2014, A&A, 566, A103Lissauer, J. J., Dawson, R. I., & Tremaine, S. 2014, Nature, 513, 336Marcy, G. W., Isaacson, H., Howard, A. W., Rowe, J. F., Jenkins, J. M.,Bryson, S. T., Latham, D. W., Howell, S. B., Gautier, III, T. N., Batalha,N. M., Rogers, L., Ciardi, D., Fischer, D. A., Gilliland, R. L., Kjeldsen,H., Christensen-Dalsgaard, J., Huber, D., Chaplin, W. J., Basu, S.,Buchhave, L. A., Quinn, S. N., Borucki, W. J., Koch, D. G., Hunter, R.,Caldwell, D. A., Van Cleve, J., Kolbl, R., Weiss, L. M., Petigura, E.,Seager, S., Morton, T., Johnson, J. A., Ballard, S., Burke, C., Cochran,W. D., Endl, M., MacQueen, P., Everett, M. E., Lissauer, J. J., Ford, E. B.,Torres, G., Fressin, F., Brown, T. M., Ste ff en, J. H., Charbonneau, D.,Basri, G. S., Sasselov, D. D., Winn, J., Sanchis-Ojeda, R., Christiansen,J., Adams, E., Henze, C., Dupree, A., Fabrycky, D. C., Fortney, J. J.,Tarter, J., Holman, M. J., Tenenbaum, P., Shporer, A., Lucas, P. W.,Welsh, W. F., Orosz, J. A., Bedding, T. R., Campante, T. L., Davies, G. R.,Elsworth, Y., Handberg, R., Hekker, S., Karo ff , C., Kawaler, S. D., Lund,M. N., Lundkvist, M., Metcalfe, T. S., Miglio, A., Silva Aguirre, V.,Stello, D., White, T. R., Boss, A., Devore, E., Gould, A., Prsa, A., Agol,E., Barclay, T., Coughlin, J., Brugamyer, E., Mullally, F., Quintana, E. V.,Still, M., Thompson, S. E., Morrison, D., Twicken, J. D., D´esert, J.-M.,Carter, J., Crepp, J. R., H´ebrard, G., Santerne, A., Moutou, C., Sobeck,C., Hudgins, D., Haas, M. R., Robertson, P., Lillo-Box, J., & Barrado, D.2014, ApJS, 210, 20McCullough, P. R., Stys, J. E., Valenti, J. A., Fleming, S. W., Janes, K. A., &Heasley, J. N. 2005, PASP, 117, 783Morton, T. D., Bryson, S. T., Coughlin, J. L., Rowe, J. F., Ravichandran, G.,Petigura, E. A., Haas, M. R., & Batalha, N. M. 2016, The AstrophysicalJournal, 822, 86Morton, T. D. & Johnson, J. A. 2011, ApJ, 738, 170 Mullally, F., Coughlin, J. L., Thompson, S. E., Rowe, J., Burke, C., Latham,D. W., Batalha, N. M., Bryson, S. T., Christiansen, J., Henze, C. E., Ofir,A., Quarles, B., Shporer, A., Van Eylen, V., Van Laerhoven, C., Shah, Y.,Wolfgang, A., Chaplin, W. J., Xie, J.-W., Akeson, R., Argabright, V.,Bachtell, E., Barclay, T., Borucki, W. J., Caldwell, D. A., Campbell, J. R.,Catanzarite, J. H., Cochran, W. D., Duren, R. M., Fleming, S. W.,Fraquelli, D., Girouard, F. R., Haas, M. R., Hełminiak, K. G., Howell,S. B., Huber, D., Larson, K., Gautier, III, T. N., Jenkins, J. M., Li, J.,Lissauer, J. J., McArthur, S., Miller, C., Morris, R. L., Patil-Sabale, A.,Plavchan, P., Putnam, D., Quintana, E. V., Ramirez, S., Silva Aguirre, V.,Seader, S., Smith, J. C., Ste ff en, J. H., Stewart, C., Stober, J., Still, M.,Tenenbaum, P., Troeltzsch, J., Twicken, J. D., & Zamudio, K. A. 2015,ApJS, 217, 31Mullally, Fergal; Barclay, T. B. G. 2016, K2fov: Field of view software forNASA’s K2 mission, Astrophysics Source Code LibraryNaoz, S., Farr, W. M., & Rasio, F. A. 2012, ApJL, 754, L36Ngo, H., Knutson, H. A., Hinkley, S., Crepp, J. R., Bechter, E. B., Batygin,K., Howard, A. W., Johnson, J. A., Morton, T. D., & Muirhead, P. S. 2015,ApJ, 800, 138Nutzman, P. & Charbonneau, D. 2008, PASP, 120, 317Pepper, J., Kuhn, R. B., Siverd, R., James, D., & Stassun, K. 2012, PASP,124, 230Pepper, J., Pogge, R. W., DePoy, D. L., Marshall, J. L., Stanek, K. Z., Stutz,A. M., Poindexter, S., Siverd, R., O’Brien, T. P., Trueblood, M., &Trueblood, P. 2007, PASP, 119, 923Pickles, A. J. 1998, PASP, 110, 863Pollacco, D. L., Skillen, I., Collier Cameron, A., Christian, D. J., Hellier, C.,Irwin, J., Lister, T. A., Street, R. A., West, R. G., Anderson, D. R.,Clarkson, W. I., Deeg, H., Enoch, B., Evans, A., Fitzsimmons, A.,Haswell, C. A., Hodgkin, S., Horne, K., Kane, S. R., Keenan, F. P.,Maxted, P. F. L., Norton, A. J., Osborne, J., Parley, N. R., Ryans, R. S. I.,Smalley, B., Wheatley, P. J., & Wilson, D. M. 2006, PASP, 118, 1407Raghavan, D., McAlister, H. A., Henry, T. J., Latham, D. W., Marcy, G. W.,Mason, B. D., Gies, D. R., White, R. J., & ten Brummelaar, T. A. 2010,ApJS, 190, 1Rasio, F. A. & Ford, E. B. 1996, Science, 274, 954Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A.,Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M.-J., G¨udel,M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco,D., Santos, ˙C., Smith, A., Su´arez, J.-C., Szab´o, R., Udry, S., Adibekyan,V., Alibert, Y., Almenara, J.-M., Amaro-Seoane, P., Ei ff , M. A.-v.,Asplund, M., Antonello, E., Barnes, S., Baudin, F., Belkacem, K.,Bergemann, M., Bihain, G., Birch, A. C., Bonfils, X., Boisse, I., Bonomo,A. S., Borsa, F., Brand˜ao, I. M., Brocato, E., Brun, S., Burleigh, M.,Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini,C., Church, R. P., Csizmadia, S., Cunha, M., Damasso, M., Davies, M. B.,Deeg, H. J., D´ıaz, R. F., Dreizler, S., Dreyer, C., Eggenberger, P.,Ehrenreich, D., Eigm¨uller, P., Erikson, A., Farmer, R., Feltzing, S., deOliveira Fialho, F., Figueira, P., Forveille, T., Fridlund, M., Garc´ıa, R. A.,Giommi, P., Giu ff rida, G., Godolt, M., Gomes da Silva, J., Granzer, T.,Grenfell, J. L., Grotsch-Noels, A., G¨unther, E., Haswell, C. A., Hatzes,A. P., H´ebrard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M.,Johansen, A., Khodachenko, M. L., Kislyakova, K. G., Kley, W., Kolb,U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F., Lebreton, Y.,Magrin, D., Marcos-Arenal, P., Marrese, P. M., Marques, J. P., Martins, J.,Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto,M., Monteiro, M. J. P. F. G., Moradi, H., Moravveji, E., Mordasini, C.,Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P., Nielsen, M. B.,Noack, L., Norton, A. J., Ofir, A., Oshagh, M., Ouazzani, R.-M., Papics,P., Parro, V. C., Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni,R., Raimondo, G., Rainer, M., Reese, D. R., Redmer, R., Re ff ert, S.,Rojas-Ayala, B., Roxburgh, I. W., Salmon, S., Santerne, A., Schneider, J.,Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I.,Snellen, I., Sohl, F., Sousa, S. G., Sozzetti, A., Stello, D., Strassmeier,K. G., ˇSvanda, M., Szab´o, G. M., Tkachenko, A., Valencia, D., VanGrootel, V., Vauclair, S. D., Ventura, P., Wagner, F. W., Walton, N. A.,Weingrill, J., Werner, S. C., Wheatley, P. J., & Zwintz, K. 2014,Experimental Astronomy, 38, 249 iegler et al . Ricker, G. R., Winn, J. N., Vanderspek, R., Latham, D. W., Bakos, G. ´A.,Bean, J. L., Berta-Thompson, Z. K., Brown, T. M., Buchhave, L., Butler,N. R., Butler, R. P., Chaplin, W. J., Charbonneau, D.,Christensen-Dalsgaard, J., Clampin, M., Deming, D., Doty, J., De Lee,N., Dressing, C., Dunham, E. W., Endl, M., Fressin, F., Ge, J., Henning,T., Holman, M. J., Howard, A. W., Ida, S., Jenkins, J. M., Jernigan, G.,Johnson, J. A., Kaltenegger, L., Kawai, N., Kjeldsen, H., Laughlin, G.,Levine, A. M., Lin, D., Lissauer, J. J., MacQueen, P., Marcy, G.,McCullough, P. R., Morton, T. D., Narita, N., Paegert, M., Palle, E., Pepe,F., Pepper, J., Quirrenbach, A., Rinehart, S. A., Sasselov, D., Sato, B.,Seager, S., Sozzetti, A., Stassun, K. G., Sullivan, P., Szentgyorgyi, A.,Torres, G., Udry, S., & Villasenor, J. 2015, Journal of AstronomicalTelescopes, Instruments, and Systems, 1, 014003Riddle, R. L., Burse, M. P., Law, N. M., Tendulkar, S. P., Baranec, C., Rudy,A. R., Sitt, M., Arya, A., Papadopoulos, A., Ramaprakash, A. N., &Dekany, R. G. 2012, in Society of Photo-Optical InstrumentationEngineers (SPIE) Conference Series, Vol. 8447, Society of Photo-OpticalInstrumentation Engineers (SPIE) Conference Series, 2Roberts, Jr., L. C., Tokovinin, A., Mason, B. D., Riddle, R. L., Hartkopf,W. I., Law, N. M., & Baranec, C. 2015, AJ, 149, 118Roell, T., Neuh¨auser, R., Seifahrt, A., & Mugrauer, M. 2012, A&A, 542,A92Rogers, L. A. 2015, ApJ, 801, 41Rowe, J. F., Bryson, S. T., Marcy, G. W., Lissauer, J. J., Jontof-Hutter, D.,Mullally, F., Gilliland, R. L., Issacson, H., Ford, E., Howell, S. B.,Borucki, W. J., Haas, M., Huber, D., Ste ff en, J. H., Thompson, S. E.,Quintana, E., Barclay, T., Still, M., Fortney, J., Gautier, III, T. N., Hunter,R., Caldwell, D. A., Ciardi, D. R., Devore, E., Cochran, W., Jenkins, J.,Agol, E., Carter, J. A., & Geary, J. 2014, ApJ, 784, 45Santerne, A., D´ıaz, R. F., Moutou, C., Bouchy, F., H´ebrard, G., Almenara,J.-M., Bonomo, A. S., Deleuil, M., & Santos, N. C. 2012, A&A, 545, A76Santerne, A., Fressin, F., D´ıaz, R. F., Figueira, P., Almenara, J.-M., &Santos, N. C. 2013, A&A, 557, A139Santerne, A., Moutou, C., Tsantaki, M., Bouchy, F., H´ebrard, G.,Adibekyan, V., Almenara, J.-M., Amard, L., Barros, S. C. C., Boisse, I.,Bonomo, A. S., Bruno, G., Courcol, B., Deleuil, M., Demangeon, O.,D´ıaz, R. F., Guillot, T., Havel, M., Montagnier, G., Rajpurohit, A. S., Rey,J., & Santos, N. C. 2015, ArXiv e-printsSchwamb, M. E., Orosz, J. A., Carter, J. A., Welsh, W. F., Fischer, D. A.,Torres, G., Howard, A. W., Crepp, J. R., Keel, W. C., Lintott, C. J., Kaib,N. A., Terrell, D., Gagliano, R., Jek, K. J., Parrish, M., Smith, A. M.,Lynn, S., Simpson, R. J., Giguere, M. J., & Schawinski, K. 2013, ApJ,768, 127 Seager, S. 2013, Science, 340, 577Selsis, F., Kasting, J. F., Levrard, B., Paillet, J., Ribas, I., & Delfosse, X.2007, A&A, 476, 1373Skrutskie, M. F., Cutri, R. M., Stiening, R., Weinberg, M. D., Schneider, S.,Carpenter, J. M., Beichman, C., Capps, R., Chester, T., Elias, J., Huchra,J., Liebert, J., Lonsdale, C., Monet, D. G., Price, S., Seitzer, P., Jarrett, T.,Kirkpatrick, J. D., Gizis, J. E., Howard, E., Evans, T., Fowler, J., Fullmer,L., Hurt, R., Light, R., Kopan, E. L., Marsh, K. A., McCallon, H. L., Tam,R., Van Dyk, S., & Wheelock, S. 2006, AJ, 131, 1163Torres, G., Kipping, D. M., Fressin, F., Caldwell, D. A., Twicken, J. D.,Ballard, S., Batalha, N. M., Bryson, S. T., Ciardi, D. R., Henze, C. E.,Howell, S. B., Isaacson, H. T., Jenkins, J. M., Muirhead, P. S., Newton,E. R., Petigura, E. A., Barclay, T., Borucki, W. J., Crepp, J. R., Everett,M. E., Horch, E. P., Howard, A. W., Kolbl, R., Marcy, G. W., McCauli ff ,S., & Quintana, E. V. 2015, ApJ, 800, 99van Dam, M. A., Bouchez, A. H., Le Mignant, D., Johansson, E. M.,Wizinowich, P. L., Campbell, R. D., Chin, J. C. Y., Hartman, S. K., Lafon,R. E., Stomski, Jr., P. J., & Summers, D. M. 2006, PASP, 118, 310Wang, J., Fischer, D. A., Horch, E. P., & Xie, J.-W. 2015a, ApJ, 806, 248Wang, J., Fischer, D. A., Xie, J.-W., & Ciardi, D. R. 2014, ApJ, 791, 111—. 2015b, ArXiv e-printsWheatley, P. J., Pollacco, D. L., Queloz, D., Rauer, H., Watson, C. A., West,R. G., Chazelas, B., Louden, T. M., Walker, S., Bannister, N., Bento, J.,Burleigh, M., Cabrera, J., Eigm¨uller, P., Erikson, A., Genolet, L., Goad,M., Grange, A., Jord´an, A., Lawrie, K., McCormac, J., & Neveu, M.2013, in European Physical Journal Web of Conferences, Vol. 47,European Physical Journal Web of Conferences, 13002Wizinowich, P., Acton, D. S., Shelton, C., Stomski, P., Gathright, J., Ho, K.,Lupton, W., Tsubota, K., Lai, O., Max, C., Brase, J., An, J., Avicola, K.,Olivier, S., Gavel, D., Macintosh, B., Ghez, A., & Larkin, J. 2000, PASP,112, 315Wizinowich, P. L., Le Mignant, D., Bouchez, A. H., Campbell, R. D., Chin,J. C. Y., Contos, A. R., van Dam, M. A., Hartman, S. K., Johansson,E. M., Lafon, R. E., Lewis, H., Stomski, P. J., Summers, D. M., Brown,C. G., Danforth, P. M., Max, C. E., & Pennington, D. M. 2006, PASP,118, 297Xie, J.-W., Wu, Y., & Lithwick, Y. 2014, ApJ, 789, 165Yelda, S., Lu, J. R., Ghez, A. M., Clarkson, W., Anderson, J., Do, T., &Matthews, K. 2010, ApJ, 725, 331Ziegler, C., Law, N. M., Baranec, C., Riddle, R. L., & Fuchs, J. T. 2015,ApJ, 804, 30Zsom, A., Seager, S., de Wit, J., & Stamenkovi´c, V. 2013, ApJ, 778, 109 obo -AO Kepler P lanetary C andidate S urvey III 21
Figure 18.
Color inverted, normalized log-scale cutouts of 61 multiple KOI systems [KOI-51 to KOI-2688] with separations < (cid:48)(cid:48) resolved with Robo-AO. Theangular scale and orientation is similar for each cutout. The smaller circles are centered on the detected nearby star, and the larger circle is the limit of the survey’s4 (cid:48)(cid:48) separation range. iegler et al . Figure 19.
Color inverted, normalized log-scale cutouts of 61 multiple KOI systems [KOI-2744 to KOI-4405] with separations < (cid:48)(cid:48) resolved with Robo-AO.The angular scale and orientation is similar for each cutout. The smaller circles are centered on the detected nearby star, and the larger circle is the limit of thesurvey’s 4 (cid:48)(cid:48) separation range. obo -AO Kepler P lanetary C andidate S urvey III 23
Figure 20.
Color inverted, normalized log-scale cutouts of 61 multiple KOI systems [KOI-4418 to KOI-6311] with separations < (cid:48)(cid:48) resolved with Robo-AO.The angular scale and orientation is similar for each cutout. The smaller circles are centered on the detected nearby star, and the larger circle is the limit of thesurvey’s 4 (cid:48)(cid:48) separation range. iegler et al . Figure 21.
Color inverted, normalized log-scale cutouts of 23 multiple KOI systems [KOI-6329 to KOI-7448] with separations < (cid:48)(cid:48) resolved with Robo-AO.The angular scale and orientation is similar for each cutout. The smaller circles are centered on the detected nearby star, and the larger circle is the limit of thesurvey’s 4 (cid:48)(cid:48) separation range. obo -AO Kepler P lanetary C andidate S urvey III 25 APPENDIX
In Table 9, we list our Robo-AO observed KOIs, includ-ing date the target was observed, observation quality (as de-scribed in Section 3.6), the estimated latest detectable com-panion spectral type (as described in Section 3.7.3), and thepresence of detected companions.
Table 9
Full Robo-AO Observation ListKOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K020 13.29 2014 Aug 22 i (cid:48) medium M4K051 14.48 2013 Jul 25 LP600 medium M4 yesK076 10.05 2014 Aug 22 i (cid:48) high M4K0104 12.78 2014 Aug 22 i (cid:48) medium M6K0126 13.11 2015 Jun 08 LP600 high M5 yesK0134 15.02 2012 Jul 16 i (cid:48) medium M4K0135 13.8 2012 Jul 17 i (cid:48) low M1K0163 13.3 2012 Jul 18 LP600 high M6 yesK0186 14.76 2014 Aug 31 LP600 medium M4K0193 14.9 2014 Aug 21 LP600 high M4 yesK0195 14.62 2014 Aug 22 i (cid:48) low M1K0196 14.24 2014 Aug 21 i (cid:48) high M5K0199 14.72 2014 Aug 20 i (cid:48) high M4K0200 14.21 2014 Sep 01 LP600 medium M4 yesK0204 14.41 2014 Aug 20 i (cid:48) low M2K0212 14.66 2014 Aug 20 i (cid:48) high M4K0217 14.88 2014 Aug 20 i (cid:48) high M5K0225 14.61 2014 Jul 16 LP600 low M0 yesK0226 14.54 2014 Jun 19 LP600 medium M5K0240 14.8 2014 Aug 21 LP600 medium M3 yesK0242 14.5 2014 Jul 16 LP600 medium M4K0249 14.77 2014 Aug 23 LP600 medium M7K0252 14.99 2014 Aug 22 i (cid:48) low M5K0255 14.52 2014 Jul 17 LP600 medium M7 yesK0262 10.3 2012 Jul 28 i (cid:48) high M4K0266 11.47 2014 Aug 20 i (cid:48) medium M3K0326 12.96 2013 Aug 15 LP600 high M6 yesK0364 9.91 2014 Aug 20 i (cid:48) highK0376 13.7 2012 Sep 01 LP600 medium M2K0398 15.04 2014 Aug 22 i (cid:48) low M3K0414 14.5 2012 Sep 01 LP600 medium M4K0422 14.56 2014 Aug 22 i (cid:48) high M4K0423 14.15 2014 Jul 16 LP600 medium M3K0426 14.53 2014 Aug 20 i (cid:48) high M4K0428 14.42 2014 Jun 19 LP600 medium M2K0430 14.4 2014 Aug 22 i (cid:48) low M5K0449 14.18 2015 Jun 04 LP600 low M0K0452 14.45 2014 Jul 17 LP600 medium M3K0454 14.53 2014 Jul 16 LP600 medium M5 yesK0458 14.49 2014 Jul 14 LP600 medium M4K0466 14.49 2014 Sep 01 LP600 high M4K0467 14.58 2014 Aug 21 LP600 medium M4K0468 14.47 2014 Aug 21 LP600 high M5K0469 14.54 2014 Sep 02 LP600 medium M3K0476 14.65 2014 Aug 21 LP600 medium M5K0483 14.45 2014 Aug 22 i (cid:48) high M5K0510 14.4 2014 Jul 14 LP600 medium M4 yesK0513 14.71 2014 Jul 14 LP600 low M0K0524 14.6 2014 Aug 23 LP600 low M3K0530 14.69 2014 Sep 02 LP600 medium M4K0532 14.53 2014 Jul 17 LP600 medium M3 yesK0533 14.41 2014 Aug 22 i (cid:48) low M3K0537 14.5 2014 Jul 19 LP600 low M1K0541 14.51 2014 Aug 29 LP600 medium M4 yesK0547 14.48 2014 Jul 18 LP600 medium M5K0557 14.67 2014 Jul 16 LP600 medium M5K0560 14.46 2014 Jul 14 LP600 medium M5K0566 14.53 2014 Sep 01 LP600 medium M3K0575 14.51 2014 Jun 19 LP600 high M4K0578 14.47 2014 Jun 19 LP600 medium M4K0580 14.65 2014 Sep 01 LP600 medium M4K0581 14.58 2014 Jul 16 LP600 medium M4K0583 14.52 2014 Sep 01 LP600 medium M4K0585 14.68 2014 Aug 21 LP600 medium M4K0598 14.55 2014 Jul 11 LP600 high M5 yesK0599 14.66 2014 Sep 03 LP600 medium M4K0600 14.64 2014 Jul 17 LP600 high M4 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K0602 14.48 2014 Aug 29 LP600 medium M3K0605 14.47 2014 Aug 22 i (cid:48) low M5K0622 14.65 2014 Aug 31 LP600 medium M5K0732 15.07 2014 Sep 02 LP600 low M3K0733 15.36 2014 Sep 02 LP600 low M3K0734 15.14 2014 Sep 02 LP600 medium M4 yesK0736 15.45 2014 Sep 01 LP600 low M5K0740 15.2 2014 Aug 22 i (cid:48) low M4K0746 14.96 2014 Sep 02 LP600 high M6K0749 15.4 2014 Sep 01 LP600 medium M4K0750 15.04 2014 Sep 02 LP600 low M4K0752 15.3 2014 Sep 01 LP600 medium M4K0755 15.29 2014 Sep 03 LP600 medium M4K0757 15.53 2014 Sep 03 LP600 medium M5 yesK0759 14.84 2014 Jul 18 LP600 high M5K0760 15.07 2014 Sep 01 LP600 medium M3K0763 15.33 2014 Aug 28 LP600 low M1K0764 15.11 2014 Aug 23 LP600 high M5K0765 15.08 2014 Sep 03 LP600 medium M4K0766 15.3 2014 Aug 26 LP600 low M1K0769 15.11 2014 Aug 28 LP600 high M5K0771 15.07 2014 Aug 27 LP600 medium M4 yesK0772 15.06 2014 Sep 03 LP600 medium M3K0773 14.96 2014 Sep 01 LP600 medium M4K0774 15.08 2014 Sep 02 LP600 medium M4K0775 14.57 2014 Aug 22 i (cid:48) low M5K0776 15.27 2014 Sep 02 LP600 high M5K0777 15.22 2014 Aug 31 LP600 medium M4K0778 14.61 2014 Aug 21 LP600 medium M7K0780 15.0 2014 Sep 01 LP600 medium M5K0782 15.1 2014 Sep 02 LP600 low M1K0783 14.82 2014 Jul 11 LP600 low M3K0784 14.86 2014 Sep 01 LP600 medium M7K0786 15.03 2014 Sep 02 LP600 medium M4K0788 14.92 2014 Sep 02 LP600 medium M5K0791 14.92 2014 Sep 02 LP600 high M5K0804 15.11 2014 Aug 27 LP600 medium M5K0805 15.39 2014 Aug 23 LP600 high M5K0806 15.3 2014 Aug 23 LP600 low M3K0809 15.32 2014 Aug 23 LP600 high M5K0810 14.81 2014 Aug 31 LP600 low M3K0811 15.04 2014 Aug 31 LP600 low M4K0812 15.43 2014 Aug 22 i (cid:48) medium M6K0814 15.32 2014 Aug 24 LP600 high M5 yesK0815 15.42 2014 Nov 09 LP600 medium M4K0816 15.42 2014 Aug 24 LP600 medium M4 yesK0826 14.87 2014 Jun 19 LP600 medium M4K0829 15.18 2014 Aug 22 i (cid:48) low M1K0830 14.91 2014 Jun 19 LP600 medium M5K0833 15.24 2014 Aug 24 LP600 medium M4K0838 15.1 2014 Aug 27 LP600 medium M4K0841 15.57 2012 Sep 02 LP600 low M3 yesK0843 15.04 2014 Aug 26 LP600 medium M4K0845 15.21 2014 Nov 09 LP600 medium M4K0847 14.97 2014 Jul 16 LP600 low M2K0849 14.76 2014 Jul 19 LP600 medium M4K0850 15.03 2014 Aug 26 LP600 high M5K0855 14.95 2014 Jun 19 LP600 medium M4K0856 15.15 2014 Aug 26 LP600 medium M3K0858 14.82 2014 Jul 17 LP600 medium M4K0861 14.71 2014 Aug 21 LP600 medium M5K0863 15.3 2014 Aug 27 LP600 low M1K0864 15.36 2014 Sep 01 LP600 high M5K0867 14.92 2014 Jun 19 LP600 low M3K0868 15.1 2014 Jun 19 LP600 low M5K0869 15.29 2014 Sep 01 LP600 medium M5K0870 14.63 2014 Aug 22 i (cid:48) low M4K0871 15.02 2014 Aug 28 LP600 medium M4K0873 14.8 2014 Jul 18 LP600 high M5K0881 15.56 2014 Aug 20 i (cid:48) low M3K0887 14.8 2014 Aug 20 i (cid:48) low M2K0889 14.95 2014 Jul 16 LP600 medium M5K0890 15.08 2014 Aug 23 LP600 high M4K0891 14.87 2014 Jul 16 LP600 medium M4K0892 14.89 2014 Aug 21 LP600 medium M5K0893 15.44 2014 Aug 31 LP600 low M1K0900 15.21 2014 Aug 24 LP600 medium M4 iegler et al . TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K0901 15.27 2014 Aug 23 LP600 low M5K0902 15.7 2014 Aug 31 LP600 low M5K0904 15.35 2014 Aug 23 LP600 low M4K0910 15.35 2014 Aug 26 LP600 high M5K0911 15.21 2014 Aug 28 LP600 medium M4K0912 14.59 2014 Jul 17 LP600 low M4K0913 14.97 2014 Jul 17 LP600 medium M4K0914 15.15 2014 Aug 28 LP600 low M2K0916 14.88 2014 Jul 18 LP600 low M3K0918 14.77 2014 Jul 16 LP600 medium M4K0920 14.83 2014 Aug 21 LP600 medium M4K0923 15.32 2014 Sep 01 LP600 medium M4K0924 15.04 2014 Sep 01 LP600 medium M3K0928 15.02 2014 Aug 23 LP600 low M3K0929 15.44 2014 Aug 27 LP600 low M1K0934 15.63 2014 Sep 02 LP600 low M1K0937 15.15 2014 Aug 28 LP600 high M5K0942 15.08 2014 Aug 28 LP600 high M5K0943 15.45 2014 Aug 28 LP600 low M3K0948 15.35 2014 Sep 02 LP600 low M3K0949 15.28 2014 Sep 02 LP600 medium M4K0951 14.85 2014 Aug 31 LP600 medium M5K0952 14.65 2012 Jul 16 i (cid:48) high M8K0953 15.71 2014 Sep 03 LP600 medium M4K0954 14.5 2014 Sep 02 LP600 low M1K0955 14.9 2014 Aug 29 LP600 medium M3K0956 15.1 2014 Jul 16 LP600 medium M5K0958 12.24 2012 Aug 02 i (cid:48) medium M5K0961 15.34 2012 Aug 04 LP600 mediumK0989 15.4 2014 Aug 24 LP600 low M3K01005 15.39 2014 Nov 09 LP600 medium M5K01017 14.75 2014 Aug 31 LP600 medium M4K01051 15.19 2014 Aug 24 LP600 medium M4K01053 15.12 2014 Aug 27 LP600 high M5K01072 14.55 2014 Aug 21 LP600 medium M3K01074 15.26 2014 Sep 01 LP600 low M0K01081 15.04 2014 Aug 26 LP600 low M1K01082 15.39 2014 Sep 01 LP600 low M3K01095 15.37 2014 Aug 31 LP600 low M2K01096 14.48 2014 Aug 22 i (cid:48) high M5K01121 12.9 2012 Sep 14 LP600 high M5K01129 15.12 2014 Aug 31 LP600 low M3K01137 13.77 2014 Jun 13 LP600 medium M5 yesK01142 15.48 2014 Aug 31 LP600 low M3K01160 15.72 2014 Sep 02 LP600 low M3K01164 15.1 2012 Aug 04 LP600 medium M7K01166 15.22 2014 Aug 26 LP600 medium M4K01170 14.45 2014 Sep 03 LP600 medium M4K01176 15.31 2014 Aug 26 LP600 high M8K01193 15.05 2014 Aug 26 LP600 medium M4 yesK01196 14.82 2014 Jul 16 LP600 low M1K01201 14.96 2012 Aug 04 LP600 medium M7 yesK01204 15.11 2014 Nov 08 LP600 medium M3K01207 14.89 2014 Sep 01 LP600 high M5K01212 14.76 2014 Jul 11 LP600 low M1K01232 14.14 2014 Aug 21 i (cid:48) medium M5K01246 14.72 2014 Jun 19 LP600 high M4K01255 15.68 2014 Sep 01 LP600 high M5K01261 14.92 2014 Aug 22 i (cid:48) low M1 yesK01264 15.52 2014 Aug 31 LP600 low M3K01268 14.64 2014 Aug 22 i (cid:48) low M0K01273 14.63 2014 Jul 17 LP600 low M2K01298 15.8 2014 Aug 21 i (cid:48) low M3K01312 14.56 2014 Jul 17 LP600 medium M3K01326 12.8 2014 Aug 22 i (cid:48) medium M5K01337 14.53 2014 Jul 14 LP600 medium M5K01351 15.35 2014 Aug 24 LP600 medium M4K01356 14.98 2014 Aug 22 i (cid:48) lowK01361 14.46 2014 Aug 20 i (cid:48) low M5K01367 14.74 2014 Jul 16 LP600 medium M5K01369 14.67 2014 Jun 19 LP600 medium M4K01377 14.6 2014 Jul 17 LP600 low M0K01385 15.64 2014 Sep 01 LP600 low M1K01387 14.46 2014 Jul 16 LP600 medium M4K01395 15.71 2014 Sep 01 LP600 low M3K01398 15.67 2014 Aug 28 LP600 high M5K01402 15.69 2014 Aug 24 LP600 low M1 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K01403 14.99 2014 Aug 21 LP600 medium M6K01404 15.49 2014 Sep 01 LP600 low M5K01405 15.79 2014 Sep 01 LP600 medium M3K01409 14.98 2014 Jul 17 LP600 medium M4 yesK01410 15.12 2014 Aug 28 LP600 low M1K01411 13.13 2014 Jun 15 LP600 medium M4K01420 15.45 2014 Sep 02 LP600 low M4K01421 15.09 2014 Aug 22 i (cid:48) low M1K01423 15.49 2014 Sep 03 LP600 medium M4K01424 14.77 2014 Sep 01 LP600 medium M5K01429 15.3 2014 Sep 01 LP600 low M2K01430 15.02 2014 Aug 23 LP600 medium M5K01433 15.43 2014 Sep 03 LP600 medium M4K01434 14.41 2014 Jul 17 LP600 medium M5K01437 15.09 2014 Sep 03 LP600 medium M4K01440 15.27 2014 Sep 01 LP600 high M4K01441 14.9 2014 Aug 31 LP600 medium M4 yesK01447 13.0 2012 Sep 04 LP600 high M4 yesK01456 14.77 2014 Jul 17 LP600 high M5K01457 15.31 2014 Sep 02 LP600 high M5K01466 15.59 2014 Aug 28 LP600 low M4K01472 14.83 2014 Aug 20 i (cid:48) low M2K01476 15.52 2014 Sep 02 LP600 low M3K01477 15.65 2014 Aug 22 i (cid:48) low M3K01481 15.22 2014 Aug 30 LP600 high M5K01483 14.11 2014 Sep 02 LP600 medium M4K01484 14.96 2014 Jul 13 LP600 high M6K01488 15.3 2014 Sep 01 LP600 medium M5K01489 15.25 2014 Sep 02 LP600 low M3K01494 15.46 2014 Aug 28 LP600 low M4K01496 15.38 2014 Aug 27 LP600 high M5K01498 15.78 2015 Jun 04 LP600 low M1K01501 15.47 2014 Aug 28 LP600 low M4K01503 14.6 2014 Aug 22 i (cid:48) low M3 yesK01505 15.49 2014 Sep 01 LP600 medium M4K01506 14.77 2014 Sep 02 LP600 medium M4 yesK01507 15.07 2014 Aug 28 LP600 low M1K01508 15.47 2014 Aug 31 LP600 low M1K01510 15.58 2014 Aug 28 LP600 high M6K01511 14.87 2014 Jul 17 LP600 low M2K01517 14.47 2014 Jun 16 LP600 high M5K01519 15.06 2014 Aug 23 LP600 high M5K01521 14.82 2015 Jun 08 LP600 medium M5K01526 15.04 2014 Sep 02 LP600 low M0K01547 15.47 2014 Aug 24 LP600 high M4K01558 14.95 2014 Jul 11 LP600 high M4 yesK01561 15.32 2014 Aug 23 LP600 low M1K01562 15.37 2014 Aug 21 LP600 high M5K01564 15.07 2014 Aug 27 LP600 medium M4K01569 15.22 2014 Aug 24 LP600 medium M5K01570 14.98 2014 Jul 17 LP600 medium M4K01572 15.25 2014 Sep 02 LP600 high M4K01577 15.49 2014 Sep 02 LP600 low M5K01581 15.23 2014 Aug 24 LP600 low M3K01582 15.16 2014 Aug 28 LP600 low M3K01583 14.85 2014 Jul 13 LP600 low M2K01584 15.44 2014 Sep 02 LP600 high M6K01587 15.41 2014 Aug 27 LP600 high M5K01593 15.57 2014 Aug 24 LP600 low M1 yesK01595 14.7 2014 Jul 13 LP600 low M1K01630 14.91 2014 Jul 16 LP600 high M5 yesK01633 14.92 2014 Aug 21 LP600 medium M4K01645 13.14 2014 Jun 19 LP600 high M5K01650 15.04 2014 Sep 03 LP600 medium M4K01651 14.55 2014 Jun 19 LP600 low M1K01656 14.82 2014 Jun 13 LP600 low M1 yesK01658 13.16 2014 Jul 16 LP600 medium M3K01659 14.95 2014 Jul 16 LP600 high M4K01660 15.41 2014 Aug 28 LP600 low M1 yesK01662 15.21 2014 Aug 24 LP600 high M5K01672 15.37 2014 Aug 28 LP600 low M4K01675 15.56 2014 Aug 27 LP600 low M2K01681 14.71 2014 Aug 24 LP600 high M8K01685 14.65 2014 Jul 16 LP600 low M0K01687 14.94 2014 Jul 17 LP600 medium M5 yesK01691 15.56 2014 Aug 26 LP600 high M5K01693 14.73 2014 Jun 19 LP600 medium M4 obo -AO Kepler P lanetary C andidate S urvey III 27
TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K01695 13.58 2014 Aug 31 LP600 high M4 yesK01705 15.26 2014 Aug 28 LP600 high M4K01708 14.55 2014 Aug 21 LP600 medium M4K01710 15.21 2014 Aug 27 LP600 low M3K01711 14.72 2014 Aug 21 LP600 medium M5K01716 14.55 2014 Jul 11 LP600 low M4K01718 15.02 2014 Aug 27 LP600 medium M3K01721 14.77 2014 Sep 01 LP600 medium M4K01722 15.31 2014 Aug 28 LP600 medium M4K01723 15.33 2014 Aug 28 LP600 high M4K01724 15.39 2014 Aug 28 LP600 low M1K01727 15.42 2014 Aug 24 LP600 low M2K01732 15.5 2014 Aug 26 LP600 low M2K01736 15.69 2014 Sep 01 LP600 low M1K01739 14.92 2014 Aug 22 i (cid:48) lowK01747 14.56 2014 Jul 18 LP600 low M2K01749 15.55 2014 Aug 26 LP600 low M2K01750 14.57 2014 Jul 16 LP600 high M5K01758 15.72 2014 Aug 24 LP600 high M5K01761 15.44 2014 Aug 24 LP600 medium M3K01771 15.76 2014 Sep 03 LP600 low M1K01772 15.63 2015 Jun 04 LP600 low M4K01773 15.4 2014 Aug 24 LP600 medium M5K01782 15.32 2014 Aug 27 LP600 low M3K01787 15.49 2014 Sep 03 LP600 medium M4K01790 15.04 2014 Aug 26 LP600 medium M4K01792 11.92 2014 Sep 02 LP600 high M5 yesK01796 12.74 2014 Aug 21 i (cid:48) medium M4K01799 15.29 2014 Aug 23 LP600 low M1K01804 15.29 2014 Sep 02 LP600 low M4 yesK01806 13.34 2014 Jul 13 LP600 medium M3K01816 15.13 2014 Aug 28 LP600 low M3K01821 14.68 2014 Jul 17 LP600 medium M4K01840 14.71 2014 Jul 17 LP600 medium M3K01846 15.52 2014 Sep 02 LP600 low M3 yesK01847 14.53 2014 Jul 18 LP600 medium M5K01858 14.53 2014 Aug 22 i (cid:48) low M2K01866 14.78 2014 Sep 02 LP600 low M1K01871 14.48 2014 Aug 22 i (cid:48) medium M5K01872 15.59 2014 Sep 02 LP600 low M3K01873 15.47 2014 Aug 24 LP600 high M4K01879 13.42 2014 Aug 28 LP600 low M6K01882 14.48 2014 Jun 19 LP600 medium M4K01892 15.26 2014 Aug 31 LP600 medium M4K01900 14.29 2014 Jul 17 LP600 medium M6K01908 14.25 2014 Aug 22 i (cid:48) low M4 yesK01910 14.41 2014 Jul 19 LP600 medium M5K01933 14.82 2014 Jul 16 LP600 medium M4K01939 14.9 2014 Jun 19 LP600 high M5K01947 12.17 2012 Aug 30 i (cid:48) high M4K01951 13.42 2014 Jul 16 LP600 medium M3K01957 12.52 2014 Jul 16 LP600 high M4K01959 13.91 2014 Aug 22 i (cid:48) low M4K01963 13.93 2014 Aug 29 LP600 medium M4K01968 14.92 2014 Aug 31 LP600 medium M3K01971 15.38 2014 Aug 28 LP600 low M4K01973 15.32 2014 Aug 28 LP600 low M4 yesK01974 14.69 2014 Jun 19 LP600 medium M4K01975 15.77 2014 Aug 24 LP600 low M1K01981 13.93 2014 Jun 19 LP600 medium M5K01982 15.49 2014 Sep 01 LP600 medium M4K01995 15.05 2014 Aug 24 LP600 high M5 yesK01996 15.27 2014 Aug 26 LP600 high M6K01998 15.19 2014 Aug 28 LP600 low M0K02000 15.34 2014 Aug 26 LP600 medium M4K02012 14.67 2014 Jul 17 LP600 low M2K02020 15.07 2014 Aug 20 i (cid:48) low M4K02021 15.16 2014 Aug 26 LP600 high M6K02028 15.9 2014 Aug 31 LP600 low M2K02048 15.49 2014 Aug 28 LP600 low M4 yesK02050 12.22 2015 Jun 07 LP600 high M5 yesK02060 14.86 2014 Sep 01 LP600 medium M5K02061 15.43 2014 Sep 02 LP600 low M3K02062 14.79 2014 Sep 01 LP600 medium M4K02063 15.38 2014 Aug 31 LP600 low M2K02065 14.09 2014 Jul 14 LP600 medium M4K02074 15.52 2014 Aug 26 LP600 high M5 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K02076 15.09 2014 Sep 02 LP600 low M1K02078 15.06 2014 Aug 31 LP600 high M6K02080 15.15 2014 Aug 31 LP600 medium M4K02091 15.48 2014 Aug 27 LP600 low M3 yesK02092 15.8 2014 Aug 31 LP600 low M0K02093 15.19 2014 Aug 27 LP600 medium M2 yesK02094 14.71 2014 Jul 17 LP600 medium M5K02101 14.56 2014 Aug 21 LP600 high M6K02103 14.5 2014 Jun 19 LP600 medium M4K02104 14.94 2014 Sep 02 LP600 low M1K02106 14.94 2014 Jul 13 LP600 low M2K02107 14.88 2014 Jul 17 LP600 high M5K02108 14.77 2014 Jul 16 LP600 medium M3K02113 15.59 2014 Aug 31 LP600 low M3K02116 14.52 2014 Aug 21 LP600 medium M3K02117 15.17 2014 Nov 09 LP600 medium M5 yesK02121 14.74 2014 Jun 19 LP600 high M5K02125 15.16 2014 Aug 28 LP600 medium M3K02126 15.55 2014 Aug 26 LP600 high M6K02128 15.69 2014 Aug 26 LP600 high M5K02129 14.54 2014 Jun 19 LP600 medium M3K02134 14.53 2014 Jul 14 LP600 medium M4K02140 15.04 2014 Aug 28 LP600 medium M4K02146 14.99 2014 Aug 31 LP600 medium M5K02150 15.04 2014 Nov 08 LP600 medium M4K02152 14.84 2014 Sep 02 LP600 low M2K02154 15.62 2014 Sep 03 LP600 medium M4K02163 14.44 2014 Aug 31 LP600 medium M4 yesK02164 14.92 2014 Aug 31 LP600 medium M4K02166 15.45 2014 Sep 03 LP600 medium M4K02167 15.08 2014 Aug 27 LP600 high M4K02171 14.77 2014 Aug 21 LP600 high M5K02177 15.21 2014 Sep 03 LP600 medium M5K02179 14.99 2014 Jul 12 LP600 high M8K02180 14.58 2014 Jun 19 LP600 high M5K02182 15.58 2014 Sep 03 LP600 high M5K02183 14.98 2014 Aug 31 LP600 medium M4K02188 15.13 2014 Sep 01 LP600 medium M4K02193 15.21 2014 Aug 24 LP600 high M6K02195 14.74 2014 Sep 02 LP600 high M4K02198 12.7 2014 Aug 29 LP600 high M3K02199 15.61 2014 Sep 03 LP600 medium M5K02200 15.12 2014 Sep 03 LP600 high M5K02205 15.12 2014 Sep 01 LP600 medium M5K02206 14.98 2014 Jul 19 LP600 high M5 yesK02210 14.86 2014 Jul 14 LP600 low M4K02212 14.74 2014 Aug 29 LP600 high M5K02213 15.13 2014 Aug 24 LP600 medium M5 yesK02216 14.97 2014 Jul 16 LP600 medium M4K02217 14.91 2014 Aug 29 LP600 low M3K02221 15.19 2014 Aug 31 LP600 medium M4K02223 14.95 2014 Aug 21 LP600 low M4K02227 14.65 2014 Aug 22 i (cid:48) low M2K02229 15.45 2014 Aug 24 LP600 medium M4K02236 15.49 2014 Sep 02 LP600 low M2K02237 14.97 2014 Jun 17 LP600 high M4K02242 15.51 2014 Sep 01 LP600 low M3K02245 14.52 2014 Jul 16 LP600 medium M4K02248 15.21 2014 Sep 01 LP600 low M3K02250 15.26 2014 Nov 09 LP600 high M6K02255 15.61 2014 Aug 24 LP600 medium M4K02257 15.24 2014 Aug 26 LP600 medium M4K02271 15.32 2014 Sep 02 LP600 low M3K02274 15.6 2014 Aug 28 LP600 high M5K02283 14.74 2014 Sep 01 LP600 low M5 yesK02285 15.71 2014 Sep 02 LP600 low M1K02291 14.88 2014 Sep 01 LP600 medium M4K02294 14.69 2014 Aug 22 i (cid:48) low M1K02307 14.61 2014 Jul 14 LP600 medium M4K02308 15.52 2014 Aug 26 LP600 low M2K02309 14.79 2014 Jul 12 LP600 high M4K02313 15.1 2014 Sep 02 LP600 low M1K02316 14.82 2014 Jul 14 LP600 medium M3K02323 15.2 2014 Aug 27 LP600 mediumK02327 15.11 2014 Sep 01 LP600 low M3K02328 15.46 2014 Sep 01 LP600 low M2K02329 15.05 2014 Sep 01 LP600 medium M7 iegler et al . TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K02338 14.65 2014 Sep 01 LP600 medium M4K02339 14.72 2014 Aug 22 i (cid:48) high M6K02340 14.53 2014 Aug 21 LP600 medium M4K02345 14.53 2014 Jul 16 LP600 medium M3K02346 15.43 2014 Aug 28 LP600 low M2K02348 15.09 2014 Aug 28 LP600 medium M4K02350 14.84 2014 Jul 17 LP600 medium M5K02353 14.7 2014 Sep 02 LP600 medium M5K02355 15.6 2014 Aug 31 LP600 low M4K02357 15.39 2014 Aug 31 LP600 low M1K02361 14.85 2014 Jul 18 LP600 medium M4K02362 15.6 2014 Aug 28 LP600 low M3K02364 15.53 2014 Aug 28 LP600 low M3K02369 15.63 2014 Nov 09 LP600 medium M4K02372 13.23 2014 Aug 22 i (cid:48) medium M3K02376 14.98 2014 Aug 21 LP600 high M5 yesK02379 14.86 2014 Aug 29 LP600 low M0 yesK02383 14.93 2014 Jul 19 LP600 medium M4K02387 15.11 2014 Sep 02 LP600 medium M3K02396 14.41 2014 Aug 21 LP600 low M3K02397 15.28 2014 Aug 28 LP600 low M3K02401 14.45 2014 Aug 22 i (cid:48) low M4K02404 15.41 2014 Sep 01 LP600 medium M4K02406 14.53 2014 Jul 17 LP600 low M0K02409 14.58 2014 Jul 17 LP600 low M3K02416 15.25 2014 Aug 31 LP600 low M1K02420 14.53 2014 Jun 19 LP600 medium M4K02424 15.59 2014 Sep 03 LP600 medium M5K02432 15.69 2014 Aug 31 LP600 medium M4K02436 15.46 2014 Aug 24 LP600 medium M4K02439 15.25 2014 Aug 27 LP600 high M4K02442 15.33 2014 Sep 02 LP600 low M3K02445 15.56 2014 Aug 28 LP600 high M5 yesK02449 14.89 2014 Sep 02 LP600 high M5K02450 14.6 2014 Jun 19 LP600 medium M4K02451 14.47 2014 Jul 16 LP600 medium M5K02453 14.9 2012 Jul 17 LP600 low M6K02458 15.13 2014 Aug 28 LP600 high M5K02460 14.6 2014 Aug 29 LP600 medium M5 yesK02461 15.66 2014 Aug 28 LP600 low M3K02466 14.57 2014 Jul 17 LP600 medium M5K02472 15.42 2014 Sep 02 LP600 low M1K02473 15.48 2014 Aug 28 LP600 low M3K02477 14.52 2014 Jul 16 LP600 medium M4K02480 15.19 2014 Aug 29 LP600 low M5K02482 14.76 2014 Aug 24 LP600 medium M4 yesK02485 15.01 2014 Sep 01 LP600 medium M5K02487 15.05 2014 Aug 24 LP600 medium M3K02491 15.34 2014 Aug 24 LP600 medium M4K02494 14.63 2014 Jul 14 LP600 high M5K02497 15.29 2014 Sep 03 LP600 medium M5K02506 14.98 2014 Jul 17 LP600 medium M4K02509 14.76 2014 Jul 18 LP600 low M3K02512 15.28 2014 Sep 01 LP600 medium M4K02513 14.67 2014 Jul 18 LP600 medium M3K02520 15.22 2014 Aug 28 LP600 low M4K02521 15.57 2014 Aug 31 LP600 high M5K02524 15.1 2014 Aug 23 LP600 medium M3K02525 15.32 2014 Aug 22 i (cid:48) low M4K02528 15.44 2014 Sep 01 LP600 medium M4K02532 15.12 2014 Aug 26 LP600 medium M5K02535 14.64 2014 Aug 23 LP600 high M6 yesK02543 15.04 2014 Aug 28 LP600 low M4K02544 15.59 2014 Sep 01 LP600 medium M4K02548 14.67 2014 Aug 29 LP600 high M6K02553 15.34 2014 Sep 01 LP600 medium M5K02554 15.4 2014 Sep 01 LP600 high M6 yesK02578 14.65 2014 Jul 14 LP600 medium M4K02579 14.95 2014 Jul 12 LP600 medium M3 yesK02580 15.53 2014 Aug 31 LP600 low M3 yesK02586 15.31 2014 Sep 01 LP600 medium M4K02589 15.33 2014 Sep 01 LP600 high M5K02592 14.87 2014 Jul 17 LP600 low M0K02594 14.96 2014 Nov 09 LP600 medium M4K02602 14.85 2014 Aug 29 LP600 medium M4K02604 14.99 2014 Aug 21 LP600 medium M5K02610 12.61 2015 Jun 04 LP600 high M4 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K02612 11.6 2014 Aug 20 i (cid:48) medium M4K02613 15.67 2014 Aug 28 LP600 high M5K02615 15.5 2014 Aug 28 LP600 low M1K02619 15.69 2014 Aug 24 LP600 high M5K02624 14.97 2014 Aug 21 LP600 high M4K02625 15.63 2014 Sep 01 LP600 low M3K02628 14.63 2014 Sep 02 LP600 medium M3K02637 14.82 2014 Aug 23 LP600 medium M4K02638 15.26 2014 Aug 31 LP600 medium M4K02639 15.33 2014 Sep 03 LP600 medium M3K02647 14.82 2014 Aug 21 LP600 low M3K02655 15.03 2014 Aug 20 i (cid:48) low M2K02660 15.21 2014 Aug 28 LP600 low M0K02668 13.94 2014 Jul 14 LP600 medium M4K02683 15.27 2014 Aug 26 LP600 medium M4K02688 16.05 2014 Aug 31 LP600 high M6 yesK02689 15.35 2014 Sep 02 LP600 low M3K02691 14.59 2014 Jul 14 LP600 low M4K02694 14.58 2014 Jul 17 LP600 high M6K02699 14.93 2014 Sep 01 LP600 medium M5K02703 14.72 2014 Jul 17 LP600 high M6K02708 15.51 2014 Aug 26 LP600 medium M5K02715 16.33 2014 Aug 28 LP600 high M6K02716 15.57 2014 Aug 28 LP600 low M2K02719 14.75 2014 Jul 16 LP600 medium M5K02721 14.93 2014 Jul 16 LP600 medium M4K02728 12.74 2014 Jul 14 LP600 medium M2K02735 15.28 2014 Aug 28 LP600 high M5K02736 15.45 2014 Sep 01 LP600 low M4K02739 14.78 2014 Jul 16 LP600 medium M4K02742 14.51 2014 Jul 17 LP600 medium M6K02744 14.93 2014 Jul 17 LP600 medium M4 yesK02745 15.03 2014 Sep 02 LP600 medium M4K02747 15.0 2014 Jul 16 LP600 medium M5K02751 15.44 2014 Sep 02 LP600 low M4K02758 11.89 2015 Jun 07 LP600 high M5K02760 14.48 2014 Aug 23 LP600 medium M5 yesK02762 14.61 2014 Aug 21 i (cid:48) low M4K02763 15.02 2014 Sep 01 LP600 medium M5K02764 15.22 2014 Sep 01 LP600 high M7K02768 14.99 2014 Aug 31 LP600 medium M4K02770 15.11 2014 Sep 01 LP600 medium M5K02780 15.34 2014 Aug 31 LP600 medium M3K02791 14.54 2014 Aug 21 LP600 low M1K02793 15.64 2014 Sep 02 LP600 low M5K02796 14.64 2014 Jul 17 LP600 medium M4K02797 15.59 2014 Aug 28 LP600 low M1 yesK02802 14.75 2014 Jul 17 LP600 medium M3K02806 15.12 2014 Aug 24 LP600 high M6K02813 13.31 2013 Aug 15 LP600 medium M5 yesK02816 15.22 2014 Sep 03 LP600 medium M4K02817 15.46 2014 Nov 07 LP600 low M3K02820 15.07 2014 Sep 01 LP600 medium M4K02821 15.05 2014 Aug 26 LP600 high M5K02828 15.37 2014 Aug 26 LP600 high M6K02832 13.63 2014 Jul 16 LP600 medium M5K02834 15.46 2014 Nov 09 LP600 medium M5K02835 15.47 2014 Aug 26 LP600 medium M5K02841 15.54 2014 Aug 30 LP600 low M3K02845 15.0 2014 Sep 02 LP600 low M5K02851 15.2 2014 Aug 26 LP600 high M5 yesK02852 15.65 2014 Aug 24 LP600 high M5K02853 14.64 2014 Sep 02 LP600 medium M5K02856 15.11 2014 Aug 26 LP600 low M1 yesK02862 15.29 2014 Aug 27 LP600 high M8 yesK02865 15.15 2014 Aug 31 LP600 low M1K02871 14.52 2014 Aug 21 LP600 medium M4K02874 14.62 2014 Sep 01 LP600 medium M4K02875 14.53 2014 Jul 17 LP600 low M3K02876 14.62 2014 Jul 16 LP600 low M4K02877 14.49 2014 Jul 17 LP600 medium M4K02878 14.45 2014 Aug 31 LP600 medium M5K02886 15.61 2014 Aug 26 LP600 high M5K02894 15.38 2014 Aug 27 LP600 low M2K02896 11.9 2015 Jun 05 LP600 high M4 yesK02898 15.35 2014 Sep 03 LP600 medium M3K02899 15.63 2014 Aug 24 LP600 high M5 obo -AO Kepler P lanetary C andidate S urvey III 29
TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K02900 14.95 2014 Sep 03 LP600 high M5 yesK02916 14.11 2014 Jul 17 LP600 medium M5K02919 14.57 2014 Sep 02 LP600 medium M4K02920 14.38 2014 Jul 14 LP600 medium M4K02921 15.18 2014 Sep 01 LP600 medium M5K02925 13.22 2014 Jul 17 LP600 high M5K02926 15.69 2014 Aug 28 LP600 high M7 yesK02927 15.65 2014 Aug 28 LP600 high M4 yesK02931 14.4 2014 Aug 22 i (cid:48) low M3K02933 15.4 2014 Aug 28 LP600 low M4K02945 15.78 2014 Aug 29 LP600 low M2K02946 15.47 2014 Sep 02 LP600 low M1K02950 14.18 2014 Jul 17 LP600 medium M4K02957 14.15 2014 Jul 16 LP600 medium M5K02958 14.59 2014 Sep 02 LP600 medium M3 yesK02975 15.1 2014 Sep 01 LP600 medium M4K02976 15.6 2014 Aug 28 LP600 low M3 yesK02980 15.29 2014 Aug 28 LP600 low M1K02981 15.42 2014 Sep 01 LP600 high M5K02995 15.42 2014 Aug 28 LP600 low M0K02996 15.41 2014 Aug 31 LP600 low M3K03009 14.87 2014 Aug 21 LP600 low M3K03010 15.17 2014 Aug 22 i (cid:48) low M5K03013 14.48 2014 Jul 13 LP600 high M5K03014 15.63 2014 Aug 24 LP600 low M1K03020 13.36 2013 Aug 13 LP600 high M4 yesK03022 15.17 2014 Aug 27 LP600 high M5K03027 15.16 2014 Sep 01 LP600 low M3K03031 15.03 2014 Aug 27 LP600 low M2K03034 14.98 2014 Jul 16 LP600 medium M6K03037 15.61 2014 Nov 09 LP600 medium M4K03042 15.75 2014 Aug 31 LP600 low M1 yesK03043 14.64 2014 Jul 12 LP600 high M5 yesK03045 15.56 2014 Nov 08 LP600 medium M3K03051 15.08 2014 Aug 31 LP600 low M1K03063 15.51 2014 Aug 28 LP600 medium M2K03066 15.85 2014 Aug 24 LP600 low M3 yesK03072 15.27 2014 Aug 23 LP600 low M3K03077 15.57 2014 Aug 31 LP600 high M6K03078 15.14 2014 Aug 28 LP600 high M4K03088 14.75 2014 Jul 12 LP600 low M1K03089 14.96 2014 Jul 17 LP600 medium M5K03090 15.07 2014 Aug 27 LP600 high M7K03091 15.21 2014 Sep 02 LP600 low M0K03094 15.13 2014 Sep 02 LP600 medium M7K03095 14.86 2014 Aug 21 LP600 medium M4K03096 13.35 2014 Jul 17 LP600 medium M4K03102 15.4 2014 Aug 23 LP600 medium M7K03104 15.13 2014 Sep 03 LP600 medium M4K03106 15.17 2014 Aug 26 LP600 high M5 yesK03110 14.7 2014 Jul 18 LP600 low M0K03111 12.66 2014 Aug 20 i (cid:48) low M1 yesK03112 15.64 2014 Sep 01 LP600 high M5 yesK03113 14.89 2014 Nov 07 LP600 low M4K03115 15.06 2014 Aug 28 LP600 low M1K03116 15.2 2014 Aug 28 LP600 high M4K03120 14.64 2014 Aug 29 LP600 low M1 yesK03131 15.36 2014 Sep 01 LP600 low M2K03136 15.4 2014 Aug 28 LP600 low M4 yesK03137 15.42 2014 Aug 28 LP600 low M3K03138 16.69 2014 Aug 31 LP600 lowK03141 14.62 2014 Jul 17 LP600 medium M4K03144 15.38 2014 Nov 09 LP600 medium M8K03161 9.58 2015 Jun 03 LP600 high M3 yesK03165 10.22 2014 Aug 22 i (cid:48) high M4K03168 10.29 2014 Aug 22 i (cid:48) high M5K03202 11.53 2014 Aug 22 i (cid:48) high M5K03214 11.81 2014 Aug 29 LP600 high M4 yesK03224 11.96 2014 Aug 23 i (cid:48) high M5K03225 11.97 2014 Aug 22 i (cid:48) high M5K03248 12.24 2014 Aug 22 i (cid:48) high M5K03258 15.45 2014 Aug 26 LP600 medium M4K03262 14.87 2014 Sep 03 LP600 medium M3K03263 15.27 2014 Aug 23 LP600 low M6 yesK03264 15.6 2014 Aug 28 LP600 low M4 yesK03266 15.04 2014 Aug 26 LP600 low M4K03267 14.53 2014 Aug 21 LP600 high M4 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K03268 15.33 2014 Sep 03 LP600 medium M4K03271 15.46 2014 Aug 31 LP600 low M3K03274 15.11 2014 Aug 24 LP600 medium M4K03279 15.56 2014 Aug 26 LP600 high M5K03280 15.37 2014 Sep 03 LP600 medium M4K03281 14.9 2015 Jun 04 LP600 low M3K03282 15.27 2014 Aug 31 LP600 medium M6K03283 15.32 2015 Jun 08 LP600 highK03287 13.88 2014 Aug 20 i (cid:48) low M1K03298 15.49 2014 Aug 26 LP600 high M6K03303 15.35 2014 Aug 26 LP600 low M4K03305 15.58 2014 Sep 03 LP600 medium M4K03306 15.54 2014 Aug 26 LP600 high M5K03307 15.35 2014 Aug 26 LP600 low M3K03312 15.54 2014 Sep 03 LP600 medium M4K03313 14.41 2014 Jul 17 LP600 medium M5K03316 15.26 2014 Aug 26 LP600 high M5K03319 14.8 2014 Aug 31 LP600 medium M4K03320 15.62 2014 Sep 01 LP600 low M3K03323 14.84 2014 Aug 31 LP600 medium M4K03329 15.62 2014 Aug 31 LP600 low M0K03330 14.72 2014 Jul 16 LP600 medium M5K03331 15.69 2014 Aug 31 LP600 high M5K03335 15.63 2014 Sep 01 LP600 low M0 yesK03337 15.66 2014 Sep 03 LP600 low M3K03341 14.69 2014 Jul 17 LP600 medium M3 yesK03342 15.53 2014 Aug 29 LP600 high M4K03344 15.04 2014 Sep 02 LP600 low M1K03347 15.23 2014 Aug 28 LP600 high M5 yesK03348 15.02 2014 Aug 31 LP600 medium M4K03349 15.11 2014 Aug 24 LP600 medium M3K03352 15.19 2014 Aug 24 LP600 high M5K03354 14.86 2014 Jul 16 LP600 high M5 yesK03355 14.93 2014 Jul 18 LP600 high M4K03356 15.24 2014 Aug 26 LP600 medium M4K03357 14.96 2014 Sep 01 LP600 high M5K03358 13.79 2014 Jul 16 LP600 medium M4K03361 15.28 2014 Aug 24 LP600 medium M4K03367 14.87 2014 Jun 19 LP600 medium M3K03370 14.43 2014 Jul 13 LP600 medium M5K03372 15.24 2014 Aug 23 LP600 high M4 yesK03375 15.45 2014 Sep 01 LP600 medium M4K03383 15.59 2014 Aug 24 LP600 high M5K03386 14.94 2014 Jul 17 LP600 medium M3K03391 15.45 2014 Aug 28 LP600 low M4K03393 15.13 2014 Sep 01 LP600 high M4K03394 15.3 2014 Aug 28 LP600 medium M3K03395 14.42 2014 Jul 14 LP600 medium M4K03396 15.33 2014 Aug 26 LP600 low M2K03397 15.2 2014 Aug 28 LP600 medium M2K03404 14.64 2014 Jul 14 LP600 low M1K03407 15.2 2014 Aug 24 LP600 medium M4K03410 15.37 2014 Aug 28 LP600 low M1K03411 14.43 2015 Jun 03 LP600 low M1K03412 14.13 2014 Jul 17 LP600 medium M5K03413 15.02 2014 Aug 26 LP600 medium M3 yesK03415 13.08 2013 Jul 27 LP600 high M5 yesK03416 15.11 2014 Nov 07 LP600 low M3K03417 14.99 2014 Jul 14 LP600 high M5K03418 15.2 2014 Aug 23 LP600 low M1 yesK03420 15.38 2014 Aug 26 LP600 low M1K03421 13.79 2014 Aug 22 i (cid:48) medium M2K03426 14.13 2014 Jul 14 LP600 high M4K03428 14.52 2014 Aug 20 i (cid:48) low M1K03432 14.76 2014 Jul 16 LP600 high M5 yesK03433 15.11 2014 Aug 21 LP600 low M3K03434 14.76 2014 Jul 18 LP600 high M4K03436 13.2 2014 Jul 14 LP600 high M6K03443 15.52 2014 Aug 31 LP600 low M3K03445 15.42 2014 Sep 02 LP600 low M2K03449 14.55 2014 Aug 21 LP600 medium M5K03455 15.57 2014 Aug 27 LP600 high M5K03458 15.44 2014 Aug 28 LP600 high M4K03463 14.56 2015 Jun 07 LP600 medium M4 yesK03465 12.89 2014 Aug 29 LP600 high M5K03467 15.0 2014 Jun 19 LP600 medium M3K03470 15.2 2014 Sep 01 LP600 medium M4 iegler et al . TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K03471 12.96 2014 Jul 11 LP600 high M6 yesK03472 14.25 2014 Jun 19 LP600 medium M3K03473 13.53 2014 Jun 15 LP600 medium M5K03478 13.35 2015 Jun 10 LP600 medium M5K03480 15.7 2014 Sep 03 LP600 low M3 yesK03482 14.9 2014 Jun 19 LP600 medium M4K03483 14.7 2014 Nov 09 LP600 medium M3 yesK03487 14.09 2014 Jul 17 LP600 high M5K03493 15.02 2014 Sep 01 LP600 medium M4K03495 14.92 2014 Jun 19 LP600 medium M4K03504 15.72 2015 Jun 06 LP600 low M2K03515 12.13 2014 Jun 13 LP600 high M4K03520 13.67 2015 Jun 04 LP600 medium M4K03522 10.66 2015 Jun 12 LP600 high M0K03527 13.85 2014 Jun 15 LP600 medium M4K03531 14.42 2014 Jul 18 LP600 low M1K03533 14.44 2014 Nov 09 LP600 high M4 yesK03545 15.47 2014 Aug 24 LP600 high M6K03554 14.99 2014 Aug 22 i (cid:48) low M2K03560 11.69 2014 Jul 16 LP600 high M4K03565 15.64 2014 Aug 28 LP600 high M5K03581 16.35 2014 Jul 18 LP600 high M6K03605 13.87 2014 Jul 16 LP600 medium M5K03606 14.05 2014 Aug 21 LP600 medium M2K03611 16.3 2014 Aug 26 LP600 low M1 yesK03617 14.61 2014 Aug 21 LP600 high M2K03620 15.05 2014 Sep 03 LP600 high M5K03626 16.21 2014 Sep 03 LP600 high M5 yesK03641 13.76 2014 Jul 14 LP600 high M5K03647 16.44 2014 Aug 23 LP600 medium M3K03649 15.21 2014 Aug 23 LP600 high M4 yesK03652 15.58 2014 Aug 29 LP600 high M5K03660 15.31 2014 Aug 24 LP600 low M2 yesK03674 15.4 2014 Sep 03 LP600 medium M4K03675 16.28 2014 Aug 31 LP600 low M3K03678 12.59 2014 Jun 17 LP600 high M5 yesK03685 14.42 2014 Aug 21 LP600 medium M4K03690 15.33 2014 Aug 31 LP600 medium M3K03692 14.92 2014 Jul 14 LP600 high M4K03696 15.47 2014 Aug 26 LP600 medium M4K03709 15.07 2014 Aug 26 LP600 high M4K03716 11.61 2015 Jun 05 LP600 highK03717 14.79 2014 Sep 02 LP600 medium M3K03720 13.26 2014 Aug 21 LP600 medium M1K03726 15.4 2014 Aug 29 LP600 high M6K03738 17.17 2014 Aug 23 LP600 high M5K03741 13.15 2014 Jun 13 LP600 medium M3K03749 15.64 2014 Aug 28 LP600 low M8K03765 16.02 2014 Sep 02 LP600 low M4K03767 17.01 2014 Aug 21 LP600 high M5K03770 13.93 2014 Jun 19 LP600 medium M3 yesK03771 16.34 2014 Aug 23 LP600 high M5K03783 12.84 2014 Aug 21 LP600 high M3 yesK03784 14.02 2014 Jul 16 LP600 medium M4K03791 13.61 2014 Aug 22 i (cid:48) low M0 yesK03794 15.26 2014 Sep 02 LP600 medium M5K03801 15.75 2014 Aug 20 i (cid:48) low M2K03815 15.23 2014 Aug 26 LP600 high M4K03818 11.91 2014 Aug 22 i (cid:48) medium K7K03823 13.86 2014 Jul 17 LP600 medium M4K03830 16.77 2014 Aug 26 LP600 high M5K03853 10.32 2014 Aug 22 i (cid:48) high M5K03855 18.23 2014 Nov 09 LP600 low M2K03867 14.64 2014 Jul 17 LP600 medium M4K03871 11.94 2014 Aug 31 LP600 high M5K03878 12.72 2015 Jun 04 LP600 medium M4K03880 10.76 2015 Jun 04 LP600 high M4K03886 9.46 2014 Aug 20 i (cid:48) high M6 yesK03890 12.87 2014 Aug 20 i (cid:48) high M6K03901 15.09 2014 Sep 03 LP600 medium M4K03909 14.78 2014 Aug 31 LP600 medium M3K03913 14.8 2014 Aug 21 LP600 medium M3K03923 15.11 2014 Aug 26 LP600 medium M6K03928 13.06 2014 Jul 14 LP600 high M4 yesK03933 14.45 2014 Jul 12 LP600 low M3K03936 13.03 2014 Jun 13 LP600 medium M5K03939 15.02 2014 Aug 28 LP600 low M0 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K03975 14.71 2014 Aug 21 LP600 medium M5K04002 14.75 2014 Jul 14 LP600 medium M5K04007 15.28 2014 Aug 24 LP600 medium M3K04009 15.06 2014 Aug 26 LP600 medium M3K04011 12.37 2014 Jul 13 LP600 high M4K04015 15.02 2014 Aug 24 LP600 medium M5K04022 13.1 2014 Jul 14 LP600 high M4K04024 13.53 2014 Jul 17 LP600 high M5K04036 13.7 2014 Aug 20 i (cid:48) low M4K04062 13.91 2014 Aug 29 LP600 medium M3 yesK04076 15.05 2014 Sep 02 LP600 low M2K04084 14.9 2014 Jun 15 LP600 high M5K04087 14.54 2014 Aug 22 i (cid:48) low M5K04091 14.71 2014 Jul 14 LP600 low M1K04099 15.05 2014 Aug 31 LP600 low M3K04103 14.84 2015 Jun 08 LP600 low M3K04117 14.69 2014 Aug 31 LP600 medium M5K04120 14.93 2014 Jul 19 LP600 low M0K04121 15.46 2014 Aug 31 LP600 low M3K04126 15.17 2014 Sep 03 LP600 medium M3K04127 15.0 2014 Aug 26 LP600 high M5K04131 13.17 2014 Jun 19 LP600 high M2 yesK04135 14.49 2014 Aug 20 i (cid:48) low M4K04139 15.15 2014 Aug 28 LP600 medium M3K04178 14.4 2015 Jun 12 LP600 high M4K04185 15.29 2014 Sep 01 LP600 low M3K04189 15.37 2014 Aug 28 LP600 high M4K04192 14.77 2014 Aug 29 LP600 high M5K04202 15.45 2014 Aug 26 LP600 medium M4K04204 13.8 2014 Aug 29 LP600 high M5K04207 14.88 2014 Jun 19 LP600 high M6K04222 13.52 2014 Jun 13 LP600 medium M4K04232 14.98 2014 Aug 21 LP600 low M1K04234 14.97 2014 Aug 21 LP600 low M1K04246 13.16 2014 Jul 11 LP600 medium M4K04255 14.68 2014 Aug 21 LP600 medium M5K04257 13.1 2014 Jul 11 LP600 high M5K04259 14.92 2014 Jul 17 LP600 low M3K04261 15.17 2014 Sep 02 LP600 low M1K04267 15.0 2014 Jun 19 LP600 medium M3 yesK04268 14.77 2014 Aug 31 LP600 high M6 yesK04290 16.58 2015 Jun 10 LP600 low M9K04294 14.66 2014 Sep 01 LP600 medium M3K04298 13.37 2014 Sep 03 LP600 high M3K04307 14.04 2014 Aug 20 i (cid:48) low M1K04323 13.4 2014 Jun 13 LP600 high M4 yesK04333 14.01 2014 Aug 20 i (cid:48) low M1K04334 15.49 2014 Sep 01 LP600 low M4 yesK04343 13.49 2014 Jun 19 LP600 medium M4 yesK04345 13.19 2014 Jul 13 LP600 medium M4 yesK04346 14.67 2014 Jul 16 LP600 medium M4K04351 14.71 2014 Jul 17 LP600 medium M5K04353 15.36 2014 Aug 24 LP600 low M1 yesK04357 14.75 2014 Jul 16 LP600 low M3K04360 14.62 2014 Jul 18 LP600 medium M3K04361 14.93 2014 Sep 01 LP600 medium M4K04363 15.71 2014 Aug 28 LP600 high M5K04364 15.17 2014 Aug 26 LP600 low M3K04366 15.29 2014 Aug 28 LP600 high M5 yesK04371 15.19 2014 Sep 03 LP600 medium M3K04372 15.14 2014 Sep 02 LP600 low M4K04377 13.34 2014 Jul 16 LP600 medium M3K04384 14.74 2014 Jul 16 LP600 medium M4K04385 15.51 2014 Aug 28 LP600 high M5K04386 15.51 2014 Aug 26 LP600 low M3K04391 14.75 2014 Jul 17 LP600 medium M4K04398 15.24 2014 Aug 31 LP600 high M5K04405 14.49 2014 Jul 17 LP600 medium M3 yesK04410 15.54 2014 Aug 31 LP600 low M1K04418 15.71 2014 Sep 03 LP600 low M2 yesK04421 12.63 2014 Jul 12 LP600 high M4 yesK04424 15.14 2014 Aug 24 LP600 medium M3K04426 13.49 2014 Aug 20 i (cid:48) low M0K04442 14.11 2014 Jul 17 LP600 medium M4K04444 15.08 2014 Aug 28 LP600 low M4K04447 14.44 2014 Aug 21 i (cid:48) low M4K04450 14.89 2014 Aug 31 LP600 medium M4 obo -AO Kepler P lanetary C andidate S urvey III 31
TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K04451 15.63 2014 Sep 01 LP600 low M4K04452 13.62 2014 Jul 16 LP600 low M1K04462 11.1 2014 Aug 20 i (cid:48) high M2K04464 14.7 2014 Aug 21 LP600 medium M5K04466 14.84 2014 Jun 19 LP600 medium M3K04467 15.63 2014 Aug 26 LP600 high M5 yesK04473 13.66 2014 Jul 17 LP600 medium M4K04477 15.23 2014 Aug 27 LP600 medium M4K04480 13.9 2014 Aug 29 LP600 medium M4K04484 14.91 2014 Jul 11 LP600 high M4K04487 14.1 2014 Aug 21 LP600 high M5K04491 14.82 2014 Jun 17 LP600 low M0K04496 15.38 2014 Nov 10 LP600 medium M4K04497 14.97 2014 Sep 03 LP600 high M5K04498 14.64 2014 Jul 16 LP600 low M1K04499 14.46 2014 Jul 16 LP600 medium M4K04500 15.55 2014 Aug 24 LP600 high M5K04503 15.47 2014 Aug 28 LP600 high M5K04504 15.69 2014 Aug 28 LP600 high M5K04506 15.42 2014 Nov 09 LP600 medium M5K04508 14.96 2014 Aug 31 LP600 medium M5K04509 15.2 2014 Sep 01 LP600 medium M6K04513 14.52 2014 Aug 21 LP600 medium M4K04519 14.6 2014 Aug 29 LP600 medium M3K04524 14.74 2014 Jul 17 LP600 medium M4K04526 15.06 2014 Aug 24 LP600 high M4 yesK04546 13.31 2014 Jul 14 LP600 medium M3K04548 14.5 2014 Jul 14 LP600 low M3K04549 15.73 2014 Aug 27 LP600 high M5 yesK04550 15.05 2014 Aug 29 LP600 high M6 yesK04551 14.46 2014 Jul 18 LP600 medium M4K04557 13.51 2014 Jul 16 LP600 high M4K04571 14.35 2014 Jul 16 LP600 medium M4K04577 14.7 2014 Aug 31 LP600 medium M4K04583 15.53 2014 Sep 01 LP600 medium M4K04585 13.37 2014 Jul 19 LP600 medium M2K04587 15.36 2014 Nov 09 LP600 medium M4K04590 15.53 2014 Sep 02 LP600 low M3 yesK04595 15.2 2014 Aug 28 LP600 low M4K04597 14.46 2014 Jul 17 LP600 medium M4K04602 14.41 2014 Aug 29 LP600 medium M4K04622 14.61 2014 Aug 23 LP600 high M6K04626 14.66 2014 Aug 31 LP600 medium M4K04630 14.66 2014 Jul 17 LP600 medium M4 yesK04632 15.34 2014 Aug 21 LP600 high M5K04636 15.23 2014 Aug 27 LP600 high M5K04640 13.48 2014 Jun 19 LP600 high M4K04643 15.09 2014 Sep 02 LP600 medium M4K04647 13.43 2014 Jul 13 LP600 high M5K04649 15.2 2014 Aug 26 LP600 medium M4K04650 15.46 2014 Sep 02 LP600 high M6K04653 13.38 2014 Jul 19 LP600 high M4 yesK04655 15.18 2014 Aug 23 LP600 low M1 yesK04659 13.47 2014 Aug 20 i (cid:48) low M1K04661 14.49 2014 Jul 18 LP600 medium M5 yesK04666 15.11 2014 Sep 03 LP600 medium M4K04667 15.24 2014 Aug 28 LP600 high M4K04676 13.68 2014 Jul 14 LP600 high M5K04686 12.09 2014 Aug 20 i (cid:48) medium M4K04694 14.68 2014 Aug 21 LP600 medium M3K04698 14.61 2014 Sep 02 LP600 medium M2K04700 15.7 2014 Aug 31 LP600 high M5 yesK04705 14.83 2014 Jul 14 LP600 low M2K04710 15.38 2014 Sep 01 LP600 medium M4 yesK04711 15.41 2014 Aug 31 LP600 low M3K04713 13.6 2014 Jul 16 LP600 medium M4 yesK04714 15.01 2014 Sep 02 LP600 medium M5K04715 13.77 2014 Aug 21 i (cid:48) medium M4K04716 12.17 2014 Aug 22 i (cid:48) medium M3K04717 15.33 2014 Sep 03 LP600 medium M4K04725 13.01 2014 Jul 17 LP600 high M6K04730 14.04 2014 Aug 21 LP600 medium M5K04733 15.63 2014 Sep 01 LP600 high M6K04735 14.4 2014 Jul 17 LP600 medium M5K04742 14.56 2014 Aug 22 i (cid:48) low M4K04743 14.71 2014 Sep 03 LP600 medium M4 yesK04745 15.54 2014 Aug 22 i (cid:48) high M6 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K04749 15.37 2014 Aug 28 LP600 medium M4K04750 15.67 2014 Aug 29 LP600 high M5 yesK04755 14.67 2014 Jul 16 LP600 medium M4K04756 15.23 2014 Aug 27 LP600 high M4K04758 15.69 2014 Sep 01 LP600 low M3K04759 14.77 2014 Jul 19 LP600 medium M4 yesK04762 15.25 2014 Sep 01 LP600 medium M5K04765 13.24 2014 Jul 17 LP600 high M4K04766 14.93 2014 Nov 08 LP600 medium M5K04771 13.85 2014 Aug 22 i (cid:48) medium M2K04774 13.5 2014 Aug 20 i (cid:48) low M3K04780 15.16 2014 Aug 28 LP600 medium M4K04790 14.25 2014 Jun 13 LP600 medium M3K04794 14.09 2014 Jul 19 LP600 medium M5K04799 14.01 2014 Jul 14 LP600 medium M4K04803 14.71 2014 Sep 03 LP600 medium M4K04804 15.0 2014 Aug 26 LP600 low M1K04810 15.04 2014 Aug 24 LP600 medium M4 yesK04815 14.76 2014 Jun 19 LP600 medium M4K04820 15.27 2014 Aug 23 LP600 medium M4K04827 15.15 2014 Aug 21 LP600 low M2K04837 15.1 2014 Aug 23 LP600 low M3K04838 14.59 2014 Jul 16 LP600 medium M6K04840 14.44 2014 Jul 14 LP600 medium M4K04848 15.14 2014 Aug 23 LP600 low M4K04857 15.17 2014 Aug 24 LP600 medium M4K04859 15.19 2014 Aug 23 LP600 low M4K04862 15.23 2014 Sep 03 LP600 medium M5K04864 13.02 2014 Jul 16 LP600 medium M4K04878 12.12 2014 Aug 22 i (cid:48) high M4K04881 12.69 2014 Aug 21 LP600 medium M2 yesK04885 14.77 2014 Jul 16 LP600 medium M4K04886 15.6 2014 Aug 24 LP600 high M5K04890 15.61 2014 Sep 01 LP600 high M4K04893 15.45 2014 Aug 28 LP600 low M1K04895 14.52 2014 Aug 31 LP600 medium M4 yesK04896 15.25 2014 Sep 02 LP600 low M1K04900 14.94 2014 Jul 14 LP600 medium M4K04902 15.15 2015 Jun 12 LP600 low M4K04912 14.69 2014 Sep 03 LP600 medium M3K04913 13.23 2014 Jul 14 LP600 high M4K04922 13.4 2014 Jul 14 LP600 medium M3K04923 13.02 2014 Jul 14 LP600 medium M3 yesK04926 15.57 2015 Jun 04 LP600 low M4K04927 14.56 2014 Jul 14 LP600 low M0K04928 14.97 2014 Sep 03 LP600 medium L0K04933 14.92 2014 Aug 30 LP600 low M0K04936 12.54 2015 Jun 04 LP600 medium M4K04938 15.37 2014 Aug 24 LP600 high M4K04939 15.97 2014 Aug 23 LP600 high M6K04946 16.84 2014 Nov 08 LP600 low M3K04950 15.92 2014 Nov 08 LP600 low M4K04958 12.1 2014 Aug 20 i (cid:48) medium M4K04959 13.71 2014 Jul 17 LP600 medium M2K04960 14.22 2014 Jul 16 LP600 mediumK04961 14.94 2014 Sep 03 LP600 medium M5K04962 14.05 2014 Jul 16 LP600 low M1K04967 15.44 2014 Aug 26 LP600 medium M3K04968 11.1 2014 Aug 30 LP600 high M6K04971 15.17 2014 Aug 29 LP600 medium M8K04972 13.83 2014 Jul 17 LP600 high M4K04974 15.51 2014 Aug 26 LP600 high M5 yesK04975 15.47 2014 Aug 24 LP600 medium M4K04976 13.41 2014 Jul 16 LP600 medium M1K04977 15.12 2014 Nov 09 LP600 medium M5K04978 15.01 2014 Aug 23 LP600 medium M4K04980 11.15 2014 Jul 14 LP600 high M4K04982 14.19 2015 Jun 04 LP600 medium M3K04985 12.53 2014 Jul 16 LP600 high M3K04986 14.59 2014 Aug 31 LP600 low M2K04988 13.66 2014 Jun 19 LP600 medium M4K04991 15.06 2014 Aug 26 LP600 high M5K04992 14.9 2014 Jun 13 LP600 high M5K04993 12.47 2014 Sep 01 LP600 high yesK04997 15.32 2014 Aug 28 LP600 low M0K04999 15.28 2014 Sep 03 LP600 medium M4K05002 12.64 2014 Aug 22 i (cid:48) medium M3 iegler et al . TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K05004 14.26 2014 Jul 16 LP600 low M2 yesK05007 13.47 2014 Jul 16 LP600 medium M4K05018 14.92 2014 Jun 15 LP600 high M5K05021 14.97 2014 Sep 03 LP600 medium M4K05023 13.46 2014 Jul 14 LP600 medium M0K05027 13.17 2015 Jun 06 LP600 high M6K05030 14.45 2015 Jun 03 LP600 low M0K05031 11.97 2014 Aug 20 i (cid:48) mediumK05033 13.83 2015 Jun 03 LP600 low M4K05034 13.25 2015 Jun 05 LP600 medium M3K05039 15.58 2014 Sep 03 LP600 medium M5K05040 14.38 2015 Jun 03 LP600 low M0K05043 15.08 2014 Aug 31 LP600 low M2K05046 12.86 2014 Jun 13 LP600 high M4K05047 14.7 2015 Jun 03 LP600 low M1K05048 13.42 2015 Jun 03 LP600 medium M5K05052 12.53 2014 Jun 17 LP600 medium M1 yesK05053 13.81 2014 Jul 16 LP600 high M5K05057 12.19 2014 Jul 14 LP600 high M6K05058 13.31 2015 Jun 08 LP600 medium M3K05059 13.03 2015 Jun 07 LP600 high M4K05067 14.25 2015 Jun 03 LP600 low M2K05068 12.95 2014 Jul 14 LP600 high M4K05070 9.9 2014 Sep 01 LP600 high M0K05071 15.66 2015 Jun 10 LP600 low M1K05079 13.05 2014 Jun 17 LP600 medium M3K05080 14.61 2014 Jul 17 LP600 lowK05081 14.08 2014 Jul 17 LP600 high M5K05083 13.81 2015 Jun 12 LP600 medium M5K05084 15.76 2015 Jun 08 LP600 low M2K05085 15.94 2015 Jun 08 LP600 low M2K05086 10.95 2015 Jun 03 LP600 high M5K05087 12.3 2014 Aug 20 i (cid:48) low M2K05088 15.53 2015 Jun 03 LP600 low M2K05092 13.89 2015 Jun 08 LP600 medium M2K05093 12.69 2015 Jun 10 LP600 high M4K05098 14.86 2015 Jun 04 LP600 low M3K05099 12.71 2015 Jun 07 LP600 high M5K05101 12.89 2014 Jul 17 LP600 high M4 yesK05102 14.85 2014 Aug 30 LP600 medium M4K05104 15.53 2015 Jun 08 LP600 low M1K05107 13.74 2015 Jun 07 LP600 medium M5K05109 14.09 2015 Jun 04 LP600 medium M4K05110 11.65 2015 Jun 03 LP600 medium M5K05115 15.77 2015 Jun 10 LP600 low M0K05117 15.71 2014 Aug 24 LP600 low M3K05119 12.64 2015 Jun 06 LP600 high M5K05121 12.41 2014 Jul 14 LP600 high M4K05122 16.16 2014 Nov 09 LP600 low M4K05123 14.03 2014 Jul 17 LP600 medium M4K05124 15.77 2015 Jun 08 LP600 low M3K05126 13.64 2015 Jun 12 LP600 medium M5K05129 11.6 2015 Jun 03 LP600 highK05131 15.22 2015 Jun 04 LP600 low M0K05132 12.78 2015 Jun 08 LP600 high M6K05135 15.28 2014 Aug 27 LP600 medium M5K05136 12.2 2014 Aug 20 i (cid:48) lowK05138 14.08 2015 Jun 12 LP600 low M1K05142 15.51 2014 Sep 03 LP600 medium M5K05143 15.67 2014 Nov 09 LP600 high yesK05148 15.1 2014 Aug 24 LP600 medium M3K05149 15.65 2015 Jun 12 LP600 low M2K05156 12.07 2015 Jun 04 LP600 high M4K05158 11.87 2015 Jun 03 LP600 medium M2K05159 14.73 2014 Jun 13 LP600 highK05164 12.37 2014 Aug 23 i (cid:48) medium M3K05169 15.17 2014 Aug 28 LP600 low M3K05176 13.17 2014 Jul 17 LP600 high M5K05178 14.28 2015 Jun 12 LP600 medium M2K05184 15.48 2014 Aug 31 LP600 low M1K05186 13.29 2014 Jul 17 LP600 high M4K05191 14.34 2014 Jul 14 LP600 medium M5K05192 14.87 2015 Jun 10 LP600 low M4K05194 13.56 2014 Jul 17 LP600 mediumK05196 12.25 2014 Aug 20 i (cid:48) low M0K05198 15.43 2014 Nov 09 LP600 medium M4K05201 15.0 2014 Aug 27 LP600 medium M3 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K05202 14.48 2014 Jun 19 LP600 medium M4K05205 12.84 2015 Jun 03 LP600 medium M3K05206 14.74 2015 Jun 03 LP600 low M1K05207 13.05 2015 Jun 03 LP600 medium M4K05210 14.86 2014 Jul 14 LP600 medium yesK05211 12.7 2014 Jun 17 LP600 high M5K05212 12.12 2014 Aug 22 i (cid:48) medium M3K05216 15.27 2014 Aug 31 LP600 medium M4 yesK05219 14.94 2014 Sep 03 LP600 medium M4K05220 11.83 2014 Sep 03 LP600 high M6 yesK05223 13.68 2015 Jun 03 LP600 medium M5K05224 14.69 2014 Jul 14 LP600 medium M4K05225 15.07 2014 Nov 08 LP600 medium M3K05228 14.61 2014 Jul 17 LP600 medium M8K05230 13.11 2014 Jun 19 LP600 high M5K05232 13.55 2014 Aug 31 LP600 high M4 yesK05235 12.74 2014 Aug 20 i (cid:48) low M0K05236 13.09 2015 Jun 06 LP600 high M4K05237 15.11 2014 Aug 29 LP600 medium M4K05238 10.86 2014 Jul 19 LP600 medium M4K05241 15.23 2015 Jun 12 LP600 low M1K05243 12.21 2014 Sep 03 LP600 high M4 yesK05245 13.03 2015 Jun 03 LP600 medium M5K05247 14.81 2015 Jun 10 LP600 low M0K05248 14.91 2014 Jul 19 LP600 medium M4K05249 14.35 2014 Sep 03 LP600 medium M3K05254 10.73 2014 Aug 22 i (cid:48) high M5K05255 13.16 2015 Jun 10 LP600 medium M3K05257 14.98 2014 Jul 16 LP600 medium M4K05261 14.92 2014 Jul 17 LP600 high M4K05267 14.33 2015 Jun 04 LP600 low M0K05269 15.39 2015 Jun 10 LP600 low M2K05279 14.78 2015 Jun 08 LP600 low M2K05281 13.48 2015 Jun 04 LP600 medium M5K05283 13.84 2014 Jun 19 LP600 medium M4K05284 14.57 2015 Jun 03 LP600 low M2K05287 13.56 2015 Jun 04 LP600 medium M5K05288 15.43 2014 Aug 29 LP600 medium M4K05290 15.67 2015 Jun 10 LP600 low M2K05297 14.44 2015 Jun 04 LP600 low M3K05298 13.54 2015 Jun 08 LP600 medium M4K05300 12.9 2014 Jul 17 LP600 high M4K05308 14.1 2015 Jun 08 LP600 medium M5K05309 14.68 2014 Jul 16 LP600 lowK05310 13.99 2015 Jun 04 LP600 low M2K05321 13.64 2014 Jul 14 LP600 low M1K05322 13.91 2015 Jun 03 LP600 low M4K05323 13.67 2015 Jun 04 LP600 medium M5K05324 13.71 2015 Jun 08 LP600 medium M5K05325 15.46 2014 Aug 27 LP600 medium M4K05326 12.41 2014 Aug 20 i (cid:48) low M1K05327 14.99 2014 Sep 01 LP600 high M8 yesK05329 15.39 2015 Jun 08 LP600 low M1K05331 14.89 2014 Aug 31 LP600 medium M5 yesK05332 14.3 2015 Jun 12 LP600 medium M3 yesK05335 11.19 2014 Jun 13 LP600 high M5K05336 13.36 2014 Jul 16 LP600 high M4K05339 15.35 2015 Jun 03 LP600 low K2K05340 14.97 2014 Jun 19 LP600 low M0 yesK05341 12.49 2015 Jun 03 LP600 medium M3K05342 15.08 2014 Aug 23 LP600 mediumK05344 13.73 2015 Jun 04 LP600 low K4K05347 14.38 2014 Jun 19 LP600 medium M5K05356 14.8 2014 Jun 19 LP600 mediumK05357 13.86 2014 Jun 19 LP600 medium M3K05372 13.79 2014 Jul 18 LP600 medium M4K05373 11.51 2015 Jun 05 LP600 high M6 yesK05376 13.56 2014 Aug 31 LP600 medium M3K05379 12.22 2014 Jul 18 LP600 high M5K05380 15.31 2014 Aug 31 LP600 low M1K05381 15.4 2014 Aug 26 LP600 high M5K05387 14.07 2014 Jul 16 LP600 high M6K05388 13.4 2014 Jul 14 LP600 medium M4K05390 14.46 2015 Jun 10 LP600 medium M5K05403 14.78 2015 Jun 10 LP600 low M0K05405 13.87 2014 Jul 17 LP600 mediumK05406 11.19 2014 Aug 20 i (cid:48) medium M3 obo -AO Kepler P lanetary C andidate S urvey III 33
TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K05408 13.74 2014 Jul 17 LP600 medium M5K05409 14.82 2015 Jun 03 LP600 low M2K05410 13.66 2015 Jun 03 LP600 medium M3K05411 13.34 2015 Jun 10 LP600 medium M0K05412 15.91 2015 Jun 10 LP600 low M2K05413 13.86 2014 Jul 18 LP600 medium M4K05416 15.91 2014 Sep 01 LP600 low M5K05417 14.93 2015 Jun 10 LP600 low M1K05418 14.92 2014 Aug 21 LP600 medium M4K05433 14.38 2014 Jun 19 LP600 medium M3K05435 15.58 2014 Aug 24 LP600 medium M5K05440 15.15 2014 Aug 28 LP600 high M4 yesK05447 12.55 2014 Aug 21 i (cid:48) highK05451 13.16 2015 Jun 10 LP600 medium M5K05458 15.6 2015 Jun 03 LP600 low M4K05459 11.32 2014 Aug 23 i (cid:48) high M4K05461 13.08 2014 Jul 17 LP600 medium M5K05465 13.67 2014 Jun 19 LP600 high M5 yesK05471 15.67 2015 Jun 03 LP600 low M3K05472 12.35 2014 Jul 14 LP600 high M5K05476 15.35 2014 Aug 26 LP600 medium M4K05480 16.27 2014 Aug 29 LP600 low M1 yesK05478 15.48 2014 Aug 24 LP600 low M1K05482 14.98 2014 Aug 31 LP600 low M1 yesK05485 16.64 2014 Jul 18 LP600 high M5K05486 12.57 2015 Jun 12 LP600 high M3 yesK05487 15.67 2014 Aug 31 LP600 low M0K05490 15.26 2014 Aug 28 LP600 medium M4K05497 10.84 2014 Aug 21 i (cid:48) high M3K05498 12.65 2015 Jun 07 LP600 high M4K05499 15.12 2014 Aug 27 LP600 low M4K05500 13.67 2015 Jun 12 LP600 medium M3K05506 14.0 2014 Jul 17 LP600 high M4K05509 15.21 2014 Aug 24 LP600 medium M4K05511 12.39 2015 Jun 12 LP600 high M5K05514 13.68 2014 Jul 17 LP600 high M4K05517 13.6 2014 Aug 21 LP600 medium M5K05520 14.37 2015 Jun 03 LP600 low M1K05521 13.69 2015 Jun 04 LP600 medium M5K05528 14.95 2014 Jul 17 LP600 low M1K05529 11.7 2015 Jun 07 LP600 high M4K05530 12.79 2014 Aug 20 i (cid:48) low M0K05533 13.35 2014 Jun 15 LP600 mediumK05541 14.7 2015 Jun 07 LP600 medium M4K05545 13.41 2014 Aug 20 i (cid:48) low M2K05546 14.69 2014 Sep 03 LP600 medium M3K05553 15.26 2014 Aug 23 LP600 low M3 yesK05554 11.04 2014 Aug 20 i (cid:48) high M4K05556 13.16 2014 Jun 13 LP600 high M5 yesK05564 10.16 2014 Jun 13 LP600 high M6K05565 11.83 2014 Aug 23 i (cid:48) high M4K05566 12.55 2015 Jun 04 LP600 medium M2K05567 14.86 2015 Jun 07 LP600 medium M4K05568 13.44 2015 Jun 12 LP600 medium M3K05570 14.55 2014 Aug 21 LP600 high M5 yesK05572 13.6 2015 Jun 08 LP600 medium M5K05577 13.29 2014 Jul 16 LP600 medium M4K05578 10.89 2014 Nov 09 LP600 high M5 yesK05579 15.24 2014 Aug 28 LP600 low M4K05583 15.04 2014 Jul 18 LP600 high M5K05585 12.1 2014 Jul 17 LP600 high M5K05587 14.27 2015 Jun 04 LP600 medium M3K05597 13.72 2015 Jun 12 LP600 medium M5K05604 12.79 2014 Jul 16 LP600 medium M3K05605 14.32 2015 Jun 12 LP600 low M3K05608 15.01 2014 Aug 27 LP600 medium M4K05612 15.6 2014 Sep 01 LP600 low M3K05622 15.44 2014 Aug 27 LP600 low M3K05623 14.34 2014 Jul 17 LP600 medium M3K05625 15.71 2014 Aug 31 LP600 low M3K05628 15.34 2014 Aug 28 LP600 medium M5K05632 11.04 2014 Jul 17 LP600 high M4K05633 10.99 2014 Aug 20 i (cid:48) medium M3K05638 14.59 2014 Jun 19 LP600 high M4K05649 14.93 2014 Jul 17 LP600 low M3K05652 14.64 2014 Jul 17 LP600 medium M5K05653 15.17 2014 Aug 21 LP600 low M4 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K05656 12.51 2014 Jul 17 LP600 highK05657 14.21 2014 Aug 21 LP600 medium M4K05660 13.28 2014 Jul 16 LP600 medium M5K05663 13.06 2015 Jun 07 LP600 medium M3K05665 11.31 2014 Jul 17 LP600 high M5 yesK05671 13.39 2014 Jun 16 LP600 medium M4 yesK05680 13.03 2014 Jul 12 LP600 high M5K05684 10.78 2014 Jun 19 LP600 high M6K05688 16.58 2014 Aug 28 LP600 low M3K05692 14.14 2015 Jun 12 LP600 high M7K05694 14.29 2015 Jun 12 LP600 medium M4K05695 14.92 2015 Jun 12 LP600 medium M3 yesK05702 15.26 2014 Aug 24 LP600 medium M3K05704 13.14 2014 Jun 13 LP600 high M5K05706 15.58 2014 Aug 28 LP600 low M1K05707 15.03 2014 Aug 23 LP600 low M0 yesK05712 16.55 2014 Aug 24 LP600 high M6K05718 16.68 2014 Aug 31 LP600 low M2K05727 15.26 2014 Sep 02 LP600 high M6K05736 13.76 2015 Jun 04 LP600 low M2K05737 13.77 2015 Jun 12 LP600 high M5K05740 14.64 2014 Aug 21 LP600 medium M3K05747 13.63 2014 Jul 16 LP600 medium M2K05748 14.49 2015 Jun 04 LP600 low M3K05749 15.4 2015 Jun 04 LP600 low M4K05758 14.84 2014 Sep 03 LP600 medium M5K05762 15.39 2014 Sep 03 LP600 medium M4 yesK05772 13.82 2015 Jun 04 LP600 low M1K05774 10.71 2014 Sep 01 LP600 high M3 yesK05782 11.09 2014 Aug 21 LP600 high M5K05785 14.76 2014 Jul 16 LP600 mediumK05786 14.48 2015 Jun 04 LP600 low M0K05788 14.37 2014 Jul 16 LP600 medium M4K05795 15.72 2014 Sep 03 LP600 lowK05796 14.52 2014 Aug 21 LP600 medium M4K05798 15.39 2014 Aug 23 LP600 low M3K05799 13.61 2015 Jun 04 LP600 medium M4K05800 15.16 2014 Sep 02 LP600 low M1K05801 15.38 2014 Sep 01 LP600 low M2K05802 13.95 2015 Jun 06 LP600 high M5K05805 14.25 2014 Jul 16 LP600 medium M5K05806 12.17 2014 Aug 20 i (cid:48) medium M4K05807 14.27 2014 Jul 16 LP600 mediumK05810 13.5 2014 Jul 16 LP600 high M5K05815 13.43 2014 Jul 16 LP600 medium M5K05816 12.24 2014 Sep 02 LP600 high M6K05819 13.95 2014 Sep 02 LP600 medium M4K05825 13.74 2014 Aug 21 LP600 medium M4K05826 15.34 2014 Aug 23 LP600 high M6K05827 13.33 2015 Jun 04 LP600 medium M4K05829 14.61 2014 Jul 18 LP600 medium M4K05834 15.56 2014 Aug 23 LP600 high M4K05835 14.91 2014 Sep 02 LP600 low M0K05840 13.29 2014 Jun 19 LP600 high M4K05842 14.58 2014 Jul 17 LP600 medium M3K05849 14.24 2014 Jun 19 LP600 medium M4K05852 15.37 2014 Sep 03 LP600 medium M4K05855 14.93 2014 Jul 18 LP600 medium M4K05856 14.55 2014 Jul 18 LP600 low M1K05869 15.35 2014 Aug 23 LP600 low M4K05875 14.5 2015 Jun 04 LP600 low M0K05877 15.34 2014 Sep 02 LP600 high M5K05885 14.66 2014 Aug 21 LP600 medium M4 yesK05888 15.23 2014 Sep 02 LP600 high M5K05889 15.24 2014 Sep 01 LP600 high M4 yesK05899 13.9 2015 Jun 04 LP600 medium M4K05902 14.18 2014 Jul 17 LP600 medium M4K05904 11.47 2014 Aug 20 i (cid:48) medium M5K05909 15.58 2014 Aug 23 LP600 high M6K05911 15.2 2014 Sep 01 LP600 low M0K05913 15.2 2014 Sep 03 LP600 medium M4K05918 13.99 2014 Aug 29 LP600 medium M5K05919 13.42 2014 Aug 29 LP600 medium M3K05920 13.59 2014 Jul 13 LP600 medium M2K05924 15.46 2014 Aug 28 LP600 low M4K05925 12.98 2015 Jun 12 LP600 medium M4K05927 13.12 2014 Aug 29 LP600 high M5 iegler et al . TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K05932 15.89 2015 Jun 12 LP600 low M2K05935 15.34 2014 Aug 31 LP600 mediumK05938 12.67 2014 Aug 22 i (cid:48) medium M3K05948 13.65 2014 Sep 03 LP600 high M5K05949 13.14 2014 Aug 29 LP600 high M4K05950 13.47 2014 Jul 11 LP600 medium M5K05952 14.79 2014 Aug 31 LP600 high M5K05959 14.29 2014 Jul 18 LP600 medium M4K05960 13.1 2014 Jul 11 LP600 high M5K05965 15.59 2014 Sep 03 LP600 medium M5K05968 11.37 2014 Aug 21 i (cid:48) high M5K05971 13.4 2014 Jul 11 LP600 medium M5K06047 11.96 2015 Jun 06 LP600 high M3K06093 13.33 2015 Jun 04 LP600 medium M4K06101 12.55 2015 Jun 07 LP600 high M5K06102 10.82 2014 Aug 22 i (cid:48) high M4K06103 13.44 2015 Jun 03 LP600 low M1K06108 11.9 2014 Aug 22 i (cid:48) medium M4K06109 11.86 2015 Jun 07 LP600 high M4 yesK06111 12.91 2015 Jun 04 LP600 medium M2 yesK06112 12.79 2015 Jun 03 LP600 medium M3K06115 13.5 2015 Jun 08 LP600 mediumK06118 12.77 2015 Jun 07 LP600 high M3K06120 15.42 2015 Jun 08 LP600 high M4 yesK06130 15.12 2015 Jun 03 LP600 low M4K06132 14.62 2015 Jun 12 LP600 high M4 yesK06134 11.94 2015 Jun 03 LP600 medium M2K06137 14.19 2015 Jun 06 LP600 high M4K06141 8.72 2014 Aug 22 i (cid:48) high M2K06145 14.26 2015 Jun 12 LP600 medium M2K06150 12.18 2015 Jun 12 LP600 mediumK06151 14.4 2015 Jun 12 LP600 high M5K06165 11.93 2015 Jun 07 LP600 high M6K06175 10.66 2015 Jun 05 LP600 high M3K06176 11.46 2014 Aug 22 i (cid:48) high M4K06178 15.86 2015 Jun 07 LP600 low M1K06183 13.25 2015 Jun 12 LP600 high M4K06194 12.06 2015 Jun 12 LP600 high M6K06202 11.38 2014 Aug 23 i (cid:48) high yesK06209 16.15 2015 Jun 05 LP600 high M5K06223 15.0 2015 Jun 04 LP600 low M1K06228 14.22 2015 Jun 10 LP600 medium M4K06245 12.43 2015 Jun 06 LP600 medium M2K06253 15.98 2015 Jun 03 LP600 low M3K06254 13.24 2015 Jun 04 LP600 medium M3K06258 11.21 2015 Jun 04 LP600 high M4 yesK06259 14.6 2015 Jun 04 LP600 low M2K06261 14.14 2015 Jun 04 LP600 low K4K06262 15.77 2015 Jun 03 LP600 low M3K06263 12.77 2015 Jun 04 LP600 medium M4K06266 14.52 2015 Jun 04 LP600 low M1K06267 15.37 2015 Jun 03 LP600 low M3K06291 13.3 2015 Jun 04 LP600 medium M4K06293 14.2 2015 Jun 03 LP600 low M0K06295 15.62 2015 Jun 04 LP600 high M6K06299 13.85 2015 Jun 03 LP600 low M3K06311 9.0 2015 Jun 04 LP600 high M2 yesK06318 15.73 2015 Jun 03 LP600 low M4K06320 13.12 2015 Jun 03 LP600 medium M5K06326 13.39 2015 Jun 06 LP600 medium M5K06329 14.02 2015 Jun 04 LP600 medium M3 yesK06338 12.16 2015 Jun 07 LP600 high M5K06341 15.2 2015 Jun 05 LP600 highK06342 12.42 2015 Jun 04 LP600 medium M2K06343 14.54 2015 Jun 04 LP600 high M4K06352 15.22 2015 Jun 03 LP600 high M5K06353 13.47 2015 Jun 03 LP600 medium M4K06355 14.7 2015 Jun 04 LP600 low M2K06357 15.42 2015 Jun 03 LP600 low M1K06361 11.27 2015 Jun 03 LP600 high M4K06368 15.81 2015 Jun 04 LP600 low M0K06372 14.6 2015 Jun 03 LP600 low M2K06375 14.56 2015 Jun 03 LP600 low M1K06378 13.43 2015 Jun 03 LP600 lowK06385 13.77 2015 Jun 03 LP600 low M0K06391 11.3 2015 Jun 04 LP600 highK06392 14.48 2015 Jun 03 LP600 low M1 TABLE 9 – Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K06398 10.59 2015 Jun 05 LP600 high M6K06399 14.72 2015 Jun 04 LP600 low M2K06401 13.75 2015 Jun 04 LP600 medium M2K06408 11.46 2015 Jun 06 LP600 high M2K06409 13.37 2015 Jun 08 LP600 medium M4K06410 13.92 2015 Jun 07 LP600 medium M3K06414 13.86 2015 Jun 03 LP600 low M0K06415 14.03 2015 Jun 03 LP600 high M5 yesK06420 14.23 2015 Jun 03 LP600 low M3K06425 14.16 2015 Jun 08 LP600 medium M4K06438 12.22 2015 Jun 03 LP600 medium M3K06447 12.96 2015 Jun 04 LP600 medium M2K06449 15.67 2015 Jun 08 LP600 high M5K06450 12.36 2015 Jun 04 LP600 high M4K06454 15.0 2015 Jun 08 LP600 low M0K06455 14.13 2015 Jun 08 LP600 medium M3K06460 11.11 2015 Jun 05 LP600 high M3K06464 13.72 2015 Jun 04 LP600 medium M3 yesK06469 12.87 2015 Jun 04 LP600 medium M4K06475 13.73 2015 Jun 07 LP600 high M8 yesK06482 13.6 2015 Jun 04 LP600 medium M4 yesK06483 12.53 2015 Jun 05 LP600 high M4 yesK06489 13.7 2015 Jun 12 LP600 mediumK06497 13.34 2015 Jun 10 LP600 medium M2K06499 13.39 2015 Jun 08 LP600 mediumK06501 13.57 2015 Jun 05 LP600 medium M4K06503 13.91 2015 Jun 06 LP600 mediumK06505 12.1 2015 Jun 05 LP600 highK06507 11.48 2015 Jun 03 LP600 high M2K06511 15.75 2015 Jun 03 LP600 low M1K06512 15.04 2015 Jun 03 LP600 highK06513 15.63 2015 Jun 04 LP600 low M5K06514 11.86 2015 Jun 07 LP600 high M2K06516 15.93 2015 Jun 07 LP600 low M4K06518 13.53 2015 Jun 08 LP600 medium M2K06519 11.4 2015 Jun 08 LP600 high M2K06521 9.81 2015 Jun 06 LP600 high M4K06522 14.13 2015 Jun 12 LP600 medium M3K06526 13.89 2015 Jun 08 LP600 medium M5K06527 12.33 2015 Jun 07 LP600 high M4 yesK06532 15.57 2015 Jun 04 LP600 low M2K06533 12.63 2015 Jun 04 LP600 high M3K06534 12.05 2015 Jun 04 LP600 high M1K06538 14.52 2015 Jun 10 LP600 medium M3K06539 12.51 2015 Jun 12 LP600 medium M1 yesK06542 11.27 2015 Jun 05 LP600 highK06546 15.42 2015 Jun 04 LP600 low M1K06557 13.8 2015 Jun 07 LP600 high M4K06559 14.77 2015 Jun 06 LP600 low M4K06560 12.94 2015 Jun 06 LP600 high yesK06563 11.78 2015 Jun 03 LP600 medium M5K06567 13.09 2015 Jun 04 LP600 medium M4K06568 15.52 2015 Jun 04 LP600 low M5K06570 10.9 2015 Jun 04 LP600 high M3K06574 14.68 2015 Jun 06 LP600 low M3K06578 11.38 2015 Jun 07 LP600 high M5K06579 15.67 2015 Jun 12 LP600 low M2K06582 15.22 2015 Jun 08 LP600 low M0K06598 11.97 2015 Jun 05 LP600 mediumK06601 14.6 2015 Jun 03 LP600 low M1K06602 10.2 2015 Jun 03 LP600 high M5 yesK06604 12.96 2015 Jun 10 LP600 high M6K06605 11.32 2015 Jun 08 LP600 high M3 yesK06610 15.34 2015 Jun 12 LP600 low yesK06611 13.33 2015 Jun 05 LP600 medium M3K06617 15.03 2015 Jun 10 LP600 low M2K06618 15.17 2015 Jun 10 LP600 low M0K06630 12.95 2015 Jun 12 LP600 medium M2K06631 13.27 2015 Jun 04 LP600 medium M4K06635 14.35 2015 Jun 07 LP600 high M8K06646 15.13 2015 Jun 03 LP600 low M4K06648 11.87 2015 Jun 08 LP600 high M3K06649 13.57 2015 Jun 12 LP600 medium M0K06653 14.93 2015 Jun 12 LP600 low M3K06654 13.48 2015 Jun 12 LP600 high M4 yesK06657 13.7 2015 Jun 12 LP600 medium M1K06668 13.18 2015 Jun 08 LP600 high M5 obo -AO
Kepler P lanetary C andidate S urvey III 35
TABLE 9 –
Continued
KOI m i ObsID Filter Obs. Qual. Latest Det. Comp.(mags) Comp. SpT Det.?K06670 12.67 2015 Jun 05 LP600 medium M2K06672 15.18 2015 Jun 04 LP600 low M3K06680 13.69 2015 Jun 03 LP600 medium M4K06687 15.79 2015 Jun 07 LP600 low M4K06689 15.03 2015 Jun 03 LP600 low M2K06705 15.67 2015 Jun 03 LP600 highK06706 13.85 2015 Jun 04 LP600 low M0 yesK06707 15.86 2015 Jun 10 LP600 low M3K06728 13.91 2015 Jun 12 LP600 high M5 yesK06731 15.26 2015 Jun 06 LP600 low M1K06733 13.9 2015 Jun 03 LP600 low M0K06734 15.48 2015 Jun 04 LP600 low M3K06744 10.21 2015 Jun 08 LP600 high M2K06745 15.23 2015 Jun 12 LP600 high M4 yesK06746 14.12 2015 Jun 12 LP600 mediumK06747 14.67 2015 Jun 08 LP600 high M4K06750 14.43 2015 Jun 03 LP600 low M1K06751 15.18 2015 Jun 03 LP600 lowK06752 15.54 2015 Jun 04 LP600 low M4K06753 9.28 2015 Jun 04 LP600 high M2K06762 14.45 2015 Jun 07 LP600 medium M4K06763 12.16 2015 Jun 04 LP600 medium M4K06774 15.57 2015 Jun 04 LP600 low M1K06781 14.95 2015 Jun 10 LP600 medium M5K06788 15.6 2015 Jun 03 LP600 low M2K06791 14.36 2015 Jun 07 LP600 high M5K06800 12.85 2015 Jun 12 LP600 medium M3 yesK06819 11.43 2015 Jun 04 LP600 high M4K06839 16.67 2015 Jun 04 LP600 low M8K06860 13.29 2015 Jun 03 LP600 medium M6K06862 14.8 2015 Jun 04 LP600 low M3K06863 15.74 2015 Jun 07 LP600 low M8K06877 10.97 2015 Jun 08 LP600 high M6K06883 14.93 2015 Jun 03 LP600 low M2K06888 12.85 2015 Jun 03 LP600 medium M3K06889 11.65 2015 Jun 04 LP600 high M4K06890 15.38 2015 Jun 04 LP600 low M3K06892 14.99 2015 Jun 12 LP600 low M1K06897 15.38 2015 Jun 03 LP600 low M4K06898 13.64 2015 Jun 03 LP600 low M3K06913 13.75 2015 Jun 08 LP600 medium K1K06919 15.86 2015 Jun 10 LP600 low M4K06921 15.1 2015 Jun 12 LP600 low M0K06925 15.66 2015 Jun 03 LP600 low M5 yesK06927 14.79 2015 Jun 03 LP600 lowK06934 14.16 2015 Jun 05 LP600 medium M5K06936 15.18 2015 Jun 04 LP600 low M4K06949 12.05 2015 Jun 03 LP600 high M3K06952 13.62 2015 Jun 04 LP600 medium M4K06954 13.11 2015 Jun 06 LP600 medium M4 K06960 13.87 2015 Jun 12 LP600 medium M3K06962 15.43 2015 Jun 12 LP600 high M5K06978 13.36 2015 Jun 03 LP600 medium M4K06980 15.19 2015 Jun 12 LP600 low M0K06993 15.57 2015 Jun 08 LP600 low M3K06994 12.83 2015 Jun 12 LP600 medium M4K07007 15.7 2015 Jun 04 LP600 low M4K07014 11.54 2015 Jun 08 LP600 high M4K07020 13.48 2015 Jun 12 LP600 high M4 yesK07033 11.51 2015 Jun 05 LP600 high M4K07044 11.52 2015 Jun 07 LP600 high M6K07051 15.86 2015 Jun 12 LP600 high M6K07054 10.29 2015 Jun 12 LP600 high M5K07069 15.57 2015 Jun 08 LP600 low M1K07084 11.96 2015 Jun 04 LP600 highK07092 15.45 2015 Jun 07 LP600 low M0K07093 13.65 2015 Jun 08 LP600 medium M2K07109 13.68 2015 Jun 04 LP600 low M2K07133 14.91 2015 Jun 08 LP600 low M2K07144 15.7 2015 Jun 04 LP600 low M3K07182 16.54 2015 Jun 04 LP600 low M4K07205 14.11 2015 Jun 04 LP600 high M5 yesK07208 15.56 2015 Jun 08 LP600 low M3K07209 13.82 2015 Jun 12 LP600 medium M3K07219 11.25 2015 Jun 12 LP600 high M4K07224 15.67 2015 Jun 04 LP600 low M1K07232 15.61 2015 Jun 04 LP600 low M3TABLE 9 –
Continued
KOI m ii